# GCN_circulars

GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11503
SUBJECT: GRB 101225: Optical follow-up of the Christmas burst
DATE:    10/12/28 13:07:20 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

C. C. Thoene, J. Gorosabel, S. Guziy, P. Kubnek, A. J. Castro-Tirado
(IAA-CSIC), A. de Ugarte Postigo (DARK-NBI) and D. Xu (Weizmann Institute)
report:

"We observed the afterglow of the "Christmas burst" GRB 101225A (GCN
11493, Racusin et al.) on Dec. 26, starting 18:49 UT (1.008 days after the
burst onset) with the 1.23m telescope at the Spanish-German Calar Alto
Observatory in Southern Spain. Observations were obtained in V, R and I
with total exposure times of 21x180s, 19x180s and 17x180s respectively.

From the stacked images we obtain the following preliminary magnitudes for
the optical afterglow (GCN 11495, Xu et al.) based on calibrations with
Landolt standard stars taken immediately after the observations:

V = 23.1
R = 22.2
I = 21.3
with errors of about 0.2 mag.

This would imply that the afterglow has rebrightened after the first day
(GCNs 11495 and 11496, Xu et al.) and, considering the possible low
redshift of the GRB from the bright X-ray afterglow (GCN 11501, Campana et
al.), this could be due to the onset of the accompanying SN, similar to
the case of GRB 060218 (Campana et al. 2006). It is more significant if we
consider the fast decay that is observed in X-rays (GCN 11498 Page et
al.).

We note that the magnitude reported by Wiersema et al. (GCN 11502) shows a
shallow decay at a similar epoch, implying that there could be a problem
of cross calibration of the different photometries or a non smooth
behavior. In any case the evolution of the optical light curve would be
rather flat, compared to other GRB light curves.

Further follow up observations are planned."


GRB_name: GRB101225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11504
SUBJECT: GRB 101225A Late-time emission observed by Swift-BAT
DATE:    10/12/29 01:38:52 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC) and T. Sakamoto (GSFC/UMBC)
on behalf of the Swift-BAT team:

We report further results of BAT observations of GRB 101225A (Racusin, et al.,
GCN Circ. 11493).

The most intense emission observed by BAT from GRB 101225A in the 14-50 keV range
occurred from T+1372 to T+1672 seconds, later than previously reported (Palmer,
et al. GCN circ #11500).  The source was not in the BAT field of view from T-4500
to T-100 sec, from T+1088 to T+1372 sec, and from T+1758 to T+4936 sec.  There was
no detectable emission prior to T-4500 sec, and the burst appears to have started
sometime before the source entered the BAT field of view at T-100 sec.

The spectrum from T+1372 to T+1672 seconds is similar to the earlier report, with
a single power law photon index of 1.87 +- 0.21.  The total fluence was greater,
possibly much greater, than 3 x 10^-6 ergs/cm^2 or about 1.6 times the fluence
reported earlier.

BAT detection of extremely long emission is similar to that of GRB 060218 and
GRB 100316D (both spectroscopically confirmed SN-GRBs).


GRB_name: GRB101225A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11505
SUBJECT: GRB 101225A: MAXI/GSC observations
DATE:    10/12/29 05:38:26 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

M. Serino, T. Mihara, Y.E. Nakagawa, M. Sugizaki, 
T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN), 
N. Kawai, M. Morii, K. Sugimori, R. Usui (Tokyo Tech),
K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
A. Yoshida, K. Yamaoka,  S. Nakahira (AGU),
H. Tsunemi, M. Kimura (Osaka U.), H. Negoro, M. Nakajima
H. Ozawa, F. Suwa (Nihon U.), Y. Ueda, N. Isobe, 
S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.), 
K. Yamazaki, A. Uzawa, T. Matsumura (Chuo U.),
report on behalf of the MAXI team:

MAXI/GSC observed the field of the Swift trigger 441015 = GRB 101225A
(Racusin et al, GCN 11493) before and after the trigger time.
The transit times (UT) and the observed fluxes in 2-10 keV energy band are

 15:51  (T-9988s)     -19 +- 11 mCrab
 17:23  (T-4483s)      20 +- 13 mCrab
 18:54  (T+1002s)      20 +- 15 mCrab
 20:05  (T+5218s)      11 +-  9 mCrab
 23:08  (T+16209s)      2 +-  7 mCrab

All the quoted uncertainties are 1-sigma statistical errors.

Note that the third transit occurred within the 1088-second Swift image trigger interval.  While it is not statistically significant, there appears be a weak X-ray enhancement at the location of the Swift trigger position during or near the BAT detection times (Cummings and Sakamoto, GCN 11504).


GRB_name: GRB101225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11506
SUBJECT: GRB 101225A: P60 Observations
DATE:    10/12/29 18:32:50 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration:

We have imaged the field of GRB101225A (Racusin et al., GCN 11493) with
the automated Palomar 60 inch telescope.  Images were obtained in the
Sloan r' and i' filters on 2010 December 28 beginning at 01:49 UT (~ 55.2
hours after the BAT trigger time).

We detect a faint source at the location of the optical afterglow (Xu et
al., GCN 11495) in both filters.  Using a set of nearby sources from the
USNO-B1 catalog for reference, we measure the following magnitudes for the
source at this time: R = 22.8 +/- 0.2; I = 22.3 +/- 0.2.

Our R-band measurement is consistent with that found by Wiersema et al
(GCN 11502) at t ~ 28 hours, but fainter (in both R and I) than the values
reported by Thoene at al (GCN 11503) at a similar time.  In either case,
we find no evidence for a re-brightening as of yet, as would be expected
for the emergence of supernova emission from a nearby event like
GRB060218/SN2006aj.


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11507
SUBJECT: GRB 101225A: MMT spectroscopy
DATE:    10/12/29 23:09:32 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock, G. H. Marion, G. Narayan, E. Berger, and A. M. Soderberg 
(Harvard/CfA) report:

We obtained spectroscopy of the optical source (Xu et al., GCN 11495; Xu 
et al., GCN 11496; Siegel et al., GCN 11499; Wiersema et al., 11502; 
Thoene et al., 11503; Cenko et al., 11506) associated with GRB 101225A 
(Racusin et al., GCN 11493) using the Blue Channel Spectrograph on the 
6.5-m MMT.  Two 2400 s observations starting on December 29.1 UT covered 
the spectral range 3175-8385 Angstroms.  The source has a smooth blue 
continuum and no clear emission or absorption features associated with a 
host galaxy are detected in our spectra, similar to the findings of 
Wiersema et al. (GCN 11502).  In addition, the continuum has no obvious 
broad undulations or evidence for line blanketing shortward of 4000 
Angstroms, such as would be expected if the spectral features of a 
supernova were emerging.  The spectrum is well fit by a power law of the 
form F_nu ~ constant * nu^(0.4), which is bluer than typical afterglow 
spectra, which typically scale as F_nu ~ nu^(-0.6).


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11508
SUBJECT: GRB 101225A: optical break from NOT observation
DATE:    10/12/31 01:43:13 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

D. Xu (Weizmann Inst.), P. Hakala (Turku U.), J.P.U. Fynbo (DARK/NBI)
report on behalf of a larger collaboration:

We imaged the filed of GRB(or XRF) 101225A (Racusin et al., GCN 11493)
at the Nordic Optical Telescope (NOT) equipped with either StanCam or
ALFOSC in B, V, R, and I filters. The R-band optical afterglow  (Xu et
al., GCN 11495) light curve was found decaying very slowly from
m(R)=22.6 +/- 0.2 at 5.47167 hrs after the BAT trigger to m(R)=22.8
+/- 0.2 at 55.2 hrs after the BAT trigger (Xu et al., GCN 11496;
Wiersema et al., GCN 11502; Thoene et al., GCN 11503; Cenko, GCN
11506).

Two 450 s R-band images were obtained with NOT/ALFOSC, starting at
21:50:46.9 UT, 30/12/2010 (i.e., 123.217 hrs after the BAT trigger)
under the conditions of seeing ~1". The afterglow was clearly detected
in the stacked image, largely pointlike, and had m(R)=23.3+/-0.2. This
indicates that R-band afterglow is now decaying faster compared with
its behavior during the past days, and that the host hasn't dominated
the brightness, being consistent with the featureless spectroscopy
(Wiersema et al., GCN 11502; Chornock et al., 11507).


GRB_name: GRB110102A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11509
SUBJECT: GRB 110102A: Swift detection of a burst with an optical detection
DATE:    11/01/02 19:06:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Gronwall (PSU),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/IASFPA),
M. H. Siegel (PSU) and G. Stratta (ASDC) report on behalf of the Swift
Team:

At 18:52:25 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110102A (trigger=441454).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 245.879, +7.619 which is 
   RA(J2000)  =  16h 23m 31s
   Dec(J2000) = +07d 37' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a weak precursor at T_zero
and then a bright FRED-like pulse at T+130 sec with a total duration
of about 170 sec.  The peak count rate was ~6000 counts/sec (15-350 keV),
at ~130 sec after the trigger. 

The XRT began observing the field at 18:54:54.0 UT, 148.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 245.8821, +7.6160 which is equivalent to:
   RA(J2000)  = 16h 23m 31.70s
   Dec(J2000) = +07d 36' 57.5"
with an uncertainty of 6.3 arcseconds (radius, 90% containment). This
location is 15 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 149 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 16:23:31.43 = 245.88096
  DEC(J2000) = +07:36:50.0  = 7.61390
with a 90%-confidence error radius of about 0.62 arc sec. This position is 8.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.93 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.08. 

Burst Advocate for this burst is S. R. Oates (sro AT mssl.ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110102A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11510
SUBJECT: GRB 110102A: Enhanced Swift-XRT position
DATE:    11/01/02 23:49:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3361 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 110102A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 245.88117, +7.61377 which is equivalent
to:

RA (J2000): 16h 23m 31.48s
Dec (J2000): +07d 36' 49.6"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11511
SUBJECT: GRB 110102A: Swift-BAT refined analysis
DATE:    11/01/03 03:07:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), S. R. Oates (UCL-MSSL), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110102A (trigger #441454)
(Oates, et al., GCN Circ. 11509).  The BAT ground-calculated position is
RA, Dec = 245.877, 7.617 deg, which is
   RA(J2000)  =  16h 23m 30.5s 
   Dec(J2000) = +07d 37' 00.1" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 66%.
 
The mask-weighted light curve shows a pair of small precursor peaks starting
at ~T-50 sec and ending at ~T+50 sec.  The main emission occurs with four peaks
that start at ~T+100 sec and ending at ~T+340 with the maximum at ~T+210 sec.
T90 (15-350 keV) is 264 +- 8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-49.2 to T+294.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.60 +- 0.04.  The fluence in the 15-150 keV band is 1.65 +- 0.03 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+208.76 sec in the 15-150 keV band
is 8.4 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/441454/BA/


GRB_name: GRB110102A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11512
SUBJECT: GRB 110102A: Fermi GBM observation
DATE:    11/01/03 05:45:05 GMT
FROM:    Lin Lin at UAH/NAOC  <ll0005@uah.edu>

Lin Lin (UAH) 
report on behalf of the Fermi GBM Team: 

"At 18:54:36.00 UT on 2 Jan. 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110102A (trigger 315687278 / 110102788).
which was also detected by the Swift/BAT
(S. R. Oates et al. 2011, GCN 11509)
The GBM on-ground location is consistent with the Swift position.


The GBM light curve shows of several peaks 
with a duration (T90) of about 254 s (50-300 keV). 
The T90 starts at T0-119 s.
The time-averaged spectrum from T0-123 s to T0+149 s is 
well fit by

a power law function with an exponential
high-energy cutoff.  The power law index is -1.49 +/- 0.02 and
the cutoff energy, parameterized as Epeak, is 476.6 +/- 68.7 keV

The event fluence (10-1000 keV) in this time interval is 
(4.39 +/- 0.09)E-5 erg/cm^2. The 1 sec peak photon flux measured 
starting from T0+78 s in the 10-1000 keV band 
is 14.07 +/- 0.35 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110102A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11513
SUBJECT: GRB110102A: MITSuME Okayama Optical Observation
DATE:    11/01/03 10:09:15 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110102A (Oates et al., GCN 11509)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2011-01-02 20:08:45 UT (~1.3 hours after
the burst).  We detected the afterglow candidate within the
enhanced XRT error circle (Goad et al., GCNC 11510) in all the three
bands.

Photometric results are listed below. We used SDSS catalog for flux
calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.06851    20:31:04  2340.0      20.0  0.4    19.6  0.3    18.3  0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110102A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11514
SUBJECT: GRB110102A: Swift/UVOT observations
DATE:    11/01/03 12:41:16 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and M. De Pasquale (MSSL-UCL) report on behalf  
of the Swift-UVOT team

The Swift/UVOT began settled observations of the field of GRB 110102A
156 s after the BAT trigger (Oates et al., GCN Circ. 11509). The optical
afterglow is detected in the white, v, b and u filters at a refined UVO
position RA(J2000)= 245.88087 deg, DEC(J2000) = 7.61383, which is:

  RA (J2000) =   16:23:31.41
  Dec (J2000) = +07:36:49.8

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence).
This position is consistent with the enhanced XRT position (Goad et  
al., GCN Circ. 11510).
The detection in u suggests a redshift of <2.5.

Preliminary magnitudes using the UVOT photometric system (Poole et al.  
2008,
MNRAS, 383, 627) for single and summed exposures are:

Filter  T_start(s)  T_stop(s)   Exp(s)       Mag/3sigUL
#####################################################
wh (FC) 156          306        147       17.97 +/- 0.06
wh          868          1018      147       18.39 +/- 0.08
u  (FC)   314          564        246       17.98 +/- 0.09
u             1122       1315      39          18.89 +/- 0.62
v             816          835        19          17.86 +/- 0.53
b             597          589        19          17.60 +/- 0.20
uvw1      693         6331      452        > 20.09
uvm2      668         6126      292        > 19.87
uvw2      619         7152      471        > 20.35
#####################################################

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110102A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11515
SUBJECT: Konus-Wind observation of GRB 110102A
DATE:    11/01/03 15:46:18 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long GRB 110102A, (Swift/BAT trigger=441454:
Oates, et al., GCN 11509; Sakamoto et.al, GCN 11511)
triggered Konus-Wind at T0=68074.462s UT (18:54:34.462)

The burst light curve consists of three major pulses,
first two of them are much harder than the third one.
The total duration of the burst is ~160 s.
The emission is seen up to ~5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB110102_T68074/

As observed by Konus-Wind the burst
had a fluence of (5.4  0.9)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+76.032s,
of (4.9  0.8)x10-6 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+164.096 s) is best fit
in the 20 keV - 5 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -1.22 (-0.16, +0.26),
the high energy photon index beta = -2.3 (< -0.9),
the peak energy Ep = 267(-91, +111) keV,
chi2 = 65/76 dof.

The spectrum at the maximum count rate
(measured from T0+73.984 to T0+82.176 s) is best fit
in the 20 keV - 5 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -1.14 (-0.12, +0.15),
the high energy photon index beta = -2.2 (-3.1, +0.3),
the peak energy Ep = 436(-122, +180) keV,
chi2 = 57/76 dof.

All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB101219B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11516
SUBJECT: GRB 101219B: After 2 weeks still detected by Swift/UVOT
DATE:    11/01/03 23:31:29 GMT
FROM:    Jonathan Gelbord at PSU/Swift  <jgelbord@astro.psu.edu>

N.P.M. Kuin (MSSL/UCL) and J.M. Gelbord (PSU) report on behalf of
the Swift/UVOT team:

As reported earlier (Gelbord et al., GCN Circ. 11473; Kuin et al.,
GCN Circ. 11482), Swift/UVOT observations of GRB 101219B detected an
optical afterglow in all its bands with initial magnitudes of about
18 mag. The optical afterglow has been unusually slow to decay, and
is around 23 mag at present in the u and uv bands. The UVOT has
obtained a good light curve in all bands up to about 300ks, with
continuing detections through 1000ks in u, uvw1, uvm2, and uvw2 (v
and b measurements after 300ks are significantly affected by the PSF
wings of a B = 15.5 mag star located 7 arcsec to the SW). The light
curve still appears to be decaying and there is some indication that
this decay may not be smooth.

GRB 101219B is further interesting because the UVOT light curve
exhibits an early decay to about 600 seconds after the trigger time
T, after which a second brightness rise to a maximum around T+850s
occurs. A corresponding break is found in the X-ray light curve, in
that the decay observed by XRT flattens approximately at T+700s.

The only constraint on the redshift of this burst is an upper limit
around 1.5 implied by the detection in uvw2, as there have not been
any spectroscopic observations announced to date. However, if this
burst is bright because it is close, then we might detect a supernova
bump in the coming days.

We consider this an interesting burst and would like to bring this
to the attention of the community as an opportunity for further
observations.


GRB_name: GRB110102A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11517
SUBJECT: GRB 110102A: Swift-XRT refined Analysis
DATE:    11/01/04 03:05:00 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia, G. Stratta (ASDC) and S. R. Oates (MSSL-UCL) report on behalf
of the Swift-XRT team:

We have analysed 18.8 ks of XRT data for GRB 110102A (Oates et
al., GCN Circ. 11509), from 139 s to 47.5 ks after the  BAT trigger.
The data comprise 400 s in Windowed Timing (WT) mode with the
remainder in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Goad et al. (GCN. Circ 11510).

The light curve shows an intital flaring activity, possibly associated
to the prompt event, followed by a canonical steep-flat-steep
behaviour, which can be modelled with double broken power-law
decay. The initial decay index is alpha= 8.6. At T+450 (+/- 0.05) s the
decay flattens to an alpha of 0.49 (+/-0.03). At T+11.38 (+/- 0.01) ks  
the decay steepens again to an alpha of 1.53 (+0.07 -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.48 (+/-0.04). The
best-fitting absorption column is  7.8 (+/- 1) x 10^20 cm^-2, in
excess of the Galactic value of 4.8 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.27 (+/-0.07) and a
best-fitting absorption column of 1.28 (+/- 0.17) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (5.8 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of 1.6,
the count rate at T+48 hours will be 0.012 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of
4.3 x 10^-13 (7.0 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00441454.

This circular is an official product of the Swift-XRT team.

[GCN OPS NOTE(04jan11):  Per author's request, the "4.3 x 10^-12 (2.1 x 10^-13)"
in the 4th paragraph was changed to "4.3 x 10^-13 (7.0 x 10^-13)".]


GRB_name: GRB101219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11518
SUBJECT: GRB 101219A: Gemini-North host redshift
DATE:    11/01/04 16:34:27 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock and E. Berger (Harvard) report on behalf of a larger 
collaboration:

We obtained 4x1800s of spectroscopy of the host galaxy candidate (Perley 
et al., GCN 11464; Cenko et al., GCN 11468; Chornock et al., GCN 11469) 
found in the XRT error circle of the short-hard GRB 101219A (Gelbord et 
al., GCN 11461) using GMOS on Gemini-North starting on January 2.25 UT. 
  Observations were obtained with the R400 grating, covering 5890-10100 
Angstroms in nod-and-shuffle mode.  The galaxy spectrum exhibits 
emission lines due to [O II] 3727 Angs and [O III] 5007 Angs at a 
redshift of 0.718.


GRB_name: GRB101225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11519
SUBJECT: GRB 101225A: Host galaxy
DATE:    11/01/05 13:44:53 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

D. Xu (Weizmann Inst.), D. Malesani, J.P.U. Fynbo, J. Hjorth
(DARK/NBI), P. Jakobsson (U. Iceland), T. Augusteijn (NOT), report on
behalf of a larger collaboration:

We imaged the field of GRB 101225A (Racusin et al., GCN 11493) at the
Nordic Optical Telescope (NOT) equipped with ALFOSC. We obtained 6x600
s R-band images with a good seeing ~0.7" and little cloud cover.
Observations started at 20:55:25 UT on 2011 Jan 4 (i.e., 10.1 days
after the BAT trigger).

The optical counterpart of the burst (Xu et al., GCN 11495) has faded
further and it is detected in the stacked image with R = 24.1+/-0.1,
calibrated against the USNO-B1 star #1345-0000324. The object is now
significantly extended along the northwest-southeast direction,
indicating a significant contribution from the underlying host galaxy.

Further observations are encouraged, especially in the NIR.


GRB_name: GRB110106A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11520
SUBJECT: GRB 110106A: Swift detection of a burst
DATE:    11/01/06 15:37:15 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. Mangano (INAF-IASFPA), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Gronwall (PSU),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/IASFPA),
M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC),
R. L. C. Starling (U Leicester), M. C. Stroh (PSU),
E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:

At 15:25:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110106A (trigger=441664).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 79.285, +64.184 which is 
   RA(J2000) = 05h 17m 08s
   Dec(J2000) = +64d 11' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a total duration of about 4 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 15:27:02.4 UT, 106.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 79.30730, 64.17394 which is equivalent
to:
   RA(J2000)  = 05h 17m 13.75s
   Dec(J2000) = +64d 10' 26.2"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 49 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.27 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4.3
(+4.88/-3.82) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of  52 seconds with the White filter
starting 109 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.24. 

Burst Advocate for this burst is V. Mangano (vanessa AT ifc.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11521
SUBJECT: GRB110106A: Xinglong TNT upper limit
DATE:    11/01/06 17:05:02 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, Z. X. Ling, Y.L. Qiu, J.Y. Wei, J. Wang, J.S. Deng, 
C. Wu, X. H. Han on behalf of EAFON report:

We began to observe GRB110106A (Mangano et al., GCN 11520 ) 
with Xinglong TNT telescope at 15:35:15.946 (UT), 10min after 
the burst. A series of white and R-band images were obtained. 
No any new source was found within the errorbox  of X-ray 
counterpart (Mangano et al., GCN 11520 ), down to 3 sigma 
upper limit of R~19.8 mag at the mean time of 11 min after 
the burst. 

This message may be cited.

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org/grb/


GRB_name: GRB101225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11522
SUBJECT: GRB 101225A: Keck redshift
DATE:    11/01/06 20:13:40 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

D. Xu, A. Gal-Yam (WIS), J. P. U. Fynbo (DARK/NBI), report on behalf
of a large collaboration:

Spectroscopy of the host galaxy of GRB 101225A (Racusin et al., GCN
11493; Xu et al. GCN 11519) was carried out at the 10m Keck-I
telescope equipped with the Low Resolution Imaging Spectrometer (LRIS)
around 10 UT, 6th Jan. 2011, with a good seeing ~0.7". A 900s spectrum
was obtained and it consists of a red and a blue channels, covering
~3200-5500 A and ~5000-8200 A, respectively. The spectrum has a low
signal-to-noise ration and the trace is best detected in the red
channel. Three weak emission lines are found at a common redshift of
z=0.40, considered as Hbeta (4861 AA), and the O III (4960 AA, 5007
AA).

Isotropic energy: >~ 7.8+/-1.6 x10^50 erg, using the BAT fluence
(Palmer et al., GCN 11500)

The absence of evidence for an emerging SN at the above redshift
suggests that GRB 101225A is a SN-less or SN-weak long GRB event.

Further deep spectroscopic observations are encouraged.


GRB_name: GRB110106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11523
SUBJECT: GRB 110106A: MASTER optical observations
DATE:    11/01/06 21:14:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB110106A (Mangano et al., GCN 
Circ 1152) 17 sec s after notice time and 41 sec after GRB time at 
2011-01-06 15:25:57.96 UT in two polarizations+filter R. On our 
first (10s exposure) set we haven't found optical transient  within SWIFT 
XRT error-box.
The 5-sigma upper limit has been about 16.0mag
We marginally see OT about 15.5 mag in XRT error box on second set at 
2011-01-06 15:26:19 (starting 69 s after trigger time with 10 sec 
exposition).

We see the like galaxy object near  (~15" distance) XRT error box ~19-20 
mag on later images. But, there is no object in NASA/IPAC EXTRAGALACTIC 
DATABASE. 
The same object is presented at DSS image.

The redaction is continueted.

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11524
SUBJECT: GRB 110106A: TNG optical observations and candidate counterparts
DATE:    11/01/06 21:38:53 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), S. Covino (INAF/Brera), L.A. Antonelli 
(INAF/Roma), D. Fugazza (INAF/Brera), A. Harutyunyan (INAF/TNG),
G. Tessicini (INAF/TNG) on behalf of the CIBO collaboration, report:

We observed the field of GRB 110106A (Mangano et al., GCN 11520) using 
the 3.6m TNG telescope, located in the Canary Islands. A set of R- and 
I-band images were acquired starting on Jan 6.8265 UT (4.41 hr after the 
GRB) for a total exposure time of 20 minutes per filter. The seeing was 
1.5" in the R band.

Within the XRT error circle (Mangano et al., GCN 11520), we marginally 
detect a source in both R and I. Its coordinates are (J2000):

RA = 05:17:14.14
Dec = 64:10:28.1

and its magnitude is R ~ 24.5. In addition, we note the presence of a 
galaxy just outside the current X-ray error circle (its centroid being 
7.3+-3.6" away of the XRT position). It is visible also in the DSS 
images and has a magnitude R = 18.2 (assuming R = 17.54 for the star at 
RA=05:17:11.43, Dec=+64:10:10.88).

We cannot assess whether any of the sources are variable, and so their 
relation to GRB 110106A remains to be proven.

Further observations are in progress.

[GCN OPS NOTE(06jan11): Per author's request, GT was added to the author list.]


GRB_name: GRB110106B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11525
SUBJECT: GRB 110106B: Swift detection of a burst
DATE:    11/01/06 21:41:40 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. Sbarufatti (INAF-OAB/IASFPA), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Gronwall (PSU),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (INAF-IASFPA),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), C. J. Saxton (UCL-MSSL),
M. Stamatikos (OSU/NASA/GSFC), E. Troja (NASA/GSFC/ORAU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 21:26:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110106B (trigger=441676).  There was a 3.8 minute delayed slew. 
The BAT on-board calculated location is 
RA, Dec 134.196, +46.998 which is 
   RA(J2000)  =  08h 56m 47s
   Dec(J2000) = +46d 59' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a total duration of about 30 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 21:31:44.2 UT, 327.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 134.15458, 47.00194 which is equivalent
to:
   RA(J2000)  = 08h 56m 37.10s
   Dec(J2000) = +47d 00' 07.0"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 102 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.37
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 332 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.03. 

Burst Advocate for this burst is B. Sbarufatti (boris.sbarufatti AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110106A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11526
SUBJECT: GRB 110106A: Enhanced Swift-XRT position
DATE:    11/01/06 21:53:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3088 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 110106A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 79.30578, +64.17349 which is equivalent
to:

RA (J2000): 05h 17m 13.39s
Dec (J2000): +64d 10' 24.6"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110106A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11527
SUBJECT: GRB 110106A: Swift-BAT refined analysis
DATE:    11/01/06 23:36:30 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), V. Mangano (INAF-IASFPA),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110106A (trigger #441664)
(Mangano, et al., GCN Circ. 11520).  The BAT ground-calculated position is
RA, Dec = 79.295, 64.199 deg, which is 
   RA(J2000)  =  05h 17m 10.8s 
   Dec(J2000) = +64d 11' 56.4" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 34%.
 
The mask-weighted light curve shows a pulse starting at ~T-1 sec and
lasting about 6 sec.  T90 (15-350 keV) is 4.3 +- 1.1 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-1.0 to T+3.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.71 +- 0.28.  The fluence in the 15-150 keV band is 3.0 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.32 sec in the 15-150 keV band
is 1.9 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/441664/BA/


GRB_name: GRB110106B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11528
SUBJECT: GRB110106B: Xinglong TNT upper limit
DATE:    11/01/06 23:53:06 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, Z. X. Ling, Y.L. Qiu, J.Y. Wei, J. Wang, J.S. Deng, 
C. Wu, X. H. Han on behalf of EAFON report:

We began to observe GRB110106B ( Sbarufatti et al., GCN 11525 ) 
with Xinglong TNT telescope at  21:35:02.5(UT), 9min after 
the burst. A series of white and R-band images were obtained. 
No any new source was found within the errorbox  of X-ray 
counterpart ( Sbarufatti et al., GCN 11525 ), down to 3 sigma 
upper limit of R~20 mag at the mean time of 14 min after 
the burst. 

This message may be cited.

Thanks to the help of TNT observation assistant for this work. 

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org/grb/


GRB_name: GRB110106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11529
SUBJECT: GRB 110106A: Swift-XRT refined Analysis
DATE:    11/01/07 00:29:39 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF-IASFPA) and B. Sbarufatti (INAF-OAB/INAF-IASFPA)
report on behalf of the Swift-XRT team:

We have analysed 7.0 ks of XRT data for GRB 110106A (Mangano  et al.
GCN Circ. 11520), from 91 s to 17.3 ks after the  BAT trigger. The data
comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN. Circ
11526).

The late-time light curve (from T0+3.5 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.2 (+0.4, -0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.7 (+0.4, -0.5). The
best-fitting absorption column is  4.0 (+1.6, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.3 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (1.0 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.0 (+1.6, -1.4) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^21 cm^-2
Excess significance: 4.8 sigma
Photon index:      2.7 (+0.4, -0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00441664.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11530
SUBJECT: GRB 110106A: TNG redshift of the closeby galaxy
DATE:    11/01/07 00:43:11 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

S. Piranomonte (INAF/Roma), D. Malesani (DARK/NBI), V. D'Elia (ASDC and 
INAF/Roma), S. Covino (INAF/Brera), L.A. Antonelli (INAF/Roma), D. 
Fugazza (INAF/Brera), A. Harutyunyan (INAF/TNG), G. Tessicini 
(INAF/TNG), report on behalf of a larger collaboration:

Following the release of the refined X-ray position (Osborne et al., GCN 
11526) of the afterglow of GRB 110106A (Mangano et al., GCN 11520), we 
further inspected our TNG images. The faint object reported by Malesani 
et al. (GCN 11524) is significantly outside the revised error circle, 
and is thus likely unrelated to the GRB.

The new X-ray position however partially covers the outskirts of the 
extended object mentioned in GCN 11520.

A 1-hr TNG spectrum of this galaxy, starting on Jan 6.878 UT (5.64 hr 
after the GRB) and covering the wavelength range 3800-8000 AA, reveals 
the presence of a few emission features, which we interpret as Halpha, 
[NII] 6583, [SII] 6730, and weak Hbeta at a common redshift z=0.093. At 
the same redshift, we also see Ca H and K in absorption.

While the XRT error circle (1.7" radius) overlaps the stellar light from 
the galaxy, its center lies 4.3" away of the galaxy nucleus (7.3 kpc in 
projection at z=0.093). Such large offset would be more typical of 
short-duration GRBs, although the duration of GRB 110106A (T90 = 
4.3+-1.1 s; Stamatikos et al., GCN 11527) seems to exclude this 
hypothesis. The relation between the galaxy and the GRB cannot be 
conclusively established at this point.


GRB_name: GRB110106A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11531
SUBJECT: GRB 110106A: Swift/UVOT Upper Limits
DATE:    11/01/07 00:53:06 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

S. T. Holland (CRESST/USRA/GSFC) and
V. Mangano (INAF-IASFP)
report on behalf of the Swift/UVOT team:

      The Swift/UVOT observed the field of GRB 110106A starting 92 s
after the BAT trigger (Mangano, et al., 2011, GCN Circ. 11520).
Settled observations started at 110 s.  We do no detect an optical
afterglow in any of the UVOT filters.  Preliminary 3-sigma upper
limits for detecting a source in the finding charts and in the
co-added images, are

Filter      T_start   T_stop    Exp(s)      Mag
-----------------------------------------------
white (fc)      110      162        52    >20.2
               3530     3680       150    >20.3

    v          3687   16,046      1278    >20.3
    b          4508   10,281      1082    >21.1
    u          4302     5939       393    >20.4
 uvw1          4097     5734       393    >20.2
 uvm2          3892     5529       393    >20.1
 uvw2          4918   11,717       706    >20.9
white           110   11,194      1280    >22.0
-----------------------------------------------

     The quoted magnitudes and upper limits have not been corrected
for the expected Galactic extinction along the line of sight
corresponding to a reddening of E_{B-V} = 0.24 mag (Schlegel, et al.,
1998, ApJS, 500, 525).  All photometry is on the UVOT photometry
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB110106B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11532
SUBJECT: GRB 110106B: Enhanced Swift-XRT position
DATE:    11/01/07 01:31:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2412 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 110106B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 134.15423, +47.00272 which is equivalent
to:

RA (J2000): 08h 56m 37.02s
Dec (J2000): +47d 00' 09.8"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110106B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11533
SUBJECT: GRB 110106B: Swift-BAT refined analysis
DATE:    11/01/07 01:56:03 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (GWU) S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. Stamatikos (OSU), J. Tueller (GSFC),
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110106B (trigger #441676)
(Sbarufatti, et al., GCN Circ. 11525).  The BAT ground-calculated position is
RA, Dec = 134.155, 47.005 deg, which is 
   RA(J2000)  =  08h 56m 37.3s 
   Dec(J2000) = +47d 00' 17.5" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.
 
The mask-weighted light curve shows 3 main overlapping peaks starting
at ~T-6 sec and ending at ~T+23 sec.  T90 (15-350 keV) is 24.8 +- 4.8 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-10.8 to T+23.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.76 +- 0.11.  The fluence in the 15-150 keV band is 2.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.87 sec in the 15-150 keV band
is 2.1 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/441676/BA/


GRB_name: GRB110106B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11534
SUBJECT: GRB 110106B: WHT candidate afterglow
DATE:    11/01/07 02:34:14 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), N.R. Tanvir, K. Wiersema (U. Leicester),
L. Coccato (ESO) report for a larger collaboration:

We observed the location of GRB 110106B (Sbarufatti et al. GCN
11525) with the William Herschel Telescope and ACAM. Observations
were obtained in the i-band, and began at 7 Jan, 00:41 UT, approximately
3 hours after the burst. Within the refined XRT localization
(Beardmore et al. GCN 11532) we find a source at

RA(J2000) 08:56:37.02 
DEC(J2000) 47:00:09.8

with an uncertainty of ~0.5" in each axis.

The source appears to be extended, but may include a point source
contribution on top of the extended emission. Photometry of the
object suggests i~22.5. This is marginally brighter than the limit
of SDSS observations of the region, and suggests some afterglow
contribution to the observed flux at this time.

Further observations are encouraged."


GRB_name: GRB110106A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11535
SUBJECT: GRB 110106A: MITSuME Okayama optical upper limits
DATE:    11/01/07 04:51:09 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110106A (Mangano  et al., GCN 11520)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2011-01-06 15:26:22 UT (~65 sec after
the burst). We did not find any new point source within the
enhanced XRT error circle (Osborne et al., GCNC 11526) in all
the three bands.

Three sigma upper limits of the OT are listed below. We used
GSC2.3 catalog for flux calibration.


T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.00424    15:31:23     540.0   >20.0  >19.7  >18.8
0.09936    17:48:21    5040.0   >20.8  >20.4  >19.5
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11536
SUBJECT: GRB 110106A: ISAS-Kanazawa optical upper limit
DATE:    11/01/07 05:48:17 GMT
FROM:    Daisuke Yonetoku at Kanazawa U  <gcn@astro.s.kanazawa-u.ac.jp>

T. Yatsu, Y. Nishikawa, D. Yonetoku, T. Murakami and S. Gima (Kanazawa University)
on behalf of the ISAS-Kanazawa collaboration, report:

We observed the field of GRB 110106A (Mangano et al., GCN 11520) in Rc-band,
using the 1.3m ISAS-Kanazawa telescope, located at Sagamihara.
The observation started on Jan 6.64375 UT at ~2 min after the burst.
No any new source was found within the revised position  of X-ray
counterpart (Osborne et al., GCN 11526), down to the 3 sigma upper limit
of Rc~17.6 mag. 


GRB_name: GRB110106B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11537
SUBJECT: GRB 110106B: Liverpool Telescope observations
DATE:    11/01/07 11:12:06 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB),
I.A. Steele, C.G. Mundell, S. Kobayashi (Liverpool JMU),
A. Gomboc (U. Ljubljana) on behalf of a large collaboration report:

The 2-m Liverpool Telescope automatically began observing
GRB 110106B (Sbarufatti et al. GCN Circ. 11525) on January 06,
21:35:46 UT, 9.5 minutes from the GRB trigger time with the
SDSS filters riz.
Within the enhanced XRT error circle (Beardmore et al. GCN Circ. 11532)
we do not find any source down to the following limiting magnitudes.

Mid time from      Tot Exposure    Filter   Limiting Magnitude
trigger (s)           (s)
------------------------------------------------------------
2594                  720           z > 20.4
2300                  720           i > 21.4
2620                 1260           r > 22.5
------------------------------------------------------------

Calibration is against some nearby SDSS stars.
The non-detection of the extended object mentioned by Levan et
al. (GCN Circ. 11534) with i~22.5 is consistent with our limit.


GRB_name: GRB110106B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11538
SUBJECT: GRB 110106B Gemini-N galaxy redshift
DATE:    11/01/07 11:29:52 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock, E. Berger (Harvard), and D. B. Fox (Penn. State) report on 
behalf of a larger collaboration:

We used GMOS on Gemini-North to observe the extended object present in 
the XRT error circle of GRB 110106B (Sbarufatti et al., GCN 11525; 
Beardmore et al. GCN 11532) discovered by Levan et al. (GCN 11534).  We 
obtained 2x1500s of spectroscopy using the R400 grating to cover the 
spectral range 3900-8100 Angstroms, starting on January 7.38 UT. 
Emission lines from [O II], H-beta, and [O III] are present at a common 
redshift of z=0.618.


GRB_name: GRB110106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11539
SUBJECT: GRB 110106A: TNG NIR observations
DATE:    11/01/07 12:51:41 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), D. Fugazza (INAF/Brera), S. Covino (INAF/Brera), 
L. Angelo Antonelli (INAF/Roma), A. Harutyunyan (INAF/TNG), G. Tessicini 
(INAF/TNG), G. Andreuzzi (INAF/TNG), report on behalf of a larger 
collaboration:

We observed the field of GRB 110106A (Mangano et al., GCN 11520) in the 
K band with the 3.6m TNG equipped with NICS. A total of 60 min 
integrations were obtained with a mean time Jan 7.07 UT (10.33 hr after 
the GRB).

We detect no sources within the refined X-ray position (Osborne et al., 
GCN 11526; see also http://www.swift.ac.uk/xrt_positions), down to a 
3-sigma limiting magnitude K > 20.3. We clearly detect the z=0.093 
galaxy just outside the error circle (Malesani et al., GCN 11524; 
Piranomonte et al., GCN 11530), with a magnitude K=14.90 +- 0.06 
(calibration against 2MASS stars in the field).


GRB_name: GRB110106B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11540
SUBJECT: GRB 110106B: Gemini-North / WHT detection of a fading afterglow
DATE:    11/01/07 15:01:07 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger (Harvard), A.J. Levan (U. Warwick), R. Chornock (Harvard), and
N.R. Tanvir (U. Leicester) report:

"In addition to the spectroscopic observations reported in GCN #11538 we
also obtained i-band imaging of the afterglow candidate of GRB 110106B found
with the WHT (GCN #11534) with Gemini-N / GMOS.  A total of 900 sec were
obtained on source at a mean epoch of 2011 Jan 7.347 UT (10.89 hours after
the burst and 7.64 hours after the WHT observation).  Digital image
subtraction of the Gemini and WHT observations reveals a fading source
located at (J2000):

RA = 08:56:37.267
DEC = +47:00:10.49

with an uncertainty of about 0.2" in each coordinate.  This position is
about 1.5" due east of the galaxy noted in GCN #11534, whose redshift is
0.618 (GCN #11538).  At this redshift the corresponding projected offset is
about 10 kpc.  We note that emission is still detected at the position of
the afterglow, indicating that an association with an underlying host
unrelated to the nearby galaxy may still be possible."


GRB_name: GRB110106B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11541
SUBJECT: GRB 110106B: Swift-XRT refined Analysis
DATE:    11/01/07 15:12:25 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/IASFPA) reports on behalf of the Swift-XRT
team:

We have analysed 6.2 ks of XRT data for GRB 110106B (Sbarufatti  et al.
GCN Circ. 11525), from 339 s to 30.3 ks after the  BAT trigger. The
data comprise 24 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN. Circ 11532).

The light curve can be modelled with a series of power-law decays. The
light curve initially rises, with an index alpha=-1.5 (+0.0, -1.3). At
T+470 s it breaks to an alpha of 0.64 (+/-0.07) before breaking again
at T+14354 s to a final decay with index alpha=1.6 (+1.0, -0.5).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.20 (+/-0.16). The
best-fitting absorption column is  2.08 (+0.44, -0.22) x 10^21 cm^-2,
in excess of the Galactic value of 2.4 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.8 x 10^-11 (6.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.08 (+0.44, -0.22) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 15.4 sigma
Photon index:      2.20 (+/-0.16)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00441676.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11542
SUBJECT: Short GRB 110106A: MASTER OT observations 
DATE:    11/01/07 15:54:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in 
Kislovodsk was pointed to the  GRB110106A (Mangano et al., GCN Circ 1152) 17 
sec s after notice time and 41 sec after GRB time at 2011-01-06 15:25:57.96 UT 
in two polarizations+filter R (Gorbovskoy et al., GCN Circ 11523).

We marginally see OT about 16.0+-0.5  mag in XRT error box on second set 
at 2011-01-06 15:26:19 (starting 69 s after trigger time with 10 sec 
exposition, Gorbovskoy et al., GCN Circ 11523).

The OT positon:
RA=  05 17 13.98
DEC= 64 10 23.5
the error +-4" and coincident with late OT  TNG position (Malesani 
et al., GCN Circ 11524).

GRB trigger time: 15:25:16

Time UT             T-T_trigger    Exp         Filter         Mag

15:25:57               41           10           Cr           >16,1
15:26:19               63           10           R+P        16,0+-0.5
15:26:40               84           20           R+P          >16,6
15:27:11               115          20           R+P          >16,6
15:27:42               146          30           R+P          >17,0
15:28:23               187          40           R+P          >17,2
15:29:14               238          50           R+P          >17,4
15:30:15               299          60           R+P          >17,5
15:31:26               370          70           R+P          >17,7
15:32:47               451          90           R+P          >17,9
15:34:28               552         110           R+P          >18,0
15:36:29               673         130           R+P          >18,1
15:38:51               815         160           R+P          >18,3
15:41:42               986         180           R+P          >18,3
15:44:53              1177         180           R+P          >18,4

The more detailed data are available at 
http://observ.pereplet.ru/images/GRB110106A/grb.html

We see the  galaxy  near  (~8" distance, in our prevous Circ 
11523 we not include the binning CCD scale = 4"/pix) OT  on later images 
with long exposition. The redshift z=0.093 (Piranomonte et al., GCN Circ 
1130) is typical for short bursts.

The origin of the GRB110106A is no connected with massive star core 
collapse because  long distance  from center of the host galaxy 
(independently  of the host galaxy type!).  The 
origin of the GRB connected with the NS+NS  or NS+BH merging
(Lipunov et al.,1995, "Evolution of the Double Neutron Star Merging Rate 
and the Cosmological Origin of Gamma-Ray Burst Sources", Astrophysical Journal 
v.454, p.593.; Lipunov, 1997, Relativistic 
Binary Merging Rates, The Invited Review on Joint Discussion "High 
Energy Transients" on XXIIIrd General Assembly of IAU, Kioto, 1997, 
http://adsabs.harvard.edu/abs/1997astro.ph.11270L).

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110106B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11543
SUBJECT: GRB 110106B: Fermi GBM detection
DATE:    11/01/07 16:12:06 GMT
FROM:    Narayana Bhat at U Alabama/Huntsville/GBM  <Narayana.Bhat@nasa.gov>

P. N. Bhat (UAH)
reports on behalf of the Fermi GBM Team:

"At 21:26:16.08 UT on 06 January 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110106B (trigger 316041978 / 110106893).
which was also detected by the Swift/BAT (Sbarufatti et al. 2011, GCN 11525)
The GBM on-ground location is consistent with the Swift position.
 
The angle from the Fermi LAT boresight was 103 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of several pulses
with a duration (T90) of about 35.5 s (50-300 keV).
The time-averaged spectrum from T0-26.6 s to T0+25.6 s is
adequately fit by a simple power law function
with index -1.61 +/- 0.04  (C-stat 849 for 242 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(5.90 +/- 0.44)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+16.13 s in the 10-1000 keV band
is 2.77 +/- 0.27 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB101213A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11544
SUBJECT: GRB 101213A: Gemini-N galaxy redshift
DATE:    11/01/07 23:49:00 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock and E. Berger (Harvard) report:

We obtained a 1200s spectrum of the SDSS galaxy within the XRT error 
circle (Malesani & de Ugarte Postigo, GCN 11449) of GRB 101213A 
(Sakamoto et al., GCN 11448; Gruber et al., GCN 11454; Golenetskii et 
al., GCN 11456; Hanabata et al., GCN 11458) using GMOS on Gemini-North 
on Jan. 7.65 UT to cover the spectral range 3900-8100 Angstroms.  The 
galaxy has a blue continuum and exhibits emission lines of H-beta and [O 
III] at a redshift of z=0.414.


GRB_name: GRB110107A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11545
SUBJECT: GRB 110107A detected in ground analysis of BAT slew data
DATE:    11/01/08 11:50:43 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC) on behalf of the Swift-BAT team


GRB 110107A occurred at 21:15:51 UTC.  It was observed by Fermi GBM (trigger
316127753) and occurred during a Swift slew with BAT event capture. There is a
strong source in a mosaic of BAT images at RA, Dec 299.890, 41.889, which is

RA (J2000)    19h 59m 33.6s
Dec (J2000)   +41d 53m 19s

with an estimated 90% uncertainty of 3 arcmin radius.

The burst was about 100 seconds long, starting at about T-70 sec and lasting
until about T+40 sec.  The BAT event data ended at about T+21 sec.  The burst
had multiple peaks, with the largest flux at about T0, the time of the Fermi
GBM trigger.  The peak count rate in BAT was about 4000 counts/sec.

A Swift Target of Opportunity observation has been requested and approved.


GRB_name: GRB110107A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11546
SUBJECT: GRB 110107A: Swift-BAT refined analysis
DATE:    11/01/08 19:45:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC)
on behalf of the Swift-BAT team:
 
Using the data set from T-70 to T+22 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110107A (a ground-found burst)
(Cummings, GCN Circ. 11545). 
 
The mask-weighted light curve shows low level multiple overlapping peaks
starting at ~T-70 sec and ending at ~T+22 sec. The event-by-event data captured
during the slew stops at T+22 sec.  Using the on-board raw rates, there is
a weak indication that the burst continued out to ~T+45 sec.  
 
The time-averaged spectrum from T-70 to T+22 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.58 +- 0.03.  The fluence in the 15-150 keV band is at least 
5.8 +- 0.5 x 10^-6 erg/cm2.  All the quoted errors are at the 90% confidence
level. 
 


GRB_name: GRB110107A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11547
SUBJECT: GRB 110107A: Swift-XRT Afterglow Candidate
DATE:    11/01/08 22:09:10 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

G. Stratta (ASDC), V. D'Elia (ASDC), P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team:

Swift began a target of opportunity observation of GRB 110107A
on January 8, 2011 at 15:07 UT, approximately 17.8 hours
after the burst detected by Fermi. The GRB was deteced during a Swift
slew with BAT event capture. Swift data for these
observations utilize Target ID 20157.

The XRT began observing the field at 15:12:43 UT, 64.8 ks after the
Fermi trigger.

Using 2517 s of XRT Photon Counting mode data and 1 UVOT
images, we find an astrometrically corrected X-ray position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec =
299.90910, 41.91400 which is equivalent to:

RA (J2000): 19 59 38.20
Dec (J2000): +41 54 50.3

with an uncertainty of 3.6 arcsec (radius, 90% confidence).
This position is 1.7 arcminutes distant from the BAT position.

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

The count rate level is (1.2+/-0.2)10^-2 counts/s.
We cannot state if the source is fading at this stage and
we need to wait for more data.

This circular is an official product of the Swift-XRT team.

----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.


GRB_name: GRB110106B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11548
SUBJECT: GRB 110106B: MASTER early optical observations 
DATE:    11/01/09 21:09:55 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB110106B (Sbarufatti et al., 
GCN Circ 11525) 23 sec s after  notice time and 44 sec after GRB time at 
2011-01-06 21:27:01.696 UT. On  our first (10s exposure) set we haven't 
found optical transient  at Gemini position (Berger et al.,GCN Circ 
11540).
The  upper limit on both telescopes  has been about 16.0 mag
The message may be cited.
We have ~5 hours observations.
The redaction are continueted.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101219B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11549
SUBJECT: GRB 101219b. Possible radio afterglow detection.
DATE:    11/01/10 08:26:41 GMT
FROM:    Dale A. Frail at NRAO  <dfrail@nrao.edu>

Dale A. Frail (NRAO) reports on behalf of a larger collaboration:

"We responded to a request (GCN#11516) for further observations of the
long-lived optical afterglow of GRB 101219B. The Expanded Very Large
Array (EVLA) observed a field toward this GRB (GCN#s 11473, 11482)
on 2011 January 7.03 UT at a center frequency of 8.46 GHz.

In a preliminary reduction of the data, we detect a weak radio source
(Flux=71+/-15 uJy) at RA(J2000)=00:48:55.40 (+/-0.01) and
Dec(J2000)=-34:34:00.1 (+/-0.7) that may be the afterglow of
GRB 101219B.

No further observations are planned.


GRB_name: GRB101225A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11550
SUBJECT: GRB 101225a
DATE:    11/01/10 08:29:09 GMT
FROM:    Dale A. Frail at NRAO  <dfrail@nrao.edu>

Dale A. Frail (NRAO) reports on behalf of a larger collaboration:

"We observed GRB 101225A (GCN#s 11494, 11497, 11498, 11499, 11500)
with the Expanded Very Large Array (EVLA) on 2011 January 6.99 UT using
the C-band wide receiver (frequency range 4-8 GHz).

No significant radio signal is detected at the enhanced Swift-XRT
position (GCN 11497) at frequencies of 4.5 and 7.9 GHz and at 3-sigma
levels of 42 uJy and 30 uJy, respectively.

No further observations are planned.


GRB_name: GRB110107A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11551
SUBJECT: GRB 110107A: Swift/UVOT upper limits
DATE:    11/01/10 19:20:46 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (CRESST/UMCP/GSFC) and G. Stratta (ASDC) report on behalf
of the Swift/UVOT team:

Swift UVOT started observing the field of GRB 110107A on January 8,
2011 at 15:12 UT, approximately T+17.9 hours (Cummings, GCN Circ 11545).

No optical afterglow consistent with the XRT position (Stratta et al.,
GCN Circ. 11547) is detected in individual or merged UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) are:

Filter      T_start   T_stop    Exp(s)      Mag
-----------------------------------------------
v            64,646   75,090      2247 >20.5
u            64,609   74,538      1638 >21.2
-----------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.459 mag (Schlegel et al., 1998, ApJS, 500, 525).


GRB_name: GRB110106B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11552
SUBJECT: GRB 110106B: early optical and near-IR observations
DATE:    11/01/11 11:38:30 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel, A.J. Castro-Tirado, M. Jelinek (IAA-CSIC, Granada), P. Kubanek (U. Valencia & IAA-CSIC, Granada), M. Visus, R. Tata (IAC, Obs. del Teide, Tenerife), A. Sota (OSN, Granada), S. Mottola, C. Faber (DLR, German  Aerospace Center, Berlin), report on behalf of a larger collaboration:

"We have carried out VRIH-band observations of the GRB 110106B XRT error circle (Sbarufatti et al. GCN Circ. 11525) using the 0.6m BOOTES2, 1.23m CAHA, the 1.5m OSN, the 0.82m IAC80 and the 1.5m TCS telescopes, as follows:

  Telescope              Date Jan.2011    Post-GRB-time   Filter    Lim.Mag.
                                               (UT)                    (min)                         (3sigma)
 -------------------------------------------------------------------------------------------
  0.6m BOOTES2    6.90041-6.90212    10.3-12.8            R        16.5
  1.23m CAHA         6.90179-6.91123    12.3-25.9            R        20.4
  1.5m OSN              6.90258-6.91564    13.4-32.2             I         21.0
  1.23m CAHA         6.91184-6.96185    26.8-98.8            V        20.5
  IAC80                     6.91533-6.92520    31.8-46.0            R        20.3
  1.5m TCS              6.94378-6.96465   72.8-102.8           H        18.0
 --------------------------------------------------------------------------------------------

No optical object is detected coincident with the optical afterglow position (Levan et al. GCN Circ. 11534, Berger et al. GCN Circ. 11540) down to the limiting magnitudes (Vega system) displayed in the above table."


GRB_name: GRB110112A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11553
SUBJECT: GRB 110112A: Swift detection of a possible short burst
DATE:    11/01/12 04:26:58 GMT
FROM:    Michael Stamatikos at OSU/GSFC  <michael.stamatikos-1@nasa.gov>

M. Stamatikos (OSU/NASA/GSFC), A. P. Beardmore (U Leicester),
J. R. Cummings (NASA/UMBC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
O. M. Littlejohns (U Leicester), K. L. Page (U Leicester),
J. L. Racusin (NASA/GSFC), T. Sakamoto (NASA/UMBC),
M. H. Siegel (PSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 04:12:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110112 A (trigger=442039).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 329.941, +26.489 which is 
   RA(J2000) = 21h 59m 46s
   Dec(J2000) = +26d 29' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak 
with a duration of about 2 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at the trigger time. 

The XRT began observing the field at 04:13:33.9 UT, 75.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 329.9330, 26.4564 which
is equivalent to:
   RA(J2000)  = 21h 59m 43.91s
   Dec(J2000) = +26d 27' 23.0"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 119 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.54
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The coverage of the XRT error circle by the 8'x8' region
for the list of sources generated on-board is uncertain because the large
number of sources filled the available telemetry. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.06. 

Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11554
SUBJECT: GRB110112A: TNT optical afterglow candidate
DATE:    11/01/12 13:17:22 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, T. M. Zhang, Y.L. Qiu, J.Y. Wei, J. Wang, J.S. Deng, 
C. Wu, X. H. Han on behalf of EAFON report:

We began to observe GRB110112A (stamatikos et al., GCN 11553 ) 
with Xinglong TNT telescope at 10:08:35.375 (UT), 6 hours after 
the burst. 16 images in R-band were obtained with an exposure 
time of 300 sec for each frame. 

After combining all these images, a new marginal source was 
found within the errorbox  of X-ray counterpart 
( stamatikos et al., GCN 11553). 

Its coordinates ( RA and Dec ) are 21:59:43.8 26:27:25.9 (J2000)
with an uncertainty of  about 1 arcsecond.

The brightness of the source is estimated to be about 
19.6 +/- 0.3 mag which is derived from USNO B1.0 R2 mag 
at the mean time of 6.5 hour after the burst. 

Further observations and confirmation are encouraged.

This message may be cited.

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org/grb/


GRB_name: GRB110106B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11555
SUBJECT: GRB 110106B: MASTER  optical observations 
DATE:    11/01/12 15:56:55 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in 
Kislovodsk was pointed to the  GRB110106B (Sbarufatti et al., GCN Circ 11525) 
23 sec s after  notice time and 44 sec after GRB time at 2011-01-06 
21:27:01.696 UT (Gorbovskoy et al., GCN Circ. 11548). On  our first (10s 
exposure) set we haven't found optical transient  at Gemini position (Berger et al.,GCN Circ 11540).
The  upper limit on both telescopes  has been about 16.0 mag.
The composed images give next results:

Lim     Exp        Start time             Last image             Telescope

18.9.  14220  2011-01-06 21:54:34.262  2011-01-07 03:24:31.621     East

19.2.  13860  2011-01-06 21:57:51.527  2011-01-07 02:51:35.346     West

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110112A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11556
SUBJECT: GRB 110112A: Enhanced Swift-XRT position
DATE:    11/01/12 16:00:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1127 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 110112A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 329.93240, +26.45636 which is equivalent
to:

RA (J2000): 21h 59m 43.77s
Dec (J2000): +26d 27' 22.9"

with an uncertainty of 3.2 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110112A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11557
SUBJECT: GRB 110112A: Swift-BAT refined analysis
DATE:    11/01/12 16:32:56 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU)
(on behalf of the Swift-BAT team):
 
Using the data set from T-60 to T+123 sec from the recent telemetry downlink,
we report further analysis of BAT short GRB 110112A (trigger #442039)
(Stamatikos, et al., GCN Circ. 11553).  The BAT ground-calculated position is
RA, Dec = 329.936, 26.470 deg, which is 
   RA(J2000)  =  21h 59m 44.6s 
   Dec(J2000) = +26d 28' 10.6" 
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 87%.
 
The mask-weighted light curve shows a single spike starting at ~T-0.1 sec
and ending at ~T+0.5 sec.  T90 (15-350 keV) is 0.5 +- 0.1 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.1 to T+0.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.14 +- 0.46.  The fluence in the 15-150 keV band is 3.0 +- 0.9 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.28 sec in the 15-150 keV band
is 0.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/442039/BA/


GRB_name: GRB110112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11558
SUBJECT: GRB 110112A: MASTER  optical observations 
DATE:    11/01/12 18:20:16 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB110112.18 48131 sec s after 
notice time and 48156 sec after GRB time at 2011-01-12 17:34:54.665 UT. On 
our first (180s exposure) set we haven't found optical transient  within 
SWIFT error-box (ra=21 59 45 dec=+26 29 24 r=0.050000).
The 5-sigma upper limit has been about 18.3 mag (V) and 19.0 (R).

  The message generated automaticaly.
cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110112A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11559
SUBJECT: GRB 110112A: WHT candidate afterglow/host galaxy
DATE:    11/01/12 22:52:49 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester), 
D. Baker (U. Leicester/U. Hertfordshire)  report for a larger collaboration:

"We observed the field of the short GRB 110112A (Stamatikos et al.
GCN 11553) with ACAM mounted on the William Herschel Telescope (WHT)
on La Palma. Observations began 15.5 hours after the GRB.  Within
the XRT localization (Evan et al. GCN 11556) we detect a faint,
possibly extended source at a position of

RA(J2000) 21:59:43.84 
DEC(J2000) 26:27:24.0

with an error of ~0.5" in each axis The source has a magnitude of
i~22, calibrated against nearby stars from the USNO B1 catalog.
This magnitude is fainter than that inferred for a candidate afterglow
of Xin et al. (GCN 11554), suggestive of fading between the two
epochs.  We note that the positions of the two objects are only
marginally consistent with each other, and suggest that the source
observed in our WHT observations is a candidate host galaxy for GRB
110112A, although with a single epoch we cannot constrain any
possible afterglow contribution at this time."


GRB_name: GRB110112A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11560
SUBJECT: GRB 110112A: Swift/UVOT upper limits
DATE:    11/01/12 22:53:06 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL/UCL) and M. Stamatikos (OSU/NASA/GSFC) report on 
behalf
of the Swift/UVOT team:

Swift UVOT started observing the field of GRB 110112A  with the white 
filter 85s after the trigger (Stamatikos et al., GCN Circ. 11553).

No optical afterglow consistent with the TNT or XRT positions (Xin et 
al., CGN Circ. 11554 and Evans et al., GCN Circ. 11556) is detected in 
individual or merged UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) are:

Filter      T_start   T_stop    Exp(s)      Mag (Upper limits)
---------------------------------------------------------------------------
white          85         235       147         >20.4
white      4499       6134        393        >21.3
v            4909        6544       393        >19.6
b            4294       5929        393        >20.3
u              287       5724        639        >20.2
uvw1     5319        5519       19.7        >18.8
uvm2     5079        6634       280         >18.9
uvw2     4705        6339        393        >19.2
----------------------------------------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.06 mag (Schlegel et al., 1998, ApJS, 500, 525).


GRB_name: GRB110112A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11561
SUBJECT: GRB 110112A: Swift-XRT refined Analysis
DATE:    11/01/12 23:05:48 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A. P. Beardmore (U. Leicester) and M. Stamatikos (OSU/NASA/GSFC) report
on behalf of the Swift-XRT team:

We have analysed 23 ks of XRT data for GRB 110112A (Stamatikos et al.
GCN Circ. 11553), from 82 s to 52.8 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN. Circ 11556).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.95 +/- 0.05.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.4, -0.3). The
best-fitting absorption column is  1.4 (+0.8, -0.7) x 10^21 cm^-2, in
excess of the Galactic value of 5.5 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (5.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.4 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 5.5 x 10^20 cm^-2
Excess significance: 3.0 sigma
Photon index:      2.3 (+0.4, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00442039.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110112B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11562
SUBJECT: GRB 110112B:  A short GRB detected by INTEGRAL
DATE:    11/01/13 10:34:53 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

S.Mereghetti (IASF-Milano), D.Gotz (CEA-Saclay), J. Borkowski (CAMK, 
Torun), E. Bozzo, C.Ferrigno, M. Beck (ISDC, Versoix), on behalf of the 
IBAS Localization Team report:

A short gamma ray burst lasting about 0.5 s has been detected by IBAS in 
the IBIS/ISGRI data at 22:24:54.6 UT of January 12.

The detection significance was slightly below the threshold for automatic 
alert delivery.

Its refined coordinates (J2000) are:
  RA:  10.599  [degrees]
  DEC: 64.406  [degrees]

with an uncertainty of 2.6 arcmin (90% c.l.).

A preliminary analysis gives a   20-200 keV fluence of about  1e-7 
erg/cm2 and a peak flux of about 5 ph/cm2 s  (0.1 s integration time)

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

NOTE: Automatic distribution of sky coordinates of low significance 
INTEGRAL IBAS triggers is currently under testing. This service will soon 
be made available to the interested users.


GRB_name: GRB101225A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11563
SUBJECT: GRB 101225A: Redshift retraction and results of additional photometric follow-up at the NOT
DATE:    11/01/13 11:12:38 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.xu@weizmann.ac.il>

J. P. U. Fynbo (DARK/NBI), D. Xu (WIS) report on behalf of a larger
collaboration:

We re-analyzed the 900s low signal-to-noise spectrum reported in our
previous GCN #11522. We found that the brightest of the three weak
emission features is due to bad removal of a cosmic ray hit. The two
other features are close to sky emission lines. We thus conclude that
the reported redshift of z=0.4 in GCN #11522 for this event is not
secure and may be wrong. Deep spectroscopic observations from 8-10 m
telescopes are strongly encouraged. We apologize for the confusing
this report may have caused.

We also continued photometric follow-ups of the optical counterpart of
GRB 101225A at NOT, and obtained 6x600 s R-band images on Jan. 9 with
a good seeing ~0.65". The object decayed to m(R)=24.5+/-0.2 compared
to m(R)=24.1+/-0.1 on Jan. 5 in GCN #11519. However, this time it was
largely pointlike, which is at odds with being found
significantly extended along the northwest-southeast direction on Jan.
5. The decay in brightness and the variation in morphology indicates
that the underlying host galaxy, if any, still hasn't dominated the
optical counterpart.

Further photometric and spectroscopic observations are underway.


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11564
SUBJECT: GRB 101225A: HST observations - no host detected
DATE:    11/01/13 12:46:08 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N.R. Tanvir (U. Leicester), A.J. Levan (U. Warwick), J.P.U. Fynbo,
D. Malesani, J. Hjorth (DARK/NBI), D. Xu, A. Gal-Yam (Weizmann Inst.)
K. Wiersema, P.A. Evans (U. Leicester) & D.F. Bersier (Liverpool JMU)
report:

We observed the location of GRB 101225A (Racusin et al. GCN 11493; Xu
et al.  GCN 11495) using HST/ACS on 2011 Jan 13 beginning at 00:25 UT,
approximately 18 days post-burst.  Images were obtained in the F606W
and F435W filters.  Contrary to the claim in Xu et al. (GCN 11519), we
find no evidence for extension in either image, and thus no indication
of a host galaxy.  We do, however, find the colour of the optical
transient is now quite red with an (AB) colour of F435W-F606W=1.6,
confirming the reddening trend from the initially very blue colour
(Chornock et al. GCN 11507).  The magnitude (F606W(AB)=24.6) is
consistent with a continuing post-break power-law decline in the
R-band with a slope t^-1.

We note that if this event is at a redshift as low as z=0.07, as
suggested by an analysis of the X-ray data (Campana et al.  GCN
11501), then any host galaxy beneath the transient would have to be
both very faint (less than about M_R=-12) and compact not to be seen
in the HST images.

We thank the STScI staff for rapidly implementing these observations.

[GCN OPS NOTE(13jan11): Per author's request, DX was added to the autor list.]


GRB_name: GRB110107A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11565
SUBJECT: GRB 110107A: Swift-XRT afterglow confirmation
DATE:    11/01/13 17:23:16 GMT
FROM:    Giulia Stratta at ASDC  <giulia.stratta@gmail.com>

G. Stratta (ASDC) reports on behalf of the Swift-XRT team:

Swift performed a second target of opportunity observation of GRB 110107A on
January 12, 2011.

The XRT began observing the field at 2011-01-12 18:07:47 UT, that is T+420.7
ks (4.87 days) (Cummings, GCN Circ. 11545).
Using 2.1 ks of Photon Counting mode data we find that the source has faded
down to a 3-sigma upper limit of 0.007 counts/s.
Assuming a power law decay starting from the first source detection (Stratta
et al., GCN Circ. 11547), the upper limit
is consistent with a decay index steeper than alpha = -0.4.

The fading nature of the source confirms its afterglow origin.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110112A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11566
SUBJECT: GRB 110112A: MITSuME Akeno and Okayama optical upper limits
DATE:    11/01/14 09:21:44 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

H. Nakajima (Tokyo Tech), D. Kuroda, K. Yanagisawa, Y. Shimizu,
H. Toda (OAO, NAOJ), S. Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto), Y. Yatsu, T. Enomoto, K. Kawakami, K. Tokoyoda,
T. Ohkawa and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 110112A (Stamatikos et al.,GCN 11553)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Akeno Observatory and Okayama
Astrophysical Observatory.

We did not find any new point source within the enhanced XRT error
circle (Evans et al., GCN 11556) in all the three bands. We could
not detect the previously reported afterglow (Xin et al., GCN 11554).

Three sigma upper limits of the OT are listed below. We used GSC2.3
catalog for flux calibration.

Akeno Observatory:
The observation started on 2011-01-12 09:07:48 UT (~5 h after the
trigger).
T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.21513    09:22:06    1200.0   >20.2  >20.0  >19.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]

Okayama Astrophysical Observatory:
The observation started on 2011-01-12 09:15:35 UT (~5.1 h after
the trigger).
T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.23603    09:52:11    3840.0   >19.9  >19.8  >19.3
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110112B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11567
SUBJECT: GRB 110112B: Swift XRT and UVOT observations of the INTEGRAL burst
DATE:    11/01/14 14:13:35 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@star.le.ac.uk>

O.M. Littlejohns (U. Leicester), M. De Pasquale (MSSL-UCL), and D.C.
Morris (GWU/GSFC) report, on behalf of the Swift team:

Swift XRT and UVOT instruments began observing the field of INTEGRAL
burst GRB 110112B (Mereghetti et al., GCN circ 11562) 55.8 ks after the
burst trigger. No candidate afterglow is detected in the INTEGRAL error
circle.

UVOT and XRT observed the field of view from 55.8 ks until 67.3 ks after
the trigger. UVOT observed in white filter, with a total exposure time
of 3.6 ks. The three sigma upper limit for any new source in the field
of view is 22.2 mag. XRT observations have a total exposure time of 4.9
ks, and yield a three sigma upper limit of 2.0e-3 counts/second for any
new source in the field of view.

This circular is an official product of the Swift Team.


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11568
SUBJECT: The Christmas burst GRB 101225A - optical spectroscopy with GTC
DATE:    11/01/14 17:35:27 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

C. C. Thoene, S. Guizy, A. Castro-Tirado, J. Gorosabel (IAA-CSIC) and A.
de Ugarte Postigo (DARK/NBI) report:

We observed the optical counterpart of GRB 101225A (the Christmas burst,
GCN 11493, Racusin et al.) with OSIRIS at the 10.4m GTC on Dec. 27,
starting at 21:20 UT (51h after the trigger). We obtained 2 exposures of
1800s using grism R300B.  We acknowledge the excellent support from the
GTC staff.

The combined and flux-calibrated spectrum shows a smooth, very blue
continuum without any absorption of emission features, consistent with the
spectral observations from WHT (GCN 11502, Wiersema et al.), MMT (GCN
11507, Chornock et al.) and Keck/LRIS (GCN 11563, Fynbo et al.) at
different times after the trigger. The continuum is well fitted using a
power law with F(nu) = nu^(0.9+/-0.5).

Considering the very flat optical light curve, the apparent color changes
in the optical SED, the shape of the X-ray spectrum (GCN 11501, Campana et
al.) and the lack of a host galaxy (GCN 11564, Tanvir et al.), we think
that this object might not be a GRB but rather a compact object from the
MW or the local group. Further follow-up is encouraged to determine the
nature of this peculiar object.

[GCN OPS NOTE(14jan11): Per author's request, the last sentence in the first
paragraph was added.]


GRB_name: GRB110112B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11569
SUBJECT: GRB 110112B: Fermi GBM observation
DATE:    11/01/14 20:44:30 GMT
FROM:    Valerie Connaughton at UAH/NSSTC  <valerie.connaughton@nasa.gov>

Valerie Connaughton (UAH) reports on behalf of the Fermi GBM Team:

"At 22:24:55.28 UT on 12 January 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110112B (trigger 316563897 / 110112934),
which was also detected by INTEGRAL IBAS in the IBIS/ISGRI data
(Mereghetti 2011, GCN 11562).

The angle from the Fermi LAT boresight is 50 degrees.

The GBM light curve consists of a single forked peak lasting
about 0.256 s.

The time-averaged spectrum from T0-0.064 s to T0+0.192 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.72  0.20 and
the cutoff energy, parametrized as Epeak, is 495  196 keV.

The event fluence (10-1000 keV) in this time interval is
(3.53  0.49)E-07 erg/cm2.  The 64 ms peak photon flux
measured starting from T0-0.064 s in the 10-1000 keV band
is 8.7  1.0 ph/s/cm2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB101225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11570
SUBJECT: GRB101225A - timing analysis
DATE:    11/01/15 11:46:51 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N.R. Tanvir, P.A. Evans, O.M. Littlejohns (U. Leicester), A.J. Levan (U. Warwick)
report:

In light of the continuing uncertainty about the nature of GRB 101225A,
we performed a search for any periodic signal in the BAT and XRT light curves
for this event.  In neither case do we find any significant periods in the data: from
~0.01 Hz (100 s periods) to ~100 Hz (0.01 s periods) in the case of BAT (data from
50-900 s post-trigger), and from ~0.004 Hz (250 s periods) to ~1 Hz in XRT (2nd orbit
data).


GRB_name: GRB110112B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11571
SUBJECT: Short GRB 110112B :  early optical limit by "Pi of the Sky"
DATE:    11/01/15 15:00:23 GMT
FROM:    Marcin Sokolowski at Soltan Inst. Nuc Studies,Warsaw  <marcin.sokolowski@fuw.edu.pl>

M.Sokolowski,T.Batsch,A.Majcher,A.Majczyna,K.Nawrocki,J.Uzycki,G.Wrochna (SINS, Swierk),
M.Cwiok,W.Dominik,L.W.Piotrowski,A.F.Zarnecki (University of Warsaw),
K.Malek,L.Mankiewicz,R.Opiela,M.Siudek,V.Repei (CFT PAN),
G.Kasprowicz,M.Zaremba (Warsaw University of Technology),
from the "Pi of the Sky" collaboration ( http://grb.fuw.edu.pl ).
M. Jelinek and A. J.Castro-Tirado (IAA-CSIC Granada) on behalf of a larger collaboration.

The wide field "Pi of the Sky North" apparatus installed in the BOOTES-1
station at ESAt/INTA-CEDEA in Mazagon (Huelva, Spain; http://grb.fuw.edu.pl/pi/index.html#piinta_site.htm )
observed position of short GRB 110112B since 2 hours 24 minutes before
  until 36 minutes after the burst.
No new source brighter than 11 mag has been identified on 10s exposures.
Images of special interest were collected at following time ranges :

      22:24:40.3 - 22:24:50.3  UT : mag > 11.0
      22:24:52.9 - 22:25:02.9  UT : mag > 11.0
      22:25:05.5 - 22:25:15.5  UT : mag > 11.0

where limits are based on the reference star magnitudo in V filter.


GRB_name: GRB081215A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11574
SUBJECT: New feature in Fermi GBM GRB Ground Position Notices
DATE:    11/01/17 04:19:13 GMT
FROM:    Valerie Connaughton at UAH/NSSTC  <valerie.connaughton@nasa.gov>

Valerie Connaughton reports for the Fermi GBM Team:

As of today, new information has been added to the GBM Ground Location
GCN notices (GCN/FERMI_GBM_GND_POSITION) that will alert observers that
a bright, hard burst has occurred in the LAT field-of-view.
This additional information is derived from the limited real-time data
extracted by the flight software, telemetered to the ground, and used
to calculate the automated on-ground burst locations currently distributed
in the notice within seconds - tens of seconds of the burst trigger.

Background-subtracted count rates above 200 keV registered in the BGO
detectors for events localized within 70 deg of the LAT boresight are
used to flag the event.  This is done for each of the localizations
performed on the ground, so that it is possible that an event can be
flagged as interesting in one notice and not in another, owing to
brightness variations and spectral evolution in the burst.

The background measure and integration time for the data provide less
information than is available after the full data download hours later,
so the method is not completely reliable, but it is fast and should
permit observers to dedicate more effort to following up the sub-set of
events that contains the LAT-detected burst population.

The identification technique is susceptible to false positives in the
case of short bursts, which can be mistakenly identified as bright owing
to short integration times being more susceptible to statistical
fluctuations above backgrounds measured in a fairly crude automated
fashion.  We have attempted to mitigate this by penalizing information
obtained from integration times shorter than 64 ms, while still
retaining the brighter short bursts.

We have set a threshold which would have flagged 13 of the 18
high-confidence LAT detections between July 2008 and December 2010, with
an additional 24 flagged events that are not high-confidence LAT
detections (though some are low-confidence LAT detections).   By
lowering the threshold, we can identify all but two of the LAT
high-confidence detections (GRB081215 was seen at 90 deg off-axis, and
GRB100116 triggered on a precursor with the main, LAT-detected emission
occurring 80 seconds later, beyond the time when the GBM FSW passes on
the information for localization).  Lowering the threshold this way
comes at a cost of flagging 81 additional bursts (out of a total 575 GBM
GRBs).

Our thresholds can easily be altered upon feedback from the community.

Statistical uncertainties on these types of localizations can be as low
as 1 deg.  An additional systematic error is associated with our
localizations.    Based on a study using 150 GRBs localized by other
instruments (LAT, Swift BAT, SuperAGILE, INTEGRAL, MAXI, the
InterPlanetary Network), this additional uncertainty is 3.2 deg for 70%
of the automated ground locations distributed in these notices, and 9.5
deg for the remaining 30% (Briggs et al., in preparation).  The GBM team
is working to reduce these uncertainties.

Please address feedback and questions tovalerie@nasa.gov


GRB_name: GRB101219B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11575
SUBJECT: GRB 101219B: Likely the GRB host emission dominates now in the uvw2 filter
DATE:    11/01/17 19:14:00 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (MSSL/UCL) and J.M. Gelbord (PSU) report
on behalf of the Swift/UVOT team:

Observations of GRB 101219B from 0.86Ms to 2.45Ms after the
BAT trigger (T) continued in the u and uvw2 filter. The
uvw2 light curve has been flat since T+1Ms. The late time
uvw2 image obtained by summing the late time data in uvw2
shows that the likely host is offset from the GRB position
by 1.2" with an estimated distance error (90% confidence)
of 0.5".

The host position is:

RA = 00h 48m 54.37s
Dec = -34d 33m 58.3s (J2000),

which is (12.23069, -34.56620) in decimal degrees.

The host magnitude is uvw2 = 23.4 +/- 0.3, which
corresponds to a flux density at 1.477 x 10^15 Hz of
(3.4 +/- 1.0)x10^(-4) mJy. In the u band (1.477 x 10^15 Hz)
the observations terminated earlier than the in the uvw2.
However, the u band data obtained between T+0.86Ms and
T+1.8Ms give a 3-sigma upper limit of u > 23.3 with a
corresponding flux density < 6.4 x 10^(-4) mJy.

Observation in the uvw2 filter limits the redshift z < 1.4.


GRB_name: GRB101219B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11576
SUBJECT: GRB 101219B: correction
DATE:    11/01/17 20:59:43 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (MSSL/UCL) reports on behalf of the Swift/UVOT Team

A typographical error slipped into the sexagesimal position given
for the possible host in GCN 11575. The position should read:

RA = 00h 48m 55.37s
DEC = -34d 33m 58.3s (J2000)

The position given in degrees was correct.

Thanks go to Daniele Malesani for pointing this out.


GRB_name: GRB101219B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11578
SUBJECT: GRB 101219B: GROND detection of a SN signature
DATE:    11/01/19 16:57:31 GMT
FROM:    Felipe Olivares Estay at MPE  <felipe@mpe.mpg.de>

F. Olivares E., P. Schady, T. Kruehler, J. Greiner (all MPE Garching),
S. Klose, and D. A. Kann (Tautenburg Observatory) report on behalf of
the GROND team:

GROND continues to observe the field of the Swift GRB 101219B (Gelbord
et al., GCN #11473) simultaneously in g'r'i'z'JHK. The light curve of
the optical transient associated with this GRB (Olivares E. et al.,
GCN #11478, Kuin & Gelbord, GCNs 11482, 11516, 11575, 11576) started
as a single power-law decay, but flattens at around day five at a
preliminary AB magnitude of r' ~ 22.7. In addition there is a clear
color change associated with the flattening.

Starting at day 15, the light curve again decreases in all optical
bands to a magnitude of r' ~ 23.7 at 27 days after the burst. This
light curve shape is typical for GRB/SN events (e.g., Zeh et al. 2004,
ApJ, 609, 952), and we hence interpret these observational features as
signatures of an emerging and decaying supernova underlying the
afterglow emission of GRB 101219B.

Assuming a luminosity equal to that of SN 1998bw for the SN component,
as well as negligible dust extinction along the line of sight, a
conservative redshift range of 0.4 < z < 0.7 is derived for GRB
101219B. We note that the peak time rather short (around 14 days after
burst, see Ferrero et al. 2006, A&A, 457, 857), which further suggests
a low redshift for this GRB.

We stress that at this stage, a possible host contribution and the SN
component cannot be accurately disentangled and all results should be
considered preliminary.

Photometric and in particular spectroscopic observations with larger
aperture telescopes aiming at the detection of the fading SN and/or
host galaxy are highly encouraged.


GRB_name: GRB101219B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11579
SUBJECT: GRB 101219B: tentative redshift and spectroscopic supernova detection
DATE:    11/01/19 18:33:31 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Antonio de Ugarte Postigo (DARK/NBI), Paolo Goldoni (APC/Univ. Paris 7 
and SAp/CEA), Bo Milvang-Jensen, Daniele Malesani, Martin Sparre, Johan 
P.U. Fynbo, Giorgos Leloudas (DARK/NBI), Stefano Covino (INAF/OABr), 
Hector Flores (GEPI/Obs. de Paris), Valerio D'Elia (ASI/ASDC and 
INAF/Roma), Andrew Levan (Univ. Warwick), report on behalf of the 
X-shooter GTO GRB collaboration:

We observed the afterglow of GRB 101219B (Gelbord et al., GCN 11473) 
with the X-shooter spectrograph mounted on the ESO-VLT UT2. Observations 
were taken on two epochs, 2010 Dec 20.17 and 2011 Jan 5.09 UT (11.6 hr 
and 16.4 days after the burst, respectively). Exposure times were 80 and 
120 min, respectively.

In the first-epoch spectrum, the afterglow is detected over the full 
spectral range from about 3200 to 22,000 AA. A careful analysis provides 
a tentative redshift z=0.5519 based on detection of weak Mg II and Mg I. 
No other clear features can be found at the same redshift either in 
absorption or emission.

The second-epoch spectrum was taken 16.4 days after the GRB, which 
corresponds to 10.6 days in the rest frame at z=0.55. The continuum is 
again detected, over the wavelength range 3500 to 22,000 AA, and is 
substantially redder. No narrow emission lines can be distinguished, but 
broad SN-like undulations are apparent, particularly around 8000 AA. We 
carried out a comparison of our spectrum with those of SN 1998bw (Patat 
et al. 2001, ApJ, 555, 900) transformed at various redshifts. We find a 
convincing match at z~0.55 after comparing with a spectrum taken on 1998 
May 4 (i.e., 12 days after the GRB). The observed flux is consistent 
assuming a roughly equal contribution from a SN as bright as SN 1998bw 
and an underlying host galaxy. The match of the spectral shape, 
brightness, and spectral epoch together strenghten both the redshift 
determination and the existence of a SN associated with GRB 101219B.

Our findings are in good agreement with the GROND observations reported 
by Olivares et al. (GCN 11578).

Further observations are planned. We acknowledge the assistence of the 
ESO observing staff at Paranal, in particular Dimitri Gadotti, Leonel 
Rivas, Thomas Rivinius, Maja Vuckovic, and Thomas Szeifert.


GRB_name: GRB110106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11580
SUBJECT: GRB110106A, mm-radio observations
DATE:    11/01/19 18:55:19 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer (Harvard), D.A. Frail (NRAO), E. Berger (Harvard), and S.R.
Kulkarni (Caltech) report:

We observed the position of the intermediate-duration GRB 110106A
(GCN #11520) with the CARMA millimeter array starting on 2011 Jan.
16.827 UT (84 min after the burst) at a frequency of 92 GHz.
A total of 32 minutes were spent integrating on
source in good weather conditions (tau230 < 0.1).  With baselines up
to ~1 km, we obtain a beam size of 3.3'' x 0.9'' (natural weighting).
We do not detect any sources within the revised XRT position
(GCN#11526) to a 5-sigma upper limit of 4.1 mJy/beam.
These observations are among the earliest millimeter wavelength
afterglow searches at milliJansky noise levels.

We thank the CARMA staff for their support of these observations.


GRB_name: GRB110119A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11581
SUBJECT: GRB 110119A: Swift detection of a burst with an optical detection
DATE:    11/01/19 22:31:42 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. Troja (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), M. M. Chester (PSU), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester) and G. Stratta (ASDC) report on behalf
of the Swift Team:

At 22:20:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110119A (trigger=442978).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 348.558, +5.985 which is 
   RA(J2000) = 23h 14m 14s
   Dec(J2000) = +05d 59' 05"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 95 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~35 sec after the trigger. 

The XRT began observing the field at 22:21:56.0 UT, 57.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 348.5881, +5.9874 which is equivalent to:
   RA(J2000)  = 23h 14m 21.14s
   Dec(J2000) = +05d 59' 14.6"
with an uncertainty of 6.2 arcseconds (radius, 90% containment). This
location is 108 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 67 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 23:14:20.61 = 348.58587
  DEC(J2000) = +05:59:10.5  = 5.98626
with a 90%-confidence error radius of about 0.61 arc sec. This position is 9.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.48 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.12. 

Burst Advocate for this burst is E. Troja (eleonora.troja AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110119A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11582
SUBJECT: GRB 110119A: Enhanced Swift-XRT position
DATE:    11/01/20 03:06:52 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1831 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 110119A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 348.58574, +5.98598 which is equivalent
to:

RA (J2000): 23h 14m 20.58s
Dec (J2000): +05d 59' 09.5"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110119A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11583
SUBJECT: GRB 110119A: PAIRITEL NIR Afterglow Detection
DATE:    11/01/20 03:43:24 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan, C. R. Klein, and J. S. Bloom (UC Berkeley) report:

We observed the field of GRB 110119A (Troja et al., GCN 11581) with the 1.3m
PAIRITEL located at Mt. Hopkins, Arizona. Observations began at 2011-Jan-20
01h24m08s UT, ~3.1 hours after the Swift Trigger, under high airmass (~1.9),
and continued until the source set beyond telescope limits.  In  mosaics
(effective exposure time of 0.64 hours) taken simultaneously in the J, H,
and Ks filters, we detect a source at the UVOT position (Troja et al., GCN
11581).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag   m_err
3.78       0.64     J     17.9  0.2
3.78       0.64     H     17.0  0.2
3.78       0.64     Ks    16.2  0.2

All magnitudes are given in the Vega system, calibrated to 2MASS. No
correction for Galactic extinction has been made to the above reported
values.


GRB_name: GRB110119A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11584
SUBJECT: GRB 110119A: Swift-BAT refined analysis
DATE:    11/01/20 04:33:59 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
E. Troja (NASA/GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+713 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110119A (trigger #442978)
(Troja, et al., GCN Circ. 11581).  The BAT ground-calculated position is
RA, Dec = 348.589, 5.982 deg, which is 
   RA(J2000)  =  23h 14m 21.3s 
   Dec(J2000) = +05d 58' 54.3" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a cluster of 4 or 5 overlapping peaks
starting at ~T-90 sec and ending at ~T+90 sec, then a second cluster
of 2 or 3 peaks starting at ~T+110 sec and ending at ~T+260 sec.
T90 (15-350 keV) is 208 +- 13 sec (estimated error including systematics).
 
The time-averaged spectrum from T-86.4 to T+215.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.44 +- 0.05.  The fluence in the 15-150 keV band is 7.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+33.16 sec in the 15-150 keV band
is 2.2 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/442978/BA/


GRB_name: GRB110119A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11585
SUBJECT: GRB110119A: MITSuME Okayama optical upper limits
DATE:    11/01/20 12:50:29 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110119A (Troja et al., GCN 11581)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2011-01-20 10:11:12 UT (~11.8 hours
after the burst). We did not find any new point source within the
enhanced XRT error circle (Goad et al., GCNC 11582) and could not
detect the previously reported afterglow (Morgan et al., GCN 11583)
in all the three bands.

Three sigma upper limits of the OT are listed below. We used
SDSS catalog for flux calibration.


T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.50235    10:24:21  1200.0     >18.9  >18.9  >18.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110119A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11586
SUBJECT: GRB 110119A: Swift-XRT refined Analysis
DATE:    11/01/20 14:46:32 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia, G. Stratta (ASDC), E. Troja (NASA/GSFC/ORAU) report on
behalf of the Swift-XRT team:

We have analysed 18 ks of XRT data for GRB 110119A (Troja  et al. GCN
Circ. 11581), from 48 s to 45.5 ks after the  BAT trigger. The data
comprise 358 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 11582).

The late-time light curve (from T0+4.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.64 (+/-0.10).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.56 (+/-0.03). The
best-fitting absorption column is  1.80 (+/-0.11) x 10^21 cm^-2, in
excess of the Galactic value of 6.4 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.23 (+0.12, -0.11)
and a best-fitting absorption column of 1.29 (+0.26, -0.14) x 10^21
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (5.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.29 (+0.26, -0.14) x 10^21 cm^-2
Galactic foreground: 6.4 x 10^20 cm^-2
Excess significance: 15.3 sigma
Photon index:      2.23 (+0.12, -0.11)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00442978.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110119A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11587
SUBJECT: GRB110119: Swift/UVOT Detection
DATE:    11/01/20 16:08:46 GMT
FROM:    Tyler Pritchard at PSU  <tapritchard@astro.psu.edu>

T. Pritchard (PSU) and E. Troja (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110119A
67 s after the BAT trigger (Troja et al., GCN Circ. 11581).  We  find
a detection in the data consistent with the enhanced  XRT position
(Evans et al., GCN Circ. 11582).

Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            67          217          147         16.52 +- 0.03
u_FC               279          529          246         17.69 +- 0.09
u                  279          529          246         17.69 +- 0.09
v                  609        23078         1298         17.8 +- 0.7
b                  535        29769         2006         16.5 +- 0.1
u                  279        28857         1347         18.0 +- 0.4
w1                 658        24777          990 >20.7
m2                5290        23984         1263 >21.0
w2                4880        18996         1165 >21.5

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.12 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11588
SUBJECT: GRB 110120A: MASTER  optical observations 
DATE:    11/01/20 18:04:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB110120.67 24 sec s after 
notice time and 63 sec after GRB time at 2011-01-20 16:00:42.913 UT. On 
our first (10s exposure) set we haven't found optical transient  within 
FERMI LAT error-box (ra=04 22 36 dec=-18 21 00 r=0.016667).
The 5-sigma upper limit has been about 13 mag.


  The message generated automaticaly.

*Add: The observations was done at high zenith distance.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11589
SUBJECT: GRB 110112A: optical upper limit
DATE:    11/01/20 21:37:07 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

K. Grankin, V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of 
larger GRB  follow-up collaboration:

We observed  the field of the Swift GRB 110112A (Stamatikos  et al., GCN 
11553)  with AZT-11 telescope of CrAO starting on Jan. 12 (UT) 16:35. In the 
enhanced Swift-XRT position  (Evanset al., GCN 11556) we do not detect 
optical afterglow (Xin et al., GCN 11554) up to R=20.6. The photometry is 
based on the
USNO B1.0 star 1164-0563915 (21 59 45.42 +26 27 18.3) assuming R=15.64.

T0+      Filter,   Exposure, mag.
(mid, d)              (s)

0.52955  R 13x180  R   >20.6


GRB_name: GRB110119A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11590
SUBJECT: GRB 110119A: Suzaku WAM observation of the prompt emission
DATE:    11/01/21 16:13:25 GMT
FROM:    Satoshi Sugita at Aoyama Gakuin U.  <sugita@phys.aoyama.ac.jp>

S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Serino, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report:

The  long GRB 110119A (Swift/BAT trigger #442978 ; Troja et al., GCN 11581
; Goad et al., GCN 11582, Baumgartner et al., GCN 11584 ; D'Elia et al., GCN 11586)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 22:20:58.220 UT (=T0).

The observed light curve shows a multi-peaked structure
starting at T0-7.5s, ending at T0+217.5s with a duration  (T90) of 206 (+/- 10) seconds.
The fluence in 100 - 1000 keV was 1.21 (+/- 0.14) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+34s was 1.60 (+/- 0.16) photons/cm^2/s in the same
energy range.

Preliminary result shows that the time-averaged spectrum from T0-7.5s to
T0+217.5s is well fitted by a single power-law with a photon index
of 1.97 (+0.20, -0.18) (chi^2/d.o.f = 27.14/25).
All the quoted errors are at statistical 90% confidence level,

The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB110120A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11591
SUBJECT: GRB 110120A: Fermi GBM detection
DATE:    11/01/21 16:23:22 GMT
FROM:    Lin Lin at UAH/NAOC  <ll0005@uah.edu>

Lin Lin (UAH)
reports on behalf of the Fermi GBM Team: 

"At 15:59:39.23 UT on 20 January 2011, the Fermi Gamma-Ray Burst
 Monitor triggered and located GRB 110120A (trigger 317231981 / 
110120666).

The on-ground calculated location, using the GBM trigger 
data, is RA = 64.54, DEC = -17.06 (J2000 degrees, 
equivalent to 04 h 18 m 09.6 s, -17 d 03 ' 36.0 "), with an 
uncertainty of 1.08 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 15 degrees.

This burst triggered the Fermi spacecraft slew because of high
 peak flux. 

The GBM light curve shows a ~5 s peak followed by a ~40 s 
tail with a duration (T90) of about 27 s (50-300 keV). 
The time-averaged spectrum from T0+0.003 s to T0+43.393 s is 
acceptably fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.87 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 1156 +/- 172 keV
(C-Stat 666.26 for 487 d.o.f.).

The event fluence (10-1000 keV) in this time interval is 
(2.55 +/- 0.05)E-5 erg/cm^2. The 64 ms peak photon flux measured 
starting from T0+0.384 s in the 10-1000 keV band 
is 15.03 +/- 1.35 ph/s/cm^2.


The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110119A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11592
SUBJECT: GRB 110119A: Fermi GBM detection
DATE:    11/01/21 16:33:25 GMT
FROM:    Adam Goldstein at Fermi-GBM/UAH  <adam.m.goldstein@msfc.nasa.gov>

A. Goldstein (UAH) reports on behalf of the Fermi GBM Team: 

"At 22:21:00.17 UT on 19 January 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110119A (trigger 317168462 / 110119931)which was 
also detected by the Swift/BAT (E. Troja et al. 2011, GCN 11581). The GBM 
on-ground location is consistent with the Swift position.  The angle from
the Fermi LAT boresight is 71 degrees.

The GBM light curve consists of ~100 s of variable outburst followed
by a small bump ~175 s after T0.  The entire burst has a duration (T90) 
of about 219 s (50-300 keV). The time-averaged spectrum from T0-16.4 s 
to T0+62.5 s is best fit by a Band function with Epeak = 126.3 +/- 16.8 keV, 
alpha = -0.60 +/- 0.13, and beta = -1.95 +/- 0.09
(C-Stat 1348 for 357 d.o.f.).

The event fluence (10-1000 keV) in this time interval is 
(1.36 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+31.4 s in the 10-1000 keV band is 4.5 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11593
SUBJECT: GRB 110106A: CrAO optical observations
DATE:    11/01/21 21:12:26 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev,  K. Antoniuk (CrAO), A. Pozanenko (IKI) report on behalf of 
larger GRB  follow-up collaboration:

We observed  the field of the Swift GRB 110106A (Mangano et al., GCN 11520) 
with AZT-11 telescope of CrAO starting on Jan. 06 (UT) 16:26. In the
enhanced Swift-XRT position  (Osborne al., GCN  11526) we do not detect 
optical afterglow candidate (Malesani et al., GCN 11524) up to R=21.9. We 
clearly detect the nearby galaxy outside the error circle (Malesani et al., 
GCN 11524, Piranomonte et al., GCN 11530, Gorbovskoy et al., GCN 11542). The 
photometry is based on the USNO B1.0 star 1541-0130790  (05:17:11.42 
+64:10:11.0) assuming R=17.81. The finding chart can be found at 
http://grb.rssi.ru/GRB110106A/grb110106a_110106_R_azt11.png

T0+      Filter,   Exposure, mag.
(mid, d)              (s)

0.06398  R 20x180       >21.9


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11594
SUBJECT: GRB 101225A: CQUEAN optical observation
DATE:    11/01/22 15:52:20 GMT
FROM:    Won-Kee Park at Seoul Nat U/Dept.Physics and Astronomy/CEOU  <wkpark@astro.snu.ac.kr>

Won-Kee Park, Myungshin Im, Changsu Choi (Seoul National Univ.),
Hyeonju Jeong, Juhee Lim, and Soojong Pak (Kyung Hee Univ.)


The field of GRB 101225A was observed with CQUEAN, an optical
CCD camera attached at the 2.1m telescope at McDonald Observatory,
USA. The observation was carried out from 01:16:23 UT, Dec. 26, 2010,
with i, r, z, and Y filters, with exposures of 3 * 300 secs for each
band.

The afterglow was clearly visible on i and r-band images at
the same position reported by Xu et al.(GCN 11495). We obtained
the preliminary magnitude of the afterglow on the stacked i-band
image calibrated with the neighboring USNO B-1.0 stars:
R = 22.60 +- 0.19 at 01:42:47 UT. Further analysis of the data is
ongoing.


GRB_name: GRB110120A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11595
SUBJECT: IPN triangulation of GRB 110120A
DATE:    11/01/23 00:07:18 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline, on behalf of the Konus-Wind team,

V. Connaughton, M. Briggs, and C. Meegan, on behalf of the Fermi GBM team,

J. Cummings, D. Palmer, S. Barthelmy, N. Gehrels, and H. Krimm, on
behalf of the Swift-BAT team,

and

K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima, on behalf of the Suzaku WAM
team, report:

Fermi (GBM), Konus-Wind, Swift (BAT), MESSENGER (GRNS), and Suzaku (WAM) 
observed the long, hard GRB 110120A at about 15:59:39 UT (Fermi/GBM 
trigger 317231981: Lin, GCN 11591). The burst was outside the coded 
field of view of the BAT.

We have triangulated it to a 3 sigma error box whose coordinates are:
-----------------------------------------------
    RA(2000), deg              Dec(2000), deg
-----------------------------------------------
Center:
   60.481 (04h 01m 55s)   -10.548 (-10d 32' 51")
Corners:
   56.433 (03h 45m 44s)    -5.247 (-05d 14' 48")
   62.714 (04h 10m 51s)   -13.354 (-13d 21' 16")
   64.578 (04h 18m 19s)   -14.953 (-14d 57' 11")
   58.278 (03h 53m 07s)    -7.456 (-07d 27' 21")
-----------------------------------------------
The error box area is 2.548 sq. deg.
This error box may be improved.
Because the Earth, the Wind, and the MESSENGER satellites are nearly 
aligned at the moment (the angular distance between Wind and MESSENGER 
is only 5.7 deg), the annuli intersect at grazing incidence and the 
resulting 3-sigma box is long.

A map is posted at http://www.ioffe.ru/LEA/GRBs/GRB110120_T57582/IPN/
showing the GBM best-fit position (blue star and circle), the IPN annuli 
(solid lines with centers dot-dashed), and the box (solid black closed 
polyline).


GRB_name: GRB101224A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11596
SUBJECT: GRB 101224A, the review of the sky area in plate archives
DATE:    11/01/23 15:59:09 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

GRB 101224A, the review of the sky area in plate archives
V.V. Golovnya, L.M. Kizyun, L.K. Pakuliak (Main Astro Obs, Kyiv)
report:

We have undertaken the review of the sky area of GRB 101224A
(K.L.Page et al., GCN 11485) on astronegatives, collected 
in Ukrainian NAS Main astronomical observatory plate archive 
(1976-1996). All the plates with the possible object appearance
are digitized using Microtek ScanMaker 9800XL TMA flatbed scanner
and the images have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
 
The list of plates is given in the table:
YYYYMMDD UT       Plates          Exp. LimMag
19770622 22:14:06 GUA040C000430A  22.5 15.50 
19840720 21:19:40 GUA040C000535A  60.0 17.60 
19860716 21:18:54 GUA040C000961   16.0 17.60 
19870701 22:16:16 GUA040C001064   16.0 17.60 
19870822 19:11:46 GUA040C0001078A 16.0 15.65 
 
No any object has been found in the point with the mentioned
coordinates of GRB. But the double image of some object has 
been found at the distance near 6 arcsec from the probable 
GRB position on the two of selected plates. Brighness of the
object is estimated as V = 17.2:
 
Plates         Obj  RA(J2000)   Dec(J2000)  Mag
GUA040C000535A Obj1 19:03:41.30 +45:42:47.2 17.2
               Obj2 19:03:41.69 +45:42:40.5 17.0
GUA040C001064  Obj1 19:03:41.64 +45:42:41.5 17.3
               Obj2 19:03:42.14 +45:42:36.4 17.4
 
Plates: the plates archive identifier of DWA D/F=400/2000,
M=103"/mm). GUA040C of the Ukrainian NAS Main Astro obs
in Kyiv (Marsden's number - 83) the plate number [1].
Exp. - Duration of the maximum exposures (minutes).
LimMag - Limited V mag, derived in the 15 minutes area around the
location given in K.L.Page et al., GCN 11485:
RA (J2000): 19h 03m 41.91s, Dec (J2000): +45d 42' 48.5".

The preview images of 5 areas together with 
the 15 min.of arc area from SkyMap can be found in 
http://gua.db.ukr-vo.org/img/grb/101224A/index.html
The images with full resolution are available via e-mail on demand.
 
References:
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org


GRB_name: GRB110120A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11597
SUBJECT: GRB 110120A: Fermi LAT detection
DATE:    11/01/24 07:50:35 GMT
FROM:    Nicola Omodei at Standford  <nicola.omodei@slac.stanford.edu>

Nicola Omodei (Stanford University), James Chiang (SLAC/KIPAC),
Valerie Connaughton (UAH) and Yasuyuki Tanaka (ISAS/JAXA)
report on behalf of the Fermi Large Area Telescope (LAT) collaboration.

Based on an on-ground analysis, the Large Area Telescope (LAT),
on-board the Fermi Gamma-ray Space Telescope, detected high energy emission
up to ~2 GeV associated with the GBM-detected burst GRB 110120A (Lin, GCN 11591). 
The emission in the LAT lasts over 100 seconds, with the highest-energy photon
arriving 72 sec after the GBM trigger time.

The best localization is RA, DEC (J2000 deg) = 61.6, -12.0 (04h 06m 24s, -12d 00' 00"),
with an error of 0.4 deg (68% CL), compatible with the IPN triangulation
from Hurley et al. (GCN 11595).

Further analysis is ongoing.

The Fermi LAT point of contact for this burst is Yasuyuki Tanaka (tanaka@astro.isas.jaxa.jp).

The Fermi LAT is a pair conversion telescope designed to cover the energy band
from 20 MeV to greater than 300 GeV. It is the product of an international collaboration
between NASA and DOE in the U.S. and many scientific institutions across France,
Italy, Japan and Sweden.

[GCN OPS NOTE(24jan11): Per author's request, his affilation and address were updated.]


GRB_name: GRB110120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11598
SUBJECT: GRB 110120A: MASTER optical observations 
DATE:    11/01/24 14:56:32 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

MASTER very wide field cameras (MASTER-Net: 
http://observ.pereplet.ru, 6 cameras 11 Mpix, 85, 1/1.2. 1 sec 
exposition, comonn FOW is 2400 square degrees) 
located in  Kislovodsk was pointed to the  GRB110120A 24 sec s after 
notice time and  64 sec after GRB time at 2011-01-20 16:00:42.913 UT.
The sky near horizont is not clear. 
On our 60 coaded images  we haven't found optical transient  within
common area of the FERMI LAT error-box  (Nicola Omodei et al., GCN Circ 
11597) and (Hurley et al., GCN 11595).

The 5-sigma upper limit has been about 10 mag (mean time = 94 sec after 
trigger).
The image is available at 
http://observ.pereplet.ru/images/GRB110120A/grb.html

The MASTER II telescopes FOW  was out 
of the  final error box and our previous results (Gorbovskoy et al., GCN 
Circ 11588) not valid.

  The observations was done at high zenith distance.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110106B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11599
SUBJECT: GRB 110106B, radio observations
DATE:    11/01/24 18:17:14 GMT
FROM:    Dale A. Frail at NRAO  <dfrail@nrao.edu>

Dale A. Frail (NRAO) report on behalf of a larger collaboration:

"We used the Expanded Very Large Array (EVLA) to observe the field of
view towards GRB 110106b, detected by Swift and Fermi GBM (GCN
11525, 11532, 11533, 11543), on 2011 January 22.22 UT at a center
frequency of 8.46 GHz.  No radio afterglow is detected. At the
position of the optical afterglow (GCN 11540) the flux density is
measured to be -27 +/- 24 uJy.

No further observations are planned.


GRB_name: GRB110123A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11600
SUBJECT: GRB 110123A: Fermi GBM detection
DATE:    11/01/25 00:31:13 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (USRA) and D. Gruber (MPE) report on behalf
of the Fermi GBM Team:

"At 19:17:45.03 UT on 23 January 2011, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 110123A (trigger 317503067 /
110123804). The on-ground location, using the GBM trigger data, is
RA = 247.0, Dec = +28.0 (J2000 degrees, equivalent to 17h40m, +28d02'),
with an uncertainty of 1.64 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which is
currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 58 degrees. This GRB was
bright enough to result in a Fermi spacecraft repointing maneuver.

The GBM light curve consists of one main peak with substructure, with
a duration (T90) of 17.9 +/- 0.8 s (50-300 keV). The time-averaged
spectrum from T0-1.8 s to T0+22.8 s is best fit by a Band function with
Epeak = 280 +/- 15 keV, alpha = -0.64 +/- 0.03, and beta = -1.96 +/- 0.05.
The event fluence (10-1000 keV) in this time interval is
(2.61 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+8.4 s in the 10-1000 keV band is
8.3 +/- 0.2 ph/s/cm^2.

The temporal and spectral analysis results presented above are
preliminary; final results will be published in the GBM GRB Catalog."


GRB_name: GRB110120A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11601
SUBJECT: Konus-Wind observation of GRB 110120A
DATE:    11/01/25 14:44:44 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long hard GRB 110120A,
(Fermi/GBM trigger 317231981/
110120666: Lin Lin, GCN 11591;
localized by IPN: Hurley et.al, GCN 11595;
detected by Fermi/LAT: Omodei et al., 11597)
triggered Konus-Wind at T0=57582.268s UT (15:59:42.268)

The burst light curve starts with a hard bright pulse,
followed by a softer decaying tail.
The total duration of the burst is ~42 s.
The emission is seen up to ~5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB110120_T57582/

As observed by Konus-Wind the burst
had a fluence of (3.1  0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.128s,
of (1.6  0.5)x10-5 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+41.216 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.6 (-0.2, +0.2),
and Ep = 680(-120, +160) keV,
chi2 = 64.5/74 dof.

The spectrum at the initial part of the burst
(measured from T0 to T0+0.256 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = 0.0 (-0.3, +0.4),
and Ep = 1193(-244, +349) keV,
chi2 = 18.0/23 dof.

All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB110128A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11603
SUBJECT: GRB 110128A: Swift detection of a burst
DATE:    11/01/28 01:55:36 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Grupe (PSU), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), M. H. Siegel (PSU),
E. Sonbas (GSFC/USRA/Adiyaman Univ.) and E. Troja (NASA/GSFC/ORAU)
report on behalf of the Swift Team:

At 01:44:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110128A (trigger=443861).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 193.874, +28.080 which is 
   RA(J2000)  = 12h 55m 30s
   Dec(J2000) = +28d 04' 47"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a weak peak
with a duration of about 20 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 01:46:53.5 UT, 140.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 193.89471, 28.06508 which
is equivalent to:
   RA(J2000)  = 12h 55m 34.73s
   Dec(J2000) = +28d 03' 54.3"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 84 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 9.02
x 10^19 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 143 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.01. 

Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110128A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11604
SUBJECT: GRB 110128A: TAROT Calern observatory upper limits
DATE:    11/01/28 02:29:39 GMT
FROM:    Myrtille LAAS-BOUREZ at U.Western Australia  <myrtille.laas@oamp.fr>

GRB 110128A: TAROT Calern observatory upper limits
----------------------------------------------------------------------
Klotz A. (CESR-OMP), Gendre B. (ASDC),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP), Laas-Bourez M. (UWA/ICRAR) report:

We imaged the field of GRB 110128A detected by SWIFT
(trigger 443861) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 73.7s after the GRB trigger
(15s after the notice). The elevation of the field increased from
58 degrees above horizon and weather conditions
were good.

The date of trigger : t0 = 2011-01-28T01:44:32.640

We do not detect any OT with a limiting magnitude of:

The first image is 60.0s exposure in tracking mode:
t0+73.7s to t0+133.7s : R > 16.9

The five following images are 30.0s exposure in tracking mode:

t0+148.6s to t0+178.6s : R > 16.4
to+193.7s to t0+223.7s : R > 16.4
to+238.9s to t0+268.9s : R > 15.9
to+284.0s to t0+314.0s : R > 15.9
to+329.2s to t0+359.2s : R > 16.9

We co-added a series of exposures:

t0+73.7s to t0+359.2s : R > 18.8


Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon= 79.7852 lat=+88.6911
and the galactic extinction in R band is 0.009 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.
======================================================================


<http://www.zt.science.uwa.edu.au/>

[GCN OPS NOTE(29oct11): The missing "A" was added the GRB name.]


GRB_name: GRB110128A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11605
SUBJECT: GRB 110128A: Afterglow detection from NOT
DATE:    11/01/28 03:41:05 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo, D. Malesani (Dark/NBI) J. McCormac (Queens Univ.,
Belfast) and P. Jakobsson (U. Iceland) report on behalf of a larger
collaboration:

We have imaged the field of GRB 110128A (Grupe et al. GCN 11603) with the
2.5m NOT telescope at Roque de los Muchachos Observatory (La Palma, Spain)
starting at 2:57 UT (1.22h after the burst). We detect an R~22.2 (as
compared to USNO-B1.0) object at coordinates:

R.A.: 12:55:35.10
Dec.: +28:03:54.1

This object is not present in SDSS DR8. We propose it as the afterglow of
GRB 110128A


GRB_name: GRB110128A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11606
SUBJECT: GRB 110128A: Enhanced Swift-XRT position
DATE:    11/01/28 09:50:33 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 920 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 110128A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 193.89661, +28.06511 which is equivalent
to:

RA (J2000): 12h 55m 35.19s
Dec (J2000): +28d 03' 54.4"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11607
SUBJECT: GRB 110128A: VLT/X-shooter redshift
DATE:    11/01/28 12:26:53 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

M. Sparre, A. de Ugarte Postigo, J. P. U. Fynbo , D. Malesani,
B. Milvang-Jensen (Dark/NBI), S. D. Vergani, H. Flores (GEPI/Obs. de Paris), 
P. Goldoni (APC/Univ. Paris 7 and SAp/CEA), and
N. R. Tanvir (U. Leicester) report on behalf of the X-shooter GRB GTO
collaboration:

We observed the optical afterglow of GRB 110128A (Grupe et al., GCN
11603; de Ugarte Postigo et al., GCN 11605) with the ESO VLT equipped
with X-shooter.

Observations lasted for two hours, with a mean time 2011 Jan 28.345 UT
(6.55 hr after the GRB). Sky transparency was non optimal, but the
seeing was around 0.9".

We detect a broad damped Lyman alpha feature, and other absorption
lines of OI, CII, SiIV, CIV, SiII and FeII at a common redshift of z=2.339. 
We also find an absorption feature at about 4960A which we tentatively
identify as an intervening CIV system at z=2.20.

We acknowledge excellent support from the astronomers at the VLT,
Dieter Nuernberger and Alvaro Alvarez.


GRB_name: GRB110128A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11608
SUBJECT: GRB 110128A: WHT redshifts of nearby field galaxies
DATE:    11/01/28 14:21:48 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir, K. Wiersema (U. Leicester), A. J. Levan (U. Warwick),
A. Kamble (U. Wisconsin), A. Cardwell (ING) and E. M. Ratti (SRON)
report on behalf of a larger collaboration:

We obtained spectroscopy of the afterglow of GRB 110128A (GCN 11603,
GCN 11605) and of two field galaxies nearby, using the 4.2 William Herschel
Telescope on La Palma.  Observations began at 04:26 UT, approximately 2.7 hours
post-burst, and comprised a 60 minute total exposure. The spectra cover a
wavelength range from about 4500A to 9400A.

The signal-to-noise, of the afterglow spectrum is not sufficient to confirm the
redshift reported in Sparre et al. in GCN 11607 (and note, our spectral range
did not cover the DLA feature), however we did measure the redshifts of
two field galaxies which are sufficiently close to the line of sight that they
might produce absorption in the afterglow:

Gal 1: RA=12:55:35.38, dec=+28:03:57.6
z=0.639 based on [OII]3727, CaII H & K, Hbeta
Offset from afterglow=5 arcsec, corresponding to ~35 kpc impact parameter to GRB

Gal 2: RA=12:55:36.40, dec=+28:04:12.1
z=0.109 based on Ha and [NII]
Offset from afterglow=25 arcsec, corresponding to ~50 kpc impact parameter to GRB


GRB_name: GRB110120A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11609
SUBJECT: GRB 110120A: Suzaku WAM observation of the prompt emission
DATE:    11/01/28 14:57:51 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

P. Tsai, Y. Urata (NCU), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa
(Hiroshima U.), N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.), 
S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara,
T. Yasuda (Saitama U.), M. Ohno, M. Serino, M. Kokubun, T. Takahashi (ISAS/JAXA), 
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka, 
M. Yamauchi (Univ. of Miyazaki), K. Nakazawa, K. Makishima (Univ.  of Tokyo), 
on behalf of the Suzaku WAM team, report:


The log GRB 110120A (Fermi/GBM trigger 317231981 / 110120666 ; Lin et
al., GCN 11591; Omodei et al., GCN 11597) triggered the Suzaku
Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV
- 5 MeV at 2011/01/20 15:59:39.22 UT (=T0).

The observed light curve shows a multi-peaked structure starting at
T0-0.7s, ending at T0+8s, with a duration (T90) of about 6.4
seconds. The fluence in 100 - 1000 keV was 2.32 (+/-0.16) x 10^-5
ergs/cm^2. The 1-s peak flux measured from T0+0.38s was 30.40
(+/-0.93) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-0.7s
to T0+8s is well fitted by a power-law with exponential cutoff
model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha       1.34 (-0.51, +0.40), and
  Epeak       418.60 (-84.64, +110.46) keV (chi^2/d.o.f. = 39.92/40).


All the quoted errors are at statistical 90% confidence level, in
which the systematic uncertainties are not included.

The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB110128A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11610
SUBJECT: GRB 110128A: Swift-XRT refined Analysis
DATE:    11/01/28 15:29:47 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

D. Grupe (PSU) reports on behalf of the Swift-XRT team:

We have analyzed 11 ks of XRT data for GRB 110128A (Grupe  et al. GCN
Circ. 11603), from 125 s to 30.0 ks after the  BAT trigger. The data
comprise 9 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN. Circ
11606).

The light curve can be modeled with an initial decay slope alpha-1 =
2.3+/-0.5 and a break at 700 (-200,+600) s followed by a decay slope of
alpha-2 = 0.6+/-0.3. Currently we are in the plateau phase. At this
point predictions of the behavior of the light curve are unreliable.


A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.64 (+0.22, -0.21). The
best-fitting absorption column is  consistent with the Galactic value
of 9.0 x 10^19 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.0 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Galactic foreground: 9.0 x 10^19 cm^-2
Intrinsic column:    0.0 (+3.0, -0.0) x 10^21 cm^-2
at z=2.339
Photon index:      1.64 (+0.22, -0.21)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00443861.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110128A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11611
SUBJECT: GRB 110128A: Swift-XRT refined Analysis
DATE:    11/01/28 15:30:24 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

D. Grupe (PSU) reports on behalf of the Swift-XRT team:

We have analyzed 11 ks of XRT data for GRB 110128A (Grupe  et al. GCN
Circ. 11603), from 125 s to 30.0 ks after the  BAT trigger. The data
comprise 9 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN. Circ
11606).

The light curve can be modeled with an initial decay slope alpha-1 =
2.3+/-0.5 and a break at 700 (-200,+600) s followed by a decay slope of
alpha-2 = 0.6+/-0.3. Currently we are in the plateau phase. At this
point predictions of the behavior of the light curve are unreliable.


A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.64 (+0.22, -0.21). The
best-fitting absorption column is  consistent with the Galactic value
of 9.0 x 10^19 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.0 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Galactic foreground: 9.0 x 10^19 cm^-2
Intrinsic column:    0.0 (+3.0, -0.0) x 10^21 cm^-2
at z=2.339
Photon index:      1.64 (+0.22, -0.21)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00443861.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110128A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11612
SUBJECT: GRB 110128A: Swift/UVOT observations
DATE:    11/01/28 15:44:03 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) & D. Grupe (PSU) report on behalf of the Swift- 
UVOT team

The Swift/UVOT began settled observations of the field of GRB 110128A
144 s after the BAT trigger (Grupe et al., GCN Circ. 11603). The optical
afterglow is detected in the first white and u exposures at a refined
UVOT position RA(J2000)=  193.89625 deg, DEC(J2000) = 28.06503,
which is:

      RA (J2000)  12:55:35.10
     Dec (J2000)  28:03:54.1

with an estimated uncertainty of 1.3 arcsec (radius, 90% confidence).
This position is consistent with the optical afterglow detection by
NOT (de Ugarte Postigo., GCN Circ 11605) and the enhanced XRT
position (Osborne et al., GCN Circ. 11606).

Preliminary magnitudes using the UVOT photometric system (Poole et al.  
2008,
MNRAS, 383, 627) for single and summed exposures are:

Filter  T_start(s)  T_stop(s)   Exp(s)       Mag/3sigUL
#####################################################
wh (FC)   144          294       147      20.98 +/- 0.29
u  (FC)   302          552    246      20.32 +/- 0.35
wh        582         6352       580        > 21.89
v         632         6763       432        > 20.09
u         707         5943       412        > 20.95
b         558         6148       432        > 21.32
uvw1      682         5738       221        > 20.34
uvm2      658         6874       340        > 20.43
uvw2      608         6558       393        > 20.88
#####################################################

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11613
SUBJECT: GRB 110128A: TAROT-Calern refined analysis
DATE:    11/01/28 15:49:13 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@asdc.asi.it>

Laas-Bourez M. (UWA/ICRAR), Gendre B. (ASDC), Atteia J.L. (IRAP-OMP),
Klotz A. (IRAP-OMP), and Boer M. (OHP-OAMP)  report:

following the detection of the optical afterglow by de Ugarte Postigo  
et al. (GCN 11605), we re-analyzed the TAROT data reported in Klotz et  
al. (GCN 11604). At the position of the afterglow, an object is  
marginally detected (2.6 sigma confidence level) within the stack of  
the first two images (73.7s -> 178.6s), with R = 18.0. A stack of the  
following 4 images (193.7s -> 359.2s) gave only an upper limit of R <  
18.7.

Combined with the NOT observation, this gives an optical decay index  
of at least 1.6 during the initial part of the light curve, that could  
indicate the presence of a reverse shock.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

This message can be cited

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GRB_name: GRB110128A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11614
SUBJECT: GRB 110128A, Swift-BAT refined analysis
DATE:    11/01/28 17:04:11 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner
(GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), D. Grupe (PSU),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110128A (trigger #443861)
(Grupe, et al., GCN Circ. 11603).  The BAT ground-calculated position is
RA, Dec = 193.871, 28.108 deg which is
     RA(J2000)  =  12h 55m 29.0s
     Dec(J2000) = +28d 06' 28.7"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.

The mask-weighted light curve shows a single broad peak extending from
approximately T-3 sec to T+40 sec. T90 (15-350 keV) is 30.7 +- 18.1 sec
(estimated error including systematics).

The time-averaged spectrum from T-1.4 to T+48.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.31 +- 0.30.  The fluence in the 15-150 keV band is 7.2 +- 1.4 x 10-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.58 sec in the 15-150 keV band
is 0.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/443861/BA/


GRB_name: GRB110128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11615
SUBJECT: GRB110128A: TNG NIR observations
DATE:    11/01/28 20:16:21 GMT
FROM:    Angelo Antonelli at Obs. Astro. di Roma  <angelo.antonelli@oa-roma.inaf.it>

L.A. Antonelli (INAF-OAR), P. D'Avanzo (INAF-OAB), D. Malesani (DARK/ 
NBI), V. Lorenzi, G. Tessicini (INAF-TNG) and E. Palazzi (INAF-IASF/ 
Bo) on behalf of the CIBO collaboration report:

"We observed the field of GRB 110128A (Grupe et al. GCN 11603) in the  
J band with the 3.6m TNG equipped with the NICS camera. A total of 15  
min integration were obtained with a mean time Jan 28.254 UT (4.37 hr  
after the GRB).

A faint, close to the detection limit, NIR source is detected in our  
image at the position of the optical afterglow reported by de Ugarte  
Postigo et al. (GCN 11605). The source has a magnitude J = 21.8+/-0.4  
(calibrated against the 2MASS stars in the field). Being the  
coincident with the optical afterglow we conclude that it is the NIR  
counterpart of  the GRB 110128A afterglow.

This message can be cited"


GRB_name: GRB101112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11616
SUBJECT: GRB 101112A: Maidanak and CrAO optical observations
DATE:    11/01/28 22:36:09 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

GRB 101112A: Maidanak and CrAO optical observations

A. Volnova (SAI MSU), A. Pozanenko (IKI), . Ezhkova (SAI MSU), M.
Ibrahimov (MAO), V. Rumyantsev (CrAO), K. Antoniuk (CrAO), B. Satovski
(Astrotel) report on behalf of larger GRB follow-up collaboration:

We observed the field of the INTEGRAL GRB 101112A (Gotz et al., GCN
11396) with AZT-22 telescope of MAO observatory in R-band on Nov.13
between (UT) 13:37:57 - 14:10:56 (Pozanenko et al, GCN 11402) and
Nov.14 between (UT) 14:42:43 - 15:15:49 under
good weather conditions and seeing ~0.9". Both observational
sequences consist of 6 images with exposure of 300 seconds.
Additionally we observed the field with AZT-11 telescope of CrAO
in R-band on Nov.13 between (UT) 16:07:10 - 16:52:23.

Near the position of the optical afterglow (Guidorzi et al.GCN 11397,
A. de Ugarte Postigo et al. GCN 11398) there are two bright stars.
They are not separated on DSS and are included in USNO-B1.0 like a
single source USNO-B1.0 1293-0343482 (R = 18.77). In our images the
stars is well separated at the distance 2.7" between them.

The afterglow is in the wing of the southern star. The star has the
magnitude R = 19.2 +/- 0.08 and coordinates (J2000) RA = 19:28:54.947,
Dec
= +39:21:12.29 with position uncertainty of 0.15 arcsec. After
subtraction of a PSF-like profile of the star from stacked image of
Nov.13 in the XRT error circle (Evans et al., GCN 11399) we found a
faint source in coordinates (J2000) RA = 19:28:54.856, Dec =
+39:21:10.67 with position uncertainty of 0.2 arcsec. This position
is in agreement with afterglow coordinates reported by Guidorzi et al.
(GCN 11397). The distance between southern star and optical afterglow
is ~ 1.9". Using the same procedure we do not detect the afterglow on
Nov.14 up to 22.5m.

The photometry of the sources based on several field stars from USNO-B1.0:

t-t0 (d), filter tstart exp.,s ,d OT  uplim(3 sigma) telescope

0.65558 R 13:37:57 6*300 22.2+/-0.20 22.5   AZT-22

0.76346 R 16:07:10 15*180 n/d       21.1   AZT-11

1.70060 R 14:42:43 6*300  n/d       22.5   AZT-22

Taken together all published photometry of the afterglow (Guidorzi et
al.GCN 11397, Fatkhullin et al. GCN 11419) we obtained light curve
which can be fairly well described by single power law with
alpha=-1.08.
The finding chart as well as light curve of the GRB 101112A can be
found at http://grb.rssi.ru/GRB101112A/


GRB_name: GRB110125A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11617
SUBJECT: GRB 110125A: Fermi GBM detection
DATE:    11/01/29 00:06:49 GMT
FROM:    Adam Goldstein at Fermi-GBM/UAH  <adam.m.goldstein@msfc.nasa.gov>

A. Goldstein (UAH) reports on behalf of the Fermi GBM Team: 

"At 21:27:28.39 UT on 25 January 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110125A (trigger 317683650 / 110125894) which
was originally classified as a solar flare.

The on-ground calculated location, using the GBM trigger data, is 
RA = 331.4, DEC = -46.2 (J2000 degrees, equivalent to 22 h 05 m, -46 d 12 '),
with an uncertainty of 5.8 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic error which is 
currently estimated to be 2 to 3 degrees).  The angle from the Fermi LAT 
boresight is 14 degrees.

The GBM light curve consists of a single pulse with a duration (T90) of 
about 4.8 s (50-300 keV). The time-averaged spectrum from T0-1.024 s to 
T0+3.072 s is best fit by a simple power law function with index 
-1.93 +/- 0.05 (Castor C-Stat 406 for 362 d.o.f.).  The event fluence 
(10-1000 keV) in this time interval is (1.17 +/- 0.08)E-6 erg/cm^2. 
The 1-sec peak photon flux measured starting from T0+0.003 s in the 
10-1000 keV band is 5.25 +/- 0.27 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110128A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11618
SUBJECT: GRB110128A: MITSuME Okayama optical upper limits
DATE:    11/01/29 09:18:32 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110128A (Grupe et al., GCN 11603)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2011-01-28 14:44:10 UT (~13 hours
after the burst). We did not find any new point source within the
enhanced XRT error circle (Osborne et al., GCNC 11606) and could not
detect the previously reported afterglow (de Ugarte Postigo et al.,
GCN 11605) in all the three bands.

Three sigma upper limits of the OT are listed below. We used
SDSS catalog for flux calibration.


T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.63108    16:53:18  6300.0     >20.6  >20.3  >19.8
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110112A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11619
SUBJECT: GRB110112A:  EVLA Observations
DATE:    11/01/31 17:26:28 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger, and W. Fong (Harvard) report:

We observed the position of the short GRB 110112A (GCN #11553) with the 
EVLA for 1 hour at 5 GHz starting on 2011 January 14.05 UT (1.87 days 
after the burst).  No radio source is detected within the XRT error 
circle (GCN #11556) to a 3-sigma limit of 75 microJy.

We acknowledge the EVLA staff for their support of these observations.


GRB_name: GRB101224A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11620
SUBJECT: GRB101224A:  EVLA Observations
DATE:    11/02/01 04:37:41 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger, and W. Fong (Harvard) report:

We observed the position of the short GRB 101224A (GCN #11484) with the 
EVLA at 5 GHz for two hours starting on 2010 December 27.95 UT  (3.72 
days after the burst).   No sources are detected within the XRT error 
circle (GCN #11488) to a 3-sigma limit of 156 microJy.

We acknowledge the EVLA staff for their support of these observations.


GRB_name: GRB110112B
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11621
SUBJECT: GRB110112B:  EVLA Observations
DATE:    11/02/01 04:39:50 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger, and W. Fong (Harvard) report:

We observed the position of the INTEGRAL short GRB 110112B (GCN #11562) 
with the EVLA at 5 GHz on four separate occasions:  Jan 13.78, 14.73, 
15.85, and 25.04 UT.  The first three epochs lasted 1 hour, while the 
last epoch lasted 2 hours.  In the initial observation we detected four 
sources within the 2.6' error circle reported for the burst location. 
Although variations in flux are present between epochs, none of the 
sources exhibit a significant decline over the 12-day baseline.  Hence, 
we report no clear indication of association between the detected 
sources and the GRB.

We are grateful to the EVLA staff for their support of our initial and 
followup observations.


GRB_name: GRB110201A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11622
SUBJECT: GRB 110201A: Swift detection of a burst
DATE:    11/02/01 09:49:06 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU), A. P. Beardmore (U Leicester),
S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester),
J. M. Gelbord (PSU), D. Grupe (PSU), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), V. Mangano (INAF-IASFPA),
C. B. Markwardt (NASA/GSFC), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-OAB/IASFPA) and
G. Stratta (ASDC) report on behalf of the Swift Team:

At 09:35:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110201A (trigger=444230).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 137.065, +88.608 which is 
   RA(J2000) = 09h 08m 16s
   Dec(J2000) = +88d 36' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 17 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:36:15.5 UT, 66.6 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 137.5802,
88.6054 which is equivalent to:
   RA(J2000)  = 09h 10m 19.25s
   Dec(J2000) = +88d 36' 19.3"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 45 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (7.08 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.1
(+3.40/-2.79) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
126 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. The
coverage of the XRT error circle by the 8'x8' region for the list of sources
generated on-board is uncertain because the large number of sources filled the
available telemetry. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.35. 

Burst Advocate for this burst is M. H. Siegel (siegel AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110201A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11623
SUBJECT: GRB 110201A: MASTER optical observations 
DATE:    11/02/01 09:59:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in MASTER-Amur was pointed to the  GRB110201A 21 sec s after 
notice time and 46 sec after GRB time at 2011-02-01 09:35:54.771 UT. On 
our first (10s exposure) set we haven't found optical transient  within 
SWIFT-XRT error-box.
The 3-sigma upper limit has been about V = 14.5mag
The message may be cited.


mailto: lipunov@sai.msu.ru


GRB_name: GRB110201A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11624
SUBJECT: GRB 110201A: Swift-BAT refined analysis
DATE:    11/02/01 15:17:14 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. H. Siegel (PSU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+878 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110201A (trigger #444230)
(Siegel, et al., GCN Circ. 11622).  The BAT ground-calculated position is
RA, Dec = 137.489, 88.610 deg, which is 
   RA(J2000)  =  09h 09m 57.3s 
   Dec(J2000) = +88d 36' 36.9" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows 3 or 4 overlapping peaks starting
at ~T-2 sec, peaking at ~T_zero, and ending at ~T+30 sec.
T90 (15-350 keV) is 13.0 +- 2.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.8 to T+13.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.09 +- 0.11.  The fluence in the 15-150 keV band is 7.0 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.28 sec in the 15-150 keV band
is 1.1 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/444230/BA/


GRB_name: GRB110201A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11625
SUBJECT: Swift/UVOT observations of GRB110201A
DATE:    11/02/01 16:11:22 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and M.H Siegel (PSU) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110201A 127
s after the BAT trigger (Siegel et al., GCN Circ. 11622).  No optical
afterglow consistent with the XRT position is detected in the initial
UVOT exposures. Preliminary 3-sigma upper limits using the UVOT
photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)  Exp(s)   Mag

u_FC               127         377     246    >20.0
u                  127        2348     627    >20.4
v                  433        2424     253    >19.5
b                  382        2373     272    >20.4
w1                 482        2324     233    >19.7
m2                 457        2449     233    >19.6
w2                 408        2400     253    >19.1

We note that a bright star (V=7) is a few arcminutes from the
GRB position.

The values quoted above are not corrected for the strong Galactic
extinction due to the reddening of E(B-V) = 0.35 in the direction
of the burst (Schlegel et al. 1998).


GRB_name: GRB110201A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11626
SUBJECT: GRB110201A: MITSuME Okayama optical upper limits
DATE:    11/02/02 09:39:55 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110201A (Siegel et al., GCN 11622)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on2011-02-01 09:59:39 UT (~25 min.
after the burst). We did not find any new point source within the
XRT error circle (Siegel et al., GCNC 11622) in all the three bands.

Three sigma upper limits of the OT are listed below. We used
GSC2.3 catalog for flux calibration.


T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.16707    13:35:43  5880.0     >21.3  >21.3  >18.7
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110201A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11627
SUBJECT: GRB 110201A: Swift-XRT refined Analysis
DATE:    11/02/02 16:02:43 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

D. Grupe and M. H. Siegel (PSU) report on behalf of the Swift-XRT team:


We have analyzed 21 ks of XRT data for GRB 110201A (Siegel  et al. GCN
Circ. 11622), from 54 s to 83.0 ks after the  BAT trigger. The data
comprise 6 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. 

The light curve can be modeled with  a broken power-law model with an
initial decay slope of alpha-1 = 3.25 (+0.40, -0.66) and a break at
Tbreak-1 = 380 (+120, -55) s. After this break the afterglow decays
with a slope of alpha-2 = 1.03 (+0.12, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.04 (+0.26, -0.29). The
best-fitting absorption column is  3.1 (+0.5, -1.0) x 10^21 cm^-2, in
excess of the Galactic value of 2.8 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.3 x 10^-11 (7.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+0.5, -1.0) x 10^21 cm^-2
Galactic foreground: 2.8 x 10^20 cm^-2
Excess significance: 5.3 sigma
Photon index:      2.04 (+0.26, -0.29)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00444230.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110128A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11628
SUBJECT: GRB 110128A: Fermi GBM detection
DATE:    11/02/03 17:21:00 GMT
FROM:    Vandiver Chaplin at UAH/Fermi-GBM  <chapliv@email.uah.edu>

V.Chaplin (UAH) reports on behalf of the Fermi GBM Team:
"At 01:44:36 UT on 28 January 2011, the Fermi Gamma-ray Burst Monitor  
(GBM)
triggered on located GRB 110128A (trigger 317871878 /110128.073).
This burst also triggered Swift,BAT (Grupe et al., GCN 11603).
The GBM on-ground calculated location is consistent with the Swift  
position.
The Swift localization had an angle of 45 degrees from the LAT  
boresight at
the GBM trigger time.

The GBM light curve shows a single pulse with a duration (T90)
of about 12 s (50-300 keV) from approximately T0-5.8 s.
The time-averaged spectrum from T0-8 to T0+6 s
is best fit by a simple power-law with index is -1.5 +/-0.1.
The 1-sec peak flux in the band 10-1000 keV and starting at
time T0-2 s is 1.6 +/- 0.2 ph/s-cm^2.

The fluence (10-1000 keV) in this time interval is (1.5 +/- 0.2)E-06  
erg/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110205A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11629
SUBJECT: GRB 110205A: Swift detection of a burst with an optical candidate
DATE:    11/02/05 02:17:32 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), M. M. Chester (PSU), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), C. J. Saxton (UCL-MSSL),
M. H. Siegel (PSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
M. Stamatikos (OSU/NASA/GSFC), C. A. Swenson (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 02:02:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110205A (trigger=444643).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 164.589, +67.516 which is 
   RA(J2000) = 10h 58m 21s
   Dec(J2000) = +67d 30' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT lightcurve shows activity
with multiple peaks until at least T+300 seconds, with a
peak count rate of 4500 counts/s (15-150 keV) at T+210 s. 

The XRT began observing the field at 02:05:16.8 UT, 155.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 164.6321, +67.5230 which is equivalent to:
   RA(J2000)  = 10h 58m 31.70s
   Dec(J2000) = +67d 31' 22.7"
with an uncertainty of 6.2 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 164 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
   RA(J2000) = 10:58:31.12 = 164.62965
   DEC(J2000) = +67:31:31.2 = 67.52532
with a 90%-confidence error radius of about 0.63 arc sec. This position is 9.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.71 with a 1-sigma error of about 0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is A. P. Beardmore (apb AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11630
SUBJECT: GRB 110205A: TAROT Calern observatory optical detection
DATE:    11/02/05 02:21:42 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (CESR-OMP), Gendre B. (ASDC), Lass M. (UWA),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 110205A detected by SWIFT
(trigger 444643) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 90.6s after the GRB trigger.
The elevation of the field decreased from
65 degrees above horizon and weather conditions
were good.

We detect a new source in the error box given by SWIFT
We detected the candidate couterpart mentioned
by Beardmore et al. (GCNC 11629) at the following
position (+/- 1 arcsec):

RA(J2000) = 10h 58m 31.25s
DEC(J2000) +67d 31' 31.4"

OT optical brightness increased until R~16.7
about 225s after GRB. Then it decreases.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB110205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11631
SUBJECT: GRB 110205A: ROTSE-III, Optical Counterpart is flaring to ~14 mag
DATE:    11/02/05 02:39:21 GMT
FROM:    Brad Schaefer at LSU  <schaefer@grb.phys.lsu.edu>

B. E. Schaefer (Louisiana State), H. Flewelling (IfA/Hawaii), W. 
Rujopakarn (Steward), T. Guver (U Arizona), report on behalf of the ROTSE 
collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
110205A (Swift trigger 444643). The first image was at 02:04:03.4 UT, 82.0
s after the burst (8.4 s after the GCN notice time). The unfiltered images
are calibrated relative to USNO A2.0. On the first images, we detect a
17.0 magnitude source with coordinates:

     10:58:31.11      +67:31:31.91    (J2000), with positional uncertainty 
of 1" or better

start UT     mag     mlim(of image)
----------------------------------
02:06:00.5     17.0     17.6 


This source is at the position of the Swift XRT and UVOT transients, and
not visible in DSS (second epoch), 2MASS or the MPChecker database.  On
our first two sets of ten images, the source is faint, near our limit,
while for our third and fourth coadded images the source has significnatly
brightened by over two magnitudes, apparently to magnitude around 13.9.

Continuing observations are in progress. 


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11632
SUBJECT: GRB 110205A: TAROT Calern observatory detection of an optical flare
DATE:    11/02/05 02:47:49 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (CESR-OMP), Gendre B. (ASDC), Lass M. (UWA),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:

We continue to acquire images the field of GRB 110205A
(cf. Klotz et al. GCNC 11630). After a first peak of
brightness R~16.7 at t~225s, the flux decreased at R~18
about 360s after the trigger.

Then, the brightness increased dramatically and
reached R~14.1 at t~1150s. Now the flux decreases
slowly: R~15.0 at t~1800s.


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11633
SUBJECT: GRB 110205A: Liverpool Telescope Afterglow Confirmation
DATE:    11/02/05 02:54:32 GMT
FROM:    Carole Mundell at ARI, JMU,Liverpool  <cgm@astro.livjm.ac.uk>

C.G. Mundell, R.J. Smith, Z. Cano (ARI, LJMU) report on behalf of a larger
collaboration:

The Liverpool Telescope began automatically observing Swift GRB 110205A
(Beardmore et al. GCN 11629) with the RINGO2 polarimeter.

Subsequent automatic imaging detects the afterglow candidate reported by
Beardmore et al., Klotz et al. (GCN 11630) and Schaefer et al. (GCN 11631) at:

RA=10:58:31.1 , Dec=+67:31:30.9 (J2000) +/-0.2"

with preliminary magnitude R=16.06 mag (wrt USNO B1) at t=924 secs.

Observations have stopped due to bad weather.


GRB_name: GRB110205A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11634
SUBJECT: GRB 110205A:  Swift/UVOT Confirmation of Flaring Afterglow
DATE:    11/02/05 05:06:33 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester(PSU) and A. P. Beardmore report on behalf of the
Swift/UVOT team:

The Swift/UVOT obtained three finding chart exposures of the field of
GRB 110205A (A. P. Beardmore et al., GCN Circ. 11629) which show the
brightening reported by Klotz et al. (GCN Circ. 11630 and 11632) and
Schaefer et al. (GCN Circ. 11631).  Preliminary magnitudes using the
UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) are:

Filter         T_start(s)   T_stop(s)      Exp(s)    Mag     Mag_err
white_FC       164           314           150       18.71   0.15
u_FC           321           571           250       18.17   0.15
white_FC       875          1025           150       15.4    0.4

Observations are continuing.


GRB_name: GRB110205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11635
SUBJECT: GRB 110205A: Possible Lick/Kast redshift
DATE:    11/02/05 06:30:21 GMT
FROM:    Jason Prochaska at UCO/Lick Obs  <xavier@ucolick.org>

R. da Silva (UCO/Lick), M. Fumagalli (UCO/Lick), G. Worseck
(UCO/Lick), and X. Prochaska (UCO/Lick) report on behalf of GRAASP:

"We have observed GRB 110205A with the Kast
dual spectrometer on the 3m Lick telescope for a series of
three 1800s exposures starting at UT 04:47 under variable
conditions and at high air mass.

We observe a significant absorption feature (EW > 100mA) at
~3600Ang which we interpret as a z~1.98 DLA associated with
the GRB host.  We identify additional absorption features at
~3875A and 3980A which are roughly consistent with OI 1302
and CII 1334 transitions at the coincident redshift.

On the other hand, we do not detect a significant feature at CIV
nor any significant features redward of ~6000Ang where we
would expect FeII 2344, 2374, and 2382 absorption."

Further analysis is in progress.


GRB_name: GRB110205A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11636
SUBJECT: GRB 110205A: PAIRITEL NIR Afterglow Detection
DATE:    11/02/05 06:30:31 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan, C. R. Klein, and J. S. Bloom (UC Berkeley) report:

We observed the field of GRB 110205A (Beardmore et al., GCN 11629)
with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations
began at 2011-Feb-05 05h14m03s UT, ~3.2 hours after the Swift trigger.
 In  mosaics (effective exposure time of 0.50 hours) taken
simultaneously in the J, H, and Ks filters, we detect a source at the
position of the optical afterglow (Klotz et al., GCN 11630; Schaefer
et al., GCN 11631; Mundell et al., GCN 11633).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
3.59       0.50     J     16.74  0.05
3.59       0.50     H     15.81  0.05
3.59       0.50     Ks    15.19  0.07

All magnitudes are given in the Vega system, calibrated to 2MASS. No
correction for Galactic extinction has been made to the above reported
values.  Observations are continuing.


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11637
SUBJECT: GRB 110205A: GRAS005 optical observations
DATE:    11/02/05 07:29:33 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:

GRAS 005 (Global-Rent-a-Scope, Mayhill, New Mexico) Takahashi Epsilon
250 10" FL 850 mm and SBIG ST-10XME camera were used to detect
GRB 110205A optical afterglow. The observations were started at
2011-02-05 02:56:38 (UT) and stopped at 2011-02-05 04:24:38 (UT). Four
unfiltered and four photometric R observations with 300s and 600s exposure
times were made. The afterglow was detected at following position
RA 10 58 31.16 and DEC +67 31 31.1 consistent those given by Klotz A.
et al. (GCN 11630) to within positional errors.

The following magnitudes were obtained from the observations using
NOMAD1 1574-0155978 (R = 16.100) as the comparison:

Tmid(s)+T0 Filter        Exp (sec)     Mag      Mag err   Limit
3537           unfilt        600             16.3         0.1         19.7    
4249           Rc            600             16.5         0.1         18.9
5327           unfilt        300             16.8         0.1         19.7
5858           Rc            600             17.0         0.1         18.9
6379           Rc            300             17.3         0.1         18.9
6903           unfilt        600             17.3         0.1         19.7
7993           Rc            300             17.6         0.1         18.9
8367           unfilt        300             17.6         0.1         19.7

A jpg image of the 600sec clear filter observation is available at the following URL link:
http://cutenews.kassiopeia.net/data/upimages/GRB110205A.jpg


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11638
SUBJECT: GRB 110205A: FAST Redshift
DATE:    11/02/05 07:57:29 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), J. L. Hora (CfA), and J. S. Bloom (UC Berkeley)
report on behalf of a larger collaboration:

We obtained a pair of spectra of the optical afterglow of GRB 110205A
(Beardmore et al., GCN 11629) with the FAST spectrograph mounted on the
FLWO 1.5 m telescope.  Observations began at 6:27 UT (~ 4.5 hours after
the burst) and cover the wavelength range from 3500-7400 A.

As reported by da Silva et al (GCN 11635), the spectrum exhibits a
prominent DLA absorption feature; however, we observe this feature at a
slightly larger wavelength (~ 3900 A).  We further identify a series of
narrow absorption features, including Si II, Si II*, C IV, and Al II, at a   
common redshift of z=2.22.  The detection of Si II*, together with the DLA
system, strongly suggest this is the host galaxy of GRB 110205A.


GRB_name: GRB110205A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11639
SUBJECT: GRB 110205A: Enhanced Swift-XRT position
DATE:    11/02/05 08:44:48 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.

Using 3847 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 110205A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 164.62969, +67.52521 which is equivalent  
to:

RA (J2000): 10h 58m 31.13s
Dec (J2000): +67d 31' 30.8"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11640
SUBJECT: GRB 110205A: NOT redshift confirmation
DATE:    11/02/05 08:49:25 GMT
FROM:    Annalisa De Cia at U of Iceland  <annalisa@raunvis.hi.is>

Paul Vreeswijk (U. Iceland), Paul Groot (Radboud U. Nijmegen),
Philip Carter (U. Warwick), Dong Xu (WIS), Annalisa De Cia, P.
Jakobsson (U. Iceland) and Johan Fynbo (DARK) report on behalf
of a larger collaboration:

We have observed the field of GRB 110205A (Beardmore et al., GCN
11629) with the 2.5m NOT telescope at Roque de los Muchachos
Observatory (La Palma, Spain) equipped with ALFOSC starting at
3:25 UT (1.4h after the burst). Despite thick clouds, the
optical afterglow is clearly detected at R ~ 16.7 (as compared
to nearby USNO-B1.0 stars).

Preliminary reduction of the subsequent spectroscopic
observations shows a clear DLA and several metal absorption
lines (OI/OI*, CII/CII*, CIV, AlII, FeII) at a common redshift
z=2.22, confirming the redshift measurement by Cenko et al. (GCN
11638).


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11641
SUBJECT: GRB 110205A: optical flare confirmation
DATE:    11/02/05 08:54:23 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>  

M. Andreev, A. Sergeev (Terskol Branch of Institute of Astronomy), A.
Pozanenko (IKI) on behalf of larger GRB follow up collaboration report:

We observed field of the Swift  GRB 110205A (Beardmore et al, GCN 11629)
with Zeiss-600 telescope of Mt.Terskol observatory in R,V filters starting
on Feb. 05 (UT) 02:16.  We clearly detect optical afterglow  (Beardmore et
al, GCN 11629, Klotz et al, GCN 11630, Schaefer  et al, GCN 11631, Mundell
et al, GCN 11633) and confirm the optical flare at ~ 1140 s  (Schaefer et
al, GCN 11631, Klotz et al, GCN 11632, Chester et al, GCN 11634) with
maximal brightness R ~ 13.7.

The finding chart and preliminary light curves can be found at
http://grb.rssi.ru/GRB110205A/


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11642
SUBJECT: GRB 101225A is likely at z~0
DATE:    11/02/05 10:52:36 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester) report for a
larger collaboration:

We obtained imaging of GRB 101225A (Racusin et al. GCN 11493)  with
GMOS on Gemini North on 5 Feb 2011. At this epoch we obtained a
total of 2400s in a narrow band H-alpha filter (centered a z~0) and
900s in the r-band.

The afterglow is weakly detected in the H-alpha image, but not in the
contemporaneous r-band imaging. This suggests substantial spectral
evolution from the early-time spectroscopy (Chornock et al. GCN
11507), and that line emission is now contributing significantly
to the emission between 6000-7000A.

Given the absence of any host galaxy, and the extremely unusual
characteristics of this event, the most natural explanation is that
we are detecting Ha at z~0 from some class of high-energy
transient. If that is the case, three possible locations seem most
likely:

(a) it could be a source within the Milky Way, sufficiently far
away that the progenitor was undetected in prior imaging,

(b) it could be in the far halo of M31 at a distance of at least
~115 kpc

(c) it could be associated with the distant Local Group dwarf
spheroidal galaxy Andromeda XVIII, which itself is located ~1.4 Mpc
from us, but is only ~12 kpc from the line of sight to 101225A.

We note that the early optical and X-ray emission (in particular
the ratio of the two) remain extremely unusual for known Galactic 
transients.

We thank the staff of Gemini North for the rapid and effective
execution of these observations.


GRB_name: GRB110205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11643
SUBJECT: GRB 110205A: LOAO B/R Observation
DATE:    11/02/05 11:53:19 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

  Myungshin Im (CEOU/SNU), and Yuji Urata (NCU) on behalf
  of a larger collaboration

   We are taking images of the field around GRB 110205A (GCN 11629)
  in B and R filters using the 1.0m telescope at Mt. Lemmon, AZ, USA,
  starting at 2011 February 5, 05:19:11 UT (roughly 3.28 hrs
  after the burst alert).

    We clearly identify the afterglow (GCN 11630 et al.) in all the
  image taken so far..
   The first image of the observation shows that the afterglow
  is at R = 18.0 +- 0.1 (Vega), calibrated against a star in the
  USNO B-1 catalog at RA=10:58:34.2 and Dec=+67:31:45.3.

   The observation and the further analysis of the data are
  onging. We thank the LOAO operator, Jae-Hyuck Youn, for his assitance
  of the observation.


GRB_name: GRB110205A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11644
SUBJECT: GRB 110205A: Swift-XRT refined Analysis
DATE:    11/02/05 13:47:05 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

A. P. Beardmore (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 14 ks of XRT data for GRB 110205A (Beardmore  et al.
GCN Circ. 11629), from 145 s to 30.7 ks after the  BAT trigger. The
data comprise 737 s in Windowed Timing (WT) mode (the first 9 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by
Beardmore et al. (GCN. Circ 11639).

The light curve comprises a number of flares (at ~T0+145 s, T0+175 s to
T0+275 s, T0+615 s) followed by a power-law decay. The late-time light
curve (from T0+5.1 ks) can be modelled with  a power-law decay with a
decay index of alpha=1.63 (+/-0.10).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.420 (+/-0.020). The
best-fitting absorption column is  4.2 (+/-0.6) x 10^21 cm^-2, at a
redshift of 2.22, in addition to the Galactic value of 1.6 x 10^20
cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index
of 1.99 (+0.08, -0.07) and a best-fitting absorption column of 3.5
(+1.6, -1.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum  is 3.7 x 10^-11
(4.2 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.6 x 10^20 cm^-2
Intrinsic column:    3.5 (+1.6, -1.5) x 10^21 cm^-2 at z=2.22
Photon index:      1.99 (+0.08, -0.07)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00444643.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11645
SUBJECT: GRB 110205A: Newcastle Observatory Optical Observations
DATE:    11/02/05 15:37:38 GMT
FROM:    Michael Cook at Newcastle Obs.  <michaeljcook@rogers.com>

Michael J. Cook, Newcastle Observatory report:

On 5 February UT, the field of GRB 110205A detected by SWIFT (trigger 444643) 
was observed, beginning approximately 49 minutes after the GRB trigger, with the 
Newcastle Observatory 0.4 meter robotic telescope, located in Newcastle, 
Ontario, Canada (Bortle Class 4-5 sky).

Observations were made under transparent skies, but with poor seeing.  Weather 
was good with an ambient temperature of -4C.  No Moon was present.

Automatic imaging in the V-band detected the afterglow candidate reported by 
Beardmore et al., Klotz et al. (GCN 11630) at:

RA 10: 58: 31.34 DEC +67 31 31.4 (J2000)

A 180s calibrated image gives a preliminary magnitude of 15.41 (V-band).
The magnitude is estimated with the nearby NOMAD1 star 1574-0155894 (Vmag 
15.240)

A time-series was taken from 02:52:09 to 07:23:05 and further analysis is in 
progress.

This message is quotable in publications.


GRB_name: GRB110205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11646
SUBJECT: GRB 110205A: Swift-BAT refined analysis
DATE:    11/02/05 16:32:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

GRB 110205A: Swift-BAT refined analysis
 
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to ~T+2000 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110205A (trigger #444643)
(Beardmore, et al., GCN Circ. 11629).  The BAT ground-calculated position is
RA, Dec = 164.603, 67.533 deg, which is 
   RA(J2000)  =  10h 58m 24.8s 
   Dec(J2000) = +67d 31' 57.1" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 29%.
 
The mask-weighted light curve shows many overlapping peaks with a general
slow rise starting at ~T-120 sec, with the tallest peak at ~T+210 sec, and
ending at ~T+1500 sec.  T90 (15-350 keV) is 257 +- 25 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-129 to T+377 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.80 +- 0.04.  The fluence in the 15-150 keV band is 1.7 +- 0.0 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+210.44 sec in the 15-150 keV band
is 3.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/444643/BA/


GRB_name: GRB110205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11647
SUBJECT: Observations GRB 110205A
DATE:    11/02/05 16:39:26 GMT
FROM:    Francois Kugel at Obs.Chante-Perdix,04 Banon,Fr  <fkugel@wanadoo.fr>

Francois Kugel at Obs.Chante-Perdix,04 Banon,Fr

Observer : C. RINNER; F. KUGEL
We imaged the field of GRB 110205A detected by SWIFT(trigger 444643) with the
0.5-m F/3 reflector + ccd kai 11k (No filter).
The observations started at 04:30:52 (UT)
The elevation of the field decreased from 54 degrees above horizon and weather
conditions were good.
We clearly identify the afterglow and the flux decreases slowly.

USNO-SA 2.0 R
 Exp  : hh:mm:ss
 180s : 04:32:22 (UT) = 10h58m31.149s +67Â°31'30.89''    17.44 +/-0.08
 180s : 04:48:32 (UT) = 10h58m31.173s +67Â°31'30.88''    17.84 +/-0.16
 120s : 05:38:46 (UT) = 10h58m31.173s +67Â°31'30.86''    18.09 +/-0.35
 120s : 05:51:26 (UT) = 10h58m31.169s +67Â°31'30.71''    17.99 +/-0.64

Image & measurement : http://astrosurf.com/obsdauban/pages/GRB110205A.html


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11648
SUBJECT: GRB 110205A: Lulin optical observations and temporal decay index
DATE:    11/02/05 17:33:40 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Yuji Urata, Chia-Jung Chuang (NCU) and Kuiyun Huang (ASIAA)
on behalf of EAFON

"We are monitoring the optical afterglow of GRB110205A (GCN 11630,
11631) in g', r' and i' filters using the 1.0m telescope at Mt. Lulin,
Taiwan. The observations are started at 2011 February 5, 13:02 UT.  
Based on our r'-band photometry against with the SDSS catalog, the
temporal decay index between 40000 and 52740 sec after the burst is
about 1.9.  The brightness in r'-band at 52740 sec after the burst is
20.64 +/-0.05 mag.

The further monitoring observation and analysis are ongoing.


GRB_name: GRB110205A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11649
SUBJECT: GRB 110205A: Swift/UVOT Continuing Observations
DATE:    11/02/05 17:55:39 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester (PSU) and A. P. Beardmore (U Leicester) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110205A
164 s after the BAT trigger (Beardmore et al., GCN Circ. 11629).
The peak near 1000s reported by Klotz et al. (GCN Circ. 11632) and
Andreev et al. (GCN Circ. 11641) is seen in the UVOT optical filters
and one of the UV filters (uvw1), consistent with the reported
redshift z=2.22 (Cenko et al., GCN Circ. 11638 and Vreeswijk et al.,
GCN Circ. 11640).  The weak detections (2-3 sigma) in uvw2 are
probably due to the filter's extended sensitivity in the red.
After 5000s, the estimated temporal slope in the white filter is 1.6.
Preliminary photometry using the UVOT photometric system (Poole et al.
2008, MNRAS, 383, 627) for the finding chart (FC) and subsequent
exposures is:


FILTER     TSTART   TSTOP    MAG    +/-   UL(2o)
white_FC     164.0    313.8  18.79  0.07
white        601.9    621.7  17.01  0.08
white        774.6    794.4  15.74  0.06
white_FC     875.4   1025.1  15.36  0.04
white       1181.0   1375.8  15.39  0.05

v            652.0    671.8  15.76  0.11
v            824.3    844.1  14.98  0.08
v           1056.5   1251.8  14.68  0.06

b            577.5    597.3  17.10  0.12
b            750.3    770.1  15.77  0.07
b           1154.7   1351.5  15.33  0.05

u_FC         321.9    571.7  18.24  0.09
u            725.4    745.2  15.59  0.09
u           1130.5   1325.1  15.02  0.06

uvw1         701.0    720.8  18.23  0.41
uvw1        1106.0   1300.8  17.09  0.17

uvm2         676.3   1276.1               19.89
uvm2        1430.1   1795.8               19.60

uvw2         627.4   1226.2  19.89  0.49
uvw2        1381.4   1747.0  19.28  0.41

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11650
SUBJECT: GRB110205A:  SMA 1.3mm Observations
DATE:    11/02/06 01:03:33 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

Glen Petitpas (SMA), Ashley Zauderer, Edo Berger, Nimesh Patel, Erin 
Brassfield (Harvard/CfA), Jen Miller, Anil Dosaj (SMA) report:

We observed GRB110205A (GCN #11629) with the Submillimeter Array (SMA) 
at 1.3 mm (225 GHz) starting 1.3 hours after the burst for a duration of 
6 hours.  No source is detected in coincidence with the optical 
afterglow (GCN #11629).  With a combined 8 GHz of bandwidth, the 
resulting 3-sigma upper limit is 1.65 mJy.


GRB_name: GRB110205A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11651
SUBJECT: GRB110205A: MITSuME Okayama Optical Observation
DATE:    11/02/06 16:19:56 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110205A (Beardmore et al., GCNC 11629)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2011-02-05 10:37:55 UT (~8.6 hours after
the burst). We detected the previously reported afterglow
(Klotz et al., GCNC 11630; Schaefer et al., GCNC 11631) in all the
three bands.


Photometric results and are listed below. We used SDSS catalog for flux
calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.39965    11:38:11   6120.0    >20.1         19.4  0.2    18.5  0.2
0.48327    13:38:36   6300.0     20.6   0.3   20.4  0.3    19.7  0.3
0.56675    15:38:49   6300.0     21.2   0.4   19.8  0.2    19.7  0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110205A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11652
SUBJECT: GRB110205A: MITSuME  Ishigakijima Optical Observation
DATE:    11/02/06 16:23:27 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 110205A (Beardmore et al., GCNC 11629)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2011-02-05 12:15:24 UT (~10.2 hours after
the burst). We detected the previously reported afterglow
(Klotz et al., GCNC 11630; Schaefer et al., GCNC 11631) in all the
three bands.

Photometric results are listed below. We used SDSS catalog for flux
calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.45691    13:00:38    4500.0    21.0   0.2   20.2   0.1   19.8   0.2
0.76876    20:29:42    4620.0    21.5   0.2   20.8   0.1   20.2   0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11653
SUBJECT: GRB 110205A : Lulin optical observation
DATE:    11/02/06 17:09:26 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Yuji Urata, Chia-Jung Chuang (NCU) and Kuiyun Huang (ASIAA)
on behalf of EAFON report

"We made a further optical afterglow observation with r'-band using
the Lulin 1m telescope. The stacked image made from 7 frames with 600s
exposure shows the afterglow clearly.  The brightness calibrated
against with the SDSS catalog is r'=22.49+/-0.12 at 1.53 days after
the burst. This is consistent with the extrapolation of the simple
power-law decay with the temporal index of about 1.9 from our previous
report (GCN 11648)."


GRB_name: GRB110206A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11654
SUBJECT: GRB 110206A: a long GRB detected by INTEGRAL
DATE:    11/02/06 19:07:49 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

S.Mereghetti, A.Paizis (IASF-Milano), D.Gotz (CEA-Saclay), J. Borkowski 
(CAMK, Torun), E. Bozzo, C.Ferrigno, M. Beck (ISDC, Versoix),
on behalf of the IBAS Localization Team  report:

a  gamma ray burst lasting about 20 s has been detected by IBAS in the 
IBIS/ISGRI data at 18:08:05  UT of February 6.

Its refined coordinates (J2000) are:

  RA:  92.35535  [degrees]
  DEC: -58.8075  [degrees]

with an uncertainty of 2  arcmin (90% c.l.).

A preliminary analysis gives  a  20-200 keV peak flux of
about 1 ph/cm2 s  (1 s integration time)

A plot of the light curve will be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB110205A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11655
SUBJECT: GRB 110205A: Lightbuckets Optical Observations
DATE:    11/02/06 22:19:34 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

T. N. Ukwatta (MSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
N. Gehrels (GSFC), J. Linnemann (MSU), K. Tollefson (MSU),
and U. Abeysekara (MSU)


We observed the Swift GRB 110205A (Beardmore et al., GCN 11629)
with the Lightbuckets 0.61m rental telescope LB-0001 in Rodeo,
NM, USA. Under good weather conditions, two observations
were carried out in the Luminance and R filter starting
2011-02-05 at 07:45:58 UT (~ 5.7 hours after the GRB trigger)
and 09:39:21 UT (~7.6 hours after the GRB trigger). Another
followup observation was performed on R filter starting
2011-02-06 at 09:29:04 UT (~1.31 days after the trigger)
under acceptable weather conditions.

The burst afterglow is clearly detected in the first two
observations and estimated magnitudes are given below:

Time after trigger       Exposure (s)   Filter     Magnitude

5.7  hours (0.24 days)     1 x 300        Lum     19.0 +/- 0.1
7.6  hours (0.31 days)     1 x 300         R      19.6 +/- 0.2
31.4 hours (1.31 days)     2 x 300         R      > 20.1

The afterglow, not corrected for Galactic extinction, is
calibrated against the USNO-B1.0 catalog.

We acknowledge the helpful assistance of the Lightbuckets staff,
in particular Stephen G. Cullen.


GRB_name: GRB110206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11656
SUBJECT: GRB 110206A: TAROT La Silla observatory optical observations
DATE:    11/02/07 07:51:16 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (CESR-OMP), Gendre B. (ASDC), Lass-Bourez M. (UWA)
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 110206A detected by INTEGRAL
(trigger 6088, Mereghetti et al. 2011 GCNC 11654)
with the TAROT robotic telescope (D=25cm) located at
the European Southern Observatory, La Silla observatory,
Chile.

The observations started 6.3h after the GRB trigger
(beginning of the night). The elevation of the field
increased from 57 degrees above horizon and weather
conditions were good.

We co-added a series of exposures
t0+6.3h to t0+7.3h : R > 19.3

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=267.5629 lat=-28.2892
and the galactic extinction in R band is 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB110206A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11657
SUBJECT: GRB 110206A: Swift detection of a probable X-ray afterglow
DATE:    11/02/07 10:10:29 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

We have analysed 4.2 ks of XRT data for the INTEGRAL-detected GRB
110206A (Mereghetti et al. et al. GCN Circ. 11654), from 26.9 ks to
34.9 ks after the  INTEGRAL trigger. The data are entirely in Photon
Counting (PC) mode. Inside the INTEGRAL error circle we find a single,
uncatalogued X-ray source. Using 2309 s of PC mode data and 2 UVOT
images, we find an enhanced XRT position (using the XRT-UVOT alignment
and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
92.33400, -58.80700 which is equivalent to:

RA (J2000): 06h 09m 20.17s
Dec(J2000): -58d 48' 25.3"

with an uncertainty of 1.9 arcsec (radius, 90% confidence). The light
curve is consistent with a constant source of mean count rate 6.8e-02
ct/sec: a power-law fit gives an index of 0.0 (+/-1.1). Given the
brightness of the source (which is more than 3-sigma above the
Rosat All Sky Survey detection limit), and the large uncertainty on the
decay index, we propose this source as the probable afterglow of GRB
110206A, however further observations are needed to confirm this.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.12 (+0.27, -0.30). The
best-fitting absorption column is  9.5 (+4.5, -6.4) x 10^20 cm^-2,
consistent with the Galactic value of 3.1 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.6 x 10^-11 (4.7 x
10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:      9.5 (+4.5, -6.4) x 10^20 cm^-2
Galactic foreground: 3.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.12 (+0.27, -0.30)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020156.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110207A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11658
SUBJECT: GRB 110207A: Swift detection of a burst
DATE:    11/02/07 11:26:09 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

O. M. Littlejohns (U Leicester), A. P. Beardmore (U Leicester),
S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
N. P. M. Kuin (UCL-MSSL), P. T. O'Brien (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA),
A. Rowlinson (U Leicester), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 11:17:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110207A (trigger=444912).  Swift could not slew to the
burst due to a Moon constraint. 
The BAT on-board calculated location is 
RA, Dec 12.542, -10.806 which is 
   RA(J2000) = 00h 50m 10s
   Dec(J2000) = -10d 48' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex multi-peaked
structure with a duration of about 40 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~0.5 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 13:20 UT on 2011 February 08. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is O. M. Littlejohns (oml2 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110205A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11659
SUBJECT: Konus-Wind observation of GRB 110205A
DATE:    11/02/07 11:34:21 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team report:

The long GRB 110205A (Swift-BAT trigger #444643: Beardmore et al., GCN
11629; Markwardt et al., GCN 11646) was detected by Konus-Wind in the
waiting mode.

The burst light curve shows a multipeaked pulse started at ~T0(BAT) with 
a total duration of ~330 s. There is a weak pulse at ~T0(BAT)-1360 s 
(seen by the same detector which observed GRB 110205A; the detection 
significance is ~4.5 sigma in the G1+G2 (20-360 keV) band; the pulse 
duration is ~25 s), which might be a burst precursor. There is a hint of 
a weak soft tail seen up to ~T0+1200 s.

As observed by Konus-Wind, the burst had a fluence of (3.66 +/- 
0.35)x10^-5 erg/cm2 and a 3-s peak flux measured from T0+211.6 s
of (5.1 +/- 0.7)x10^-7 erg/cm2/s (both in the 20 - 1200 keV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0 s to
T0+330 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.52 +/- 0.14, and Ep = 222 +/- 74 keV.

Assuming z = 2.22 (Cenko & Hora, GCN 11638; Vreeswijk et al. GCN 11640) 
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, 
Omega_Lambda = 0.73, the isotropic energy release E_iso is (1.36 +/- 
0.13)x10^54 erg, the peak luminosity (L_iso)_max is (5.9 +/- 0.8)x10^51 
erg/s, and Ep_rest is 715 +/- 238 keV.

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB110205A/


GRB_name: GRB110207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11660
SUBJECT: GRB 110207A: MASTER prompt and early optical observations 
DATE:    11/02/07 13:52:28 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

Two MASTER II  robotic telescopes (MASTER-Net: http://observ.pereplet.ru) 
located in  Amur-Blagoveschensk  and Tunka-Baykal was pointed to the 
GRB110207A 65 and 30 sec after GRB time correspondingly. On our first (10s exposure) 
set we haven't found optical transient  within SWIFT-BAT error-box 
(Littlejohns et al., GCN Curc 11658).
Because GRB duration is 40 sec, the first images from Tunka is prompt.
The obdervations was done at high zenith distance (>80 degrees).

The 3-sigma upper limit has been about:
-----------------------------------------------------------------------
Start Time     mean time       Exp     Limit   Filter    Site 
after trigger  after trigger   (s)
-----------------------------------------------------------------------
    30s           35s           10      13.0     V+P\/   Tunka-Baykal
    65s           70s           10      14.1     V+P-|  Amur-Blagoveschensk
    65s          747s         1370      17.0     V+P-|  Amur-Blagoveschensk
   1700s        1790s          180      17.4      R       Tunka-Baykal

------------------------------------------------------------------------

P - is polarization.


The message may be cited.


mailto: lipunov@sai.msu.ru


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11661
SUBJECT: GRB110205A:  CARMA 3mm Observations
DATE:    11/02/07 16:13:16 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

GRB110205A:  CARMA 3mm Observations

Ashley Zauderer, Edo Berger (Harvard) and Dale Frail (NRAO) report:

We observed GRB110205A (GCN 11629) with CARMA at 3 mm (93 GHz) starting 
2.1 hours after the burst for a total on-source time of 2.3 hours.  No 
millimeter emission is detected in coincidence with the optical 
afterglow position (GCN 11629) to a 3-sigma limit of 0.6 mJy.

We thank the CARMA observatory staff for support of these observations.


GRB_name: GRB110206A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11662
SUBJECT: GRB 110206A:  UVOT detection of afterglow candidate
DATE:    11/02/07 17:27:08 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and P. A. Evans (U. Leicester) report on behalf of
the Swift UVOT team:

We have analyzed Swift UVOT observations of the INTEGRAL-detected
GRB 110206A (Mereghetti et al. et al. GCN Circ. 11654).  UVOT  
observations
began 26.9 ks after the INTEGRAL trigger.  The UVOT data reveal a  
faint new
source that does not appear in archival MAST DSS images.  The refined  
UVOT
position of the new source is:

      RA (J2000)  06:09:20.14  =  92.33392 (deg)
     Dec (J2000) -58:48:25.3   =  -58.80703 (deg)

with an estimated uncertainty of 0.8 arcsec (radius, 90% confidence,
statistical + systematic).  This position is within 0.2 arcseconds of  
the
enhanced XRT position (Evans, GCN Circ. 11657) which is well within the
measurement errors.

The source is detected in the uvw1, u, and b filters, while an upper  
limit
was found in uvm2.  The observed magnitudes and 3-sigma upper limits  
using
the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) are:

Filter  T_start(s)  T_stop(s)   Exp(s)     Mag
=============================================================
b        28761       29253       480   21.00 +/- 0.37
u        27847       34952      1044   20.56 +/- 0.24
uvw1     26941       34783      1771   20.36 +/- 0.26
uvm2     32977       33876       885      > 20.61

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11663
SUBJECT: GRB 110205A: WSRT radio observation
DATE:    11/02/07 17:35:33 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (USRA), C. Kouveliotou (NASA/MSFC), A.P. Kamble
(U of Wisconsin Milwaukee) and R.A.M.J. Wijers (U of Amsterdam)
report on behalf of a larger collaboration:

"We observed the position of the GRB 110205A afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at February 6 19.44 UT to
February 7 07.41 UT, i.e. 1.72 - 2.22 days after the burst (GCN 11629).
We do not detect a radio source at the position of the optical
counterpart (GCN 11633). The three-sigma rms noise in the map around
that position is 105 microJy per beam. The formal flux measurement for
a point source at the position of the optical counterpart is 44 +/- 35 
microJy.

We would like to thank the WSRT staff for scheduling and obtaining these
observations."


GRB_name: GRB110207A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11664
SUBJECT: GRB 110207A: Swift-BAT refined analysis
DATE:    11/02/07 19:22:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
O. M. Littlejohns (U Leicester), C. B. Markwardt (GSFC), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110207A (trigger #444912)
(Littlejohns, et al., GCN Circ. 11658).  The BAT ground-calculated position is
RA, Dec = 12.540, -10.790 deg, which is 
   RA(J2000)  =  00h 50m 09.5s 
   Dec(J2000) = -10d 47' 23.8" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows at least seven short peaks starting
at ~T-0.1 sec and ending at ~T+20 sec with a long decay extending out
to ~T+110 sec.  T90 (15-350 keV) is 80.3 +- 16.2 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-0.1 to T+108.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.30 +- 0.12.  The fluence in the 15-150 keV band is 1.6 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.11 sec in the 15-150 keV band
is 1.1 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/444912/BA/


GRB_name: GRB110206A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11665
SUBJECT: GRB 110206A:  GROND detection of afterglow candidate
DATE:    11/02/07 21:43:09 GMT
FROM:    Robert Filgas at MPI  <filgas@mpe.mpg.de>

J. Elliott, R. Filgas, T. Kruehler and J. Greiner (all MPE Garching),
report on behalf of the GROND team:

GROND observed the field of the INTEGRAL GRB 110206 (Mereghetti et al.,
GCN# 11654) starting at 00:33 UT on 2011-02-07, which is 6.42 hours
after the trigger. In total, 1.7 hours of imaging was obtained
simultaneously in g'r'i'z'JHK. Within the enhanced XRT error circle
(Evans, GCN #11657), we detect a single point source at

RA (J2000): 06:09:20.04
Decl (J2000): -58:48:24.9

with typical uncertainties of 0.5" in each coordinate. These coordinates
are consistent with the source detected by UVOT (Hoversten & Evans, GCN#
11662).
At a midtime of 6.7 hours after the trigger we measure a preliminary AB
magnitude of r' = 21.2 +/- 0.1 based on the GROND zeropoint.
The source is detected in all GROND filters, which implies a redshift
constraint of z < 4.

Within the observational errors, no variability is evident in the
timeframe of the GROND observations, and hence we cannot claim the
association of the source with GRB 110206A at the current stage.


GRB_name: GRB110205A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11666
SUBJECT: GRB 110205A - Continued PAIRITEL NIR Observations
DATE:    11/02/07 22:24:21 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan and J. S. Bloom (UC Berkeley) report:

We continued to observe the location of the NIR afterglow of GRB
110205A (Morgan et al. GCN 11636) with the 1.3m PAIRITEL located at
Mt. Hopkins, Arizona throughout the night of February 5th and again on
2011-02-06.  The afterglow continued to be well detected throughout
the first night.

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
4.63       0.64     J     17.01  0.05
4.63       0.64     H     16.26  0.06
4.63       0.64     Ks    15.43  0.07

5.63       0.64     J     17.23  0.06
5.63       0.64     H     16.37  0.07
5.63       0.64     Ks    15.71  0.09

6.63       0.64     J     17.46  0.07
6.63       0.64     H     16.71  0.09
6.63       0.64     Ks    16.0   0.1

7.64       0.64     J     17.9   0.1
7.64       0.64     H     17.0   0.1
7.64       0.64     Ks    16.3   0.2

8.64       0.64     J     17.8   0.1
8.64       0.64     H     17.3   0.2
8.64       0.64     Ks    16.3   0.2

9.64       0.64     J     18.2   0.2
9.64       0.64     H     17.5   0.3
9.64       0.64     Ks    16.8   0.3

10.6       0.64     J     18.4   0.2
10.6       0.64     H     17.6   0.3
10.6       0.64     Ks    16.7   0.3

30.7       4.45     J     >20.1  3sig
30.7       4.45     H     >19.0  3sig
30.7       4.45     Ks    >18.3  3sig

The late time decay index is consistent with that seen in the optical
(Urata et al. GCN 11648).  All magnitudes are given in the Vega
system, calibrated to 2MASS. No correction for Galactic extinction has
been made to the above reported values.


GRB_name: GRB110207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11667
SUBJECT: GRB 110207A: TAROT Calern observatory optical observations
DATE:    11/02/07 23:00:01 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (CESR-OMP), Gendre B. (ASDC), Laas-Bourez M. (UWA)
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 110207A detected by SWIFT
(trigger 444912) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 6.62h after the GRB trigger
(beginning of the night). The elevation of the field
decreased from 25 degrees above horizon and weather
conditions were good.

We co-added a series of exposures.
No OT was detected :
t0+6.62h to t0+7.79h : R > 19.8

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=121.8238 lat=-73.6747
and the galactic extinction in R band is 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB110206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11668
SUBJECT: GRB 110206A: SMARTS optical/IR afterglow candidate observations
DATE:    11/02/07 23:35:22 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU) reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained 
optical/IR imaging of the error region of GRB 110206A (GCN 11654, 
Mereghetti et al.) with a mid-exposure time of 6.8 hours post-burst 
(2011-02-07 00:57:41 UT).  Total summed exposure times amounted to 
36 minutes in I and 30 minutes in J.

The source which is the possible optical afterglow of GRB 110206A 
(GCN 11662, Hoversten et al. and GCN 11665, Elliott et al.) is detected 
in our optical image.  Preliminary comparison to Landolt standards stars in 
I and 2MASS stars in J indicates the following I-band magnitude and J-band 
3-sigma upper limit for this source:

time post-burst       I mag             J 3-sigma limit
6.8 hours               20.6+/-0.1      >18.8

Our data do not allow for a test of variability at this time, so we
cannot confirm that this source is the optical afterglow of GRB 110206A.


GRB_name: GRB110206A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11669
SUBJECT: GRB 110206A: Decay of afterglow candidate
DATE:    11/02/08 02:50:25 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

J. Elliott, R. Filgas and J. Greiner (all MPE Garching),
report on behalf of the GROND team:

GROND observed the field of INTEGRAL GRB 110206A (Mereghetti et al., GCN
#11654) again starting at 01:10 UT on 2011-02-08, which is 24.62 hours
after the first epoch. In total 8 minutes of imaging was obtained
simultaneously in g'r'i'z'JHK.

The candidate (GCN 11662, Hoversten et al.,  GCN 11665, Elliott et al. and
GCN 11668, Cobb et al.) has been seen to have decayed by 1.2 magnitudes
suggesting that it is the afterglow of GRB110206A

We measure a preliminary magnitude of the second epoch of r' = 22.4 +/-
0.1 based on the GROND zeropoint.


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11670
SUBJECT: GRB 110205A : HCT optical observations
DATE:    11/02/08 09:28:45 GMT
FROM:    D.K. Sahu at Indian Inst of Astrophysics,Bangalore  <dks@iiap.res.in>

D.K. Sahu and Pepsi Anto (Indian Institute of Astrophysics,
Bangalore) report.
Optical afterglow of the Swift GRB 110205A (Beardmore et al.,
GCN 11629) was observed with the 2m. Himalayan Chandra
Telescope of the Indian Astronomical Observatory, Hanle,
India, under poor sky  condition.  The optical afterglow
was observed in Bessell R filter and was detected in
all the frames.

The preliminary magnitudes of the optical afterglow,
calibrated using NOMAD1 1574-0155978 (R = 16.100)
(Veli-Pekka et al., GCN11637), are as under:
Date  Mid UT Exposure       R mag
05-02-2011 20:50 6 x 180sec  21.11 +/- 0.05
05-02-2011 21:13 3 x 180sec  21.19 +/- 0.08
05-02-2011 22:09 1 x 600sec  21.18 +/- 0.10

This message may be cited.


GRB_name: GRB110207A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11671
SUBJECT: GRB 110207A: Fermi GBM observation
DATE:    11/02/08 16:02:07 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: 

"At 11:17:20.29 UT on 07 February 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110207A (trigger 318770242/ 110207470), which was
also 
detected by the Swift/BAT (Littlejohns et al. 2011, GCN 11658)
The GBM on-ground location is consistent with the Swift position.
 
The angle from the Fermi LAT boresight is 72.8 degrees.

The GBM light curve shows a multi-peaked structure
with a duration (T90) of about 39 s (50-300 keV). 
The time-averaged spectrum from T0-0.256 s to T0+38.912 s is 
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.09 (+0.13/-0.12) and
the cutoff energy, parameterized as Epeak, is 450 (+290/-130) 
keV. The event fluence (10-1000 keV) in this time interval is 
(4.4 +/- 0.6)E-06 erg/cm^2. The 1.024-sec peak photon flux measured 
starting from T0+0.211 s in the 10-1000 keV band 
is 2.3 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary; 
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11672
SUBJECT: GRB 110205A: optical observations in Mondy observatory
DATE:    11/02/08 19:00:44 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova , E. Klunko (ISTP), A. Pozanenko (IKI) on behalf of larger
GRB follow up collaboration report:

We observed the  Swift GRB 110205A (Beardmore et al., GCN 11629) with
AZT-33IK telescope of Sayan observatory (Mondy) on Feb.05 between (UT)
12:06:19 and 20:25:34, and we took several series in R-band with
exposures 60 - 180s.

The optical afterglow  (Beardmore et al., GCN 11629) is clearly
detected on the stacked images.  The photometry calibration performed
against the USNO-B1.0 star 1575-0155390 ((J2000) RA = 10:58:34.20, Dec
= +67:31:45.3), assuming R = 16.7:

T0+      Filter,   Exposure,          OT mag.,  UpperLimit
(mid, d)              (s)

0.43968 R  51x60                     19.88+/-0.04    21.9
0.71912 R  25x120+20x180     20.85+/-0.05    22.8

The power-law decay index during our observation is alpha ~1.8 which
is consistent with the index reported by Urata et al., GCN 11648.

[GCN OPS NOTE(08aug11): Per author's request, the spelling of the EK
author was corrected.]


GRB_name: GRB110208A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11674
SUBJECT: GRB 110208A: Swift detection of a burst
DATE:    11/02/08 21:21:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. Campana (INAF-OAB), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU),
E. Sonbas (GSFC/USRA/Adiyaman Univ.), G. Stratta (ASDC),
C. A. Swenson (PSU) and E. Troja (NASA/GSFC/ORAU) report on behalf of
the Swift Team:

At 21:10:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110208A (trigger=445038).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 22.484, -20.628 which is 
   RA(J2000)  =  01h 29m 56s
   Dec(J2000) = -20d 37' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows one peak
with a duration of about 15 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at 0 sec after the trigger. 

The XRT began observing the field at 21:12:06.5 UT, 80.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 22.46404, -20.59248 which is equivalent
to:
   RA(J2000)  = 01h 29m 51.37s
   Dec(J2000) = -20d 35' 32.9"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 145 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.31
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 84 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.02. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11675
SUBJECT: GRB 110206A: SMARTS optical/IR afterglow decay
DATE:    11/02/08 22:24:32 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU) reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained
optical/IR imaging of the error region of GRB 110206A (GCN 11654,
Mereghetti et al.) with a mid-exposure time of 34.2 hours post-burst
(2011-02-08 04:22 UT).  Total summed exposure times amounted to
36 minutes in I and 30 minutes in J.

In agreement with Elliott et al. (GCN 11669), we observe that the
candidate optical afterglow of GRB 110206A (GCN 11662, Hoversten et al.
and GCN 11665, Elliott et al.) has decayed significantly from our
previous observations (GCN 11668), indicating that this is the optical
afterglow of GRB 110206A.  Preliminary comparison to Landolt standard
stars indicates the following magnitude for the optical afterglow:

time post-burst       I mag
 6.8 hours              20.6+/-0.1
34.2 hours             21.6+/-0.2

This indicates that the decay rate of the burst between ~7 and 34 hours
post burst is alpha ~ 0.6 (where afterglow flux is proportional
to t^-alpha).


GRB_name: GRB110208A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11676
SUBJECT: GRB 110208A: Magellan optical observations
DATE:    11/02/09 03:29:03 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger, W. Fong (Harvard), and J. Mulchaey (OCIW) report:

"We observed the position of GRB 110208A (GCN #11674) with LDSS3 on the
Magellan/Clay 6.5-m telescope on 2011 February 9.022 UT (3.35 hours after
the burst) in the r- and i-band filters.  In single 180 sec exposures in
each filter no object is detected inside the XRT error circle (GCN #11674)
to the limit of the Digitized Sky Survey."


GRB_name: GRB110208A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11677
SUBJECT: GRB 110208A: Swift-BAT refined analysis
DATE:    11/02/09 04:22:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110208A (trigger #445038)
(D'Ella, et al., GCN Circ. 11674).  The BAT ground-calculated position is
RA, Dec = 22.487, -20.561 deg, which is 
   RA(J2000)  =  01h 29m 56.9s 
   Dec(J2000) = -20d 33' 40.5" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a single peak starting at ~T-2 sec,
peaking at ~T+0.5 sec, and ending at ~T+20 sec.  T90 (15-350 keV) is
37.4 +- 7.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.5 to T+40.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.08 +- 0.31.  The fluence in the 15-150 keV band is 2.7 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.46 sec in the 15-150 keV band
is 0.6 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/445038/BA/


GRB_name: GRB110208A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11678
SUBJECT: GRB 110208A: Enhanced Swift-XRT position
DATE:    11/02/09 06:19:23 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 5594 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 110208A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 22.46218, -20.59277 which is equivalent
to:

RA (J2000): 01h 29m 50.92s
Dec (J2000): -20d 35' 34.0"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110208A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11679
SUBJECT: GRB 110208A: Swift-XRT refined Analysis
DATE:    11/02/09 14:42:48 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC) reports on behalf of the Swift-XRT team:

We have analysed 20 ks of XRT data for GRB 110208A (D'Elia  et al. GCN
Circ. 11674), from 64 s to 47.3 ks after the  BAT trigger. The data
comprise 55 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 11678).

The late-time light curve (from T0+4.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.21 (+0.20, -0.18).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.27 (+/-0.25). The
best-fitting absorption column is  1.1 (+0.4, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 2.3 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (4.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+0.4, -0.6) x 10^21 cm^-2
Galactic foreground: 2.3 x 10^20 cm^-2
Excess significance: 3.2 sigma
Photon index:      2.27 (+/-0.25)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00445038.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110207A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11680
SUBJECT: GRB 110207A: Swift-XRT observations
DATE:    11/02/09 14:44:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans and O.M. Littlejohns (U. Leicester) report on behalf of the 
Swift team:

Swift observed the field of GRB 110207A (Littlejohns et al., GCN Circ. 
11658) for 5 ks from T0+99 ks to T0+112 ks; earlier observations were 
impossible due to the proximity of the GRB to the Moon. We find no X-ray 
sources in the BAT field of view, placing a 3-sigma upper limit on the 
afterglow brightness of 7.6e-14 erg/cm^2/sec during this interval 
(0.3-10 keV; assuming a typical GRB spectrum). Due to the proximity of 
the GRB to the Sun, no further observations are planned.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110208A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11681
SUBJECT: GRB 110208A: Potential afterglow from Magellan
DATE:    11/02/09 14:52:13 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger, W. Fong (Harvard), and J. Mulchaey (OCIW) report:

"We inspected our Magellan/LDSS3 r- and i-band images (GCN #11676) at the
location of the refined XRT error circle (GCN #11678). We detect a single
point source in coincidence with the new XRT position in both filters.  The
position of the optical source is (J2000):

RA = 01:29:50.86
DEC = -20:35:33.5

with an uncertainty of about 0.3" in each coordinate.  The i-band magnitude
is about 21.8 mag.  At present we do not have any evidence
for fading of this source."


GRB_name: GRB110205A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11682
SUBJECT: GRB 110205A: Suzaku WAM observation of the prompt emission
DATE:    11/02/09 15:19:09 GMT
FROM:    Satoshi Sugita at Aoyama Gakuin U.  <sugita@phys.aoyama.ac.jp>

S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo),
S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report:

The long GRB 110205A (Swift/BAT trigger #444643 ; Beardmore et al.,
GCN 11629; Beardmore et al., GCN 11639,; Markwardt  et al., GCN 11646)
was detected by the the Suzaku Wide-band  All-sky Monitor (WAM)
which covers an energy range of 50 keV - 5 MeV at 02:02:41 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0+20s,
ending at T0+318s with a duration  (T90) of 248 (+/- 51) seconds.
The fluence in 100 - 1000 keV was 1.33 (+/- 0.23) x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+211s was 1.15 (+/- 0.23) photons/cm^2/s in the same
energy range.

Preliminary result shows that the time-averaged spectrum from T0+20s to
T0+318s is well fitted by a single power-law with a photon index
of 2.12 (+/- 0.17) (chi^2/d.o.f = 82.1/50).
All the quoted errors are at statistical 90% confidence level.

The light curves with 1-sec time resolution for this burst is appeared at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB110208A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11683
SUBJECT: Swift/UVOT observations of GRB110208a
DATE:    11/02/09 19:16:17 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and V. D'Elia (ASI-ASDC) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110208a 85s
s after the BAT trigger (D'Elia, GCN Circ. 11674).  No optical afterglow
consistent with the enhanced XRT position (Evans et al, GCN Circ. 11678)
or the Magellan position (Berger et al., GCN Circ. 11681) is detected in 
the initial UVOT exposures or in the summed ones.
  Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
  exposures and subsequent exposures are:

Filter         T_start(s)   T_stop(s)  Exp(s)   Mag

white_FC           85          240     147  >20.6
white              85        18443    1425  >21.5

u_FC               298         548     246  >20.0
u                  298       30010    3111 > 21.2

v                  628       11030    1190  >20.0
b                  553       24229    2021  >21.4
w1                 703       29283    2919  >21.3
m2                 652       28376    1771  >21.1
w2                 603        6810     393  >20.5

We note that there is a bright galaxy a few arcminutes from
the GRB position.

The values quoted above are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.02 in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB110208A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11685
SUBJECT: GRB 110208A: Magellan confirmation of the optical afterglow
DATE:    11/02/10 03:56:49 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, E. Berger (Harvard), and J. Mulchaey (OCIW) report:

"We re-observed the position of GRB 110208A (GCN #11678) with LDSS3 on the
Magellan/Clay 6.5-m telescope starting on 2011 February 10.03 UT (27.5 hrs
post-burst). In a single 180-sec i-band exposure we no longer detect the
point source described by Berger et al. (GCN #11681) to a limiting
magnitude of i>22.8 mag (3-sigma). We therefore conclude that this source
is the optical afterglow of GRB 110208A."


GRB_name: GRB110206A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11686
SUBJECT: GRB 110206A: Swift-XRT confirmation of the X-ray afterglow
DATE:    11/02/10 08:32:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Swift performed a second epoch observation of the INTEGRAL GRB 110206A 
(Mereghetti et al. GCN Circ. 11654), collecting 4.8 ks of data from 
T0+253 ks to T0+277 ks. The X-ray source reported by Evans et al. (GCN 
Circ. 11657) has clearly faded, confirming that this is the afterglow. 
The decay can be modelled as a single power-law decay with an index of 
1.1 (+0.2, -0.1).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110210A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11687
SUBJECT: GRB 110210A: Swift detection of a burst
DATE:    11/02/10 10:11:13 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), S. Campana (INAF-OAB),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
J. M. Gelbord (PSU), B. Gendre (ASDC), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), C. B. Markwardt (NASA/GSFC),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester), M. Perri (ASDC),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester) and
G. Stratta (ASDC) report on behalf of the Swift Team:

At 09:52:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110210A (trigger=445141).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 13.077, +7.792 which is 
   RA(J2000) = 00h 52m 19s
   Dec(J2000) = +07d 47' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve did not show a significant
peak, which is typical for an image trigger. 

The XRT began observing the field at 09:54:57.8 UT, 136.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 13.05706, 7.78019 which is
equivalent to:
   RA(J2000)  = 00h 52m 13.69s
   Dec(J2000) = +07d 46' 48.7"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 83 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.28
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 2.16e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 144 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.06. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110201A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11688
SUBJECT: GRB 110201A: optical observations
DATE:    11/02/10 10:58:01 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

V. Rumyantsev (CrAO), A. Pozanenko (IKI), A. Volnova (SAI MSU), E.
Klunko (ISTP) report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 110201A (Siegel et al., GCN
11622) with Shajn telescope of CrAO in filter R between Feb. 01 (UT)
17:01 - 18:04, and with AZT-33IK telescope between Feb. 01 (UT) 16:31
- 17:07. Using stacked image of CrAO observations we detect a diffuse
source (A) at ~4" offset of a center of the XRT error circle (Siegel
et al., GCN 11622), see also http://www.swift.ac.uk/sper/444230/. The
coordinates of the center of the source (A) are (J2000) RA =
09:10:29.84, Dec = +88:36:17.5 with uncertainty of 0.5" in both
coordinates.

The photometry of the source is based on the USNO-B1.0 star
1786-0003311 (09:12:09.70 +88:36:01.0) assuming R=17.64 is following:

T0+     Filter,  Exposure, source A, mag, UpperLimit
(mid, d)       (s)

0.3305  R    45x60     21.9 +/- 0.1   23.4

Would be the source (A) a host galaxy of GRB 110201A, the galaxy could
be a relatively close (z <1) taking into account its brightness.
The finding chart can be found at
http://grb.rssi.ru/GRB110201A/GRB110201a_110201_R_ZTSh.gif


GRB_name: GRB110210A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11689
SUBJECT: GRB 110210A: Enhanced Swift-XRT position
DATE:    11/02/10 13:59:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1592 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 110210A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 13.05659, +7.77968 which is equivalent
to:

RA (J2000): 00h 52m 13.58s
Dec (J2000): +07d 46' 46.9"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11691
SUBJECT: GRB 110210A: Swift-BAT refined analysis
DATE:    11/02/10 18:30:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110210A (trigger #445141)
(D'Elia, et al., GCN Circ. 11687).  The BAT ground-calculated position is
RA, Dec = 13.108, 7.778 deg, which is 
   RA(J2000)  =  00h 52m 25.9s 
   Dec(J2000) = +07d 46' 39.5" 
with an uncertainty of 3.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.
 
The mask-weighted light curve shows the emission starting at ~T-100 sec,
peaking at ~T+50 sec, and ending at ~T+150 sec.  T90 (15-350 keV) is
233 +- 60 sec (estimated error including systematics).
 
The time-averaged spectrum from T-102.9 to T+153.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.73 +- 0.29.  The fluence in the 15-150 keV band is 9.6 +- 1.9 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-54.44 sec in the 15-150 keV band
is 0.3 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/445141/BA/


GRB_name: GRB110205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11692
SUBJECT: GRB 110205A: Swift/BAT and Suzaku/WAM joint spectral analysis
DATE:    11/02/10 18:55:44 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <Taka.Sakamoto@nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), 
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):

S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.)
(i.e. the Suzaku WAM team):

We performed the Swift/BAT and the Suzaku/WAM joint spectral analysis
of GRB 110205A (Swift/BAT trigger #444643: Beardmore et al., GCN Circ. 
11629, Markwardt et al. GCN Circ. 11646).  The joint spectral analysis 
of the Swift/BAT and the Suzaku/WAM data allows us to derive the broad-band 
spectral parameters of this burst.

The time interval of the spectral data for each instrument is chosen
from T0(BAT)+20.2 to T0(BAT)+318.2 sec where T0(BAT) is the trigger time
of BAT at 02:02:41.3 UTC.  The energy ranges which we used in the joint
spectral analysis are 15-150 keV and 100-3000 keV for the Swift/BAT and 
the Suzaku/WAM respectively. The spectral data of two instruments are 
fitted with the spectral model multiplied by the constant factor to take
into account the systematic effective area uncertainties in the response
matrices of each instrument.

The spectrum is well fitted with a power-law with exponential cutoff 
model: dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak). The constant factors 
of each instrument agree within 10%.  No systematic residual from the 
best fit model is seen in the spectral data of each instrument.  The 
best fit spectral parameters are: alpha = -1.59 (-0.06/+0.07) and Epeak 
= 230 (-65/+135) keV (chi2/dof = 96.6/85).  A simple power-law fit 
shows a poor fit to the data (chi2/dof=126.4/86).  The best fit spectral 
parameters for the Band function fixing beta = -2.5 are: 
alpha = -1.57 (-0.08/+0.10), and Epeak = 200 (-60/+130) keV (chi2/dof = 96.9/85).
Our best fit spectral parameters are consistent with the Konus-Wind 
result based on the 3 channel data (Golenetskii et al. GCN Circ. 11659).  
The energy fluence in the 15-3000 keV band calculated by a power-law with 
exponential cutoff model for this 298 sec interval is 2.7 (-0.4/+0.7)x10^-5 erg/cm2.

Assuming z = 2.22 (Cenko et al. GCN Circ. 11638; Vreeswijk et al. GCN Circ. 11640) 
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, 
Omega_Lambda = 0.73, the isotropic energy release is 
E_iso = 4.6 (-0.7/+0.4) x10^53 erg in 1 keV to 10 MeV at the GRB rest frame.  

All the quoted errors are at the 90% confidence level.


GRB_name: GRB110210A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11693
SUBJECT: GRB 110210A: Swift-XRT refined Analysis
DATE:    11/02/10 20:12:41 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

G. Stratta, V. D'Elia (ASDC) report on behalf of the Swift-XRT team:

We have analysed 5.6 ks of XRT data for GRB 110210A (D'Elia  et al. GCN
Circ. 11687), from 126 s to 19.3 ks after the  BAT trigger. The data
comprise 226 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 11689).  After an initial fading behavior, the light curve
is consistent with a constant source of mean count rate 4.5e-01 ct/sec.
A power-law fit gives an index of 0.0 (+/-0.3).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.10 (+0.09, -0.08). The
best-fitting absorption column is  2.16 (+0.17, -0.16) x 10^21 cm^-2,
in excess of the Galactic value of 5.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.16 (+0.15, -0.19)
and a best-fitting absorption column of 7.5 (+4.5, -1.9) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (4.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.5 (+4.5, -1.9) x 10^20 cm^-2
Galactic foreground: 5.3 x 10^20 cm^-2
Excess significance: 6.4 sigma
Photon index:      2.16 (+0.15, -0.19)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00445141.

This circular is an official product of the Swift-XRT team.

[GCN OPS NOTE(10feb11): Per author's request, the fourth sentence
was replaced. Acknowledgement to H.Kann.]


GRB_name: GRB110210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11694
SUBJECT: GRB 110210A: optical upper limit
DATE:    11/02/10 21:40:39 GMT
FROM:    Giuseppe Greco at U Bologna  <giuseppe.greco2@studio.unibo.it>

G. Greco (INAF-Astronomical Observatory of BOLOGNA), C. Bartolini, A. Guarnieri,
A. Piccioni (University of Bologna), G. Pizzichini (INAF/IASF-Bologna),
G. Gavazzi (University of Milano-Bicocca) and R. Gualandi
(INAF-Astronomical Observatory of BOLOGNA) report:

We observed the location of the GRB 110210A (D'Elia, et al., GCN Circ. 11687)
with the 152 cm Cassini Telescope located in Loiano, Italy, equipped with BFOSC.

Two R-band observations (2x900 sec) were obtained during twilight at high airmass.
The mean time was February 10.756 UT (0.345 day after the burst).

No source was detected inside the XRT error circle
(Goad, et al., GCN. Circ. 11689) in the coadded frame.
The limiting magnitude is R = 18  based on the USNO-A2 catalog
and not corrected for the Galactic extinction.

This message can be cited.


GRB_name: GRB110207A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11695
SUBJECT: GRB 110207A: Suzaku WAM observation of the prompt emission
DATE:    11/02/11 10:20:52 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

P. Tsai, Y. Urata (NCU), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa
(Hiroshima U.), N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.), 
S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara,
T. Yasuda (Saitama U.), M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), 
Y. E. Nakagawa, T. Tamagawa,  M. Serino (RIKEN), N. Ohmori, A. Daikyuji, 
Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), 
K. Nakazawa, K. Makishima (Univ. of Tokyo), 
on behalf of the Suzaku WAM team, report:

The GRB 110207A (Swift/BAT trigger #444912 ; Littlejohns et al., GCN 11658;
Palmer et al., GCN 11664) triggered the Suzaku Wide-band All-sky Monitor
(WAM) which covers an energy range of 50 keV - 5 MeV at 2011/02/07
11:17:20.05 UT (=T0).

The observed light curve shows a multi-peaked structure lasting from T0-0.2s
to T0+3.2s with a duration (T90) of about 2.9 seconds. The fluence in 100 -
1000 keV was 5.98 (+/-0.54) x 10^-7 erg/cm^2. The 1-s peak flux measured
from T0+0.32s was 0.27 (+/-0.06) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-0.2s to
T0+3.2s is well fitted by a single power-law with a photon index of 1.53
(-0.24, +0.29) (chi^2/d.o.f = 34.22/34).

All the quoted errors are at statistical 90% confidence level, in which the
systematic uncertainties are not included.

The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11696
SUBJECT: GRB 110205A: detection of optical linear polarization from CAHA
DATE:    11/02/11 11:05:19 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), R. Duffard (IAA-CSIC), P. Kubanek (IAA-CSIC & U. of Valencia), A. Guijarro (CAHA), report on behalf of a larger collaboration:

"We carried out optical linear polarization observations of the GRB 110205A afterglow (GCN Circ. 11629, Beardmore et al.) using the 2.2m telescope of the Calar Alto Observatory equipped with CAFOS. The data were acquired in the R-band on Feb 5.19879-5.26570 UT (2.73-4.33 hours post burst) with a total exposure time of 10x500s. A preliminary analysis reveals an afterglow linear polarization at a level of P~1.4%. This value is higher than the polarization (P ~< 0.4%) measured for the bright field stars, so we conclude that most of the measured afterglow polarization has very likely an extragalactic origin."


GRB_name: GRB110205A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11697
SUBJECT: Konus-Wind observation of GRB 110205A (correction to GCN 11659)
DATE:    11/02/11 11:35:08 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

V. Pal'shin report on behalf of the Konus-Wind team:

The isotropic equivalent energy and peak luminosity of GRB 110205A given 
in GCN Circular 11659 have been erroneously computed.

The correct values for the isotropic equivalent energy is E_iso = (4.34 
+/- 0.42)x10^53 erg, and for the isotropic peak luminosity is 
(L_iso)_max = (1.95 +/- 0.27)x10^52 erg/s
(assuming z = 2.22 (Cenko & Hora, GCN 11638; Vreeswijk et al. GCN 11640)
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27,
Omega_Lambda = 0.73).

I thank Max De Pasquale and Takanori Sakamoto for pointing this out to 
me and I apologize for the error.


GRB_name: GRB110201A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11698
SUBJECT: GRB 110201A: Subaru/MOIRCS Ks-band photometry
DATE:    11/02/11 21:06:49 GMT
FROM:    Masato Onodera at ETH Zurich  <monodera@phys.ethz.ch>

M. Onodera (ETH Zurich), E. Daddi (CEA/Saclay), I. Tanaka (Subaru Telescope),
and Y. Yamada (NAOJ) report:

We observed the field of GRB 110201A (Siegel et al., GCN Circ. 11622)
in Ks-band with MOIRCS on the Subaru telescope.

The observations was carried out on 2011-02-02 16:27:33 UT
(~31 hours after the burst) for 200 seconds integration and
on 2011-02-03 16:16:20 UT (~54.5 hours after the burst)
for 520 seconds integration. Within the XRT error circle,
we did not find any evidence for fading sources. On the other hand,
a faint galaxy is detected at (RA, Dec)=(9:10:23.01, +88:36:21.82).
Our preliminary photometry shows the galaxy is Ks=19.7 (Vega) or
Ks=21.5 (AB) with an error of ~0.2 mag.  There is another source
slightly outside of the XRT error circle at (RA, Dec)=(9:10:31.5, +88:36:18.4)
with an magnitude of Ks=19.3 (Vega) or Ks=21.1 (AB) with an error of ~0.15 mag.
Flux calibration was carried out by using 2MASS sources.

Images are provided for consultation at the following web site:
http://www.astro.phys.ethz.ch/people/monodera/grb110201a/


GRB_name: GRB110212A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11699
SUBJECT: GRB 110212A: Swift detection of a burst
DATE:    11/02/12 01:18:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), C. B. Markwardt (NASA/GSFC),
D. M. Palmer (LANL), M. H. Siegel (PSU) and G. Stratta (ASDC) report
on behalf of the Swift Team:

At 01:09:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110212A (trigger=445321).  Swift did not slew immediately 
to the burst because of an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 69.053, +43.702 which is 
   RA(J2000) = 04h 36m 13s
   Dec(J2000) = +43d 42' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiply-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 19:02 UT on 2011 February 13. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11700
SUBJECT: GRB 110212A: ROTSE-III Optical Limits
DATE:    11/02/12 01:51:42 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (U Mich), report on behalf of the ROTSE collaboration: 

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
110212A (Swift trigger 445321; D'Elia et al., GCN 11699), producing
images beginning 31.0 s after the GCN notice time. An automated response
took the first image at 01:09:39 UT, 31.0 s after the burst.
Unfortunately the sky is still under twilight conditions, the first
useful image stared 725s after the burst.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle for co-added images with a sets of 10
calibrated relative to USNO A2.0 (R). We set the following specific
limits. 

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
01:21:13.5   01:25:54.7       281     16.8          725.5       Y
01:26:04.0   01:30:45.5       281     17.1         1016.0       Y
01:30:54.3   01:35:35.5       281     17.2         1306.3       Y
01:35:44.3   01:40:25.0       280     17.4         1596.3       Y


GRB_name: GRB110212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11701
SUBJECT: GRB110212A: BOOTES-2/TELMA optical limits
DATE:    11/02/12 03:25:14 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek and Javier Gorosabel (IAA-CSIC Granada)
on behalf of BOOTES collaboration report:

"  The 60 cm robotic telescope TELMA at the BOOTES-2 station
located in Malaga (Spain) reacted automatically to GRB110212A
(GCNC 11699). The first image was obtained 32.1s after the GRB
trigger time (and 7.3s after the reception of the trigger).

A large number of 3-s R-band images was obtained.

No new source was found on 40 individual images (R>~15) taken
between 32 and 253s after the GRB, nor at their 120s (40x3s)
combination (R>~16.5).  "


GRB_name: GRB110212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11702
SUBJECT: GRB 110212A: SARA-N Optical Limits
DATE:    11/02/12 04:19:52 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike (NASA/GSFC), Dieter H. Hartmann (Clemson University),
Brian Murphy, and Andrew N. Darragh (Butler University) report:

We observed the field of GRB 110212A (D'Elia et al., GCN 11699) with the
SARA-North 0.9m telescope at KPNO beginning 58 minutes after the trigger
under good conditions.  We obtained 24 minutes of stacked exposures in the
R band and 6 minutes of stacked exposures in the I band.

We detect no new sources within nearly 2 sigma of the BAT error circle
down to limiting magnitudes of R > 20 and I > 19 relative to the USNO B1.0
catalog.


GRB_name: GRB110212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11703
SUBJECT: GRB 110212A, Swift-BAT refined analysis
DATE:    11/02/12 14:17:53 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

T. N. Ukwatta (MSU),S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), (i.e. the Swift-BAT team):

Using the data set from T-239 to T+630 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110212A (trigger #445321)
(D'Elia, et al., GCN Circ. 11699).  The BAT ground-calculated position is
RA, Dec = 69.025, 43.716 deg which is
     RA(J2000)  =  04h 36m 06.0s
     Dec(J2000) = +43d 42' 56.2"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.

The mask-weighted light curve shows two peaks, the first from T-0.6 s to T+1.6 s
and the second from T+1.8 to T+2.6 s. T90 (15-350 keV) is 3.3 +- 0.5 sec
(estimated error including systematics).

The time-averaged spectrum from T-1.8 to T+2.6 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.78 +- 0.85,
and Epeak of 44.6 +- 10.2 keV (chi squared 54.29 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.4 +- 0.3 x 10-7  erg/cm2
and the 1-sec peak flux measured from T+0.26 sec in the 15-150 keV band is
1.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.93 +- 0.15 (chi squared 61.44 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/445321/BA/


GRB_name: GRB110212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11704
SUBJECT: GRB 110212A: GRT Optical Observation
DATE:    11/02/13 04:13:57 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (UMD/GSFC), N. Gehrels (GSFC),
T. Okajima (GSFC), Y. Urata (NCU), C.A. Wallace (FGCU)

We observed the field of GRB 110212A detected by Swift
(trigger #445321; D'Elia et al., GCN Circ. 11699) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

A total 209 images of 5 sec (200 images) and 30 sec (9 images) 
exposures were taken in the R filter starting from February 12 01:10:20 (UT), 
about 71 seconds after the trigger (37 seconds after the BAT position notice), 
and stopped on February 12 01:45:53 (UT).  We do not detect the optical 
afterglow both in the individual images and the stacked image inside the 
BAT error circle (Ukwatta et al., GCN #11703).  The estimated five sigma upper 
limit of the combined image (total exposure of 1270 sec) is ~18.9 mag using 
the USNO-B1 catalog.


GRB_name: GRB110213A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11705
SUBJECT: GRB 110213A: Swift detection of a burst with optical afterglow
DATE:    11/02/13 05:33:13 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU),
E. Sonbas (GSFC/USRA/Adiyaman Univ.), E. Troja (NASA/GSFC/ORAU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 05:17:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110213A (trigger=445414).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 43.004, +49.291 which is 
   RA(J2000) = 02h 52m 01s
   Dec(J2000) = +49d 17' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 05:19:01.2 UT, 91.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 42.9641, +49.2726 which is equivalent to:
   RA(J2000)  = 02h 51m 51.38s
   Dec(J2000) = +49d 16' 21.3"
with an uncertainty of 5.5 arcseconds (radius, 90% containment). This
location is 115 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 100 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
 RA(J2000)  = 02:51:51.40 =  42.96417
 DEC(J2000) = +49:16:23.6  =  49.27321
with a 90%-confidence error radius of about 0.61 arc sec. This position is 2.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.31 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.32. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110213A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11706
SUBJECT: GRB 110213A: P60 Optical Afterglow Detection
DATE:    11/02/13 05:36:43 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration:

We have imaged the error circle of GRB110213A (D'Elia et al., GCN
11705) with the automated Palomar 60 inch telescope.  Observations began
at 05:19 UT (~ 2 minutes after the burst trigger time) and were taken in
the r' filter.  We detect a bright source at the location of the UVOT
afterglow, with coordinates:

   02:51:51.43   +49:16:23.3

Using several USNO-B1 field stars for comparison, we measure a magnitude
of R ~ 17.1 at this time.  Observations are ongoing.


GRB_name: GRB110213A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11707
SUBJECT: GRB 110213A: ROTSE-III Detection of Optical Counterpart
DATE:    11/02/13 05:44:46 GMT
FROM:    Brad Schaefer at LSU  <schaefer@grb.phys.lsu.edu>

W. Rujopakarn (Steward), B. E. Schaefer (Louisiana State), E.S. Rykoff 
(LBNL), report on behalf of the ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 
110213A (Swift trigger 445414). The first image was at 05:17:56.7 UT, 27.1 
s after the burst (0.7 s after the GCN notice time). The unfiltered images 
are calibrated relative to USNO A2.0. We detect a 15.8 magnitude, fading 
source with coordinates:

02:51:51.11 +49:16:20.57 (J2000), with positional uncertainty of 1' or 
better

start UT mag mlim(of image)
----------------------------------
05:17:56.7 15.8 17.0


This source is not visible in DSS (second epoch), 2MASS or the MPChecker 
database.

Our light curve shows a beautiful rise starting 100 seconds after the 
Swift trigger, reaching a peak around 14.5 mag at 200 seconds after the 
trigger and then starting a fast decline.   Continuing observations are in 
progress. 


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11708
SUBJECT: GRB 110213A: Bok Telescope Redshift
DATE:    11/02/13 07:23:19 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

P. A. Milne (U. Arizona) and S. B. Cenko (UC Berkeley) report on behalf of
a larger collaboration:

We have obtained a series of optical spectra of the afterglow of GRB
110213A (D'Elia et al, GCN 11705) with the Boller and Chivens Spectrograph
mounted on the 2.3-m Bok telescope.  Observations began at 05:53 UT (~ 36
minutes after the Swift trigger time) and cover the wavelength range from
~ 4000-8300 A.

We detect a series of strong, narrow absorption features corresponding to
Mg II and Fe II at a common redshift of z = 1.46.  Without the detection
of fine structure lines or a DLA system, we cannot definitively identify
this as the redshift of the GRB host galaxy.  However, the lack of
detection of Lyman alpha absorption down to ~ 4000 A limits the redshift
of the host galaxy to z <~ 2.3.


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11709
SUBJECT: GRB 110213A: GRAS011 optical observations
DATE:    11/02/13 08:10:35 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:

GRAS 011 (Global-Rent-a-Scope, Mayhill, New Mexico) CDK20 20 
inch (0.51 m) f/6.8 and FLI ProLine PL11002M CCD camera were used 
to detect GRB 110213A optical afterglow. The observations were started 
at 2011-02-13 05:39:52 (UT) and stopped at 2011-02-13 06:14:37 (UT). 
Two unfiltered and one photometric R observations with 600s exposure 
times were made. The afterglow was detected at following position 
RA 02:51:51.42 and DEC +49:16:23.7 consistent those given by Cenko 
S.B. et al. (GCN 11706) to within positional errors.

The following magnitudes were obtained from the observations using 
NOMAD1 1392-0071642 (R = 15.230) as the comparison:

Tmid(s)+T0  Filter        Exp (sec)     Mag      Mag err   Limit
1643           unfilt         600             15.6       0.1         16.9
2306           unfilt         600             15.8       0.1         16.9
3128           Rc            600             15.9       0.2         16.5

A jpg image of the 600sec unfiltered observation is available at the following URL link:
http://cutenews.kassiopeia.net/data/upimages/GRB110213A_text.jpg 


GRB_name: GRB110213A
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11710
SUBJECT: GRB 110213A: KAIT observations
DATE:    11/02/13 08:19:36 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li and A. V. Filippenko, University of California, Berkeley,
on behalf of the KAIT GRB team, report:

The robotic 0.76-m Katzman Automatic Imaging Telescope (KAIT) at Lick
Observatory observed GRB 110213A (D'Elia et al., GCN 11705). 
The automatic sequence started at 05:18:43 UT, 74 s after the BAT trigger.
The BAT location has been monitored in V, I, and clear filters, with
varying exposure times. Our image processing pipeline found a new
object within the BAT error circle, with the following position:

R. A. = 02:51:51.40
DEC.  = +49:16:23.2  (J2000), 

which is consistent with the reported afterglow position by D'Elia et al.
(GCN 11705), Cenko (GCN 11706), and Rujopakarn et al. (GCN 11707).
The OA has magnitude of 17.0 at t = 74 s, brightened to a peak of 14.6
at t = 300 s, then declined to mag 16.0 at t = 2000 s. The OA 
then displayed several episodes of re-brightening between t = 2000 s
and 2600 s, at which point the observation was stopped due to a 
physical limit of KAIT.  


GRB_name: GRB110212A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11711
SUBJECT: GRB110212A: MITSuME Okayama optical upper limits
DATE:    11/02/13 08:42:44 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110201A (D'Elia et al., GCN 11699)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2011-02-12 11:11:56 UT (~10 hours
after the burst). We did not find any new point source within the
BAT refined error circle (Ukwatta et al., GCNC 11703) in all the
three bands.

Three sigma upper limits of the OT are listed below. We used
GSC2.3 catalog for flux calibration.


T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.46043    12:12:08  5880.0     >20.0  >19.7  >19.0
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110213A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11712
SUBJECT: GRB 110213A: Enhanced Swift-XRT position
DATE:    11/02/13 12:17:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2597 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 110213A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 42.96403, +49.27257 which is equivalent
to:

RA (J2000): 02h 51m 51.37s
Dec (J2000): +49d 16' 21.2"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11713
SUBJECT: GRB 110213A: optical observations
DATE:    11/02/13 14:40:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

I. Korobtsev (ISTP),  E. Klunko (ISTP), A. Volnova (SAI MSU),  A. Pozanenko 
(IKI) on behalf of larger GRB follow up collaboration report:

We observed the  Swift GRB 110213A (D'Elia et al., GCN 11705)  with AZT-33IK 
telescope of Sayan observatory (Mondy) starting Feb.13  (UT) 11:26.
In a few first images of exposure 60 s we clearly detect the UVOT afterglow 
with a preliminary brightness estimation R ~ 18.0 at 0.2566 days after 
burst.
The photometry is based on USNO-B1 field stars.

Observation is continuing. 

[GCN OPS NOTE(30apr11): Per author's request, Elunko was changed to Klunko.]


GRB_name: GRB110213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11714
SUBJECT: GRB 110213A, Swift-BAT refined analysis
DATE:    11/02/13 14:53:10 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
V. D'Elia (ASDC),E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110213A (trigger #445414)
(D'Elia, et al., GCN Circ. 11705).  The BAT ground-calculated position is
RA, Dec = 42.978, 49.278 deg which is
     RA(J2000)  =  02h 51m 54.8s
     Dec(J2000) = +49d 16' 41.4"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 5%.

The masked-tagged light curve shows low-level emission starting at about T-30 s
and then a steep rise starting at T-3 s to a peak at T+0.5 s, followed by a
slow decline out to about T+30 s.  T90 (15-350 keV) is 48.0 +- 16.0 sec
(estimated error including systematics).

The time-averaged spectrum from T-31.2 to T+32.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.83 +- 0.12.  The fluence in the 15-150 keV band is 5.9 +- 0.4 x 10-6  erg/cm2.
The 1-sec peak photon flux measured from T+8.31 sec in the 15-150 keV band
is 1.6 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/445414/BA/


GRB_name: GRB110213A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11715
SUBJECT: GRB 110213A: Lightbuckets Optical Observations
DATE:    11/02/13 15:07:06 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

T. N. Ukwatta (MSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
N. Gehrels (GSFC), J. Linnemann (MSU), K. Tollefson (MSU),
and U. Abeysekara (MSU)

We observed the Swift GRB 110213A (D'Elia et al., GCN 11705)
afterglow with the Lightbuckets 0.61m rental telescope LB-0001
in Rodeo, NM, USA. Under good weather conditions, four
observations were carried out in the R filter starting
2011-02-13 at 05:33:14 UT (~ 15.7 mins after the GRB trigger).

The burst afterglow is clearly detected in all four
observations and estimated magnitudes are given below:

Time after trigger       Exposure (s)   Filter     Magnitude

15.7  mins (0.26 hours)     60              R      15.4 +/- 0.1
17.8  mins (0.30 hours)     60              R      15.5 +/- 0.1
19.9  mins (0.33 hours)     60              R      15.5 +/- 0.1
22.6  mins (0.38 hours)     60              R      15.7 +/- 0.1

The afterglow, not corrected for Galactic extinction, is
calibrated against the USNO-B1.0 catalog.


GRB_name: GRB110213B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11716
SUBJECT: GRB 110213B: MAXI/GSC detection of a probable GRB 
DATE:    11/02/13 17:15:58 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

H. Negoro, M. Nakajima, H. Ozawa, F. Suwa (Nihon U.), N. Kawai, M. Morii, 
K. Sugimori, R. Usui, T. Toizumi (Tokyo Tech), M. Serino, T. Mihara, 
Y.E. Nakagawa, M. Sugizaki, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN),
K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
A. Yoshida, K. Yamaoka,  S. Nakahira (AGU), H. Tsunemi, M. Kimura (Osaka U.),
Y. Ueda, N. Isobe, S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.), 
A. Uzawa, T. Matsumura, K. Yamazaki (Chuo U.) report on behalf of the MAXI team:

MAXI/GSC triggered at UT 2011-02-13T14:31:48 on a bright uncatalogued X-ray 
transient source.  Judging from its location and spectral hardness ratio, 
this transient is probably a gamma-ray burst. 
Since the emission was detected only for a fraction of the triangular 
transit response, the uncertainty of its position along the scan direction 
is large.  The center of the error box is 

(R.A., Dec) = (+41.768,  0.952 deg) = (02 47 04,  00 57 07)(J2000)

with an uncertainty of 0.5 deg (90% containment radius).
The preliminary flux of the transient source was 1.3 Crab (2-4 keV),
2.2 Crab (4-10 keV), and 3.5 Crab (10-20 keV).
There was no significant detection at the transit location in the
previous orbit (92 min before the detection) with an upper limit of 20 mCrab.  
There is no known bright X-ray source at the detected position. 

Follow-up observations are encouraged.


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11717
SUBJECT: GRB 110213A: THO optical observations
DATE:    11/02/13 22:41:33 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen, Tuomo Salmi and Harri Vilokki 
(Taurus Hill Observatory, Varkaus, Finland) report:

We continued optical observations of GRB 110213A optical afterglow. 
We used Celestron C14 XLT and SBIG ST-8XME CCD (Taurus Hill 
Observatory, Varkaus, Finland). The observations were started at 
2011-02-13 17:18:32 (UT) and stopped at 2011-02-13 18:24:28 (UT).
Three unfiltered and three photometric R observations with 600s exposure
times were made. The afterglow was detected at following position 
RA 02:51:51.41 and DEC +49:16:23.0.

The following magnitudes were obtained from the observations using 
NOMAD1 1392-0071642 (R=15.230) as the comparison:

Tmid(s)+T0    Filter     Exp (sec)     Mag         Mag err      Limit
44163             unfilt     3x600            19.1       0.2             20.3
46231             Rc        3x600            19.2       0.3             20.1 


GRB_name: GRB110213A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11718
SUBJECT: GRB 110213A: Swift/UVOT refined analysis
DATE:    11/02/13 22:57:40 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (MSSL/UCL) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110213A
100 s after the BAT trigger (D'Elia et al., GCN Circ. 11705). This GRB
was reported by many observers. We see an initial peak around T+300s
after which the GRB declines in brightness until around T+1500s when
a small rebrightening occurs. A tentative redshift was reported by
P.A. Milne (GCN Circ. No 11708) of z=1.46, which is consistent with
the much fainter magnitudes we find in the uvm2 and uvw2 filters.

The refined uvot position (90% confidence limit, 0.5" accuracy) with
reference to USNO-B1 is:

RA  (J2000) =  02h 51m 51.39s
DEC (J2000) =  49d 16' 23.54"

Preliminary magnitudes and 3-sigma upper limits in the UVOT
photometric system (Poole et al. 2008, MNRAS, 383, 627) for
the first finding chart (FC) exposures and summed with subsequent
exposures up to about 2500s are:

Filter         T_start(s)   T_stop(s)      Exp(s)     Mag (VEGA)

white_FC           100          250          147         16.36 +/- 0.05
u_FC               312          562          246         15.54 +/- 0.04

white              100         2579          517         16.57 +/- 0.01
v                  642         2455          227         16.19 +/- 0.04
b                  568         2206          178         16.77 +/- 0.03
u                  312         2529          448         15.94 +/- 0.02
uvw1               692         2505          198         17.28 +/- 0.08
uvm2               667         2479          218         18.72 +/- 0.20
uvw2               618         2606          238         19.10 +/- 0.18

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.32 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110213A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11719
SUBJECT: GRB110213A: MITSuME Okayama Optical Observation
DATE:    11/02/14 00:25:08 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110213A (D'Elia et al., GCNC 11705)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2011-02-13 09:45:46 UT (~4.5 hours after
the burst). We detected the previously reported afterglow
(Cenko, GCNC 11706) in all the three bands.


Photometric results and are listed below. We used GSC2.3 catalog for
flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.19696    10:01:06   1620.0    18.26  0.09  17.15  0.05  16.53  0.06
0.21845    10:32:02   1620.0    18.78  0.11  17.51  0.05  16.75  0.05
0.23993    11:02:59   1620.0    18.79  0.16  17.60  0.07  17.05  0.07
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110213B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11720
SUBJECT: GRB 110213B: MAXI/GSC refined analysis
DATE:    11/02/14 01:21:42 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

M. Morii, N. Kawai, K. Sugimori, R. Usui, T. Toizumi (Tokyo Tech),
H. Negoro, M. Nakajima, H. Ozawa, F. Suwa (Nihon U.), , M. Serino, T. Mihara, 
Y.E. Nakagawa, M. Sugizaki, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN),
K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
A. Yoshida, K. Yamaoka,  S. Nakahira (AGU), H. Tsunemi, M. Kimura (Osaka U.),
Y. Ueda, N. Isobe, S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.), 
A. Uzawa, T. Matsumura, K. Yamazaki (Chuo U.) report on behalf of the MAXI team:


We report further analysis of MAXI/GSC GRB 110213B (GCN #11716).
The refined position of the GRB is

(R.A., Dec) = (+41.61 deg, +1.19 deg) = (02 46 27, +01 11 14)(J2000)

with a rectangular 90% statistical error box with the following corners:

(R.A., Dec) = (+41.62 deg, +1.11 deg) = (02 46 29, +01 06 23)(J2000)
(R.A., Dec) = (+41.53 deg, +1.18 deg) = (02 46  7, +01 10 48)(J2000)
(R.A., Dec) = (+41.61 deg, +1.27 deg) = (02 46 26, +01 16  2)(J2000)
(R.A., Dec) = (+41.70 deg, +1.19 deg) = (02 46 48, +01 11 37)(J2000)

Without assumptions on the source constancy,
we obtain a rectangular error box with the following corners:

(R.A., Dec) = (+41.40 deg, +0.87 deg) = (02 45 36, +00 52 14)(J2000)
(R.A., Dec) = (+41.31 deg, +0.94 deg) = (02 45 13, +00 56 41)(J2000)
(R.A., Dec) = (+41.75 deg, +1.42 deg) = (02 46 59, +01 25 10)(J2000)
(R.A., Dec) = (+41.84 deg, +1.35 deg) = (02 47 22, +01 20 45)(J2000)

There is additional systematic uncertainty of 0.2 deg (90% containment radius).


GRB_name: GRB110213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11721
SUBJECT: GRB 110213A: Swift-XRT refined Analysis
DATE:    11/02/14 10:34:12 GMT
FROM:    Giulia Stratta at ASDC  <stratta@asdc.asi.it>

G. Stratta (ASDC) and V. D'Elia (ASDC) report on behalf of the
Swift-XRT team:

We have analysed 22 ks of XRT data for GRB 110213A (D'Elia  et al. GCN
Circ. 11705), from 81 s to 54.5 ks after the  BAT trigger. The data
comprise 121 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 11712).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=5.2 (+0.5, -0.4). At T+141 s  the decay
flattens to an alpha of -0.22 (+0.10, -0.14). The light curve breaks
again at T+1489 s to a decay with alpha=1.10 (+0.07, -0.08),  before a
final break at T+9954 s s after which the decay index is 2.14 (+0.10,
-0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.11 (+/-0.07). The
best-fitting absorption column is  2.81 (+0.24, -0.23) x 10^21 cm^-2,
in excess of the Galactic value of 2.2 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.1 x 10^-11 (6.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.81 (+0.24, -0.23) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: 20.5 sigma
Photon index:      2.11 (+/-0.07)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00445414.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110213B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11722
SUBJECT: Konus-Wind observation of GRB 110213B
DATE:    11/02/14 11:22:18 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team, report:

The GRB 110213B discovered and localized by MAXI/GSC (Negoro et al., GCN 
11716) was detected by Konus-Wind in the waiting mode at T0(KW)=52293 s 
  UT (14:31:33).

The burst light curve shows a single pulse with a duration of ~50 s.

As observed by Konus-Wind, the burst had a fluence of (1.77 +/- 
0.16)x10^-5 erg/cm2 (in the 20 - 1400 keV range).

Modeling the K-W 3-channel time-integrated spectrum (from T0 to
T0+50 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.52 +/- 0.25, and Ep = 123 +/- 19 keV.

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB110213B/


GRB_name: GRB110213A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11723
SUBJECT: Konus-Wind observation of GRB 110213A
DATE:    11/02/14 11:36:03 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long GRB 110213A, (Swift/BAT trigger=445414:
D'Elia, et al., GCN 11705; Barthelmy et.al, GCN 11714)
triggered Konus-Wind at T0=19048.893s UT (05:17:28.893)

The burst light curve consists of a single pulse
with a total duration of ~50 s.
The emission is seen up to ~2 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB110213_T19048/

As observed by Konus-Wind the burst
had a fluence of (1.0  0.15)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+1.024s,
of (1.4  0.2)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+24.832 s) is best fitted
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = -1.65 (-0.2, +0.3),
and Ep = 91(-26, +31) keV,
chi2 = 62.5/61 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+8.448 s) is well fitted
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = -1.53 (-0.21, +0.24),
and Ep = 110(-20, +32) keV,
chi2 = 52.8/61 dof.
This spectrum is nearly well fitted
in the 20 keV - 2 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -1.28 (-0.32, +0.44),
the high energy photon index beta = -2.4 (-0.7, +0.2),
the peak energy Ep = 89(-19, +28) keV,
chi2 = 49.1/60 dof.

Assuming the Bok telescope redshift z = 1.46 (Milne & Cenko, GCN 11708)
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27,
Omega_Lambda = 0.73, the isotropic energy release
E_iso is (5.5  0.08)x10^52 erg, the peak luminosity
L_iso_max is (1.9  0.3)x10^52 erg/s,
and Ep_rest is 224  74 keV.


All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB110213A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11724
SUBJECT: GRB 110213A: MITSuME Akeno Optical Observation
DATE:    11/02/14 14:52:06 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

H. Nakajima, Y. Yatsu, T. Enomoto, K. Kawakami, K. Tokoyoda, T. Ohkawa, and
N. Kawai (Tokyo Tech)  report on behalf of the MITSuME collaboration:

We observed the field of GRB 110213A (D'Elia et al , GCNC 11705)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Akeno Observatory.
The observation started on 2011-02-13 8:37 UT (~3.3 hours after the burst).
We detected the previously reported afterglow (Cenko et al., GCN 11706)
in all three bands.

Photometric results and are listed below. We used GSC2.3 catalog for
flux calibration.

T0+[day]   MID-UT   T-EXP[sec]    g'             Rc           Ic
-----------------------------------------------------------------------
0.2083    10:17:51    2340      18.20+-0.06   17.28+-0.04   16.62+-0.04
-----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110213B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11725
SUBJECT: GRB 110213B: Swift XRT observation 
DATE:    11/02/14 15:22:15 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

S. Nakahira (AGU), N. Kawai, M. Morii (Tokyo Tech), and H. Negoro 
(Nihon U.) report on behalf of the MAXI team:

Swift observed the field of GRB 110213B (Negoro et al., GCN Circ. 11716) 
centered at the refined MAXI/GSC position reported by Morii et al. 
(GCN Circ. 11720) for 2 ks from 2011-02-14T03:42:19 (T0+47 ks).

We find three point sources in the XRT field of view:

Source          (R.A., Dec.)  J2000                         flux
------   -----------------------------------------------   -------
  A      (41.562 deg, +1.245 deg)= (02 46 15, +01 14 42)   0.008 c/s
  B      (41.757 deg, +1.146 deg)= (02 47 02, +01 08 46)   0.029 c/s
  C      (41.550 deg, +1.391 deg)= (02 46 12, +01 23 28)   0.003 c/s

Source A is located 0.1' from 1RXS J024615.3+011427, a RASS source 
identified to an AF star.
Source C is located 0.1' from a quasar Q 0243+011.
No catalogued source was found for Source B.

Source B, the brightest of the three, and found near the edge of the 
field of view, is the most likely candidate for the afterglow of 
GRB 110213B.  Another Swift observation is planned to confirm its fading.

We thank the Swift operation team for performing a prompt TOO observation 
and making the data available quickly.


GRB_name: GRB110205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11726
SUBJECT: GRB 110205A: Konkoly optical observations
DATE:    11/02/14 15:40:15 GMT
FROM:    Janos Kelemen at Konkoly Obs/Hungary  <kelemen@konkoly.hu>

J. Kelemen (kelemen at konkoly.hu) on behalf of the GRB OT observing program
at the Konkoly Observatory.

Starting on 05/02/2011 we observed the field of GRB 110205A detected
by Swift (trigger #444643; Beardmore et al., GCN 11629)) with a 60/90 cm 
Schmidt telescope located at the Mountain Station of the Konkoly Observatory
using V,R,I filters. Although the OT was visible on the frames we coadded
images to achieve better S/N ratio due to the cloudy weather.
The time column contains seconds counting from the trigger (J.D. 2455597.58520)

Time     Exp    Mag.    Error.   Filter    Flag.
 [s]     [s]          [3-sigma]
-------------------------------------------------
 61782    300 19.53   0.5       V
 66022   1800 18.97   0.4   R
 70312    300 19.63   0.4       V     
 71671   1500 19.92   0.5   R
 74194   1500 20.11   0.5   I
 75323    300 19.67   0.4   V
159722   2700 21.52   0.6   R     Upper Level
--------------------------------------------------


GRB_name: GRB110213A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11727
SUBJECT: GRB 110213A: Fermi GBM observation
DATE:    11/02/14 16:06:55 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (MPE)
reports on behalf of the Fermi GBM Team:

"At 05:17:11.27 UT on 13 February 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110213A (trigger 319267033 / 110213220)
which was also detected by the Swift/BAT
(D'Elia et al. 2011, GCN 11705).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 101 degrees.

The GBM light curve consists of two main pulses
with a duration (T90) of about 33 s (50-300 keV).
The time-averaged spectrum from T0-3.072 s to T0+31.745 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.44 (+/- 0.05) and
the cutoff energy, parameterized as Epeak, is 98.4 (+8.5/-6.9) keV.

The event fluence (10-1000 keV) in this time interval is
(1.03 +/- 0.03)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+18.17 s in the 10-1000 keV band
is 17.7 +/- 0.5 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110213A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11728
SUBJECT: Swift GRB110213A: interesting behaviour
DATE:    11/02/14 17:27:41 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL-UCL), V. D'Elia (ASDC) and P. Kuin (MSSL-UCL)
report, on behalf of the Swift team:

GRB110213A (D'Elia et al., GCN circ 11705) exhibits an interesting 
behaviour both in the X-ray and optical bands. After a broad peak and 
phase of normal decline, the lightcurves show achromatic breaks at about
T0+10 ks, after which the slopes in both bands becomes about -2. These 
data strongly indicate that we are seeing a very early jet break. We 
encourage observations from ground facilities.

The predicted magnitudes for 00:00 UT of 15/2/2011 are R ~ 22.6,
v ~ 21.7, b ~ 23.8, u ~ 21.7.


GRB_name: GRB110212A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11729
SUBJECT: GRB 110212A: Swift XRT and UVOT observations
DATE:    11/02/14 19:59:12 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia, G. Stratta (ASDC), N.P.M. Kuin (MSSL-UCL), report on behalf  
of the Swift team:

Swift XRT and UVOT instruments began observing the field of the BAT
burst GRB 110212A (D'Elia et al., GCN circ 11699) on 2011-02-13 at 23:21,
that is, 46 h (166.3 ks) after the burst trigger due to a Moon constraint.
The observations ended on 2011-02-14 at 02:47.
No candidate afterglow is detected in the BAT error circle.

UVOT observed in the uvm2 filter, with a total exposure time of 5885 s.
No new source is found in or near the BAT error circle from comparison
to the DSS image. The 5-sigma upper limit for a source is uvm2 > 20.3  
magnitudes.

XRT observations have a total exposure time of 5967 s, and yield a three sigma
upper limit of 1.4e-3 counts/second for any new source in the BAT  
error circle.

This circular is an official product of the Swift Team.

----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.


GRB_name: GRB110213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11730
SUBJECT: GRB110213A: RAPTOR Early Optical Peak and Plateau Measurements
DATE:    11/02/14 23:04:03 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis,
of Los Alamos National Laboratory report:

The RAPTOR telescope system responded to Swift trigger 445414
(V. D'Elia et al., GCN 11705) under fair observing conditions. Our
narrow-field instruments began observing the location at 05:17:58.2 UTC,
28.7 seconds after the initial BAT trigger.  We detect the optical
counterpart at the location reported by the Swift UVOT team.  The
counterpart brightens from below our threshold at around 100 seconds
after the BAT trigger.  It reaches a peak magnitude of 14.7 at T~300 s.
The counterpart then begins a steady decline to magnitude 16.0 at
T~2000 s.  At that point, the counterpart re-brightens to a plateau at
roughly magnitude 15.8 for about an hour before resuming the fading
behavior.  The following table gives a sample of our observations:

t-mid(s)    exp(s)     mag     mag-err
--------------------------------------------
143.80      10.0      15.23    0.03
352.60      10.0      14.68    0.02
2179.60     30.0      16.12    0.03
4522.90     30.0      15.58    0.03
7172.30     30.0      16.00    0.04

The unfiltered images were calibrated against the USNO-B1 R-band.


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11731
SUBJECT: GRB 110213A:  TNT optical observations
DATE:    11/02/15 03:08:19 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L.P. Xin, Y.L. Qiu, J.Y. Wei, J. Wang, J.S. Deng, 
C. Wu, X. H. Han, M, Zhai on behalf of EAFON report:

We observed GRB 110213A (V. D'Elia et al. GCN11705 ) 
with Xinglong TNT telescope for two epochs from Feb 13th to Feb 14th.
A series of R-band  images were obtained with an exposure 
time of 300 sec for each frame. 

The optical afterglow counterpart  (e.g.  V. D'Elia et al. GCN11705; 
Cenko GCN 11706; Wren et al. GCN 11730 ) 
could be clearly detected in each frame otained at Feb 13th. 
It was also detected at Feb 14th after combining 12 frames.

The brightness of the afterglow was estimated to be about 
20.2 +/- 0.2 mag relatively to USNO B1.0 R2 mag 
at the mean time of 1.24 days after the burst. 

Further observations  are encouraged.

This message may be cited.


GRB_name: GRB110213B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11732
SUBJECT: GRB 110213B: P60 Optical Afterglow Candidate
DATE:    11/02/15 06:24:24 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), E. O. Ofek, S. R. Kulkarni (Caltech), and A.
Rau (MPE Garching) report on behalf of a larger collaboration:

We have imaged the location of the possible X-ray afterglow
(Source "B"; Nakahira et al., GCN 11725) of the MAXI GRB110213B (Negoro et
al., GCN 11716) with the automated Palomar 60-inch telescope.
Observations began at 3:38 UT on 2011 February 15 (~ 37.1 hours after the
burst) in the r' filter.

We detect a source near the reported XRT position with coordinates
(J2000):

   02:47:01.41  +01:08:46.3

Using several nearby objects in the USNO-B1 catalog for reference, we
measure a magnitude at this time of R = 19.8.  No object is present at
this location, either in the USNO-B1 catalog or the Digitized Sky Survey.
Given the positional coincidence and the relative brightness, we consider
it likely this is the optical afterglow of GRB110213B.  However, future
observations to establish fading will be required for confirmation.


GRB_name: GRB110213A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11733
SUBJECT: GRB 110213A: YNAO-GMG  Observations
DATE:    11/02/15 06:46:12 GMT
FROM:    Jirong Mao at INAF-OAB  <jirong.mao@brera.inaf.it>

Zhao X. H., Bai J. M., & Mao J. report on behalf of the YNAO-GMG Observation:

We observed GRB110213A (D'Elia et al., GCN circ 11705)  using one 2.4m
telescope of Yunnan Observatory located at Gao-Mei Gu (GMG) about 7hr
after the trigger. The afterglow was clearly detected. The preliminary
results are:

mid time (UT)          filter   exposure time (min)  magnitude
2011-02-13 12:48:22       R           20                17.4
2011-02-13 13:08:55       V           20                18.2
2011-02-13 13:34:29       B           30                18.9
2011-02-13 14:00:28       B           20                19.0
2011-02-13 14:20:39       V           20                18.3
2011-02-13 14:40:50       R           20                18.3

The magnitudes were calibrated by NOMAD1.

This meesage may be cited.


GRB_name: GRB110210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11734
SUBJECT: GRB 110210A: ROVOR Upper Limit
DATE:    11/02/15 21:31:38 GMT
FROM:    J. Ward Moody at BYU  <rovor.byu@gmail.com>

Bret L. Little, Ben Boizelle, Kimberly Bates, Michael Abbott, and J.
Ward Moody report for
Brigham Young Universitys ROVOR team:

We report our observations in the field of GRB 110210A (Swift trigger
445141, D'Elia et al., GCN 11687) on Feb 11 beginning 16.25 hours post-burst
at 02:09:18 UT. The 0.41m ROVOR telescope in Delta, Utah,
automatically imaged this location upon power up.

We combined sixteen 120 second exposures, four each in BVRI. No
detection of an afterglow
inside the XRT error circle (Goad, et al., GCN. Circ. 11689) was obtained
after stacking the images. An upper limit of 20.0  0.5 mag in R2
was found by comparing against USNOB values.


GRB_name: GRB110213B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11735
SUBJECT: GRB 110213B: Possible Host Galaxy in SDSS Stripe 82 Imaging
DATE:    11/02/16 01:20:22 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko, J. S. Bloom, and A. A. Miller (UC Berkeley) report on behalf
of a larger collaboration:

The location of the X-ray (Nakahira et al., GCN 11725) and optical (Cenko
et al., GCN 11732) afterglow of GRB 110213B (Negoro et al, GCN 11716) was
observed repeatedly over the seven year period beginning in 1998 as part
of the SDSS Stripe 82 Survey (Bramich et al., MNRAS 2008, 386, 887).  We
have extracted all images covering this location from the SDSS Stripe 82
database to create stacked frames in the g, r, and i filters.  A
false-color composite image of the afterglow location can be found at:

   http://astro.berkeley.edu/~cenko/public/grb/GRB110213B/sdss.png

Using 10 nearby point sources from SDSS for astrometry, we measure a
revised position for the P60 optical afterglow candidate of (J2000):

  RA: 02:47:01.45  Dec: +01:08:46.5

The measured uncertainty in the P60-SDSS astrometric tie is 100 mas in
each coordinate.

Offset by 0.9" from the location of the afterglow, we find an extended
source in the pre-outburst SDSS Stripe 82 imaging in all three filters.
We measure coordinates (J2000) for this source:

   RA: 02:47:01.41  Dec: +01:08:47.2

Using several nearby point sources from SDSS for comparison, we measure
magnitudes of g' = 23.7, r' = 22.8, i' = 22.3  Additional emission is
marginally detected in the i' filter approximately 3" south of this
position, but its relation to this object is unclear.

This extended source could be a relatively nearby host galaxy for
GRB110213B, although the red colors are somewhat unusual for GRB hosts.


GRB_name: GRB110213B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11736
SUBJECT: GRB 110213B: Gemini South Redshift
DATE:    11/02/16 04:10:22 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), J. X. Prochaska (UC Santa Cruz / Lick
Observatory), A. Cucchiara, D. A. Perley, and J. S. Bloom (UC Berkeley)
report on behalf of a larger collaboration:

We have obtained a spectrum of the candidate optical afterglow of GRB
110213B (Negoro et al., GCN 11716) with the Gemini Multi-Object
Spectrograph mounted on the 8-m Gemini South telescope.  Observations
began at 00:44 UT on Feb. 16 and cover the wavelength range from 3900 -
6700 A.

Superposed on a smooth continuum, we detect a series of strong, narrow
absorption lines corresponding to Mg I, Mg II, Fe II, and Fe II* at a
common redshift of z = 1.083.  The detection of fine structure lines
firmly establishes this as the redshift of the GRB host galaxy.

An additional, strong Mg II absorption system is also present at z =
0.717.  This may be related to the potential host candidate identified in
pre-outburst SDSS Stripe 82 imaging (Cenko et al., GCN 11735).

At z = 1.083, the prompt fluence measured by Konus (Golenetskii et al.,
GCN 11722) correponds to a prompt isotropic energy release of 5.5e52 erg
(20 - 1400 keV observer-frame bandpass).

We wish to thank the staff at Gemini Observatory, in particular Fredrik
Rantakyro, for the prompt execution of these observations.


GRB_name: GRB110210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11737
SUBJECT: GRB 110210A: optical upper limit
DATE:    11/02/16 09:14:17 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (SAI MSU), Korobtsev (ISTP),  E. Klunko (ISTP),  A.
Pozanenko (IKI) on behalf of larger GRB follow up collaboration
report:

We observed the field of the Swift GRB 110210A (D'Elia et al., GCN
11687) with AZT-33IK telescope of Sayan observatory (Mondy) on Feb. 10
between (UT) 11:10 - 12:28 under poor weather conditions and mean
seeing of about ~2.3". We took several series with exposure of 60
seconds in R-band. In a stacked image we do not detect any source in
enhanced XRT error circle (Goad et al. GCN 11689). The upper limit (3
sigma) of the stacked image based on SDSS field star
J005218.01+0746740.1 (assuming R = 18.73) is the following:

T0+      Filter,   Exposure,      OT mag.,  UpperLimit
(mid, d)              (s)

0.08122  R      69x60               n/d           19.4


GRB_name: GRB110210A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11738
SUBJECT: Swift/UVOT observations of GRB110210a.
DATE:    11/02/16 13:25:39 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and V. D'Elia (ASDC) on behalf of the
Swift/UVOT team report:

The Swift/UVOT began settled observations of the field of GRB
110210A 144 s after the BAT trigger (D'Elia et al., GCN Circ.
11687). No optical afterglow consistent with the enhanced XRT position 
(Goad et al., GCN Circ. 11689) is detected in the initial UVOT finding 
charts nor in the summed exposures in all filters. (Poole  et al. 2008, 
MNRAS, 383, 627) for the finding chart (FC) exposures and subsequent 
exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           144          294          147         >20.1
u_FC               302          552          246         >19.4
white              144         7686          746         >21.0
v                  633        13497         1238         >19.7
b                  558         7481          526         >20.1
u                  302         7276          756         >19.9
w1                 682         7072          294         >19.5
m2                 660        18180          839         >20.6
w2                 608        12588         1291         >21.0

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.06 in the direction of the burst
(Schlegel et al. 1998).

[GCN OPS NOTE(16feb11): Per author's request, the author list was added.]


GRB_name: GRB110205A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11740
SUBJECT: GRB110205A:  EVLA Observations
DATE:    11/02/16 17:37:36 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer (Harvard), D. Frail (NRAO), and E. Berger (Harvard) report:

We observed the position of GRB 110205A (GCN 11629) with the EVLA 
starting 1.2 days after the burst.  Preliminary reduction of these data 
gives a flux density of 182 +/-12 microJy at a frequency of 22 GHz. 
Further EVLA observations are on-going.

We thank the EVLA staff for their support of these observations.


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11742
SUBJECT: GRB 110213A: optical observations in Mondy
DATE:    11/02/16 19:00:13 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU), A. Pozanenko (IKI),  I. Korobtsev (ISTP),  E. Klunko 
(ISTP) on behalf of larger GRB follow up collaboration report:

We observed the  Swift GRB 110213A (D'Elia et al., GCN 11705)  with AZT-33IK 
telescope of Sayan observatory (Mondy) between Feb.13  (UT) 11:23 - 13:21 
(Korobtsev et al.,  GCN 11713) and Feb. 15 (UT) 11:55 - 12:55. We took 
several series in both epochs in R filter. The optical afterglow (D'Elia et 
al., GCN 11705, Cenko GCN 11706, Rujopakarn et al., GCN 1707) is clearly 
visible on single 60 s exposure images on Feb. 13, and  afterglow is visible 
in a stacked image on Feb. 15. During our observations within 2 hours on 
Feb. 13 (0.2555 - 0.3316 days after burst) the brightness of the afterglow 
was not changing within error bars of about 0.06m. One can suggest that we 
observed a plateau phase or a broad peak of the afterglow light curve. The 
afterglow is still bright (R ~ 20.45) at 2.297 days after burst.

The photometry based on the USNO-B1.0 star 1392-0070724 (J2000) RA=02 51 
53.41, Dec= +49 16 02.9, assuming R=16.83:

T0+       Filter,   Exposure, OT mag.,
(mid, d)              (s)

0.2555  R          4x60        17.61 +/- 0.06
0.3260  R          4x60        17.76 +/- 0.07
2.2973  R          3600        20.45 +/- 0.12

The photometry above is still preliminary.

[GCN OPS NOTE(30apr11): Per author's request, Elunko was changed to Klunko.]


GRB_name: GRB110213B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11743
SUBJECT: GRB 110213B: GROND observations of the optical/NIR afterglow
DATE:    11/02/16 19:35:01 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

J. Elliott (MPE Garching), A. Nicuesa Guelbenzu (TLS Tautenburg), T.
Kruehler and J. Greiner (both MPE Garching) report on behalf of the GROND
team:

We observed the afterglow (Cenko et al., GCNs #11732, 11736) of GRB
110213B (Negoro et al., GCN #11716 & Morii et al., GCN #11720)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPI/ESO telescope at La Silla Observatory
(Chile).

Observations started at 01:22 UT on 16.02.2011, 2.45 days after the GRB
trigger and were performed at high airmass.

Based on a stacked image with exposure time of 460 s, we estimate a
preliminary r' band magnitude of r' = 20.8 +/- 0.1 calibrated against SDSS
field stars. This implies a fading with respect to the earlier measurement
of Cenko et al. (#GCN 11732). In addition, the SED of the object is
consistent with a power-law, and hence we confirm the source as the
optical afterglow of GRB 110213B.


GRB_name: GRB110213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11744
SUBJECT: GRB 110213A: optical observations in CrAO
DATE:    11/02/17 05:56:48 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

V. Rumyantsev(CrAO),  K. Antoniuk (CrAO), A. Pozanenko (IKI) report on
behalf of larger GRB  follow-up collaboration:

We observed  the field of the Swift GRB 110213A (D'Elia et al., GCN 11705)
with AZT-11 telescope of CrAO between Feb. 14 (UT) 19:25 - 20:25 under poor
seeing of about 5". We do not detect the UVOT afterglow up to R=19.5 (3
sigma). The photometry based on the USNO-B1.0 star 1392-0070724 (J2000) 02
51 53.41 +49 16 02.9, assuming R=16.83:

T0+      Filter,   Exposure, OT mag., UpperLimit
(mid, d)              (s)

1.6095  R         20x180     n/d          19.5


GRB_name: GRB110213B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11748
SUBJECT: GRB110213B: X-ray afterglow confirmation
DATE:    11/02/18 09:11:45 GMT
FROM:    Raffaella Margutti at U. di Milano Bicocca  <raffaella.margutti@brera.inaf.it>

R. Margutti, (INAF-OAB), Nakahira (AGU), M. Morii, N. Kawai (Tokyo Tech),
H. Negoro (Nihon U.) and A. Melandri (INAF-OAB) report on behalf of the
Swift-XRT and MAXI team:

The Swift-XRT conducted a second observation of GRB 110213B (Negoro et
al. GCN. Circ. 11716), gathering 4.9 ks of data between T0+250ks and
T0+275 ks. Source B reported by Nakahira (GCN Circ. 11725)
has faded to a level of  0.005 +/- 0.001 count/sec, with a power-law decay
index of alpha= -1.4 +/- 0.3. This source is thus confirmed as the X-ray
afterglow of GRB 110213B.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020157.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110213B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11749
SUBJECT: GRB 110213B: Swift/UVOT observations
DATE:    11/02/18 13:51:47 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) & R. Margutti, (INAF-OAB) reports on behalf of  
the Swift-UVOT team

The Swift/UVOT began settled observations of the field of the MAXI GRB  
110213B
~13hrs after the trigger (Negoro et al., GCN Circ. 11716). The optical  
afterglow
detected by P60 (Cenko et al, GCN Circ. 11732, 11735) and GROND  
(Elliott et al,
GCN Circ. 11743) only lies in the UVOT field of view for 3 images, one  
per
filter (white, v and u) obseved at ~3 days after the trigger.

Preliminary magnitudes using the UVOT photometric system (Poole et al.  
2008,
MNRAS, 383, 627) for the single exposures at the location of the optical
afterglow are:

Filter  T_start(s)  T_stop(s)   Exp(s)       3sigUL
#####################################################
wh        256170     256432      259         > 20.78
v         256438     256691      249         > 19.23
u         255901     256164      259         > 19.62
#####################################################

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB101225A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11751
SUBJECT: GRB 101225A, the review of the sky area in plate archives
DATE:    11/02/20 13:39:08 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

GRB 101225A, the review of the sky area in plate archives 
V.V. Golovnya, L.M. Kizyun, L.K. Pakuliak (Main Astro Obs, Kyiv) 
report: 

We have undertaken the review of the sky area of GRB 101225A  
(P.A. Evans et al., GCN 11497) on astronegatives, collected  
in Ukrainian NAS Main astronomical observatory plate archive  
(1976-1996). All the plates with the possible object appearance 
are digitized using Microtek ScanMaker 9800XL TMA flatbed scanner 
and have been placed into Golosiiv Plate Archive database DBGPA  
with open access to them. No any object has been found in the 
point with the mentioned coordinates of GRB.

The list of plates is given in the table:
 
YYYYMMDD UT Plates                  Exp. LimMag 
19850815 00:26:01 GUA040C000702A 16.0 16.15 
19841212 16:51:23 GUA040C000587  16.0 15.35
19840827 23:46:55 GUA040C000468A 16.0 15.35
19930923 21:33:33 GUA040C002237         18.0 15.35
19840827 23:12:28 GUA040C000467A 16.0 16.10
19840905 22:33:06 GUA040C000491  18.0 16.35
19850815 00:02:05 GUA040C000701  16.0 16.15
19871024 19:40:17 GUA040C001153A 18.0 15.35
19840809 01:08:44 GUA040C000441  16.0 14.10
19840905 22:58:22 GUA040C000492A 18.0 16.55

Plates: the plate's identifier in GUA040C archive of DWA 
           (D/F=400/2000, M=103"/mm)
           of the Ukrainian NAS Main Astro obs in Kyiv
          (Marsden's number - 83)[1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 15 minutes area around the  
        location given in P.A. Evans et al., GCN 11497: 
        RA (J2000): 00h 00m 47.47s, Dec (J2000): +44d 36' 01.0". 

The preview images of 10 areas together with  
the 15 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/101225A/index.html
The images with full resolution are available via e-mail on demand. 

References: 
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0), 
http://gua.db.ukr-vo.org 


GRB_name: GRB110223A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11753
SUBJECT: GRB 110223A: Swift detection of a burst
DATE:    11/02/23 21:09:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

T. Sakamoto (NASA/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
P. A. Evans (U Leicester), J. M. Gelbord (PSU),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
M. Stamatikos (OSU/NASA/GSFC) and C. A. Swenson (PSU) report on behalf
of the Swift Team:

At 20:56:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110223A (trigger=446674).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 345.599, +87.567 which is 
   RA(J2000)  =  23h 02m 24s
   Dec(J2000) = +87d 34' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 5 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 20:58:27.8 UT, 88.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 345.85923, 87.55851 which
is equivalent to:
   RA(J2000)  = 23h 03m 26.22s
   Dec(J2000) = +87d 33' 30.6"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 50 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (5.61 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.5
(+1.82/-1.63) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 8.97e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 97 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.34. 

Burst Advocate for this burst is T. Sakamoto (Taka.Sakamoto AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110223B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11754
SUBJECT: GRB 110223B: Swift detection of a burst
DATE:    11/02/23 21:39:45 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@astro.psu.edu>

M. Stamatikos (OSU/NASA/GSFC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
S. Campana (INAF-OAB), P. A. Evans (U Leicester), J. M. Gelbord (PSU),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC),
E. Sonbas (GSFC/USRA/Adiyaman Univ.), R. L. C. Starling (U Leicester),
C. A. Swenson (PSU) and E. Troja (NASA/GSFC/ORAU) report on behalf of
the Swift Team:

At 21:25:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110223B (trigger=446677).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 150.276, -68.329 which is 
   RA(J2000) = 10h 01m 06s
   Dec(J2000) = -68d 19' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 21:27:00.0 UT, 72.0 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 150.2339,
-68.3019 which is equivalent to:
   RA(J2000)  = 10h 00m 56.15s
   Dec(J2000) = -68d 18' 06.7"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 112 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.29
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 77 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The coverage of the XRT error circle by the 8'x8' region
for the list of sources generated on-board is uncertain because the large
number of sources filled the available telemetry. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.23. 

Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110223A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11755
SUBJECT: GRB 110223A: Observations from BOOTES-2
DATE:    11/02/23 22:49:23 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

M. Jelinek, (IAA-CSIC), A. de Ugarte Postigo (DARK/NBI), 
P. Kubanek and A.J. Castro-Tirado (IAA-CSIC) 
on behalf of a larger collaboration report:

   We have observed the afterglow of GRB 110223A (Sakamoto 
et al., GCNC 11753) with the 0.6m TELMA/BOOTES-2 located in
Malaga (Spain). R-band observations began 228 seconds after
the burst. We do not detect any source within the XRT error
box down to the following detection limits, as compared with
the USNO-B1.0 catalogue:

exp start(t-t0) integration 3-sigma limit
228  3  15.4
228      669  17.6
930  1035  18.0

This message can be cited.


GRB_name: GRB110223B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11756
SUBJECT: GRB 110223B: GROND Detection of Optical Afterglow Candidate
DATE:    11/02/24 01:49:21 GMT
FROM:    Felipe Olivares Estay at MPE  <felipe@mpe.mpg.de>

V. Sudilovsky, J. Elliott, F. Olivares E., and J. Greiner (MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 110223B (Swift trigger 446677; Stamatikos
et al., GCN #11754) simultaneously in g'r'i'z'JHK with GROND (Greiner
et al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at
La Silla Observatory (Chile).

Observations started at 00:05 UT on February 24th, 2.7 hours after the
GRB trigger, and are continuing. They were performed at an average
seeing of 1.4" and at an average airmass of 1.6.

We found a single point source within the 2.1" Swift/XRT error circle
reported by Stamatikos et al. (GCN #11754) at

RA (J2000) = 10h 00m 55.98s
DEC (J2000) = -68d 18' 06.0"

with an uncertainty of 0.3" in each coordinate.

Based on 7.7 min exposure started at 00:30 UT, we estimate a
preliminary r'-band magnitude of 22.1 +/- 0.1 calibrated against GROND
zero points (AB system). No statements about the variability can be
made at this stage. This measurement is not corrected for the
considerable Galactic foreground extinction corresponding to a
reddening of E(B-V)=0.226 mag in the direction of the burst (Schlegel
et al. 1998).


GRB_name: GRB110223B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11757
SUBJECT: GRB 110223B: Swift-BAT refined analysis
DATE:    11/02/24 04:32:27 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-120 to T+293 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110223B (trigger #446677)
(Stamatikos, et al., GCN Circ. 11754).  The BAT ground-calculated position is
RA, Dec = 150.340, -68.329 deg, which is 
   RA(J2000)  =  10h 01m 21.6s 
   Dec(J2000) = -68d 19' 44.3" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows the burst start with a small peak
at ~T-45 sec, a slightly larger peak at ~T+2 sec out to ~T+20 sec, with on-going
low-level emission out to ~T+150 sec.  T90 (15-350 keV) is 54.0 +- 8.5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-45 to T+20 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.65 +- 0.21.  The fluence in the 15-150 keV band is 6.1 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.99 sec in the 15-150 keV band
is 0.6 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/446677/BA/


GRB_name: GRB110223B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11758
SUBJECT: GRB 110223B: Enhanced Swift-XRT position
DATE:    11/02/24 07:31:33 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2282 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 110223B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 150.23341, -68.30155 which is equivalent
to:

RA (J2000): 10h 00m 56.02s
Dec (J2000): -68d 18' 05.6"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110223A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11759
SUBJECT: GRB 110223A: Enhanced Swift-XRT position
DATE:    11/02/24 08:51:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 539 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 110223A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 345.85354, +87.55766 which is equivalent
to:

RA (J2000): 23h 03m 24.85s
Dec (J2000): +87d 33' 27.6"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110223B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11760
SUBJECT: GRB 110223B: Swift-XRT refined Analysis
DATE:    11/02/24 09:48:29 GMT
FROM:    Antonia Rowlinson at U.of Leicester  <bar7@star.le.ac.uk>

A. Rowlinson (U. Leicester) and M. Stamatikos (OSU/NASA/GSFC) report on
behalf of the Swift-XRT team:

We have analysed 5.3 ks of XRT data for GRB 110223B (Stamatikos  et al.
GCN Circ. 11754), from 56 s to 24.6 ks after the  BAT trigger. The data
comprise 85 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 11758).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.8 (+0.9, -0.7), followed by a break at T+99.5 s to an
alpha of 0.92 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.85 (+/-0.16). The
best-fitting absorption column is  1.7 (+0.5, -0.4) x 10^21 cm^-2,
consistent with the Galactic value of 1.3 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.5 x 10^-11 (5.9 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.85 (+/-0.16)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00446677.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110223A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11761
SUBJECT: GRB 110223A: Swift-XRT refined Analysis
DATE:    11/02/24 09:52:03 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@star.le.ac.uk>

O. M. Littlejohns (U. Leicester) and T. Sakamoto (NASA/UMBC) report on
behalf of the Swift-XRT team:

We have analysed 2.7 ks of XRT data for GRB 110223A (Sakamoto  et al.
GCN Circ. 11753), from 78 s to 29.6 ks after the  BAT trigger. The data
comprise 40 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 11759).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.96 (+0.50, -0.27), followed by a break at T+386 s to
an alpha of 0.52 (+0.15, -0.16).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.4 (+0.4, -0.3). The
best-fitting absorption column is  2.3 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 5.6 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (6.6 x 10^-11) erg
cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 5.6 x 10^20 cm^-2
Excess significance: 4.5 sigma
Photon index:      2.4 (+0.4, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00446674.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110223A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11762
SUBJECT: GRB 110223A: Liverpool Telescope observations
DATE:    11/02/24 11:24:50 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB),
I.A. Steele, C.G. Mundell, S. Kobayashi (Liverpool JMU),
A. Gomboc (U. Ljubljana) on behalf of a large collaboration report:

The 2-m Liverpool Telescope automatically began observing
GRB 110223A (Sakamoto et al. GCN Circ. 11753) on February 23,
20:59:47 UT, 2.8 minutes from the GRB trigger time with the
SDSS filters riz.
Within the UVOT-enhanced XRT error circle (Evans et al.,
GCN Circ. 11759) we do not find any source down to the following
limiting magnitudes.

Mid time from      Tot Exposure    Filter   Limiting Magnitude
trigger (s)           (s)
------------------------------------------------------------
1920                  780           r > 22.2
2320                  720           i > 21.6
2620                  720           z > 19
------------------------------------------------------------

Calibration is against some nearby USNOB-1 stars (R2 and I magnitudes).
However, we note the presence of an uncatalogued source at

RA  =  23:03:20.31,
Dec = +87:33:29.3 (J2000),

lying 3.4" from the XRT centre with the following magnitudes:

r = 21.6 +- 0.1
i = 20.9 +- 0.1

This source does not exhibit any fading during the observations.


GRB_name: GRB110223A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11763
SUBJECT: GRB 110223A :  early optical limit by "Pi of the Sky"
DATE:    11/02/24 11:24:51 GMT
FROM:    Marcin Sokolowski at Soltan Inst. Nuc Studies,Warsaw  <marcin.sokolowski@fuw.edu.pl>

M.Sokolowski,T.Batsch,A.Majcher,A.Majczyna,K.Nawrocki,J.Uzycki,G.Wrochna (SINS, Swierk),
M.Cwiok,W.Dominik,L.W.Piotrowski,A.F.Zarnecki (University of Warsaw),
K.Malek,L.Mankiewicz,R.Opiela,M.Siudek,V.Repei (CFT PAN),
G.Kasprowicz,M.Zaremba (Warsaw University of Technology),
from the "Pi of the Sky" collaboration ( http://grb.fuw.edu.pl ).
M. Jelinek and A. J.Castro-Tirado (IAA-CSIC Granada) on behalf of a larger collaboration.

The wide field "Pi of the Sky North" apparatus installed in the BOOTES-1
station at ESAt/INTA-CEDEA in Mazagon (Huelva, Spain; 
http://grb.fuw.edu.pl/pi/index.html#piinta_site.htm )
started observing position of GRB 110223A 25 seconds after BAT trigger,
165 seconds after the burst. No new source has been identified on 10s exposures
nor on the sums of images corresponding to 50s exposure. 
Following limits were obtained:

t_start - t0      start (UT)  end (UT)     3-sigma limit

    165            20:59:44  - 20:59:54        11.0

    165            20:59:44  - 21:00:45        12.0


where limits are based on the reference star magnitudo in V filter.


GRB_name: GRB110223A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11764
SUBJECT: GRB 110223A: Swift-BAT refined analysis
DATE:    11/02/24 13:27:17 GMT
FROM:    Michael Stamatikos at OSU/GSFC  <michael.stamatikos-1@nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), 
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt 
(GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos 
(OSU/NASA/GSFC), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+300 sec from the recent telemetry downlink, 
we report further analysis of BAT GRB 110223A (trigger #446674) 
(Sakamoto, et al., GCN Circ. 11753).  The BAT ground-calculated position is 
RA, Dec = 345.386, 87.586 deg which is 
   RA(J2000)  =  23h 01m 32.7s 
   Dec(J2000) = +87d 35' 11.3" 
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.
 
The mask-weighted light curve shows a FRED-like peak at ~T+0.5 sec. T90 (15-350 keV) 
is 7.0 +- 2.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.1 to T+8.1 sec is best fit by a simple 
power-law model.  The power law index of the time-averaged spectrum is 
1.70 +- 0.33.  The fluence in the 15-150 keV band is 1.6 +- 0.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+0.08 sec in the 15-150 keV band is 
0.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at 
http://gcn.gsfc.nasa.gov/notices_s/446674/BA/


GRB_name: GRB110223B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11765
SUBJECT: Swift/UVOT observations of GRB110223b
DATE:    11/02/24 13:46:54 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

  Swift UVOT observations of GRB110223b

M. De Pasquale (MSSL-UCL) and M. Stamatikos (GSFC) report, on behalf of 
the Swift team:

Swift/UVOT began settled exposures of GRB110223b (Stamatikos et al. GCN 
circ. 11754) 77 s after the trigger with a white finding chart. There is 
an uncatalogued source 1.5 arcseconds from the enhanced XRT afterglow 
position (Beardmore et al., GCN  circ. 11758). This position is also 
consistent with the optical transient found by GROND (Sudilovsky et al., 
GCN circ. 11756)

This source, which we identify as the optical afterglow of the burst, is 
detected in white, v, b, u. Magnitudes and 3 sigma upper limits, derived 
using the UVOT photometric system  (Poole et al. 2008, MNRAS, 383, 627),
are shown in the table below. We caution that the photometry is complicated
by a crowded field.

Filter        T_start(s)    T_end(s)        exp           Magnitude

white (FC)       77            227          147.4       18.98  0.10
white           620            814           39.0       19.70  0.30
white           870           1546          206.0       19.61  0.13

v               620           1596          117.3       17.88  0.15

b               546           1522           97.4       19.57  0.30

u (FC)          290            540          245.8       19.20  0.19
u               694           1496           77.8       >19.30

uw1             670           1471           97.4       >19.16

um2             645           1445           97.4       >18.78

uw2             596          1572           116.7       >19.16

These magnitudes are not corrected for the strong Galactic extinction 
along the line of sight, corresponding to E(B-V) = 0.23 (Schlegel et al. 
1998)


GRB_name: GRB100703A
Detection_method: IBAS
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11766
SUBJECT: IBAS distribution of coordinates for low significance INTEGRAL GRB triggers
DATE:    11/02/24 16:18:42 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

S.Mereghetti (INAF IASF-Milano), D.Gotz (CEA-Saclay), J. Borkowski (CAMK, 
Torun), M. Beck, C.Ferrigno (ISDC, Versoix), on behalf of the IBAS 
Localization Team announce:

A new version of the IBAS Alert Distribution system is operational at the 
INTEGRAL Science Data Center. In addition to the already available 
functionalities, the new version distributes in real time also Alert 
Packets for low significance triggers discovered in the field of view of 
the IBIS imager.

The new Alert Packets are called WEAK Alerts and are identified by the 
field PKT_TYPE=6 (see http://www.isdc.unige.ch/integral/science/grb#IBAS 
for details on the different Alert types).

Users interested to receive the Alert Packets of the new type "WEAK" 
should contact the ISDC IBAS team (isdc-ibas@unige.ch).

The threshold for the distribution of the usual high significance IBAS 
triggers remains unchanged at

SIGMA= 8.0   (Alert Packets with PKT_TYPE= 3 (WAKEUP))

while the threshold for the distribution of low significance IBAS triggers is 
currently set at

SIGMA= 6.5   (Alert Packets with PKT_TYPE= 6 (WEAK))

This threshold corresponds to a rate of a few WEAK Alert Packets per week, 
but it could be adjusted in the future.

Many WEAK alerts will be produced by statistical fluctuations, but there 
is also a non negligible probability that some of them are due to real 
astrophysical events. In most cases it is not possible to recognize the 
GRBs based only on the INTEGRAL data, but the detection of afterglows 
could confirm some of these events as genuine GRBs.

Several bursts that were confirmed by off-line interactive analysis of the 
INTEGRAL data produced triggers above the threshold currently adopted for 
the WEAK alerts. Recent examples include the two short bursts GRB 100703A 
(GCN Circ. n.10936) and GRB 110112B (GCN Circ. n.11562) and the long burst 
GRB 100909A (GCN Circ. n.11260).

WEAK Alert Packets provide a single sky position, with error radius 
smaller than 4 arcmin. They are intended for robotic telescopes which can 
react without a negative impact on scheduled observing programmes. The 
value of SIGMA in the WEAK Alert Packet can be used as a figure of merit.

WEAK Alert Packets may or may not be followed by the usual WAKEUP and/or 
REFINED Alert Packets, depending on the evolution of the detected signal.
WEAK alerts for events belows WAKEUP threshold are neither confirmed nor
cancelled with an OFFLINE packet.

For further details see
http://ibas.iasf-milano.inaf.it/IBAS_News.html

It is recommended that current ibas clients upgrade their IBAS Client 
Software to the version 2.1.0 (available at 
http://www.isdc.unige.ch/integral/analysis#Software), although the 
previous versions should process WEAK alert without problems.


GRB_name: GRB110223A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11767
SUBJECT: GRB GRB 110223A: MASTER VWF early optical observations 
DATE:    11/02/24 16:32:33 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk

K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University

E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University

V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

MASTER II  robotic telescopes (MASTER-Net: http://observ.pereplet.ru) 
located in  Amur-Blagoveschensk  was pointed to the GRB110223A 7sec after 
notice time and  147 sec after GRB time.
Unfortunately, main telescopes was not  in focus.
But we have images from Very Wide Filed Cameras mounted on telescope. 
On our first (5s exposure) set 
we haven't found optical transient  within SWIFT-BAT error-box 
(Littlejohns et al., GCN Curc 11761) brighter 12 mag (unfiltered).
12   coaded first images give limit 13 mag (mean time ~ 177 sec after 
trigger).

The message may be cited.
The first image is available at 
http://observ.pereplet.ru/images/GRB110223A/first.jpg
There is Polar star at right  botom  angle of the image.

mailto: lipunov@sai.msu.ru


GRB_name: GRB110215A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11768
SUBJECT: No IPN GRB detected in conjunction with candidate GRB 110215
DATE:    11/02/24 18:39:38 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN,

V. Connaughton, M. Briggs, and C. Meegan, on behalf of the
Fermi-GBM team,

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team,

A. von Kienlin and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team,

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, 

J. Goldsten, on behalf of the MESSENGER NS GRB team,

K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team,

E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci,
I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta, 
for the SuperAGILE team,

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi, 
on behalf of the AGILE MCAL team,

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of
the Swift-BAT team, and

I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin,
W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on 
behalf of the Mars Odyssey GRB team, report:

We have examined the data from  9 IPN spacecraft (RHESSI, Konus,
INTEGRAL SPI-ACS, Swift BAT, MESSENGER, Mars Odyssey-HEND, Fermi GBM,
Suzaku WAM, and AGILE) for evidence of a gamma-ray burst in conjunction
with the optical transient associated with 2MASS J00264184+8324093 (GCN
11739).  In most cases, the GRB-sensitive instruments were on,
operating under good conditions, and the source was not Earth-blocked
to them.  There were two exceptions, however.  There was a gap in the
Mars Odyssey-HEND data which prevented the search for a response.
Also, the position was far outside the Swift-BAT field of view (148
degrees from the boresight) and close to the Earth's limb, making BAT
rather insensitive to gamma-rays from the source.

The Fermi GBM was the most sensitive instrument; the source position
was not occulted to Fermi by the Earth at the time of the OT, and
several GBM detectors had a favorable geometry to the source position.

No trigger or rate increase was detected around the time of the
transient in any of the data.  The most sensitive instruments in the
IPN detect short duration bursts with fluences down to several times
10^-8 erg cm^-2 , and long duration bursts with fluences which are
several times this value; thus we suggest that any burst associated
with the transient must have had a fluence lower than ~3 x 10^-8 erg
cm^-2, depending on its time history and energy spectrum.


GRB_name: GRB110223A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11769
SUBJECT: Swift/UVOT observations of GRB110223A
DATE:    11/02/24 23:12:30 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and T. Sakamoto (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110223A
97 s after the BAT trigger (Sakamoto et al., GCN Circ. 11753).
No optical afterglow consistent with the XRT enhanced position
(Evans et al., GCN circ. 11759) is detected in the initial UVOT exposures
nor in the summed exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

Filter       T_start(s)    T_end(s)   Exp     Magnitude

white (fc)        97          246     147 >20.81
white             97         5588     344 >21.16

v                639         5998     217 >19.40

b                565         5383     216 >20.00

u (fc)           310          559     196 >19.41
u                310         5177     443 >20.15

uw1             4773         6408     393 >20.13

um2              663         6203     412 >20.14

uw2              615         5794     216 >19.89

The above magnitudes are not corrected for the strong Galactic
extinction along the line of sight, corresponding to E(B-V) = 0.34
(Schlegel et al. 1998).


GRB_name: GRB101225A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11770
SUBJECT: GRB101225A:  early EVLA Observations of Christmas Burst
DATE:    11/03/03 05:05:26 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger, and W. Fong (Harvard) report:

We observed the position of the Christmas GRB 101225A for 32 minutes 
with the EVLA at a frequency of 5 GHz on 2010 December 30.03, less than 
five days after the burst (GCN 11493).  We find no significant radio 
source at the XRT position (GCN 11497) to a 3-sigma upper limit of 60 
microJy.

We thank the EVLA staff for their support of these observations over the 
holidays.


GRB_name: GRB110301A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11771
SUBJECT: GRB 110301A: Fermi GBM detection
DATE:    11/03/03 08:56:47 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (MPE)
reports on behalf of the Fermi GBM Team:

"At 05:08:43.07 UT on 01 March 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 110301A (trigger 320648925 / 110301214).

The on-ground calculated location, using the GBM trigger
data, is RA = 229.35, DEC = 29.40 (J2000 degrees,
equivalent to 15 h 17 m 24 s, 29 d 24 ' 00"), with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 94 degrees.

GBM triggered an automatic repoint request to the Fermi
Observatory to execute a maneuver following this trigger
and track the burst location for the next 5 hours.
However due to Earth-avoidance constraints, the slew did not
commence until ~40 minutes after the trigger.

The GBM light curve consists of a structured single pulse
with a duration (T90) of about 5 s (50-300 keV).
The time-averaged spectrum from T0+0.002 s to T0+5.824 s is
best fit by a Band function with Epeak = 106.80 (+1.85/-1.75) keV,
alpha = -0.81 (+/-0.02), and beta = -2.70 (+0.04/-0.05).

The event fluence (10-1000 keV) in this time interval is
(3.65 +/- 0.03)E-05 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+3.97 s in the 10-1000 keV band
is  125.73 +/- 3.47 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB110223A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11772
SUBJECT: GRB 110223A: optical upper limits
DATE:    11/03/03 14:41:32 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

V. Rumyantsev(CrAO), N. Pit (CrAO), A. Pozanenko (IKI) report on
behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 110223A (Sakamoto et al., GCN
11753) with AZT-11 telescope of CrAO starting on Feb. 23 (UT) 22:44
and under
seeing of about 2.2 arsces. In the enhanced Swift-XRT position (Evans
et al., GCN 11759) we do not detect any object. We also do not detect
the uncatalogued source reported by Guidorzi et al., GCN 11762. The
photometry is based on the USNO B1.0 star 1775-0024257 (23 03 42.29
+87 32 38.4) assuming R=17.73.

T0+   Filter,  Exposure, mag.
(mid, d)       (s)

0.0965 R 21x180    >21.5 (3 sigma)

The finding chart can be found at
http://grb.rssi.ru/GRB110223A/GRB110223A_110223_azt11.gif


GRB_name: GRB110305A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11773
SUBJECT: GRB 110305A: Swift detection of a burst
DATE:    11/03/05 07:00:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Grupe (PSU), W. H. Baumgartner (GSFC/UMBC), J. M. Gelbord (PSU),
E. A. Hoversten (PSU), C. B. Markwardt (NASA/GSFC),
D. M. Palmer (LANL), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
M. C. Stroh (PSU) and C. W. Wolf (PSU) report on behalf of the Swift
Team:

At 06:38:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110305A (trigger=448229).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 260.877, -15.790 which is 
   RA(J2000) = 17h 23m 31s
   Dec(J2000) = -15d 47' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a flat-topped
structure with a superimposed short spike and an overall
duration of about 10 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 06:39:50.2 UT, 109.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 260.8809, -15.8023
which is equivalent to:
   RA(J2000)  = 17h 23m 31.42s
   Dec(J2000) = -15d 48' 08.2"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 46 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.73
x 10^21 cm^-2 (Kalberla et al. 2005). 

Due to bright stars in the field there will be no white finding chart
for this field.  UVOT information is not available at this time. 

Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110305A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11774
SUBJECT: GRB 110305A: GROND Detection of Optical Afterglow
DATE:    11/03/05 11:56:58 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

A. Nicuesa Guelbenzu (TLS Tautenburg), V. Sudilovsky, P. Schady and J.  
Greiner (MPE Garching) report on behalf of the GROND team:


We observed the field of GRB 110305A (Swift trigger 448229; Grupe et  
al., GCN #11773) simultaneously in g'r'i'z'JHK with GROND (Greiner et  
al. 2008, PASP 120, 405) mounted at the 2.2m MPI/ESO telescope at La  
Silla Observatory (Chile).

Observations started at 06:40 UT on March 5th, 2 minutes after the GRB  
trigger. They were performed at an average seeing of 0.8" and at an  
average airmass of 1.8.

We found a fading source within the 2.2" Swift/XRT error circle  
reported by Grupe et al. (GCN #11773) at

RA (J2000) = 17h 23m 31.3s
DEC (J2000) = -15d 48' 08.8"

with an uncertainty of 0.3" in each coordinate.

The source decayed by 0.8mag in 60.5 minutes, suggesting that it is  
the optical afterglow of GRB110305A. At T+116.9 minutes the source had  
an r'-band magnitude of 23.7 +/- 0.1.

These measurements are not corrected for the considerable Galactic  
foreground extinction corresponding to a reddening of E(B-V)=0.390 mag  
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB110305A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11776
SUBJECT: GRB 110305A: Swift-BAT refined analysis
DATE:    11/03/05 14:24:03 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), D. Grupe (PSU), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110305A (trigger #448229)
(Grupe, et al., GCN Circ. 11773).  The BAT ground-calculated position is
RA, Dec = 260.877, -15.810 deg which is 
   RA(J2000)  =  17h 23m 30.4s 
   Dec(J2000) = -15d 48' 37.6" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 22%.
 
The mask-weighted light curve shows a single pulse starting at ~T-1 sec and
ending at ~T+12 sec.  T90 (15-350 keV) is 12.0 +- 2.2 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-0.9 to T+12.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.62 +- 0.19.  The fluence in the 15-150 keV band is 8.0 +- 1.0 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+6.06 sec in the 15-150 keV band
is 1.2 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/448229/BA/


GRB_name: GRB110305A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11777
SUBJECT: GRB 110305A: Enhanced Swift-XRT position
DATE:    11/03/05 23:28:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 451 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 110305A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 260.88069, -15.80241 which is equivalent
to:

RA (J2000): 17h 23m 31.37s
Dec (J2000): -15d 48' 08.7"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11778
SUBJECT: GRB 110305A: Swift-XRT refined Analysis
DATE:    11/03/06 16:43:19 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

D. Grupe (PSU) reports on behalf of the Swift-XRT team:

We have analyzed 34 ks of XRT data for GRB 110305A (Grupe  et al. GCN
Circ. 11773), from 116 s to 99.9 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN. Circ 11777).

The light curve can be modeled with  a single power-law decay with a
decay index of alpha=1.12 (+0.07, -0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.98 (+0.22, -0.20). The
best-fitting absorption column is consistent with the Galactic value of
1.7 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.9 x 10^-11 (6.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 x 10^21 cm^-2
Galactic foreground: 1.7 x 10^21 cm^-2
Excess significance: 
Photon index:      1.98 (+0.22, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00448229.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110305A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11779
SUBJECT: GRB 110305A: Swift/UVOT Upper Limits
DATE:    11/03/06 17:12:42 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) and D. Grupe (PSU) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110305A
113 s after the BAT trigger (Grupe et al., GCN Circ. 11773). No optical
afterglow consistent with the GROND position (Guelbenzu et al., GCN
Circ. 11774) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           113          263          147 >20.5
u_FC               271          521          246 >19.6
white              113        18938         1608 >22.3
v                  601        11519         1203 >19.7
b                  527        24719         2136 >20.9
u                  271        30501         3468 >21.5
w1                 650        29759         2976 >20.9
m2                 632        28858         2261 >20.8
w2                 749         7376          426 >19.8

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.39 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110305A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11780
SUBJECT: GRB110305A: MITSuME Ishigakijima Optical upper limits
DATE:    11/03/07 12:46:17 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 110305A (Grupe et al., GCNC 11773) with the optical
three color (g', Rc and Ic) CCD camera attached to the Murikabushi 1m telescope
of Ishigakijima Astronomical Observatory.

The observation started on 2011-03-05 18:37:53 UT (~12 hours after the burst).
We could not detected the previously reported afterglow (Guelbenzu et al., GCNC
11774) in all the three bands.

Three sigma upper limits of the OT are listed below. We used GSC2.3 catalog for
flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.51372    18:57:46    1620.0    >19.8  >20.1  >19.3
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110305A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11781
SUBJECT: GRB 110305A: REM detection of a possible NIR afterglow
DATE:    11/03/07 15:08:51 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

D. Fugazza, P. D'Avanzo, S. Covino, S.D. Vergani, A. Melandri (INAF-OAB)
on behalf of a larger collaboration report:

The robotic 60-cm REM telescope located at La Silla (Chile) observed
automatically the field of GRB 110305A (Grupe et al. GCN 11773) with the
ROSS optical and REMIR near-infrared cameras in imaging mode.

Observations started 93s from the GRB time (51s from the trigger time). No
counterpart is visible in the optical frames, down to R > 16 (3sigma c.l.,
calibrated against the USNO B1.0 catalogue) while an object is visible
with low significance in the first coadded NIR frames at a position
consistent with the one of the optical afterglow (Nicuesa Guelbenzu et al.
GCN 11774).

Preliminary photometry shows that the source has H = 15.0 +/- 0.3
(calibrated against the 2MASS catalogue) at t-t0 = 4.5 min and is not
detected anymore at t-t0 = 26.3 min down to a limiting magnitude H > 16.5
(3sigma c.l.). This implies an early power-law decay with index steeper
than 0.8, consistent with the reported X-ray decay (Grupe, GCN 11778).


GRB_name: GRB110312A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11782
SUBJECT: GRB 110312A: Swift detection of a burst
DATE:    11/03/12 18:14:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), R. L. C. Starling (U Leicester),
E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (MSU) report on behalf of
the Swift Team:

At 17:55:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110312A (trigger=449074).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 157.479, -5.255 which is 
   RA(J2000)  =  10h 29m 55s
   Dec(J2000) = -05d 15' 18"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for image triggers, the BAT lightcurve
does not show anything significant. 

The XRT began observing the field at 17:58:16.3 UT, 159.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
157.4813, -5.2628 which is equivalent to:
   RA(J2000)  = 10h 29m 55.50s
   Dec(J2000) = -05d 15' 46.0"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 28 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.72
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 4.19e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 167 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.04. 

Burst Advocate for this burst is S. R. Oates (sro AT mssl.ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB110312A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11783
SUBJECT: GRB 110312A: Swift-BAT refined analysis
DATE:    11/03/12 22:36:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
S. R. Oates (UCL-MSSL), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110312A (trigger #449074)
(Oates, et al., GCN Circ. 11782).  The BAT ground-calculated position is
RA, Dec = 157.500, -5.259 deg, which is 
   RA(J2000)  =  10h 30m 00.0s 
   Dec(J2000) = -05d 15' 32.6" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 26%.
 
The mask-weighted light curve shows a single start at ~T+25 sec, peaking
around T+45 sec, and ending at ~T+65 sec.  T90 (15-350 keV) is 28.7 +- 7.6 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+24.1 to T+64.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.32 +- 0.26.  The fluence in the 15-150 keV band is 8.2 +- 1.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+44.08 sec in the 15-150 keV band
is 1.2 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/449074/BA/


GRB_name: GRB110312A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11784
SUBJECT: GRB 110312A: Enhanced Swift-XRT position
DATE:    11/03/13 00:21:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1937 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 110312A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 157.48111, -5.26262 which is equivalent
to:

RA (J2000): 10h 29m 55.47s
Dec (J2000): -05d 15' 45.4"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB110312A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11785
SUBJECT: GRB 110312A: GROND Upper Limits
DATE:    11/03/13 08:10:50 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

 A. Nicuesa Guelbenzu (TLS Tautenburg), F. Olivares E., and J. Greiner
(MPE Garching) report on behalf of the GROND team:

 We observed the field of GRB 110312A (Swift trigger 449074; Oates et
 al., GCN #11782) simultaneously in g'r'i'z'JHK with GROND (Greiner et
 al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La
 Silla Observatory (Chile).

 Observations started at 23:57 UT on March 11, 2011, 6 hours after the
 GRB trigger, and continued for 2.6 hours. They were performed at an
 average seeing of 1.3" and at an average airmass of 1.5.

 We find no sources within the the 1.7" enhanced XRT error circle
 (Osborne et al.; GCN #11783). Co-added images of 64.5 min of
 integration time in g'r'i'z' and 56 min in JHK yield the following
 3-sigma upper limits (all in the AB system):

 g' > 24.3,
 r' > 24.1,
 i' > 23.0,
 z' > 23.1,
 J  > 22.0,
 H  > 21.4, and
 K  > 19.3


calibrated against GROND zeropoints and 2MASS field stars. No
corrections for the expected Galactic foreground extinction were made,
which correspond to a reddening of E(B-V)=0.04 mag in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB110312A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11786
SUBJECT: GRB 110312A: Swift-XRT refined Analysis
DATE:    11/03/13 09:11:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and S. R. Oates (UCL-MSSL) report on behalf
of the Swift-XRT team:

We have analysed 2.9 ks of XRT data for GRB 110312A (Oates  et al. GCN
Circ. 11782), from 147 s to 18.1 ks after the  BAT trigger. The data
comprise 82 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 11784).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.8 (+0.8, -1.1), followed by a break at T+356 s to an
alpha of 0.55 (+0.10, -0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.36 (+0.22, -0.21). The
best-fitting absorption column is  4.3 (+/-0.8) x 10^21 cm^-2, in
excess of the Galactic value of 3.7 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (8.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.3 (+/-0.8) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: 9.5 sigma
Photon index:      2.36 (+0.22, -0.21)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00449074.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB110312A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11787
SUBJECT: GRB 110312A: Swift/UVOT Upper Limits
DATE:    11/03/13 13:26:40 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R Oates (UCL-MSSL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110312A
168 s after the BAT trigger (Oates et al., GCN Circ. 11782).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 11784) is detected in the initial UVOT  
exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag
----------------------------------------------------------------
white_FC           168          318          147         >21.8
u_FC               327          577          246         >20.1
white              168         1896          429         >21.3
v                  657         1946          156         >19.2
b                  582         6063          315         >20.6
u                  327         2020          382         >20.1
w1                 706         1995          136         >19.6
m2                 682         1970          156         >19.6
w2                1036         1402           39         >18.8

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB110312A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11788
SUBJECT: GRB 110312A: RTT150 optical observations
DATE:    11/03/13 15:32:35 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

I. Bikmaev, R. Zhuchkov, R. Gumerov, A. Nemtinov, N. Sakhibullin 
(Kazan University),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
Z. Eker, I. Khamitov (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

The field of GRB 110312A (Oates et al., GCN 11782) was observed with
Russian-Turkish 1.5-m telescope (RTT150,Bakirlitepe, TUBITAK National
Observatory, Turkey) in March 12, 2011, during UT 20:00 - 21:40,
i.e. starting approximately 2 hours after the burst. 

We obtained serie of 16 exposures by 300 sec each in Rc filter.

We found no optical source within the 1.7" enhanced XRT error circle
(Osborne et al.; GCN 11784) in co-added image with frame limit of 
Rc ~ 23.5 mag


GRB_name: GRB110312A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11789
SUBJECT: GRB110312A: MITSuME Okayama Optical upper limits
DATE:    11/03/14 08:41:28 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110312A (Oates et al., GCN 11782)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2011-03-12 18:35:03 UT (~39 mins
after the burst). We did not find any new point source within the
enhanced XRT circle (Osborne et al., GCNC 11784) in all the
three bands.

Three sigma upper limits of the OT are listed below. We used
GSC2.3 catalog for flux calibration.


T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.02269    18:28:18    1020.0    >17.8  >18.0  >17.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB110315A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11790
SUBJECT: GRB 110315A: Swift detection of a burst
DATE:    11/03/16 00:09:22 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC),
P. D'Avanzo (INAF-OAB), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
C. Gronwall (PSU), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
V. Mangano (INAF-IASFPA), R. Margutti (INAF-OAB),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/IASFPA) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 23:57:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110315A (trigger=449399).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 279.191, +17.532 which is 
   RA(J2000)  =  18h 36m 46s
   Dec(J2000) = +17d 31' 56"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows 3 or 4 peaks
with a total duration of about 20 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 23:58:49.1 UT, 104.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 279.1928, +17.5388 which is equivalent to:
   RA(J2000)  = 18h 36m 46.27s
   Dec(J2000) = +17d 32' 19.6"
with an uncertainty of 5.8 arcseconds (radius, 90% containment). This
location is 25 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 112 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The coverage of the XRT error circle by the 8'x8' region for the list of
sources generated on-board is uncertain because the large number of sources
filled the available telemetry. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.25. 

Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


