# GCN_circulars

GRB_name: GRB111215A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12694
SUBJECT: GRB 111215A: MITSuME Okayama Optical upper limits
DATE:    11/12/16 12:27:18 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 111215A (Oates et al., GCNC 12681)
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 2011-12-15 14:10:37 UT (~6.5 min after
the burst). We did not find any new point source within the enhanced
XRT circle (Beardmore et al., GCNC 12690) 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'     Rc     Ic
------------------------------------------------------
0.03242    14:50:49    3420.0    >18.6  >19.0  >18.7
--------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12695
SUBJECT: GRB 111215A: TNG K-band observations
DATE:    11/12/16 15:08:56 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@brera.inaf.it>

P. D'Avanzo, A. Melandri, S. Covino (INAF/OABr), L. A. Antonelli, V. D'Elia (INAF/OAR and ASDC/ASI), E. Palazzi (INAF/IASF Bo), D. Fugazza (INAF/OABr), G. Tagliaferri (INAF/OABr), and S. D. Vergani (INAF/OABr), report on behalf of the CIBO collaboration:

We observed the field of GRB 111215A (Oates et al., GCN 12681) with the TNG telescope located in the Canary Islands. We secured 30 min Ks-band imaging with the NICS instrument, with a mean time Dec 15.845 UT (6.30 hr after the GRB trigger).

Within the UVOT-enhanced XRT error circle (Beardmore et al., GCN 12690), we detect no new source down to a limiting magnitude K > 19 (Vega, calibrated against the 2MASS catalog).

Taking the X-ray flux at the time of the TNG observation from the UK X-ray light curve repository (http://www.swift.ac.uk/xrt_curves/00509717/), we compute a broad-band optical-to-X-ray spectral index beta_OX < 0.25, which classifies GRB 111215A as dark according to the widely adopted definition of Jakobsson et al. (2004, ApJ, 617, 21). The non detection in the K band, coupled with the significant absorption in the X-ray spectrum (Beardmore et al., GCN 12692), suggests a highly extinguished, rather than a high redshift, event. Deep observations to look for a host galaxy are encouraged.

We acknowledge excellent support from the observing staff at the TNG, especially Marco Pedani and Giovanni Mainella.


GRB_name: GRB111215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12696
SUBJECT: GRB 111215A: WHT, LT and NOT imaging
DATE:    11/12/16 17:24:54 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir, K. Wiersema (U. Leicester), A. Melandri (INAF-OAB),
T. Kruehler, J. Fynbo (DARK), A. J. Levan (U. Warwick), C. G. Mundell,
R. J. Smith (LJMU), C. Guidorzi (U. Ferrara), D. Xu (WIS) and
I. Skillen (ING) report:

We imaged the field of GRB111215A (Oates et al. GCN12681) using the
WHT, the LT and the NOT, all on La Palma, on the night of 2011-Dec-15 (UT).
Seeing conditions were rather poor (FWHM~2"), and no counterpart was
located to the following 3-sigma limits at the given mid-times post-burst:

WHT/LIRIS (calibrated against 2MASS)
K>19.3 at 4hr 55m
J>19.4 at 5hr 15m

LT/RATCam (calibrated against SDSS)
z'>21.7 at 6hr 50m

NOT/StanCam (calibrated against SDSS)
z'>22.5 at 6hr 50m

The K-band limit is consistent with that provided by D'Avanzo et
al. (GCN12695) from the TNG, and confirms this source to be dark even
in the infrared.

We are grateful to Ilia Ilyin for assistance in obtaining the NOT observations.


GRB_name: GRB111215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12697
SUBJECT: GRB111215A: Pre-Outburst Palomar 48 inch Imaging
DATE:    11/12/16 20:26:36 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), P. E. Nugent (LBNL / UC Berkeley), and S. R.
Kulkarni (Caltech) report on behalf of a larger collaboration:

We have examined pre-outburst imaging of the location of GRB111215A (Oates
et al., GCN12681) obtained over the last 7 years with the Palomar 48 inch
Oschin Schmidt telescope.

As part of the Palomar Transient Factory, we have imaged the location of
GRB111215A regularly (every ~ 3-4 nights) over the time period from June -
October 2011.  Coadding all images of this location, no sources are
detected within the XRT error circle (Beardmore et al., GCN12690) to a
limiting magnitude of r' > 22.8 mag (calibrated with respect to several
nearby field stars from SDSS).  Furthermore, no previous outbursts are
detected in any individual frames over this period, to a typical limiting
magnitude of r' > 20.5 mag.

In addition, we co-added 117 archival images from the DeepSky* project at
Palomar Observatory obtained over the time period from 2004-2008 as part
of the Palomar-Quest Consortium.  No source is detected at the XRT
position to a limiting magnitude of i' > 22.6 mag.

* http://supernova.lbl.gov/~nugent/deepsky.html


GRB_name: GRB111215B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12698
SUBJECT: IPN Triangulation of GRB 111215B (long/intense)
DATE:    11/12/16 21:21:48 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley, on behalf of the Mars Odyssey and MESSENGER GRB teams,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey 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,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

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

The long-duration, intense GRB 111215B was observed by Konus-Wind, 
Suzaku-WAM, MESSENGER (GRNS), and Mars Odyssey (HEND) at about 73686 s 
UT (20:28:06). We have triangulated it to a preliminary, 3 sigma error 
box whose coordinates are:
---------------------------------------------
  RA(2000), deg                  Dec(2000), deg
---------------------------------------------
  Center:
   222.403 (14h 49m 37s) +16.439 (+16d 26' 21")
  Corners:
   222.265 (14h 49m 04s) +16.514 (+16d 30' 51")
   222.532 (14h 50m 08s) +16.665 (+16d 39' 53")
   222.540 (14h 50m 10s) +16.364 (+16d 21' 49")
   222.274 (14h 49m 06s) +16.212 (+16d 12' 43")
---------------------------------------------

The error box area is 282 sq. arcmin, and its maximum
dimension is 31 arcmin.

This box can be improved.

The time history and spectrum will be given in a forthcoming GCN Circular.

A Swift ToO observation has been requested.


GRB_name: GRB111205A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12699
SUBJECT: GRB 111205A: Confirmation of X-ray Afterglow
DATE:    11/12/16 22:33:55 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and C. A. Wolf (PSU) report on behalf of the  
Swift team:

We have analyzed 8.3 ks of XRT data for the IPN detected burst GRB  
111205A (Hurley et al.  GCN Circ. 12626) from 828 to 853 ks after the  
burst.  The data are entirely in Photon Counting (PC) mode.   
Previously an uncataloged X-ray source was detected by XRT 200 ks  
after the burst (Wolf & Hoversten GCN Circ. 12630) which was  
identified as the potential afterglow for GRB 111205A, but could not  
be confirmed as it was not possible to discern if the source was  
fading in a single observation.  The follow-up observation reveals  
that the source is still detected, but has faded by a factor of 4,  
which corresponds to a decay index of 1.0 (+1.3, -0.6) which is  
consistent with a GRB late time afterglow.  Thus we conclude that the  
X-ray source previously reported is the afterglow.


GRB_name: GRB111215B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12700
SUBJECT: GRB 111215B: Swift-XRT observations
DATE:    11/12/17 12:07:31 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O. M. Littlejohns (U. Leicester) reports on behalf of the Swift-XRT
team:

We have analysed 4.9 ks of XRT data for the IPN-detected burst: GRB
111215B (Hurley et al. et al. GCN Circ. 12698), from 113.3 ks to 130.4
ks after the  IPN trigger. The data are entirely in Photon Counting
(PC) mode.  An X-ray source is detected within the IPN error circle.
The refined XRT position is RA, Dec = 222.3994, +16.45412 which is
equivalent to:

RA (J2000): 14 49 35.86
Dec(J2000): +16 27 14.8

with an uncertainty of 3.7 arcsec (radius, 90% confidence). This
position is 55 arcsec from the IPN position.  The light curve is
consistent with a constant source of mean count rate 2.6e-02 ct/sec. A
power-law fit gives an index of 1.9 (+0.9, -2.8).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.5 (+0.5, -0.3). The
best-fitting absorption column is  2 (+11, -1) x 10^20 cm^-2,
consistent with the Galactic value of 1.6 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 4.9 x 10^-11 (5.1 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2 (+11, -1) x 10^20 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.5 (+0.5, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020193.

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


GRB_name: GRB111215B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12701
SUBJECT: Konus-Wind observation of GRB 111215B
DATE:    11/12/17 12:20:31 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 intense GRB 111215B
(localized by IPN: Hurley et al., GCN 12698)
triggered Konus-Wind at T0=72682.720s UT (20:28:02.720)

The light curve shows multiple partly overlapping pulses
with the brightest peak at ~T0+12s.
A total duration of the burst is ~75 s.
The emission is seen up to ~8 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111215_T73682/

As observed by Konus-Wind the burst
had a fluence of 5.3(-1.1,+1.1)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+11.776 s,
of 6.1(-0.6,+0.6)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+72.192 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.18 (-0.12, +0.18),
the high energy photon index beta = -2.3 (-0.6, +0.2),
the peak energy Ep = 250(-60, +65) keV,
chi2 = 88.2/88 dof.

The spectrum at the maximum count rate
(measured from T0+7.680 to T0+14.848 s)
is best fitted in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -1.03 (-0.10, +0.11),
and Ep = 413(-57, +75) keV,
chi2 = 101.9/89 dof.
Fitting this spectrum by the GRB (Band) function yields
the same alpha and Ep with a high energy photon index
beta < -2.6 (chi2 = 101.9/88 dof).

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


GRB_name: GRB111215B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12702
SUBJECT: GRB 111215B: Swift/UVOT Upper Limits
DATE:    11/12/17 16:33:03 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R .Oates (MSSL-UCL) and C. J. Saxton (MSSL-UCL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of the IPN-detected 
burst: GRB 111215B, 31.5 hrs after the IPN trigger (Hurley et al. et al. GCN Circ. 12698)
No optical afterglow consistent with the XRT position (Littlejohns et al. et al. GCN Circ. 12700)
is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

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

u           113,256    130,435        4889         >21.4

The magnitudes in the table 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: GRB111215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12703
SUBJECT: GRB111215A: optical upper limit
DATE:    11/12/17 20:17:28 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev, N. Pit' (CrAO), A. Volnova (SAI MSU),  M. Andreev (Terskol 
Branch of INASAN), N. Parakhin, (IC AMER, NASU), A. Pozanenko (IKI) report 
on behalf of larger GRB follow-up collaboration:

We observed the field of GRB  111215A (Oates  et al. GCN 12681) with AZT-11 
telescope of CrAO observatory starting on Dec.15  (UT) 15:18:22  under mean 
seeing (FWHM) of 3.1 arsces and with Zeiss-600 telescope of Mt.Terskol 
observatory starting on Dec.15  (UT) 21:03:45   under mean seeing (FWHM) of 
1.8 arsces . We took several frames  in R-band. Within enhanced Swift-XRT 
position (Beardmore et al. GCN  12690) we do not detected any optical 
source. A photometry is based on the nearby USNO-B1.0 stars (R2):

T_start UT  T0+        Filter, Exposure, OT,  uplim (3 sigma)
                  (mid, d)            (s)

15:18:22  0.0738       R     21x180    n/d     21.0
21:03:45  0.3113       R     51x60      n/d     19.3 


GRB_name: GRB111211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12704
SUBJECT: GRB 111211A: optical ovservations at  Mt. Terskol observatory 
DATE:    11/12/19 19:48:14 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.Volnova (SAI MSU), M. Andreev, A. Sergeev  (Terskol Branch of INASAN), V. 
Petkov (Baksan Neutrino Observatory of INR), N. Karpov, O. Andrienko, K. 
Martynyuk-Lototsky, N. Parakhin, N. Borachok, V. Kozlov, G. Butenko, V. 
Godunova (IC AMER, NASU), A. Pozanenko (IKI) report:

We observed field of the SuperAGILE GRB 111211A  (Lazzarotto et al. GCN 
12666) with  Zeiss-600 telescope of Mt.Terskol observatory in R filter 
between Dec. 12 (UT) 23:09:07 -- Dec.13 00:55:27.   We took several images 
of 60 exposure under good weather conditions and mean seeing (FWHW) of about 
1.8". We  detect the source reported as candidate in afterglow  (Kann et 
al., GCN 12668; Kruehler et al., GCN 12675). A photometry is based on the 
USNO-B1.0 1011-0183238 (10:12:26.16 +11:11:26.6) star assuming R = 14.41.

  T0+      Filter,  Exposure, OT,                  UpperLimit
(mid, d)               (s)

1.07273  R       104x60    19.25 +/- 0.10  20.0


GRB_name: GRB111215B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12705
SUBJECT: GRB 111215B: Suzaku WAM observation of the prompt emission
DATE:    11/12/20 06:18:49 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

W. Iwakiri, M. Tashiro, Y. Terada, T. Yasuda, K. Takahara, M. Asahina, 
S. Kobayashi, A. Sakamoto (Saitama U.) Y. Hanabata, T. Uehara, T. 
Kawano, K. Takaki, M. Mizuno, M. Ohno, Y. Fukazawa (Hiroshima U.), S. 
Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), M. Kokubun, T. 
Takahashi (ISAS/JAXA), Y. E. Nakagawa (Waseda U.), N. Ohmori, M. 
Akiyama, M. Yamauchi (Univ. of Miyazaki), C-J. Chuang, Y. Urata, P. Tsai 
(NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),

The long bright GRB 111215B (localized by IPN: Hurley et al., GCN 12698)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 20:28:05.704 UT (=T0).

The observed light curve shows a multi-peaked structure starting at
T0-0.5 s, followed by a long weak tail seen up to T0+75 s with a
duration (T90) of about 61 seconds. The fluence in 100 - 1000 keV was
2.81(-0.06, +0.09) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+13 s was
8.68 (-0.52, +0.36) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-0.5 s 
to T0+74.5 s is well fitted by a single power-law with a photon index of
2.05 (-0.06, +0.07) (chi^2 / d.o.f = 19.7/25).

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

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


GRB_name: GRB111103A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12706
SUBJECT: GRB 111103A: optical upper limit of Mt. Terskol observatory
DATE:    11/12/20 12:42:29 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

 A.Volnova (SAI MSU), M. Andreev, A. Sergeev  (Terskol Branch of INASAN), V.
 Petkov (Baksan Neutrino Observatory of INR), N. Karpov, O. Andrienko, K.
 Martynyuk-Lototsky, N. Parakhin, N. Borachok, V. Kozlov, G. Butenko, V.
 Godunova (IC AMER, NASU), A. Pozanenko (IKI) report:


 We observed field of the Swift  GRB 111103A  (Stroh et al. GCN 12518) with
 Zeiss-600 telescope of Mt.Terskol observatory in R filter between Nov. 3
 (UT) 16:16:02 - 16:49:00. We took 60 frames with exposure of 30
 seconds under favourable weather conditions and seeing (FWHM) of about
 1.5''. We do not detect any source on a stacked frame within BAT
 ground-calculated error circle (Sakamoto et al., GCN 12523). A
 photometry is based on the USNO B1.0  nearby stars.

  T0+      Filter,   Exposure, OT,  UpperLimit
 (mid, d)               (s)

 0.24836  R         60x30       n/d   16.6


GRB_name: GRB110820A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12707
SUBJECT: GRB 110820A: optical observations in Maidanak observatory
DATE:    11/12/20 12:49:33 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

 A. Volnova (SAI MSU), M. Ibrahimov (UBAI), A. Pozanenko (IKI) report
on behalf of larger GRB  follow-up collaboration:

 We observed the field of the Swift GRB 110820A (Troja et al., GCN
12288) with AZT-22 telescope of Maidanak observatory on Aug. 20
starting on 21:54:54 UT in R band. We took 6 frames with exposure of
300 seconds under good weather condition and seeing (FWHM) of about
0.7". On the stacked image we do not detect the source reported by Im
et al. (GCNs 12295, 12297). The photometry is based on the USNO B1.0
star USNO-B1.0 1603-0160240, (J2000) RA = 22:52:56.89 Dec =
+70:18:37.5, assuming R =17.19:

 Tstart UT,  T0+,       Filter, Exposure, OT, Upper Limit (3 sigma)
                 (mid, d)            (s)

 21:54:54   0.18924  R        6*300        n/d  22.5


GRB_name: GRB111103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12708
SUBJECT: GRB 111103B: optical upper limit
DATE:    11/12/20 13:00:59 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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


 We observed field of the Swift GRB 111103B (Grupe et al. GCN 12519)
with Zeiss-600 telescope of Crimean branch of SAI MSU in R filter
between Nov. 3 (UT) 15:44:07 - 17:02:29. We took 73 images of 60
exposure under bad weather conditions and mean seeing (FWHW) of about
3.4". We do not detect any source within enhanced XRT position (Goad
et al., GCN 12525). A photometry is based on the USNO B1.0 star
0916-0323572 (RA = 17:42:46.95, Dec =  +01:36:05.2, J2000) assuming R
= 15.67.

 T0+        Filter, Exposure, OT,  UpperLimit
 (mid, d)            (s)

 0.22517  R        73x60      n/d   20.4


GRB_name: GRB111215A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12710
SUBJECT: GRB111215A: CARMA Detection
DATE:    11/12/20 19:52:45 GMT
FROM:    Assaf Horesh at Caltech  <assafh@astro.caltech.edu>

Authors: 
A. Horesh (Caltech), J. Carpenter (Caltech), A. Corsi (Caltech), A. Zauderer (CfA), S. R. Kulkarni (Caltech), E. Berger (CfA), D. A. Frail (NRAO), S. B. Cenko (UC Berkeley), D. Perley (Caltech)


On 2011 December 17.04 UT (1.46 days after burst) we observed GRB111215A (Oates et al., GCN12681) with CARMA at 93 GHz. We detected the source at RA=23:18:13.32, Dec=+32:29:39.09 (J2000). This position is consistent with the Swift-XRT position. 
 
We continue to monitor the source with CARMA. 


GRB_name: GRB111215A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12711
SUBJECT: GRB 111215A:  EVLA observations
DATE:    11/12/20 19:59:32 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer and E. Berger (Harvard) report on behalf of a larger
collaboration:

"We observed the position of GRB 111215A (GCN 12681) with the EVLA at 
21.8 GHz beginning on 2011 Dec 18.93 UT (3.35 days after the burst).  We 
report a radio counterpart consistent with the Swift-XRT position (GCN 
12690, http://www.swift.ac.uk/xrt_positions) and the reported CARMA 
detection by Horesh et al. (GCN 12710).

The position of the detected EVLA radio source is (J2000):
RA  =   23:18:13.310 +/- 0.001
Dec =  +32:29:39.18 +/- 0.01

Follow-up observations are ongoing."


GRB_name: GRB111210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12713
SUBJECT: GRB 111210A: optical upper limit of Mt. Terskol observatory
DATE:    11/12/22 14:48:58 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A.Volnova (SAI MSU), M. Andreev, A. Sergeev (Terskol Branch of INASAN), V.
Petkov (Baksan Neutrino Observatory of INR), N. Karpov, O. Andrienko, K.
Martynyuk-Lototsky, N. Parakhin, N. Borachok, V. Kozlov, G. Butenko, V.
Godunova (IC AMER, NASU), A. Pozanenko (IKI) report:


We observed the field of GRB 111210A (Siegel et al., GCN 12650) with
Zeiss-600 telescope of Mt.Terskol observatory on Dec 11 between
01:06:25 and 03:09:45 UT under poor weather condition and mean seeing
of about 2.2". We took 120 frames in R-band with exposure of 60
seconds. In a stacked frame we did not detect any source within the
enhanced XRT error circle (Goad et al., GCN 12652). The photometry of
the field is based on a few stars from USNO-B1.0 catalogue.

t-t0        filter  exp.    OT  uplim (3sigma)
(mid., days)      (s)

0.48006     R   120x60  n/d   18.6


GRB_name: GRB111222A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12714
SUBJECT: IPN Triangulation of GRB 111222A (short/hard/intense)
DATE:    11/12/23 16:27:26 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley, on behalf of the Mars Odyssey and MESSENGER GRB teams,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

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

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

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

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

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

The short-duration, hard, intense GRB 111222A has been observed by
Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), Mars
Odyssey (HEND), and Swift (BAT) (outside the coded field of view) so
far, at about 53515 s UT (14:51:55). We have triangulated it to a
preliminary, 3 sigma error box whose coordinates are:
---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
---------------------------------------------
Center:
  179.193 (11h 56m 46s) +69.036 (+69d 02' 10")
Corners:
  179.439 (11h 57m 45s) +68.877 (+68d 52' 37")
  179.815 (11h 59m 16s) +69.133 (+69d 07' 59")
  178.942 (11h 55m 46s) +69.195 (+69d 11' 41")
  178.575 (11h 54m 18s) +68.936 (+68d 56' 11")
---------------------------------------------
The error box area is 317 sq. arcmin, and its maximum
dimension is 29 arcmin.
This box can be improved.

The time history and spectrum will be given in a forthcoming GCN Circular.

A Swift ToO observation has been requested.


GRB_name: GRB111222A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12715
SUBJECT: Konus-Wind observation of GRB 111222A
DATE:    11/12/23 18:25:13 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 short hard intense GRB 111222A
(localized by IPN: Hurley et al., GCN 12714)
triggered Konus-Wind at T0=53515.918s UT (14:51:55.918)

The light curve consists of a single multi-peaked pulse with
a total duration of ~300 ms.
The emission is seen up to ~3 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111222_T53515/

As observed by Konus-Wind the burst
had a fluence of (7.2  0.7)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0 s,
of (5.1  0.7)x10-5 erg/cm2/s
(both in the 20 keV - 3 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.256 s)
is best fitted in the 20 keV - 3 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.35 (-0.13, +0.14),
and Ep = 762(-89, +101) keV,
chi2 = 51.1/45 dof.

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


GRB_name: GRB111222A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12716
SUBJECT: GRB 111222A: Swift-XRT observations
DATE:    11/12/23 21:24:29 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

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

We have analyzed 2.3 ks of XRT data for the IPN-detected burst: GRB
111222A (Hurley et al. et al. GCN Circ. 12714), from 92.9 ks to 95.2 ks
after the  IPN trigger. The data are entirely in Photon Counting (PC)
mode.  An X-ray source is detected within the IPN error circle. Using
1964 s of PC mode data and 1 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 = 179.21977, +69.07116 which is
equivalent to:

RA (J2000): 11h 56m 52.74s
Dec(J2000): +69d 04' 16.2"

with an uncertainty of 3.1 arcsec (radius, 90% confidence). This
position is 322 arcsec from the IPN position.  We cannot determine at
the present time whether the source is fading.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.5 (+4.9, -4.3). The
best-fitting absorption column is  consistent with the Galactic value
of 1.7 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 6.8 x 10^-11 (7.0 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+2.1, -0) x 10^22 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.5 (+4.9, -4.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020194.

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


GRB_name: GRB111222A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12717
SUBJECT: GRB 111222A: Swift/UVOT Observations
DATE:    11/12/24 06:29:06 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

We have analyzed 2.3 ks of UVOT data for the IPN-detected burst: GRB
111222A (Hurley et al. et al. GCN Circ. 12714), from 92.9 ks to 95.2 ks
after the  IPN trigger. The data are entirely in the white filter.  We detect a faint
optical source consistent with the XRT source reported in Grupe (GCN Circ.
12716) at a position of RA, Dec = 179.22008, Dec = 69.07096 , which
is equivalent to:

RA (J2000): 11h 56m 52.82s
Dec(J2000): +69d 04' 15.4"

with an uncertainty of 0.51 arcsec (radius, 90% confidence). Preliminary
photometry using the UVOT photometric system (Breeveld et al. 2011, AIP
Conf. Proc. 1358, 373) shows a white magnitude of 19.34+-0.03.  The magnitude
is 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).

We note, however, that a source is present at this position in the DSS.  Follow-up
observations will be needed to determine if the X-ray/optical source is indeed the
GRB afterglow.


GRB_name: GRB111222A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12718
SUBJECT: GRB 111222A: Xinglong TNT observation
DATE:    11/12/25 01:52:57 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 111222A ( Hurley  et al., GCN 12714)
with Xinglong TNT telescope at  Dec 24th, 18:23:18.453 (UT), about  2.15d after 
the burst.  15 R-band images  were obtained. The exposure time is 300 sec 
for each frame.

The source reported by Siegel et al. (GCN 12717) 
was detected in the each R band image. 
The brightness of this source was estimated 
to be about 17.6 mag and without any significant change 
during our observations time 
relatively to the reference object in USNO B1.0 R2 mag.

The Coordinates of the reference object and its brightness are  
11:56:39.863   +69:03:55.50  J2000  R2=16.86 mag, respectively.

The brightness of the reported source ( Siegel et al.  GCN 12717 ) 
we observed is brighter than the magnitude reported by USNO B1.0 R2mag
which was R2=18.06 mag. 

This message may be cited.

More observations are encouraged. 

Thanks for the observation assistant of TNT telescope at Xinglong observatory. 


GRB_name: GRB111222A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12719
SUBJECT: GRB111222A: GMG optical observation
DATE:    11/12/25 02:09:23 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS/NAOC), X.-H. Zhao, J.-M. Bai (YNAO), J.-R. Mao (KASI/YNAO) report:

We observed the field of GRB 111222A (Hurley et al., GCN 12714; Grupe
et al., GCN 12716; Siegel et al., GCN 12717) with the 2.4m GMG
telescope equipped with YFOSC. Observations started at 17:34 UT on
2011-12-24 (i.e., 50.717 hrs after the burst) in a seeing of ~3.2",
and 3x600s SDSS r-band and 3x600s SDSS z-band images were obtained.

As noted in GCN 12717, there was a SDSS star present at the UVOT
position which has the following mags:

u=22.34+/-0.30
g=19.47+/-0.01
r=18.08+/-0.01
i=16.66+/-0.01
z=15.85+/-0.01.

The star had r=18.08+/-0.01 mag and z=15.83+/-0.02 mag in our stacked
images (calibrated with nearby SDSS stars), being consistent with the
SDSS r- and z-band archival mags.

We thank the GMG staff, especially J.-J. Zhang for performing these
observations.


GRB_name: GRB111225A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12720
SUBJECT: GRB 111225A: Swift detection of a burst with an optical counterpart
DATE:    11/12/25 04:12:26 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), W. H. Baumgartner (GSFC/UMBC),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC), D. Grupe (PSU),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), C. A. Swenson (PSU),
T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report on behalf of the
Swift Team:

At 03:50:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111225A (trigger=510341).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 13.102, +51.589 which is 
   RA(J2000) = 00h 52m 24s
   Dec(J2000) = +51d 35' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The immediately available lightcurve was
truncated for contact with the ground station. The BAT lightcurve showed 
a rise at around T-10 seconds with flux continuing at least until
T+8 seconds, the limit of of the immediately available data.  
The peak count rate was ~1300 counts/sec (15-350 keV), at ~-2 sec 
after the trigger. 

The XRT began observing the field at 03:52:05.9 UT, 88.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 13.1548, 51.5741 which is equivalent to:
   RA(J2000)  = +00h 52m 37.15s
   Dec(J2000) = +51d 34' 26.8"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 129 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. 

The initial flux in the 2.5 s image was 2.96e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting 95
seconds after the BAT trigger. There is a candidate afterglow in the rapidly
available 2.7'x2.7' sub-image at
  RA(J2000)  = 00:52:37.21 =  13.15503
  DEC(J2000) = +51:34:19.5  =  51.57207
with a 90%-confidence error radius of about 0.75 arc sec. This position is 7.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.42 with a 1-sigma error of about  0.20. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.26. 

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: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12721
SUBJECT: GRB 111225A: TAROT Calern observatory optical observations
DATE:    11/12/25 04:31:51 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (OHP-CNRS), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 111225A detected by SWIFT
(trigger 510341) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 59.7s after the GRB trigger
(15.5s after the notice). The elevation of the field decreased from
10 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT in the XRT error box (Siegel et al.
CGNC 12720) with a limiting magnitude of:
t0+59.7s to t0+119.7s : R > 15.9

The second image is 30.0s exposure in tracking mode:
t0+134.4s to t0+164.4s : R > 16.2

We co-added a series of exposures:
t0+134.4s to t0+326.7s : R > 18.0

No OT was detected in the next images until
t0+1700s at the level R > 17.6.

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

This message may be cited.


GRB_name: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12722
SUBJECT: GRB 111225A: TAROT Calern observatory optical detection
DATE:    11/12/25 04:59:02 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (OCA-CNRS), Atteia J.L. (IRAP-OMP) report:

We imaged the field of GRB 111225A detected by SWIFT
(trigger 510341) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

Following the previous report (Klotz et al. GCNC 12721)
we co added only long exposure images obtained later
than 1100 seconds after the trigger and we detect
marginally the UVOT OT mentioned by Siegel et al.
(CGNC 12720):

t0+1100s to t0+1800s : R = 19.1 (+/- 0.6)

The OT detected by TAROT has a comparable magnitude
as NOMAD1 1415-0026136 locaded 20 arcsec from the
UVOT OT position.

This message may be cited.


GRB_name: GRB111225A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12723
SUBJECT: GRB 111225A: Super-LOTIS early detection
DATE:    11/12/25 05:51:01 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike (Dickinson College), Dieter H. Hartmann (Clemson
University), Peter A. Milne (Steward Observatory) and G. Grant Williams
(MMT Observatory) report:

We observed the field of GRB 111225A (Siegel et al., GCN 12720) with the
0.6m Super-LOTIS telescope located at Kitt Peak National Observatory under
good conditions and airmass of 1.1.  Observations began 49 seconds after
the trigger.  The OT (Siegel et al. GCN 12720, Klotz et al. GCN 12722) is
marginally detected in 300 seconds of stacked images (with a midtime of
480 seconds after the trigger) with an R-band magnitude of 19.9 +/- 0.2
(on comparison to the USNO B1.0 catalog).  Observations are continuing.

This message may be cited.


GRB_name: GRB111225A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12724
SUBJECT: GRB 111225A: Enhanced Swift-XRT position
DATE:    11/12/25 08:38:19 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 1857 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 111225A, 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 = 13.15557, +51.57157 which is equivalent
to:

RA (J2000): 00h 52m 37.34s
Dec (J2000): +51d 34' 17.6"

with an uncertainty of 2.2 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: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12725
SUBJECT: GRBv111225A: Xinglong TNT optical afterglow
DATE:    11/12/25 13:27:24 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 111225A ( Siegel  et al., GCN 12720)
with Xinglong TNT telescope from 10:50:40  (UT), about 7 hour  after 
the burst.  

Preliminary analysis shows that the brightness of the optical afterglow counterpart ( Siegel  et al., GCN 12720, Klotz et al. GCN 12722, 
Adria et al. GCN 12723) has decayed to about R~20.4 mag 
relatively to USNO B1.O R2 mag, at the mean time of 7.7 hour 
after the burst.

More observations are encouraged.

This message may be cited.

Thanks for the observation assistant of TNT telescope at Xinglong observatory.


GRB_name: GRB111225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12726
SUBJECT: GRB 111225A, Swift-BAT refined analysis
DATE:    11/12/25 15:51:38 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-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. H. Siegel (PSU) 
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111225A (trigger #510341)
(Siegel, et al., GCN Circ. 12720).  The BAT ground-calculated position is
RA, Dec = 13.158, 51.573 deg which is 
  RA(J2000)  =  00h 52m 37.9s 
  Dec(J2000) = +51d 34' 21.8" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 93%.

The mask-weighted light curve shows a FRED like structure with the emission 
starting at ~T-15 sec, peaking at ~T-5 sec and ending at ~T+150 sec.  
T90 (15-350 keV) is 106.8 +- 26.7 sec (estimated error including systematics).

The time-averaged spectrum from T-14.28 to T+111.24 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.70 +- 0.15.  The fluence in the 15-150 keV band is 1.3 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T-4.40 sec in the 15-150 keV band
is 0.7 +- 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/510341/BA/


GRB_name: GRB111225A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12727
SUBJECT: GRB 111225A: Swift-XRT refined Analysis
DATE:    11/12/25 16:01:44 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

B.-B. Zhang and M. H. Siegel (PSU) reports on behalf of the Swift-XRT
team:

We have analysed 10 ks of XRT data for GRB 111225A (Siegel  et al. GCN
Circ. 12720), from 94 s to 23.3 ks after the  BAT trigger. The data
comprise 556 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 12724).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.6 (+0.4, -0.3). At T+114 s  the decay
steepens to an alpha of 1.83 (+0.10, -0.09). The light curve breaks
again at T+353 s to a decay with alpha=3.1 (+/-0.5),  before a final
break at T+590 s s after which the decay index is 1.80 (+0.11, -0.12).
An early time flare (from T+214.6 to T+321.8 s) and a possible late
time flare (from ~T+20000s) are excluded from the fit.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.43 (+/-0.07). The
best-fitting absorption column is  2.09 (+0.16, -0.15) x 10^21 cm^-2,
in excess of the Galactic value of 1.7 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.71 (+0.17, -0.15)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.5 x 10^-11 (5.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+7.7, -0) x 10^20 cm^-2
Galactic foreground: 1.7 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.71 (+0.17, -0.15)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00510341.

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


GRB_name: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12728
SUBJECT: GRB 111225A: 1.23m CAHA optical observations
DATE:    11/12/25 22:59:12 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), P. Martorell (Obs. Guirguillano), P. Kubanek  
(IAA-CSIC & U. Valencia),  S. Mottola (DLR, Berlin), report on behalf  
of a larger collaboration:

"We have observed the field of GRB 111225A (Siegel et al. GCNC 12720)  
with the 1.23m CAHA telescope. The observations were carried out in  
Dec 25.74725 - 25.83561 UT (14.1--16.2 hours post burst) in the R-band  
with a total exposure time of 11x300+15x180s. We detect the optical  
afterglow of the burst with an R-band magnitude of R=21.60+/-0.16,  
with respect to the USNO B1.0 catalogue."


GRB_name: GRB111225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12729
SUBJECT: GRB 111225A: GRT Optical Observation
DATE:    11/12/26 00:16:14 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),
T. Okajima (GSFC), Y. Urata (NCU)

We observed the field of GRB 111225A detected by Swift
(trigger #510341; Siegel et al., GCN Circ. 12720) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

A total 20 images of 60 sec (10 images), 180 sec (5 images) and 
300 sec (5 images) exposures were taken in the R filter starting 
from December 25 03:52:12  (UT) about 94 seconds after the trigger 
(50 seconds after the BAT position notice) and stopped on December 25 
04:43:53 (UT).  We do not detect the optical afterglow both in the 
individual images and the stacked image inside the enhanced XRT position 
(Evans et al., GCN #12724).  The estimated upper limit of the combined 
image (total exposure of 3000 sec) is ~18.5 mag using the USNO-B1 catalog.


GRB_name: GRB111225A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12730
SUBJECT: GRB111225A: MITSuME Okayama optical upper limits
DATE:    11/12/26 02:09:16 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 111225A (Siegel et al., GCNC 12720)
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 2011-12-25 09:00:08 UT (~5.2 hours
after the burst). We did not find any new point source within the
enhanced XRT error circle (Evans et al., GCNC 12724) and could not
detect the previously reported afterglow (Klotz et al., GCNC 12722;
Updike et al., GCNC 12723) in g' and Ic 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'     Ic
------------------------------------------------------
0.25569    09:58:49  5700.0     >20.2  >19.6
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111225A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12731
SUBJECT: GRB 111225A: PAIRITEL NIR Upper Limits
DATE:    11/12/26 06:06:41 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 111225A (Siegel et al., GCN 12720) with
the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began
at 2011-12-26 01h13m05 UT, ~21.35 hr after the Swift Trigger.  In
mosaics taken simultaneously in the J, H, and Ks filters, we do not
detect the optical afterglow (Siegel et al., GCN 12720; Klotz et al.,
GCN 12722; Updike et al., GCN 12723; Xin et al., GCN 12725; Gorosabel
et al., GCN 12728).

The preliminary photometry yields:

post burst
t_mid(h) exp.(s) filt  U. Limit (3 sig)
22.45    4774    J     > 18.4
22.45    4774    H     > 17.6
22.45    4774    Ks    > 16.9

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: GRB111222A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12732
SUBJECT: GRB 111222A : Suzaku WAM observation of the prompt emission
DATE:    11/12/26 06:09:28 GMT
FROM:    Norisuke Ohmori at Miyazaki U  <ohmori@astro.miyazaki-u.ac.jp>

N. Ohmori, M. Akiyama, M. Yamauchi (Univ. of Miyazaki), M. Ohno, 
Y. Hanabata, T. Uehara, T. Kawano, K. Takaki, M. Mizuno, Y. Fukazawa 
(Hiroshima U.), K. Yamaoka (Aoyama Gakuin U.), W. Iwakiri, M. Tashiro, 
Y. Terada, T. Yasuda, K. Takahara, M. Asahina, S. Kobayashi, A. Sakamoto 
(Saitama U.), S. Sugita (Nagoya U.), M. Kokubun, T. Takahashi (ISAS/JAXA), 
Y. E. Nakagawa (Waseda U.), C-J. Chuang, Y. Urata, P. Tsai (NCU), 
K. Nakazawa, K. Makishima (Univ. of Tokyo),

The short hard intense GRB111222A (localized by IPN: Hurley et al., GCN 12714)
was detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers 
an energy range of 50 keV - 5 MeV at 14:51:55 UT (=T0).

The observed light curve shows a double-peaked structure starting at
T0 s, ending at T0+2 s with a duration (T90) of about 1 seconds. 
The fluence in 100 - 1000 keV was 3.98 (-1.21, +0.74) x 10^-6 erg/cm^2. 
The 1-s peak flux measured from T0 s was 4.70 (-1.18, +1.00) 
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+2 s is well fitted by a power-law with exponential cutoff model:
 dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
 alpha : -0.28 (-0.49, +0.43), and
 Epeak : 629 (-50, +61) keV (chi^2/d.o.f. = 94.8/98).
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/untrig/grb_table.html


GRB_name: GRB111225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12733
SUBJECT: GRB 111225A: Keck/LRIS Afterglow Photometry
DATE:    11/12/27 06:20:27 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko, J. S. Bloom, J. M. Silverman, A. N. Morgan (UC Berkeley), D.
A. Perley (Caltech), A. Cucchiara, J. X. Prochaska (UCSC / UCO Lick), A.
V. Filippenko (UC Berkeley), and P. E. Nugent (LBNL / UC Berkeley) report
on behalf of a larger collaboration:

We have imaged the field of GRB111225A (Siegel et al., GCN 12720) with the
Low-Resolution Imaging Spectrometer (LRIS) mounted on the 10 m Keck I
telescope beginning at 4:56 UT on 2012 Dec 26 (~ 25.1 hours after the
Swift BAT trigger).  We detect the optical afterglow in both the g' and
R-band filters, with an approximate magnitude at this time of R ~ 23.2
(estimated uncertainty of 0.3 mag, due largely to preliminary calibration
with respect to the USNO-B1 catalog).  Compared with previously reported
detections (Xin et al, GCN 12725, Gorosabel et al., GCN 12728), this
suggests a steep fading of the afterglow emission at this late time
(power-index alpha ~ 2.5).


GRB_name: GRB111215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12734
SUBJECT: GRB 111215A: Keck/LRIS Imaging
DATE:    11/12/27 06:24:47 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko, J. S. Bloom, J. M. Silverman, A. N. Morgan (UC Berkeley), D.
A. Perley (Caltech), A. Cucchiara, J. X. Prochaska (UCSC / UCO Lick), A.
V. Filippenko (UC Berkeley), and P. E. Nugent (LBNL / UC Berkeley) report
on behalf of a larger collaboration:

We have imaged the field of GRB111215A (Oates et al., GCN 12681) with the
Low-Resolution Imaging Spectrometer (LRIS) mounted on the 10 m Keck I
telescope beginning at 5:12 UT on 2012 Dec 26 (~ 10.6 days after the Swift
BAT trigger).  Near the position of the radio and mm counterpart (Horesh
et al., GCN 12710; Zauderer et al., GCN 12711), we detect a faint source
with coordinates:

 RA: 23:18:13.29      Dec: +32:29:38.8  (J2000)

Astrometric calibration was performed with respect to several 2MASS point
sources in the field of view, and we estimate an uncertainty of ~ 200 mas
in each coordinate.  We measure a magnitude for this object of R ~ 25.2
(referenced to nearby point sources from the Sloan Digital Sky Survey).

Using the sky density of objects of this brightness (Hogg et al., 1997,
MNRAS, 288, 404), we estimate the probability of chance alignment (e.g.,
Bloom et al., 2002, AJ, 123, 1111) to be relatively small (<~ 1%).  We
therefore consider it likely that this object is associated with
GRB111215A.

A second, fainter source is visible ~ 1.5" NE of the radio position.  The
relation of this source to GRB111215A is not clear at the moment, as the
probability of chance coincidence at this radius and brightness is not
negligible.


GRB_name: GRB111225A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12735
SUBJECT: GRB 111225A: Swift/UVOT Observations
DATE:    11/12/27 16:51:36 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111225A
95 s after the BAT trigger (Siegel et al., GCN Circ. 12720).
A source consistent with the XRT position is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  00:52:37.22 =  13.15510 (deg.)
   Dec (J2000) = +51:34:19.5  =  51.57208 (deg.)
with an estimated uncertainty of 0.67 arc sec. (radius, 90% confidence).

The afterglow has not been detected since the first orbit.  Preliminary detections and
3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

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

u (fc)              95          345          246         19.46 +/- 0.17
v                  610        18443         2140        >21.1
u                 4385        16744         1475        >20.66 
uvw1               659        12668         1212        >20.4
uvm2               634        11879         1337        >20.5
uvw2               354        17652         1780         21.36 +/- 0.31

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.26 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12736
SUBJECT: GRB 111205A: optical observations
DATE:    11/12/28 09:04:33 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  A. Volnova (SAI MSU),  A. Pozanenko (IKI)  report on 
behalf of  larger GRB  follow-up collaboration:

We observed the field of IPN of hard intense GRB 111205A  (Hurley et al., 
GCN 12626; Golenetskii et al., GCN 12627) with 0.45-m telescope If ISON-NM 
observatory on Dec 8 (09:55:52 - 11:52:34 UT). We took several unfiltered 
images of  300 s exposure. All our images cover full IPN error box.  On a 
stacked image we do not find any new objects within IPN error box in 
comparison with DSS. We detect DSS source mentioned by Wolf & Hoversten in 
the XRT error circle (Wolf & Hoversten, GCN 12630).  However due to bad 
seeing we cannot resolve this source into separate sources of a double star 
(Kann et al., GCN 12636).

Photometry of the unresolved source based on several nearby USNO-B1.0 stars 
(R2 magnitudes) is the following:

t-t0             filter      Exp.     source             uplim (3 sigma)
(mid, days)             (s)

2.90513      none     21x300   15.40 +/- 0.05     19.8


GRB_name: GRB111228A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12737
SUBJECT: GRB 111228A: Swift detection of a burst with an optical counterpart
DATE:    11/12/28 16:00:13 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

T. N. Ukwatta (MSU), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), S. Campana (INAF-OAB), P. D'Avanzo (INAF-OAB),
B. Gendre (ASDC), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (NASA/GSFC), A. Melandri (INAF-OAB),
J. P. Osborne (U Leicester), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), E. Sonbas (NASA/GSFC/Adiyaman Univ.) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 15:44:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111228A (trigger=510649).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 150.079, +18.293 which is 
   RA(J2000) = 10h 00m 19s
   Dec(J2000) = +18d 17' 35"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a strong triple-peaked
structure with a duration of about 100 sec.  The peak count rate
was ~5000 counts/sec (15-350 keV), at ~93 sec after the trigger. 

The XRT began observing the field at 15:47:08.6 UT, 145.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 150.06478, 18.29912 which
is equivalent to:
   RA(J2000)  = 10h 00m 15.55s
   Dec(J2000) = +18d 17' 56.8"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 53 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 (2.95 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.4
(+2.09/-1.76) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 0.1 s image was 8.82e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 155 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 10:00:16.01 = 150.06669
  DEC(J2000) = +18:17:51.8  =  18.29773
with a 90%-confidence error radius of about 0.75 arc sec. This position is 8.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.19 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
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: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12738
SUBJECT: GRB 111228A:  Xinglong TNT confirms the optical afterglow
DATE:    11/12/28 16:46:27 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 111228A (Ukwatta et al., GCN 12737)
with Xinglong TNT telescope at 15:46:18 (UT), about 96 sec  after 
the burst.  A series of White, R-band images were obtained. 
The optical counterpart (Ukwatta et al., GCN 12737) 
was detected in all the images. 
The brightness of OT is about 16.5 magnitude at the 
mean time of  106 sec after the burst,
relatively to  USNO B1.0 catalogure.

Follow-up observations are ongoing.

This message may be cited.

For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org:8080/grb/index.html"


GRB_name: GRB111020A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12739
SUBJECT: XMM-Newton observation of the short GRB 111020A
DATE:    11/12/28 16:55:48 GMT
FROM:    Sergio Campana at INAF-OAB  <sergio.campana@brera.inaf.it>

S. Campana (INAF-Osservatorio astronomico di Brera) reports:

XMM-Newton observed the short GRB 111020A (Sakamoto et al.
2011, GCN 12460) on Oct 20, 2011 21:50:05 UT (15.3 hr after
the burst onset).
The ~20 ks observation was affected in the first part by a mild enhanced
background event which we filtered out. The resulting pn/MOS1/MOS2
exposure times were 15, 17 and 17 ks, respectively.

A source is well detected at a position consistent with the Swift's
(Osborne et al. 2011, GCN 12463) and Chandra's (Berger et al. 2011,
GCN 12492) ones.
The pn count rate is (2.2+/-0.2)x10^{-2}  cts/s.
We extracted 422, 166, and 142 source photons from the pn, MOS1,
and MOS2, respectively.
The spectrum can be fitted with a power law model including a 
non-negligible
absorption component in addition to the Galactic one (6.9x10^{20} cm^{-2}).
The best fit power law implies a photon index of Gamma=1.9+/-0.3
(90% c.l. for one parameter of interest) and an additional column 
density of
NH=(6+/-2)x10^{21} cm^{-2} (90% c.l.). This provides a lower limit to the
intrinsic column density. The reduced chi^2 of the fit is 0.83 (31 d.o.f.).
The unabsorbed 0.5-10 keV is ~2x10^{-13} erg/cm^2/s.


GRB_name: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12740
SUBJECT: GRB 111225A, optical observations
DATE:    11/12/28 18:26:56 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

TITLE: T100 observations of GRB 111225A

Sonbas, E.(Adiyaman Univ.), Guver, T. (Sabanci Univ.), Gogus, E. (Sabanci
Univ.),
Uysal, O. (Akdeniz Univ.), Sahin T. (Akdeniz Univ.), Eker, Z. (TUG), T.
Ozisik (TUG) on behalf of a larger collaboration.


We observed the field of GRB 111225A (Siegel et al., GCN #12720) with the
1.0 meter T100 telescope (TUBITAK National
Observatory, Antalya - Turkey), starting on December 25, 21:14 UT (~ 17
hours after the trigger). We obtained
3 x 60 s + 2 x 300 s exposures with R and B filters under moderate weather
conditions (seeing 1.8").

We do not detect an optical afterglow at the enhanced XRT error circle
reported by Evans et al., GCN #12724
in the combined R and B band images. We determine the following 3-sigma
upper limits (calibrated to R2 and B2 mag. of USNO-B1)
in the two bands:

   t - t0        Exposure (s)          Filter              mag.
~17.4 h           780                    R                 > 22.5
~17.5 h           780                    B                 > 21.9

We are grateful to the TUBITAK National Observatory staff for promptly
scheduling the observations and their
technical support.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12741
SUBJECT: GRB 111228A: Possible host galaxy in the SDSS arhive
DATE:    11/12/28 20:40:10 GMT
FROM:    Tolga Guver at UA  <tolga@physics.arizona.edu>

Guver, T. (Sabanci Univ.)

The field of the GRB 111228A (Ukwatta et al. GCN 12737) was observed
with the SDSS survey (Abazajian et al. 2009, ApJS, 182, 543).

Within 2.2 arcseconds of the XRT coordinates, SDSS detected a galaxy namely
SDSS J100015.45+181755.1. The exact coordinates of the galaxy are given as
RA : 150.06439037, DEC : +18.29865952 (J2000).

SDSS magnitudes of the galaxy are  :

u = 21.99 +/- 0.20
g = 21.34 +/- 0.05
r  = 20.90 +/- 0.05
i  = 20.72 +/- 0.06
z = 20.72 +/- 0.21

SDSS also provides a photometric redshift for the galaxy as z =
0.192859 +/- 0.04821.

For further information SDSS page for the galaxy is :
http://skyserver.sdss3.org/dr8/en/tools/explore/obj.asp?id=1237667734494445890

----------------------------------------------------------------
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GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12742
SUBJECT: GRB 111228A: TAROT Calern observatory. OT seems still bright
DATE:    11/12/28 21:48:59 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (OHP-CNRS), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 111228A detected by SWIFT
(trigger 510649) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The trigger occured during daytime over Calern.
The observations started 289 min after the GRB trigger
The elevation of the field increased from 7 degrees
above horizon and weather conditions were good.

We detect the candidate couterpart mentioned by Ukwatta et al.
(GCNC 12737) and confirmed by Xin et al. (GCNC 12738) using
a co-addition of 10 images of 3mins. Surprisingly, the OT
is bright R~18 (Tstart=289 min, Tend=336 min) corresponding
to an optical decay alpha~0.3 taken TNT and TAROT data.
We suspect a rebrightening occured during the first minutes
after the trigger.

Netherveless, the low elevation and the 3 arcsec/pix
sampling of TAROT does not allow to discriminate
the OT from the star NOMAD1 1082-0210617 (RA=150.0646861
DEC=+18.2997694 R=19.9). Now TAROT continues observations
in better airmass conditions but other observations are
encouraged.

This message may be cited.


GRB_name: GRB111228A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12743
SUBJECT: GRB111228A: MITSuME Okayama Optical Observation
DATE:    11/12/28 21:50:56 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 111225A (Ukwatta et al., GCNC 12737)
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 2011-12-28 15:47:03 UT (~2.3 min after
the burst). We detected the previously reported afterglow
(Ukwatta, GCNC 12737; Xin et al., GCNC 12738) 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
----------------------------------------------------------------------
0.00511    15:52:04     540.0   17.45  0.06  17.13  0.05   16.52  0.05
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111228A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12744
SUBJECT: GRB 111228A: Fermi GBM observation
DATE:    11/12/28 23:03:23 GMT
FROM:    Michael S. Briggs at UAH and MSFC  <michael.briggs@nasa.gov>

M. S. Briggs (UAH) and G. Younes (USRA)
report on behalf of the Fermi GBM Team:

"At 15:45:30.80 UT on 28 Dec 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111228A (trigger 346779932 / 111228657),
which was also detected by the Swift BAT/XRT/UVOT (Ukwatta et al.
2011, GCN 12737).  The GBM on-ground location is consistent with the
Swift position.  The angle from the Fermi LAT boresight is 70 degrees.

The GBM light curve shows multiple peaks in three groups
with a duration (T90) of about 100 s (50-300 keV) starting
50 seconds before the GBM trigger time.  The time-averaged spectrum
from T0+0 s to T0+57 s is well fit by a power law function with an
exponential high-energy cutoff.  The power law index is -1.9 +/- 0.1
and the cutoff energy, parameterized as Epeak, is 34 +/- 4 keV
A Band function fits the spectrum equally well with
Epeak= 34 +/- 3 keV, alpha = -1.9 +/- 0.1 and beta = -2.7 +/- 0.3.

The event fluence (10-1000 keV) in this time interval is
1.8E-5 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+7.7 s in the 10-1000 keV band
is 27 +/- 1 ph/s/cm^2.

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



 

 

 

 

 
 


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12745
SUBJECT: GRB 111228A, optical observations
DATE:    11/12/29 00:09:07 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey, Vijay Kumar Bhatt, Brajesh Kumar and Ram Kesh Yadav (ARIES,
NainiTal, India, on behalf of larger Indian GRB collaboration).

We have observed GRB 111228A field (Ukwatta et al., GCN 12737; Briggs and
Younes, GCN 12744) with the 1.04m telescope at ARIES NainiTal starting
~1.9 hours post-burst. Several sets of exposures varying 100s to 300 s each
were taken in Bessel filters. The afterglow candidate (Xin et al., GCN
12738)
is visible in individual frames.

Preliminary photometry of the R_c band data in comparison to nearby USNO
stars,
indicates that the afterglow candidate has decayed by ~ 0.7 mag in ~ 3.5
hours
of observations. This corresponds to a temporal decay index of ~ 0.3,
similar
to what has been noticed by Klotz et al. (GCN 12742). Further observations
are
continued.

This message may be cited.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12746
SUBJECT: GRB 111228A: TAROT Calern observatory. OT decay stopped
DATE:    11/12/29 00:14:59 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (OHP-CNRS), Atteia J.L. (IRAP-CNRS-OMP) report:

We continue to obtain images of the field of GRB 111228A detected
by SWIFT (trigger 510649) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France (cf. GCNC 12742).

We confirm the OT observed by TAROT is not the galaxy
mentioned by Guver (GCNC 12741) neither the object
referenced as NOMAD1 1082-0210617 (Klotz GCNC 12742).
The OT observed by TAROT is the afterglow of GRB 111228A
and lies 9 arcsec eastern from these objects.

As we previously announced (GCNC 12742), we confirm that
the OT of GRB 111228A is brighter than a simple extrapolation
of the very early observations using a standard decay.
Current TAROT observations show that the decay is stopped.

Unfiltered TAROT images were co-added
to obtain a temporal series that shows clearly that
the brightness remains almost constant since the beginning
of the TAROT observations.

Photometry is relative to the star NOMAD1 1083-0203467
(RA=150.0946028 DEC=+18.3231806 J2000) R=17.28 (V-R)=+0.69.

  Tstart   Tend   Rmag OT
    (min)  (min)
     289    318   18.6 +/- 0.4
     321    352   18.9 +/- 0.4
     358    389   18.5 +/- 0.3
     392    421   18.7 +/- 0.3
     429    459   18.7 +/- 0.3
     462    492   18.9 +/- 0.3

This message may be cited.


GRB_name: GRB111228A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12747
SUBJECT: GRB 111228A: Enhanced Swift-XRT position
DATE:    11/12/29 00:26:33 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 1689 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 111228A, 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 = 150.06699, +18.29781 which is equivalent
to:

RA (J2000): 10h 00m 16.08s
Dec (J2000): +18d 17' 52.1"

with an uncertainty of 1.4 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: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12748
SUBJECT: GRB 111228A: optical observations
DATE:    11/12/29 01:07:55 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

V. Nascimbeni (Univ. Padova), E. Palazzi (INAF-IASFBo), D. Fugazza, A. 
Melandri, S. Covino (INAF-OABr), L. Borsato, A. Cunial, V. Granata 
(Univ. Padova), report on behalf of a larger collaboration:

We observed the field of GRB 111228A (Ukwatta et al., GCN 12737) with 
the 1.82m Asiago Telescope equipped with the AFOSC optical camera. A 900 
s R-band image was acquired with mean time Dec 28.939 UT (6.79 hr after 
the burst trigger).

We clearly detect the afterglow (Ukwatta et al., GCN 12737; Xin et al., 
GCN 12738; Klotz et al., GCN 12472) at a magnitude R = 18.6 +/- 0.02 
assuming R = 17.28 for the star USNO-B1 1083-0199833 (RA = 10:00:22.72, 
Dec = +18:19:23.85 - same as used by Klotz et al., GCN 12746).

We also clearly detect the SDSS object reported by Guver (GCN 12741), 
and confirm that it is not related to the GRB (Klotz et al., GCN 12746). 
Further observations are underway.


GRB_name: GRB111228A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12749
SUBJECT: GRB 111228A, Swift-BAT refined analysis
DATE:    11/12/29 01:16:35 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

J. R. Cummings (GSFC/UMBC),S. D. Barthelmy (GSFC),
W. H. Baumgartner (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), 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+746 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111228A (trigger #510649)
(Ukwatta, et al., GCN Circ. 12737).  The BAT ground-calculated position is
RA, Dec = 150.063, 18.284 deg which is
     RA(J2000)  =  10h 00m 15.0s
     Dec(J2000) = +18d 17' 02.2"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 39%.

The mask-weighted light curve shows multiple peaks in several clusters.  The first
set of peaks is at a low level from T-12 s to T+12 s.  There is another low level
set from T+32 to T+42 s, followed by a much brighter set of three overlapping peaks
from T+45 to T+60 s. The final cluster is broad and relatively soft from T+85
to T+110 s. T90 (15-350 keV) is 101.20 +- 5.42 sec (estimated error including
systematics).

The time-averaged spectrum from T-12.82 to T+115.43 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.27 +- 0.06.  The fluence in the 15-150 keV band is 8.5 +- 0.2 x 10^-6  erg/cm2.
The 1-sec peak photon flux measured from T+54.56 sec in the 15-150 keV band
is 12.4 +- 0.5 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/510649/BA/


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12750
SUBJECT: GRB 111228A: NOT optical observation
DATE:    11/12/29 03:04:32 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS/NAOC),  J. McCormac (Queen's Univ. Belfast), and P.
Jakobsson (Univ. Iceland) report on behalf of a larger collaboration:

We observed the field of GRB 111228A (Ukwatta et al., GCN 12737) with
the 2.5m Nordic Optical Telescope (NOT) equipped with the AFOSC
optical camera. A 600s R-band image was taken with mean time 01:32 UT
on 2011-12-29 (9.8 hr after the burst trigger).

We clearly detected the afterglow (Ukwatta et al., GCN 12737; Xin et
al., GCN 12738; Klotz et al., GCN 12742) at a magnitude R = 19.01 +/-
0.05, calibrated with the USNO-B1 1083-0199833 star (R2 = 17.28 mag;
also used by Klotz et al., GCN 12746 and Nascimbeni et al., GCN
12748).

Further observations are ongoing.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12751
SUBJECT: GRB 111228A: Skynet/Dolomiti Optical Observations
DATE:    11/12/29 03:51:36 GMT
FROM:    Melissa Nysewander at UNC-Chapel Hill  <mnysewan@unc.edu>

M. Nysewander, J. Haislip, K. Ivarsen, A. LaCluyze, M. Maturi, D. Reichart, J. Moore, T. Cromartie, R. Egger, A. Foster, N. Frank, A. Oza, E. Speckhard, A.Trotter, and J. A. Crain report:

Skynet observed the field of GRB 111228A (Ukwatta et al., GCN 12737) with the 16" Dolomites Astronomical Observatory telescope (DAO) in Italy beginning 6.4 hrs after the burst, and lasting for one hour.

We detect the afterglow in g' (11 x 180s) and r' (7 x 180s) exposures.  Using ~20 SDSS field stars, we measure the OT to be g' = 19.4 +- 0.1 at 6.73 hours and r' = 19.3 +- 0.2 at 7.30 hours in stacked images.  The OT faded by r' ~ 0.1 mag from 7.15 to 7.41 hours.


GRB_name: GRB111228A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12752
SUBJECT: GRB 111228A: Swift/UVOT Detection
DATE:    11/12/29 04:40:16 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and Ukwatta (MSU)  report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of
GRB 111228A  155 s after the BAT trigger (Ukwatta et al.,
GCN Circ. 12737).  The UVOT position is consistent with
the enhanced XRT position  (Goad et al., GCN Circ. 12747)
within the measurement accuracy.

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc.
1358, 373) for the early exposures are:

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

white              155          305          147         17.30 +/- 0.03
v                  389          759           58         17.73 +/- 0.16
b                  488          508           19         17.71 +/- 0.15
u                  463          483           19         16.70 +/- 0.12
w1                 439          459           19         16.59 +/- 0.17
m2                 764          784           19         16.84 +/- 0.24


The preliminary lightcurves show achromatic behavior during the
first 1200s and appears to maintain brightness levels until around
7000s after the trigger, when the decay in brightness sets in.

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12753
SUBJECT: GRB 111228A: IAC80 BVI-band observations
DATE:    11/12/29 05:10:43 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), R. Gimeno (IAC), A. Nicuesa Guelbenzu (TLS Tautenburg), report on behalf of a larger collaboration:

"We observed the field of GRB 111228A (Ukwatta et al., GCNC 12737) with the 82cm IAC80 telescope at the Observatorio del Teide, Tenerife, Spain. The observations were carried in the BVI-bands on Dec 29.08662 - 29.19141 UT (10.3-12.8 hours post burst). The optical afterglow of the burst (Ukwatta et al., GCNC 12737; Xin et al., GCNC 12738; Klotz et al., GCNC 12742; Pandey et al. GCN 12745; Nascimbeni et al. GCNC 12748; Xu et al., GCNC 12750; Nysewander et al. GCN 12751; Kuin et al. GCN 12752) is well detected in the three bands with an approximate magnitude of I~18.5 with respect to the USNO B1.0 catalogue."


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12754
SUBJECT: GRB 111228A: GRAS017 optical observations
DATE:    11/12/29 05:24:38 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 017 (Global-Rent-a-Scope, Nerpio, Spain) CDK17 17" (0.43 m)
 f/6.8 and FLI ProLine CCD camera were used to detect GRB 111228A
optical afterglow 9.0 hours after the burst trigger. The observations were 
started at 2011-12-29 00:35:06 (UT) and stopped at 2011-12-29 00:58:26 
(UT). Nine photometric R observations with 120s exposure times were 
made. The afterglow was detected at following position RA 10 00 16.07
and DEC +18 17 52.1.

The following magnitude was obtained from the observations using 
USNO-B1 1083-0199853 (R2 = 17.28) as the comparison:

Tmid(s)+T0    Filter        Exp (sec)     Mag      Mag err   Limit
32522               R           9x120          18.7        0.2        19.8

A png image of our observations is available at the following URL link:
http://cutenews.kassiopeia.net/data/upimages/GRB111228A_web.png


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12756
SUBJECT: GRB 111228A: MASTER OT observations
DATE:    11/12/29 07:29:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
  Blagoveschensk Educational State University, Blagoveschensk

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

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

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

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


MASTER II  robotic double telescope (MASTER-Net: 
http://observ.pereplet.ru) located in Blagoveschensk was pointed
to the  GRB111228.66 191 sec  after notice time and 244 sec after
GRB time at 2011-12-28 15:48:47.127 UT. The some delay was due to weather conditions.
  On our first (20s exposure, two polarizations, unfiltered) set we found 
optical transient  at Swift OT position (Ukwatta et al., GCN Circ R12737).
The OT magnitude is  about 16.5 mag in both polarizations.

The reduction is continuated.

The message may be cited.


GRB_name: GRB111228A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12757
SUBJECT: GRB 111228A: GROND observations
DATE:    11/12/29 07:55:33 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Klose (both TLS Tautenburg), and J. Greiner (MPE 
Garching) report on behalf of the GROND team:

We observed the field of GRB 111228A (Ukwatta et al., GCN 12737) 
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 
405) mounted at the 2.2-m MPG/ESO telescope on La Silla.

Observations started as soon the object was visible over La Silla, at 
04:46 UT on December 29, about 13 hr after the burst. We detect the 
afterglow (Ukwatta et al., GCN 12737; Xin et al., GCN 12738) in all bands. 
At a mean time of December 29, 05:35 UT, in an 8min exposure, we measure 
the following preliminary magnitudes (AB system):

    g' = 20.17  +/- 0.01,
    r' = 19.84  +/- 0.01,
    i' = 19.67  +/- 0.02,
    z' = 19.50  +/- 0.03,
    J  = 19.29  +/- 0.07,
    H  = 18.93  +/- 0.08.

The SED is best fit with a spectral slope of 0.90 +/- 0.05, with no 
evidence for additional extinction.

Optical data are calibrated against SDSS and NIR data against 2MASS field 
stars. Observations are continuing.


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12758
SUBJECT: GRB 111228A: TAROT La Silla observatory observations
DATE:    11/12/29 08:10:05 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (OHP-CNRS), Atteia J.L. (IRAP-CNRS-OMP) report:

We continue to obtain images of the field of GRB 111228A detected
by SWIFT (trigger 510649) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory, La Silla observatory,
Chile (early observations were done using TAROT Calern, reported
in GCNC 12742 and GCNC 12746).

Photometry is relative to the star NOMAD1 1083-0203467
(RA=150.0946028 DEC=+18.3231806 J2000) R=17.28 (V-R)=+0.69.

  Tstart   Tend   Rmag OT
    (min)  (min)
     788    837   19.0 +/- 0.4
     840    890   19.2 +/- 0.3

Taking account for the magnitudes obtained earlier from TAROT Calern
we deduce that the plateau phase may be now finished and an optical
decay of ~0.5 could now occur.

This message may be cited.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12759
SUBJECT: GRB 111228A: MMT Redshift
DATE:    11/12/29 08:16:27 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

J. Dittman, T. Laskar, and E. Berger (Harvard) report:

"Starting on 2011 December 29.312 UT (15.7 hours after the burst) we
used the Blue Channel spectrograph mounted on the MMT 6.5-m telescope
to observe GRB111228A (GCN #12737).  Our spectra cover the range
3400-8500A and reveal absorption lines of MgII and FeII at a common
redshift of z=0.714, which we consider to be the redshift of
GRB111228A.  Additional observations are in progress."


GRB_name: GRB111228A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12760
SUBJECT: GRB 111228A: PAIRITEL NIR Detection
DATE:    11/12/29 08:18:18 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

GRB 111228A: PAIRITEL NIR Detection

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 111228A (Ukwatta et al., GCN 12737) with
the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began
at 2011-12-29 06:55:25 UT, ~15.2 hours after the Swift Trigger.  In
mosaics (effective exposure time of 0.46 hours) taken simultaneously
in the J, H, and Ks filters, we marginally detect a source at the
optical afterglow location (Ukwatta et al., GCN 12737; Xin et al., GCN
12738; Klotz et al., GCN 12742; Pandey et al., GCN 12745; Nascimbeni
et al., GCN 12748; Xu et al. GCN 12750; Nysewander et al., GCN 12751;
Kuin & Ukwatta, GCN 12752; Gorosabel et al., GCN 12753; Hentunen et
al., GCN 12754; Sinykov et al., GCN 12756; Guelbenzu et al., GCN
12757).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
15.56      0.46     J     18.3   0.2
15.56      0.46     H     17.8   0.3
15.56      0.46     Ks    16.2   0.3

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


GRB_name: GRB111228A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12761
SUBJECT: GRB 111228A: Gemini South Redshift
DATE:    11/12/29 08:25:14 GMT
FROM:    Antonino Cucchiara at LBNL  <acucchiara@lbl.gov>

A. Cucchiara (UCSC/UCO Lick), A. J.  Levan (U. Warwick), 
and S. B. Cenko (UC Berkeley) report:

We obtained spectroscopy of the optical afterglow of 
GRB 111228A (Ukwatta et al., GCN 12737) using GMOS-South 
on the Gemini-South 8-m telescope.  
Observations began on December 29.28 UT (15 hrs after the 
BAT trigger). 

Inspection of the first two exposures (range 4160-8140 Angstroms) 
reveals MgII2796,2803, MgII2853 and CaH&K absorption features 
at a common redshift of 0.716.

We therefore suggest this to be the redshift of GRB 111228A.

We thank the Gemini staff for performing this observation, 
in particular Pascale Hibon.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12763
SUBJECT: GRB111228A: TNG spectroscopy analysis
DATE:    11/12/29 12:36:46 GMT
FROM:    Dino Fugazza at INAF-OAB  <dino.fugazza@brera.inaf.it>

E. Palazzi (INAF-IASFBo), D. Fugazza (INAF-OAB), S. Piranomonte 
(INAF-OAR) on behalf of a larger collaboration report:

The afterglow of GRB 111228A (Ukwatta et al. GCN 12737) was observed 
with the DOLORES instrument mounted at the Telescopio Nazionale Galileo 
on La Palma, Canary Islands. Starting on December 29.1200 (~11 hour 
after the burst), a series of three spectra of 1800s each were secured 
with LR-B grism (range 3500-8000 Angstroms).

Preliminary reduction of the spectra reveals absorption features that we 
identify with the following absorption lines:

Lines ID       Lambda_observed
              (Angstroms)
FeII_2344.21   4019.83
FeII_2374.46   4073.40
FeII_2382.76   4088.32
FeII_2585.65   4436.05
FeII_2600.17   4460.64
MgII_2795.50   4795.65
MgII_2802.70   4808.58
MgI_2852.96    4891.53
CaII_3933.68   6756.61
CaII_3968.49   6807.44

The derived redshift is z=0.7156  0.0005 which confirms the results 
obatined by Dittman et al. (GCN 12759) and Cucchiara et al (GCN 12761).

In addition to the GRB afterglow we observed the SDSS galaxy reported by 
Guver (GCN 12741). We detect many emission lines (OII_3726+3728, Hbeta, 
OIII_4958, OIII_5006, Halpha) at a common redshift of 0.218  0.001 
which is in agreement with the reported photometric redshift. This 
galaxy is therefore not related to the GRB.

We acknowledge the excellent support from the TNG staff, in particular 
Walter Boschin and Gianni Tessicini

[GCN OPS NOTE(22jan12): Per author's request, the affilation was changed
from "U.Milano-Bicocca,INAF/Brera" to "INAF-OAB".]


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12764
SUBJECT: GRB 111228A: NOT redshift
DATE:    11/12/29 12:43:17 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS/NAOC), J.P.U. Fynbo (DARK), J. McCormac (Queen's Univ.
Belfast), and P. Jakobsson (Univ. Iceland) report on behalf of a
larger collaboration:

We secured spectroscopy of the afterglow of GRB 111228A (Ukwatta et
al., GCN 12737) with the 2.5m Nordic Optical Telescope (NOT) equipped
with the ALFOSC optical camera. Observations started immediately after
the 600s R-band photometry in Xu et al. (GCN 12750).

The NOT spectrum covers 2750-9000A and shows clear absorption lines of
MgII2803 and CaH&K, at a common redshift of z=0.713.

Further observations are planned.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12765
SUBJECT: GRB111228A: TNG spectroscopy analysis
DATE:    11/12/29 12:53:17 GMT
FROM:    Dino Fugazza at U.Milano-Bicocca,INAF/Brera  <dino.fugazza@brera.inaf.it>

E. Palazzi (INAF-IASFBo), D. Fugazza (INAF-OAB), S. Piranomonte
(INAF-OAR) on behalf of a larger collaboration report:

The afterglow of GRB 111228A (Ukwatta et al. GCN 12737) was observed 
with the DOLORES instrument mounted at the Telescopio Nazionale Galileo 
on La Palma, Canary Islands. Starting on December 29.1200 (~11 hour 
after the burst), a series of three spectra of 1800s each were secured 
with LR-B grism (range 3500-8000 Angstroms).

Preliminary reduction of the spectra reveals absorption features that we 
identify with the following absorption lines:

Lines ID       Lambda_observed
               (Angstroms)
FeII_2344.21   4019.83
FeII_2374.46   4073.40
FeII_2382.76   4088.32
FeII_2585.65   4436.05
FeII_2600.17   4460.64
MgII_2795.50   4795.65
MgII_2802.70   4808.58
MgI_2852.96    4891.53
CaII_3933.68   6756.61
CaII_3968.49   6807.44

The derived redshift is z=0.7156 +/- 0.0005 which confirms the results 
obatined by Dittman et al. (GCN 12759) and Cucchiara et al (GCN 12761).

In addition to the GRB afterglow we observed the SDSS galaxy reported by 
Guver (GCN 12741). We detect many emission lines (OII_3726+3728, Hbeta, 
OIII_4958, OIII_5006, Halpha) at a common redshift of 0.218 +/- 0.001 
which is in agreement with the reported photometric redshift. This 
galaxy is therefore not related to the GRB.

We acknowledge the excellent support from the TNG staff, in particular 
Walter Boschin and Gianni Tessicini


GRB_name: GRB111228A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12766
SUBJECT: GRB 111228A: Swift-XRT refined Analysis
DATE:    11/12/29 13:01:33 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB) and T. N. Ukwatta (MSU) report on behalf of the
Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 111228A (Ukwatta  et al.
GCN Circ. 12737), from 135 s to 29.3 ks after the  BAT trigger. The
data comprise 331 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 12747).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=5.41 (+0.09, -0.07). At T+418 s  the decay
flattens to an alpha of 0.26 (+0.05, -0.06) before breaking again at
T+6950 s to a final decay with index alpha=1.27 (+0.19, -0.15).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 4.16 (+0.12, -0.11). The
best-fitting absorption column is  2.92 (+0.18, -0.17) x 10^21 cm^-2,
in excess of the Galactic value of 3.0 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.19 (+0.11, -0.10)
and a best-fitting absorption column of 1.52 (+0.27, -0.26) x 10^21
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (5.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.52 (+0.27, -0.26) x 10^21 cm^-2
Galactic foreground: 3.0 x 10^20 cm^-2
Excess significance: 7.9 sigma
Photon index:      2.19 (+0.11, -0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00510649.

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


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12767
SUBJECT: GRB 111228A: GMG optical observation
DATE:    11/12/29 15:16:14 GMT
FROM:    Xiao-hong Zhao at Yunnan Observatory  <zhaoxiaohong78@gmail.com>

X.-H. Zhao (YNAO), D. Xu (WIS/NAOC), J.-R. Mao (KASI/YNAO), J.-M. Bai
(YNAO) report:

We observed the field of GRB 111228A (Ukwatta et al., GCN 12737) at the
2.4m Gao-Mei-Gu (GMG) telescope equipped with YFOSC. Observations
started at 16:31:38 UT on 2011-12-28  (i.e., 47 mins after the burst) and 
4x600s R-band images were obtained in a seeing of
~3.36". We found the afterglow was decaying. The results are as follows:
mid time (UT)                            magnitude (err)
 2011-12-28 16:36:38                     17.11 (0.01)  
 2011-12-28 17:19:14                    17.42 (0.01)  
 2011-12-28 17:44:57                    17.56 (0.01)  
 2011-12-28 17:56:15                    17.62 (0.01). 

The magnitudes were calibrated with the USNO-B1 #1083-0199833 star (R2 = 17.28 mag; also
used by Klotz et al., GCN 12746; Nascimbeni et al., GCN 12748; Xu et
al., GCN 12750; Hentunen et al., GCN 12754).

Further observations are planned.

We thank the GMG staff, especially Y.-X. Xin, Fen He, and Gui-Hua He for
performing these observations.

[GCN OPS NOTE(29dec11): Per author's request, the affiliation of X-H.Z. 
was changed to Yunnan Observatory.]


GRB_name: GRB111228A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12768
SUBJECT: GRB111228A: MITSuME Akeno photometry of the optical afterglow
DATE:    11/12/29 15:34:59 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

R. Usui,  Y. Aoki, S. Song, M. Hayashi, K. Kawakami, K. Tokoyoda,
Y. Saito, Y. Yatsu, and N. Kawai (Tokyo Tech)  report on behalf of
the MITSuME collaboration:

We observed the field of GRB 111228A (Ukwatta et al., GCNC 12737)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2011-12-28 15:45:47 UT (~ 64 sec after
the burst).  We detected the previously reported afterglow
(Ukwatta, GCNC 12737; Xin et al., GCNC 12738) 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
----------------------------------------------------------------------
0.00074    15:46:02     30.0   17.3  0.2  16.12  0.09   15.5  0.1
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111228A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12769
SUBJECT: GRB 111228A: T100 observations
DATE:    11/12/29 16:36:46 GMT
FROM:    Tolga Guver at UA  <tolga@physics.arizona.edu>

T. Guver (Sabanci Univ.), E. Sonbas (Adiyaman Univ.), S. Kaynar  
(Akdeniz Univ.), E. Gogus (Sabanci Univ.), Z. Eker (TUG) report on  
behalf of a larger collaboration

We observed the field of Swift GRB 111228A (Ukwatta et al., GCN 12737)  
with the 1.0 meter T100 telescope (TUBITAK National Observatory,  
Antalya - Turkey), starting December, 28, 22:48 UT (~ 7 hours after  
the trigger). Observations were carried out in the B, R, and V filters  
under good weather conditions. The afterglow is clearly detected in  
all images.

Using the USNO-B1 star USNO-B1 1083-0199833 (RA = 10:00:22.72, Dec =  
+18:19:23.85 - same as used by Klotz et al., GCN 12746 and Nascimbeni  
et al., GCN 12748) in the field we estimated the following magnitudes  
for the OT:

t - t0 (h)       Exp. (s)      Filter            mag.        err
6.859            300            B               19.12      +/- 0.04
6.958            300            B               19.56      +/- 0.07
8.219            300            B               19.58      +/- 0.04
8.317            300            B               19.39      +/- 0.05
7.057            300            R               18.45      +/- 0.02
7.155            300            R               18.50      +/- 0.02
8.416            300            R               18.58      +/- 0.02
8.514            300            R               18.61      +/- 0.03

We are grateful to the TUBITAK National Observatory staff for promptly  
scheduling the observations and their technical support.


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GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12770
SUBJECT: GRB 111228A: X-shooter spectroscopy
DATE:    11/12/29 19:19:59 GMT
FROM:    Steve Schulse at U. of Iceland  <steve@raunvis.hi.is>

S. Schulze (U Iceland), S. Covino (INAF-OABr), H. Flores (GEPI/Obs. de  
Paris), J. P. U. Fynbo (DARK/NBI), B. Milvang-Jensen (DARK/NBI), J.  
Sollerman (U Stockholm), D. Xu (WIS) report on behalf of the X-shooter  
GRB collaboration:

We observed the afterglow of GRB 111228A (Ukwatta et al. GCN 12737)  
with the ESO VLT equipped with the X-shooter spectrograph on 29  
December 2011, beginning 07:40 UT (15.93 hr after the GRB). The  
afterglow had an R-band brightness of 20.08 mag in a series of five  
acquisition images with an exposure time of 30 s each (mid-exposure  
time = 15.98 hours). The magnitude is not corrected for Galactic  
extinction.

We acquired four spectra with an exposure time of 600 seconds each,  
beginning at 07:47 UT. We detect several absorption lines

wave_obs wave_rest  Ion     redshift
(AA, vac)   (AA, vac)
3880.28     2260.78     FeII     0.71634
4023.15     2344.21     FeII     0.71620
4075.26     2374.46     FeII     0.71629
4089.47     2382.77     FeII     0.71627
4422.70     2576.88     MnII    0.71630
4439.44     2586.65     FeII     0.71629
4453.10     2594.50     MnII    0.71636
4462.57     2600.17     FeII     0.71626
4799.05     2796.35     MgII    0.71618
4811.32     2803.53     MgII    0.71616
4896.33     2852.96     MgI     0.71623
6753.24     3934.78     CaK    0.71630
6813.09     3969.59     CaH    0.71632

at a common redshift of z = 0.71627 +/- 0.00002. In addition we detect  
[OIII]5007 at z_em = 0.71635, similar to the absorption line redshift.  
Our measurements confirm the results by of Cucchiara et al (GCN 12761)  
and Palazzi et al (GCN 12763) and are similar to Dittmann et al (GCN  
12759) and Xu et al (GCN 12764).

The seeing conditions over the entire campaign were around 0.8 arcsec.

We acknowledge the support of the VLT staff, in particular Claudio  
Melo and Christophe Martayan.


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12771
SUBJECT: GRB 111228A: P60 Observations
DATE:    11/12/29 20:00:39 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 GRB111228A (Ukwatta et al., GCN 12737) with
the automated Palomar 60 inch telescope.  Observations were obtained in
the r' and i' filters beginning at 10:27 UT on 2011 December 29 (~ 18.9
hours after the Swift trigger).

We detect the optical afterglow with a magnitude of r' = 20.3 +/- 0.1 mag
(AB, calibrated with respect to several point sources from the Sloan
Digital Sky Survey in the field).  Compared with previous reported
measurements of the afterglow brightness, this suggests a steeper decay
than observed at early times (e.g., Klotz et al., GCN 12742).

Further observations are planned.


GRB_name: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12772
SUBJECT: GRB 111225A: Lightbuckets Optical Observations
DATE:    11/12/29 20:12:26 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

T. N. Ukwatta (MSU), E. Sonbas (GSFC/Adiyaman Univ.),
T. Sakamoto (GSFC/UMBC), N. Gehrels (GSFC), J. Linnemann (MSU),
K. Tollefson (MSU), and U. Abeysekara (MSU)

We observed the field of Swift GRB 111225A
(Siegel et al., GCN 12720) with the Lightbuckets 0.43m
rental telescope LB-0002 in South Alpen, France. Ten 60 s
observations were carried out in the R filter starting
2011-12-25 at 17:01:47 UT (~ 47 ks after the GRB trigger).

We do not detect the optical afterglow both in the individual
images and in the stacked image inside the XRT location. Our
upper-limit based on the stacked observation (using the
USNO-B1 catalog) is given below.

Time after trigger       Exposure (s)   Filter     Magnitude
  13.2 hours             10 x 60          R         > 19.7


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12773
SUBJECT: GRB 111228A: Liverpool Telescope Observations
DATE:    11/12/29 21:14:20 GMT
FROM:    Carole Mundell at ARI, JMU,Liverpool  <cgm@astro.livjm.ac.uk>

A. Melandri (INAF-OAB), C. Guidorzi (U. Ferrara), C. G. Mundell (Liverpool JMU) 
and N. R. Tanvir (U. Leicester), on behalf of a large collaboration report:

"We observed the optical afterglow of GRB 111228A (Ukwatta et al., GCN 
12737) with the 2-m Liverpool Telescope, starting at 02:55 UT on 2011 December 29. We 
took a sequence of images in Br'i' bands, with exposure time of 300s for each 
individual frame.

We clearly detect the optical afterglow in all individual images. In 
stacked frames we find the following magnitudes for the OT:

Mid time from  Total Exp   Filter    Magnitude
trigger (hr)    (s)
--------------------------------------------------
12.08          4x300       r'        19.68 +- 0.06
13.28          3x300       r'        19.89 +- 0.09
12.54          5x300       i'        19.57 +- 0.05
11.34          4x300       B         19.71 +- 0.08
12.96          4x300       B         19.79 +- 0.11
--------------------------------------------------

The magnitudes are calibrated against nearby SDSS-5 (r' and i' bands) and 
USNO-B1.0 (B band) field stars and are not corrected for the Galactic 
extinction.

This message may be cited."


GRB_name: GRB111229A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12774
SUBJECT: GRB 111229A: Swift detection of a burst
DATE:    11/12/29 22:55:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), P. D'Avanzo (INAF-OAB), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (INAF-IASFPA),
A. Melandri (INAF-OAB), J. L. Racusin (NASA/GSFC),
P. Romano (INAF-IASFPA), E. Troja (NASA/GSFC/ORAU) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 22:37:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111229A (trigger=510736).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 76.282, -84.723, which is 
   RA(J2000)  =  05h 05m 08s
   Dec(J2000) = -84d 43' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two or three peaks
with a total duration of about 25 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 22:39:15.5 UT, 83.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 76.2885, -84.7108 which
is equivalent to:
   RA(J2000)  = 05h 05m 09.25s
   Dec(J2000) = -84d 42' 38.8"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 43 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 (1.04 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 9.2
(+7.65/-5.74) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 87 seconds after the BAT trigger. No credible
afterglow candidate has  been found in the initial data products. The
2.7'x2.7' sub-image processing  failed because of no aspect solution. 
Results from the list of sources  generated on-board are not available
at this time. A full analysis will not be possible until the full data
set is downlinked. 

Burst Advocate for this burst is A. Y. Lien (yarleen AT gmail.com). 
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: GRB111229A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12775
SUBJECT: GRB 111229A: GROND afterglow candidate
DATE:    11/12/30 01:57:34 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Klose, D. A. Kann (all TLS Tautenburg), and J.
Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 111229A (Lien et al., GCN 12774) 
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 
405) mounted at the 2.2-m MPG/ESO telescope on La Silla.

Observations started in twilight, at 00:45 UT on December 30, 2.12 hr 
after the burst. In the refined XRT error circle (Lien et al., GCN 12774), 
we detect a new source in all bands which is significantly brighter than 
the DSS2 limit at RA, DEC (J2000) = 05:05:08.84, -84:42:38.7. At a mean 
time of December 30, 00:51 UT, in an 8min exposure, we measure the 
following preliminary magnitudes (AB system):

     g' = 20.50  +/- 0.04,
     r' = 19.96  +/- 0.03,
     i' = 19.74  +/- 0.03,
     z' = 19.58  +/- 0.03,
     J  = 19.01  +/- 0.11.

We propose this source to be the afterglow of GRB 111229A, implying a 
redshift of less than 3.5.

After correcting for a Galactic reddening of 0.18 mag, the SED is best fit 
with a spectral slope of 0.72 +/- 0.06.

Optical data are calibrated against GROND zero points and NIR data against 
2MASS field stars. Observations are continuing.


GRB_name: GRB111229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12776
SUBJECT: GRB 111229A: Swift-BAT refined analysis
DATE:    11/12/30 02:12:44 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), E. E. Fenimore (LANL), N. Gehrels (GSFC),
A. Y. Lien (NASA/GSFC/ORAU), 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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111229A (trigger #510736)
(Lien, et al., GCN Circ. 12774).  The BAT ground-calculated position is
RA, Dec = 76.561, -84.687 deg which is 
   RA(J2000)  =  05h 06m 14.5s 
   Dec(J2000) = -84d 41' 14.8" 
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.
 
The mask-weighted light curve shows an initial peak starting at ~T-2 sec,
peaking at ~T+1 sec, and returning to baseline at ~T+7 sec.  The second
weaker peak starts at ~T+15 sec and ends at ~T+22 sec.  T90 (15-350 keV)
is 25.4 +- 5.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.97 to T+26.15 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.85 +- 0.33.  The fluence in the 15-150 keV band is 3.4 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.12 sec in the 15-150 keV band
is 1.0 +- 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/510736/BA/


GRB_name: GRB111229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12777
SUBJECT: GRB 111229A: Gemini-South Redshift
DATE:    11/12/30 02:32:04 GMT
FROM:    Antonino Cucchiara at LBNL  <acucchiara@lbl.gov>

A. Cucchiara (UCSC/UCO Lick), A. J.  Levan (U. Warwick), 
and N. Tanvir (U. Leicester) report:

On December 30.05 UT (157 minutes after the BAT trigger) 
we observed the field of GRB 111229A (Lien et al., GCN 12774) 
using GMOS-South on the Gemini-South 8-m telescope.  

An optical afterglow is detected at a position reported by
Nicuesa Guelbenzu et al. (GCN 12775).
Subsequent spectroscopic observation of the optical afterglow of 
GRB 111229A  (range 5900-10080 Angstroms) reveals several absorption 
features, including FeII2586,2600, MnII2606, MgII2796,2803 
and MgII2853 at a common redshift of 1.3805.

We therefore suggest this to be the redshift of GRB 111229A.

We thank the Gemini staff for performing this observation, 
in particular Pascale Hibon.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12778
SUBJECT: GRB111228A: Further GMG observations
DATE:    11/12/30 04:04:44 GMT
FROM:    Xiao-hong Zhao at Yunnan Obs  <zhaoxiaohong78@gmail.com>

X.-H. Zhao (YNAO), L. P. Xin (NAOC), J.-R. Mao (KASI/YNAO), J.-M. Bai
(YNAO) report on behalf of a larger collaboration:

We made a further observation of GRB 111228A (Ukwatta et al., GCN 12737) with  2.4m Gao-Mei-Gu (GMG) telescope. Observations
started at 16:07:37 UT on 2011-12-29  (i.e., ~24.4 hrs after the burst) . We found the afterglow has faded significantly. The magnitudes are as follows:
mid time (UT)                   Exp. (s)     Filter               magnitude (err)
 2011-12-29 16:12:37        600            R                    20.24 (0.12)  
 2011-12-29 16:27:55        600            V                    20.67 (0.18)
 2011-12-29 16:38:54        600            B                    21.13 (0.15) 
 2011-12-29 16:52:46        600            R                    20.33 (0.12)  
 2011-12-29 17:03:24        600            V                    20.73 (0.18)
 2011-12-29 17:14:06        600            B                    21.31 (0.16)  
 2011-12-29 17:28:50        600            R                    20.54 (0.13)  
 2011-12-29 17:39:39        600            V                    20.96(0.21)   
 2011-12-29 17:51:19        600            B                    21.40 (0.17)  
  
 The magnitudes were calibrated with the USNO-B1 #1083-0199833 star (R2 = 17.28 mag and (V-R)=+0.69; also
used by Klotz et al., GCN 12746; Nascimbeni et al., GCN 12748; Xu et
al., GCN 12750; Hentunen et al., GCN 12754; Klotz et al. GCN 12758).

We thank the GMG staff, especially Y.-X. Xin, Fen He, and Gui-Hua He for
performing these observations.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12779
SUBJECT: GRB 111228A: Continued Skynet PROMPT/Dolomiti Optical Observations
DATE:    11/12/30 04:32:27 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, M. Nysewander, J. Haislip, K. Ivarsen, M. Maturi, D. 
Reichart, J. Moore, T. Cromartie, R. Egger, A. Foster, N. Frank, A. Oza, 
E. Speckhard, A.Trotter, and J. A. Crain report:

Skynet continued observing the field of GRB 111228A (Ukwatta et al., GCN 
12737) with the PROMPT telescope array at CTIO in Chile and the 16" 
Dolomites Astronomical Observatory telescope (DAO) in Italy.

We detect the afterglow in g', r', i' and B, R, I bands, with a 
chromatic variation suggested by late time data.  A preliminary light 
curve, calibrated to SDSS catalog sources can be found at the following 
link:

http://skynet.unc.edu/grb/grb111228a.png

Further observations are ongoing to attempt to confirm or refute the 
chromatic variation.


GRB_name: GRB111229A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12780
SUBJECT: GRB 111229A: Enhanced Swift-XRT position
DATE:    11/12/30 07:20:00 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 943 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 111229A, 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 = 76.28979, -84.71099 which is equivalent
to:

RA (J2000): 05h 05m 9.55s
Dec (J2000): -84d 42' 39.6"

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: GRB111229A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12781
SUBJECT: GRB 111229A: Swift-XRT refined Analysis
DATE:    11/12/30 10:55:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester), O.M. Littlejohns (U. Leicester), B.
Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC), P. D'Avanzo (INAF-OAB),
M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), J.P. Osborne
(U. Leicester) and A.Y. Lien report on behalf of the Swift-XRT team:

We have analysed 6.7 ks of XRT data for GRB 111229A (Lien  et al. GCN
Circ. 12774), from 93 s to 22.6 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Osborne et al. (GCN. Circ 12780).

The late-time light curve (from T0+4.4 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.54 (+0.14, -0.13).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.06 (+0.17, -0.14). The
best-fitting absorption column is  1.9 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 1.0 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 3.7 x 10^-11 (5.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.0 x 10^21 cm^-2
Excess significance: 2.7 sigma
Photon index:      2.06 (+0.17, -0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00510736.

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


GRB_name: GRB111229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12782
SUBJECT: GRB 111229A: Faulkes Telescope South observations
DATE:    11/12/30 12:16:31 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB)
report on behalf of the LJMU GRB group:

The 2-m Faulkes Telescope South observed Swift
GRB 111229A (Lien et al. GCN Circ. 12774)
on December 30, from 10:08 UT, corresponding to
11.5 hours after the BAT trigger time.
We clearly detect the optical afterglow (Nicuesa
Guelbenzu et al. GCN Circ 12775; Cucchiara et al.
GCN Circ. 12777) in the R filter and marginally
in the i' filter with the following magnitude:

Mid time from  Total Exp   Filter    Magnitude    Limit
trigger (hr)   (s)
--------------------------------------------------------
11.77          6x300       i'        21.6 +- 0.5 >20.9
12.34          6x300       R         21.4 +- 0.1
--------------------------------------------------------

Magnitudes are calibrated against nearby USNOB-1 stars.
Comparing with GROND observations (Nicuesa Guelbenzu
et al GCN 12775), we derive an average power-law decay
index of about 0.8.


GRB_name: GRB111229A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12783
SUBJECT: GRB 111229A: Swift/UVOT Detection
DATE:    11/12/30 13:32:12 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and A. Y. Lien (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111229A
87 s after the BAT trigger (Lien et al., GCN Circ. 12774).
A source consistent with the XRT position (Osborne et al., GCN Circ. 12780) and 
the GROND optical position (Nicuesa Guelbenzu et al., GCN Circ. 12780) is 
detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  05:05:08.86 =  76.28692 (deg.)
  Dec (J2000) = -84:42:39.1  = -84.71085 (deg.)
with an estimated uncertainty of 0.55 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

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

white (FC)        87            237           147          18.78 +/- 0.10
white            5230          5430           200          20.48 +/- 0.27
v                      630            649              20          17.70 +/- 0.49
b                     554             574             20          18.75 +/- 0.53
u (FC)            300             549           250          19.03 +/- 0.23
u                   4820          5020           200       20.67 +/- 0.53
w1                  679           6251          413           >20.4
m2               4410           6046          393           >20.4
w2                  779        22585        1597           >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.18 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12784
SUBJECT: GRB 111228A: SMARTS optical/IR afterglow observations
DATE:    11/12/30 17:34:16 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained
optical/IR imaging of the error region of GRB 111228A (GCN 12737,
Ukwatta et al.) with a mid-exposure time of 15.9 hours
(2011-12-29 07:39 UT) and 39.5 hours (2011-12-30 07:13 UT) post-burst.
Total summed exposure times amounted to 36 minutes in I and 30 minutes
in J.

The optical afterglow of GRB 111228A (e.g. GCN 12737, Ukwatta et al.;
GCN 12738, Xin et al.) is detected and observed to decay between our
imaging.  Preliminary comparison to Landolt standard stars in the optical
and 2MASS stars in the IR indicates the following magnitudes
for the afterglow:

time post-burst       I mag             J mag
15.9 hours            19.3 +/- 0.1      20.6 +/- 0.1
39.5 hours            18.4 +/- 0.1      > 19.1 (3-sigma limit)

This indicates that the decay rate of the burst between ~16 and 40 hours
post burst is alpha ~ 1.3 (where afterglow flux is proportional
to t^-alpha). In agreement with Cenko et al. (GCN 12771), this later-time
decay is much steeper than the earlier-time decay noted by Klotz et al.
(GCN 12742) and Pandey et al. (GCN 12745).


GRB_name: GRB111228A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12785
SUBJECT: GRB 111228A: correction to GCN 12784
DATE:    11/12/30 17:52:34 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

The data in the table in GCN 12784 was incorrectly placed.  The corrected
table is given below.

time post-burst      I mag              J mag
15.9 hours            19.3 +/- 0.1      18.4 +/- 0.1
39.5 hours            20.6 +/- 0.1       > 19.1 (3-sigma limit)

We apologize for any confusion.  We thank Adam Miller for pointing out this
error.


GRB_name: GRB110915A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12786
SUBJECT: GRB 110915A, the review of the sky area in plate archives
DATE:    11/12/30 17:58:18 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V. Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 110915A (Evans et al., GCN Circ.12340) 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 
and Epson Expression 10000XL flatbed scanners and have been 
placed into Golosiiv Plate Archive database DBGPA with open 
access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19810930/180433 GUA040C000001A 27.0 16.50 0825-18636133
19820827/205711 GUA040C002422 60.3 14.40 0825-18638528
19820827/205711 GUA040D002423 60.3 14.40 0825-18638528
19820827/223853 GUA040C002424 15.0 13.75 0825-18638504
19820909/165505 TAS040A000325 23.0 17.10 0825-18635715
19820918/160521 TAS040A000331 23.0 16.50 0825-18636133
19910709/231157 GUA040C001830A 22.5 15.50 0825-18638699
Plates:  
GUA040C,the plates archive identifier of DWA (D/F=400/2000, 
GUA040D  M=103"/mm) of the Ukrainian NAS Main Astro obs.
         (Marsden's number - 83) the plate number [1].
TAS040A -the plates archive identifier of DAZ (D/F=400/3000,
         M=68.8"/mm) of the Tashkent Astro obs.
         (Marsden's number - 186) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 15 minutes area around 
       the location given in GCN Circ.12340: 
       RA(J2000): 20h 43m 17.87s, Dec(J2000): -00d 43' 23.2"
Star USNOA2 - Comparison star.
  The preview images of 7 areas together with  
the 15x15 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/110915A/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: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12787
SUBJECT: GRB 111228A: Optical and NIR observations with Kanata telescope
DATE:    11/12/31 01:04:46 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

R. Itoh, K. Takaki, M. Yamanaka, M. Sasada, K. Sakimoto, M. Yoshida,
K. S. Kawabata, Y. Hanabata, M. Ohno, Y. Fukazawa (HiroshimaUniv.),
A. Nakashima (Tokyo Univ.) report on behalf of the Kanata collaboration:

We performed optical and near infrared observations of GRB 111228A
(Ukwatta et al., GCN 12737; Xin et al., GCN 12738) with the 1.5 m Kanata
Telescope of Higashi-Hiroshima observatory, Japan. The observation
started at 15:47 UT on 2011 December 28. We took a sequence of images
in Rc and K bands, and detected the optical-infrared afterglow of the
GRB (Veli-Pekka Hentunen et al. GCN 12754; Kuroda et al. GCN 12743;
Nicuesa Guelbenzu et al. GCN 12757; Usui et al. GCN 12768).

Photometric results are listed below. We used USNO-B1 catalog for flux
calibration of Rc band, and 2-MASS catalog for Ks band.

Mid time from  Total Exp   Filter    Magnitude
trigger (hr)    (s)
-------------------------------------------------
0.34            180x5        Ks    14.94 $B!^(B 0.10
1.12            300x10       Rc    17.67 $B!^(B 0.04
3.75            300x9        Rc    18.53 $B!^(B 0.02
-------------------------------------------------


GRB_name: GRB111228A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12788
SUBJECT: GRB 111228A: correction for GCN 12787
DATE:    11/12/31 01:21:32 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

R. Itoh, K. Takaki, M. Yamanaka, M. Sasada, K. Sakimoto, M. Yoshida,
K. S. Kawabata, Y. Hanabata, M. Ohno, Y. Fukazawa (HiroshimaUniv.),
A. Nakashima (Tokyo Univ.) report on behalf of the Kanata collaboration:

Character corruption occurred in the table of the Kanata telescope
photometric results inthe GCN circular 12787. We resubmit the corrected
table. We are sorry for the inconvenience.

Mid time from  Total Exp  Filter  Magnitude
trigger (hr)    (s)
-------------------------------------------------
0.34           180x5       Ks    14.94 +- 0.10
1.12           300x10      Rc    17.67 +- 0.04
3.75           300x9       Rc    18.53 +- 0.02
-------------------------------------------------


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12789
SUBJECT: GRB 111228A: MASTER-Net optical photometry 
DATE:    11/12/31 08:48:50 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
  Blagoveschensk Educational State University, Blagoveschensk

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

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

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


MASTER II  robotic double telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed
to the  GRB111228A (Ukwatta et al., GCN Circ R12737) 191 sec  after notice 
time and 244 sec after
GRB time at 2011-12-28 15:48:47.127 UT (Sinykov et al., GCN Circ 12756).

MASTER II  robotic double telescope (MASTER-Net: 
http://observ.pereplet.ru)
located near Kislovodsk was pointed
to the  GRB111228A  ~6.5 hours after
GRB time at 2011-12-28 22:24:47 UT.

The results of our photometry are:


    Date        UT       Exp  mag   Err      Filter
               Start     (s)

2011-12-28  15:48:47.1   20  16.9  0.2       P|
2011-12-28  15:48:47.1   20  16.5  0.2       P-
2011-12-28  15:49:34.7   30  17.1  0.2       P|
2011-12-28  15:49:34.7   30  16.7  0.2       P-
2011-12-28  15:50:37.3   40  16.8  0.2       P|
2011-12-28  15:50:37.3   40  17.3  0.2       P-
2011-12-28  15:51:43.1   50  17.6  0.2       P|
2011-12-28  15:51:43.1   50  17.5  0.2       P-
2011-12-28  15:52:59.7   70  16.8  0.2       P|
2011-12-28  15:52:59.7   70  17.1  0.2       P-
2011-12-28  15:54:41.3   90  17.3  0.2       P|
2011-12-28  15:54:41.3   90  17.3  0.2       P-
2011-12-28  15:56:38.4  110  17.0  0.2       P|
2011-12-28  15:56:38.4  110  17.6  0.2       P-
2011-12-28  16:01:44.8 180  17.3  0.2       P|
2011-12-28  16:01:44.8  180  17.6  0.2       P-
2011-12-28  22:24:47.9  180  19.0  0.3       V
2011-12-28  22:24:47.9  180  18.3  0.3       R
2011-12-28  22:28:14.1 180  18.9  0.3       V
2011-12-28  22:28:14.1  180  18.8  0.3       R
2011-12-28  22:31:42.7 180  19.3  0.3       V
2011-12-28  22:31:42.7  180  18.6  0.3       R
2011-12-29  00:13:44.5  180  18.8  0.3       R
2011-12-29  00:17:12.7  180  19.4  0.3       R
2011-12-29  00:20:45.7  180  18.9  0.3       R
2011-12-29  00:20:45.7  180  19.5  0.3       V
2011-12-29  01:45:51.9  180  19.4  0.3       R
2011-12-29  01:52:48.1  180  18.7  0.3       R

P|, P-   - are the 2 polarisations in white

The message may be cited.


GRB_name: GRB111228A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12790
SUBJECT: Konus-Wind observation of GRB 111228A
DATE:    11/12/31 11:38:24 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 111228A (Swift-BAT trigger #510649:
Ukwatta et al., GCN 12737; Cummings et al., GCN 12749)
triggered Konus-Wind at T0=56736.171s UT (15:45:36.171).

The light curve shows two groups of pulses separated by ~45 s.
A total duration of the burst is ~50 s.
The emission is seen up to ~1500 keV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111228_T56736/

As observed by Konus-Wind the burst
had a fluence of (7.5  1.3)x10-6 erg/cm2,
and a 256-ms peak flux, measured from T0+3.584 s,
of (2.0  0.3)x10-6 erg/cm2/s
(both in the 20 keV - 2000 MeV energy range).

The time-integrated spectrum of the burst (measured from T0 to T0+49.408 s)
is best fit in the 20 keV - 2000 keV range
by a simple power law function with the photon
index of (2.4  0.2), chi2 = 53.7/62 dof.

The spectrum at the maximum count rate (measured from T0 to T0+8.448 s)
is also best fit in the 20 keV - 2000 keV range
by a simple power law function with the photon
index of (2.25  0.15), chi2 = 77.1/62 dof.

Assuming the redshift z~0.715 (Dittman et al., GCN 12759;
Cucchiara et al., GCN 12761; Palazzi et al., GCN 12765;
Xu et al., GCN 12764) 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 (1.0  0.2)x10^52 erg, and
the isotropic peak luminosity L_iso_max is (4.6  0.7)x10^51 erg/s.

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


GRB_name: GRB111228A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12791
SUBJECT: GRB 111228A: LOAO Optical Observation
DATE:    11/12/31 11:58:29 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

  Yiseul Jeon, Myungshin Im, Minsung Jang (CEOU/Seoul National
  Univ.), and Yuji Urata (NCU) on behalf of a larger collaboration

  We observed GRB 111228A (Ukwatta et al., GCN 12737) in
  B- and R-bands with a 1 m telescope at Mt. Lemmon, Arizona, US.

  The observation started at 2011-12-30 08:03:16 UT,
  or 1.7 days after the BAT aleart. We detected the afterglow
  in the images taken with both filters.
  Using the the photometry calibration based on an USNO B1 star
  USNO-B1 1083-0199833 with B=18.85 and R=17.28 following Klotz et al.
  (GCN 12746), we find the following.

  Filter Mid-Time[UT] Mid-Time[Since BAT] Mag
  B-band 2011-12-30 08:33:55 40.82 hours 21.75+-0.14
  R-band 2011-12-30 10:41:29 42.95 hours 20.67+-0.09

  Further observation is ongoing. We thank the LOAO operator,
  J. Yoon for his help with the observation.


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12792
SUBJECT: GRB 111228A, optical observations
DATE:    11/12/31 12:19:21 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey, R. K. S. Yadav, Ram Sagar (ARIES, NainiTal, India) and
C. S. Stalin (IIA, Bangaluru); on behalf of larger Indian GRB 
collaboration.


The newly installed 1.3m Devasthal Fast Optical Telescope (79.7 E, 29.4 N,
altitude ~ 2450 m) started looking towards the Swift trigger 510649
(Ukwatta
et al., GCN 12373) ~ 2.7 hours after the burst. The optical afterglow
candidate (Ukwatta et al., GCN 12373; Xin et al., GCN 12738) was clearly
detected in the individual frames with an exposure time of 120 sec each,
taken in R_c band.

The decaying afterglow (Klotz et al., GCN 12742; Pandey et al., GCN 12745;
Cenko et al., GCN 12771) was also detected during the observations taken on
consecutive night in the frames having exposure time of 300 sec each.
Preliminary photometry of the frames yields following.

Time (UT)                  Exp (s)     Filter      Magnitude
-------------------------------------------------------------
2011-12-28,18:30:46.0       120 s       R_c        18.1+/-0.1
2011-12-29,23:56:38.0       300 s       R_c        19.8+/-0.1
-------------------------------------------------------------

The magnitudes are calibrated against nearby USNO stars. Further
observations
are continued.

This massage may be cited.


GRB_name: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12793
SUBJECT: GRB 111225A: optical observations in CrAO
DATE:    11/12/31 15:26:40 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 111125A (Siegel  et al. GCN  12720) with Shajn 
telescope of CrAO observatory on Dec. 28 between (UT) 21:28: and 22:38 under 
a mean seeing of 1.7 arsces. We took several frames with exposure of 60 s in 
R-band. We clearly detect afterglow of GRB 111225A (Klotz et al. GCN 12722) 
on a stacked image. A photometry is based on the USNO B1.0 star 1415-0025726 
(00 52 35.11 +51 33 58.9, J2000) assuming R=16.50.

T_start UT  T0+        Filter, Exposure, OT,  uplim (3 sigma)
                  (mid, d)            (s)

21:28:14     3.7590    R       62x60      22.51 +/- 0.10    24.0


GRB_name: GRB120102A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12794
SUBJECT: GRB 120102A: Swift detection of a burst with an optical counterpart
DATE:    12/01/02 02:28:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (NASA/GSFC),
T. Sakamoto (NASA/UMBC), C. J. Saxton (UCL-MSSL), C. A. Swenson (PSU)
and T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 02:15:55 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120102A (trigger=510922).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 276.201, +24.732 which is 
   RA(J2000)  =  18h 24m 48s
   Dec(J2000) = +24d 43' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows an initial small peak
and then a much larger peak 32 sec later with a toal duration of about 50 sec. 
The peak count rate was ~15,000 counts/sec (15-350 keV), at ~33 sec
after the trigger. 

The XRT began observing the field at 02:17:47.9 UT, 112.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 276.22495,
24.71375 which is equivalent to:
   RA(J2000)  = 18h 24m 53.99s
   Dec(J2000) = +24d 42' 49.5"
with an uncertainty of 3.7 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.03 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4.1
(+2.17/-1.89) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.02e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 121 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 18:24:53.90 = 276.22457
  DEC(J2000) = +24:42:47.3  =  24.71314
with a 90%-confidence error radius of about 0.62 arc sec. This position is 3.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.04 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.13. 

Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.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: GRB120102A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12795
SUBJECT: GRB 120102A: Enhanced Swift-XRT position
DATE:    12/01/02 05:09:12 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 967 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120102A, 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 = 276.22471, +24.71352 which is equivalent
to:

RA (J2000): 18h 24m 53.93s
Dec (J2000): +24d 42' 48.7"

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: GRB120102A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12796
SUBJECT: GRB 120102A: Swift/UVOT Detection
DATE:    12/01/02 12:41:27 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120102A
121 s after the BAT trigger (Marshall et al., GCN Circ. 12794).
A fading source consistent with the XRT position (Beardmore et al., GCN 
Circ. 12795) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  18:24:53.89 = 276.22456 (deg.)
     Dec (J2000) = +24:42:47.1  =  24.71309 (deg.)
with an estimated uncertainty of 0.51 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT 
photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the finding chart 
(FC) and early exposures are:

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

white (FC)         121          271          147         18.10  0.06
white              788         1014          167         19.9   0.2
v                  663         1239           78         18.16  0.31
b                  589        11310         1147        >20.8
u                  334          583          246         18.52  0.14
w1                 713         6983          452        >20.2
m2                 688         6778          452        >20.1
w2                 639        12879         1112        >20.9

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.13 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB120102A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12797
SUBJECT: GRB 120102A: Swift-XRT refined Analysis
DATE:    12/01/02 14:28:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

O.M. Littlejohns (U. Leicester), G. Stratta (ASDC), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), D.N. Burrows (PSU), J.A. Kennea (PSU),
M.C. Stroh (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester)
and F.E. Marshall report on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 120102A (Marshall  et al.
GCN Circ. 12794), from 119 s to 34.6 ks after the  BAT trigger. The
data comprise 240 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 12795).

The late-time light curve (from T0+4.5 ks) can be modelled with an
initial power-law decay with an index of alpha=1.99 (+0.27, -0.11),
followed by a break at T+13.0 ks to an alpha of 0.97 (+0.27, -0.22).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.04 (+/-0.08). The
best-fitting absorption column is  2.59 (+0.26, -0.25) x 10^21 cm^-2,
in excess of the Galactic value of 1.0 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 4.0 x 10^-11 (6.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.59 (+0.26, -0.25) x 10^21 cm^-2
Galactic foreground: 1.0 x 10^21 cm^-2
Excess significance: 10.3 sigma
Photon index:      2.04 (+/-0.08)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00510922.

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


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12798
SUBJECT: GRB 111228A: optical observations in CrAO
DATE:    12/01/02 14:52:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 111128A (Ukwatta  et al. GCN  12737) with Shajn 
telescope of CrAO observatory between (UT) 2011-12-28T23:08:08 and 
2011-12-29T01:04:41  under a mean seeing of 1.5". We took several frames 
with exposure of 60 s in BVRI. The photometry optical afterglow (Ukwatta  et 
al. GCN  12737; Xin et al. GCN 12738) is based on the USNO B1.0 star 
1083-0199833 (10 00 22.70 +18 19 23.5) assuming B=18.85, R=17.28, I=17.02
.
      T0+        Filter, Exposure, OT,  uplim (3 sigma)
    (mid, d)            (s)

0.3476     B       27x60      19.270 +/- 0.007  23.6
0.3491     R       27x60      18.710 +/- 0.005  23.5
0.3499     I        27x60      18.608 +/- 0.006  23.2

 


GRB_name: GRB120102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12799
SUBJECT: GRB 120102A: Swift-BAT refined analysis
DATE:    12/01/02 15:24:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC), 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), F. E. Marshall (NASA/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-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120102A (trigger #510922)
(Marshall, et al., GCN Circ. 12794).  The BAT ground-calculated position is
RA, Dec = 276.224, 24.713 deg, which is 
   RA(J2000)  =  18h 24m 53.8s 
   Dec(J2000) = +24d 42' 46.7" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.
 
The mask-weighted light curve shows a weak peak starting at ~T_0 and returning
to baseline at ~T+20 sec.  The main emission starts at ~T+25 sec with 2, or
possibly 3, overlapping peaks, with the peak emission at ~T+33 sec,
which then approximately exponentially decays out to 510 sec or possibly
out to ~750 sec.  At the 3- or 4-sigma level, there is a possible precursor
peak at ~T-70 sec with a duration of 10-20 sec.  T90 (15-350 keV) is
38.7 +- 3.5 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.77 to T+53.94 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.59 +- 0.05.  The fluence in the 15-150 keV band is 4.3 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+32.75 sec in the 15-150 keV band
is 10.3 +- 0.4 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/510922/BA/


GRB_name: GRB120102A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12800
SUBJECT: Konus-Wind observation of GRB 120102A
DATE:    12/01/03 13:53:11 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@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 120102A (Swift-BAT trigger=510922: Marshall et al., GCN 
12794; Markwardt et al., GCN 12799) triggered Konus-Wind at T0=8181.530 
s UT (02:16:21.530).

The burst light curve shows a single pulse with a duration of ~15 s. 
There is a weak precursor marginally seen at ~T0-30 s.

As observed by Konus-Wind the burst had a fluence of 
1.75(-0.26,+0.30)x10^-5 erg/cm2,
and a 256-ms peak flux measured from T0+3.536 s
of 5.56(-1.02, +1.12)x10^-6 erg/cm2/s
(both in the 20 keV - 4 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+16.640 s) is well fitted (in the 20 keV - 4 MeV
range) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep), with
alpha = -1.47(-0.07, +0.09),  and
Ep = 805(-180, +288) keV (chi2 = 68.4/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.04.

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

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120102_T08181/


GRB_name: GRB120102A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12801
SUBJECT: GRB 120102A: Fermi GBM observation
DATE:    12/01/03 16:58:55 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

S. Xiong (UAH)
reports on behalf of the Fermi GBM Team:

"At 02:16:23.24 UT on 02 Jan 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120102A (trigger 347163385 / 120102095),
which was also detected by the Swift BAT/XRT/UVOT
(F. E. Marshall et al. 2012, GCN 12794)
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 84 degrees.

The GBM light curve consists of two main pulses
with a duration (T90) of about 17 s (50-300 keV).
The time-averaged spectrum from T0-1 s to T0+13 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.19 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 380 +/- 33 keV.
A Band function fits the spectrum equally well with
Epeak = 291 +/- 33 keV, alpha = -1.13 +/- 0.04, and beta = -2.14 +/- 0.13.

The event fluence (10-1000 keV) in this time interval is
(1.26 +/- 0.03)E-5 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+4.8 s in the 10-1000 keV band
is 22.8 +/- 1.6 ph/s/cm^2.

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


GRB_name: GRB111211A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12802
SUBJECT: GRB 111211A: Detection of the SN with the 10.4m GTC
DATE:    12/01/03 23:30:26 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene and J. Gorosabel (IAA-CSIC) report on behalf of a larger collaboration:

Using the 10.4m GTC telescope + OSIRIS, at the Roque de los Muchachos Observatory (La Palma, Spain), we obtained late imaging and spectroscopy of the SuperAGILE GRB 111211A (Lazzarotto et al. GCN 12666, Kann et al. GCN 12668), located at a redshift of 0.478 (Vergani et al. GCN 12677) at 2 epochs.

On 27 December 2011 (15.3 days after the burst) we obtained imaging in r-band of 6x180s with a seeing of ~0.9". This image clearly shows the afterglow of GRB 111211A at a magnitude of r ~ 22.6 (compared to SDSS stars) superposed to its resolved host galaxy but slightly offset towards the North East.

Spectroscopy of the afterglow was obtained on 1 January 2012 (20.3 days after the burst) under good seeing conditions (~1"). At that time, the afterglow was detected at r ~ 22.7 in the acquisition frame, implying an almost flat evolution since the previous epoch which indicates a possible supernova component contributing to the light curve. We obtained 3x1800s spectroscopy at a resolution of ~ 500 and wavelength coverage from ~ 5 000 to 10 000 Angstrom. The spectrum shows both emission from the GRB and the host galaxy. The host shows emission lines of [OII], H-beta, [OIII] and H-alpha at a redshift of 0.478, consistent with the redshift of the GRB (Vergani et al. GCN 12677). The spectrum at the position of the afterglow shows undulations typical of a SN spectrum similar to the spectrum of the type Ic SN 2006aj / GRB 060218 close to maximum.

We acknowledge excellent support from the GTC staff, in particular D. Reverte, A. Cabrera Lavers and R. Rutten.


GRB_name: GRB111225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12803
SUBJECT: GRB111225A: RAPTOR Early Detection of the Optical Counterpart
DATE:    12/01/04 01:15:03 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W. T. Vestrand, P. Wozniak, and H. Davis
of Los Alamos National Laboratory report:

The RAPTOR network of robotic optical telescopes responded to Swift trigger
510341 (GRB 111225A, Siegel et al., GCN 12720).  Unfiltered observations of
the source location began at 03:51:27.2 UTC, 49.4 seconds after the BAT
trigger time.  The initial short exposures during the first two mintues of our
response sequence do not clearly show the counterpart.  However, stacking
those images, 8 5-second exposures taken between 03:51:37.6 UTC and
03:52.46.0 UTC, gives a 5-sigma detection at counterpart location
(Klotz et al., GCN 12722, and Updike et al., GCN 12723).  Based on
comparison to the USNO-B1 R-band, the measured brightness is R~18.7 +\- 0.3
at a t-mid of 03:52:12 UTC, 94 seconds after the Swift BAT trigger.


GRB_name: GRB111209A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12804
SUBJECT: GRB111209A: ATCA detection at 5.5, 9, and 18GHz
DATE:    12/01/04 05:37:27 GMT
FROM:    Paul Hancock at U of Sydney  <hancock@physics.usyd.edu.au>

Paul J. Hancock, Tara Murphy, Bryan Gaensler (U of Sydney), Ashley
Zauderer (Harvard)

Following our 34GHz non-detection (GCN12664) we observed GRB 111209A
(GCN12632) with the Australia Telescope Compact Array (ATCA) at 5.5,
9, and 18GHz on the 14th of December (T=+5.1days). The mean observing
time was 11:12UT at 5.5 and 9GHz, and 11:47UT at 18GHz. We easily detect
the GRB at each frequency as listed below:
Freq        Flux
5.5GHz    0.85+/-0.04mJy
9GHz       0.97+/-0.06mJy
18GHz     3.23+/-0.05mJy

We thank the staff of the ATCA for their help in organising these observations.


GRB_name: GRB111222A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12805
SUBJECT: GRB 111222A: Second Swift observation 
DATE:    12/01/04 17:34:01 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

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

Swift re-observed the field of the IPN burst GRB 111222A (Hurley et 
al., GCN circ. 12714) on 2011-12-31 for 5 ks. We do not detect the 
X-ray source reported by Grupe (GCN circ. 12716) in a 2.5 ks 
observation 27 hours after the burst anymore. The 3-sigma upper 
limit at the position of the afterglow is 2.2e-3 counts/s in the 
Swift XRT. We conclude that the X-ray source has faded and is the 
afterglow of GRB 111222A.

Swift/UVOT observed the burst for 4.9 ks, with all data taken 
in the white filter. We confirm the previously reported optical 
source noted in Siegel and Grupe (GCN Circ. 12717) that was also 
present in the DSS images.  We find that the source has faded 
significantly since the initial observation from a white magnitude 
of 19.34+-0.03 to 19.89+-0.03.  This implies that the previous 
observation recorded light from both the host galaxy and the 
optical afterglow of the burst.  Further observations of the 
host galaxy are strongly encouraged.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020194.

This circular is an official product of the Swift team.


GRB_name: GRB111222A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12806
SUBJECT: GRB 111222A: Fermi GBM observations
DATE:    12/01/05 07:54:09 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) and Charles Meegan (USRA) report on behalf of the Fermi 
GBM Team:

"At 14:51:55.02 UT on 22 December 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111222A (trigger 346258317 / 111222619). The 
burst
was was also detected by the 3rd Interplanetary Network (Hurley et al. 
2011, GCN 12714)
and The GBM on-ground location is consistent with the IPN position.

The angle from the Fermi LAT boresight is 136 degrees. Moreover, this 
burst was bright
enough to result in a Fermi spacecraft autonomous rapid repoint (ARR) 
maneuver.

The GBM light curve shows a single pulse with a duration (T90) of about 
0.32 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.320 s is best fit by 
a power law
function with an exponential high-energy cutoff. The power law index is 
-0.38 +/- 0.06
and the cutoff energy, parameterized as Epeak, is 725 +/- 45 keV.

The event fluence (10-1000 keV) in this time interval is (1.502 +/- 
0.034)E-05 erg/cm^2.
The 64-msec peak photon flux measured starting from T0+0.0 s in the 
10-1000 keV band
is 60.2 +/- 3.4 ph/s/cm^2.

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


GRB_name: GRB111222A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12807
SUBJECT: GRB 111222A, the review of the sky area in plate archives
DATE:    12/01/05 11:24:18 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V. Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 111222A (M. H. Siegel and D. Grupe, GCN Circ.12717) 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 and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19850424/193653 GUA040C000630 16.0 15.35 1575-03212355
19860301/224314 GUA040C000837A 18.0 16.35 1575-03212664
19860409/202551 GUA040C000846 16.0 15.75 1575-03212662
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C M=103"/mm) of the Ukrainian NAS Main Astro obs.
        (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 20 minutes area around 
        the location given in GCN Circ.12717: 
        RA (J2000): 11h 56m 52.82s,Dec(J2000): +69d 04' 15.4"
Star USNOA2 - Comparison star.
  The preview images of 3 areas together with  
the 20x20 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/111222A/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: GRB111225A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12808
SUBJECT: GRB 111225A, the review of the sky area in plate archives
DATE:    12/01/05 13:04:16 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya, L.M.Kizyun, L.K.Pakuliak (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 111225A (M. H. Siegel, GCN Circ.12735) 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 
and Epson Expression 10000XL flatbed scanners and have been 
placed into Golosiiv Plate Archive database DBGPA with open 
access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19831109/192323 GUA040C000250A 13.5 15.70 1350-00882390
19831109/194519 GUA040C000251A 13.0 15.20 1350-00878189
19840828/001418 GUA040C000469A 16.0 15.70 1350-00882390
19841019/211508 GUA040C000511A 15.9 15.70 1350-00882390
19841020/205803 GUA040C000525A 16.0 14.85 1350-00882046
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C M=103"/mm) of the Ukrainian NAS Main Astro obs.
        (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 20 minutes area around 
       the location given in GCN Circ.12735: 
       RA (J2000) = 00:52:37.22, Dec (J2000) = +51:34:19.5
Star USNOA2 - Comparison star.
  The preview images of 5 areas together with  
the 20x20 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/111225A/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: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12809
SUBJECT: GRB111228A :LOAO R-band Observations
DATE:    12/01/06 02:50:13 GMT
FROM:    Yiseul Jeon at SNU/CEOU  <ysjeon@astro.snu.ac.kr>

Minsung Jang, Myungshin Im, Yiseul Jeon (CEOU/Seoul National Univ.), and
Yuji Urata (NCU) on behalf of a larger collaboration

We continued our observation (Jeon et al. GCN 12791) of GRB 111228A
(Ukwatta et al., GCN 12737) in R-band with a 1 m telescope at Mt. Lemmon,
Arizona, US. Data were taken at 2011-12-31 UT and 2012-01-01 UT. For both
of them, we detected the afterglow in stacked R-band images.

We used a USNO B1 star near the afterglow, USNO-B1 1083-0199833 with
R=17.28 following Klotz et al. (GCN 12746) for our photometry calibration,
and current, rough estimates are given below.

Mid-time [UT]           | Mid-time[Since BAT] | Exptime [sec] | R-magnitude
|
-------------------------------------------------------------------------------------------------------------

2011-12-31 08:40:25 |        64.92 hours       |    300sec X 7  | 21.5 +/-
0.28 |
2012-01-01 11:19:52 |        91.58 hours       |    300sec X 9  | 22.3 +/-
0.36 |


We thank the LOAO operator, J. Yoon for his help with these observations.


GRB_name: GRB120106A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12810
SUBJECT: GRB 120106A: Swift detection of a burst
DATE:    12/01/06 14:26:13 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. Immler (CRESST/GSFC/UMD), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
O. M. Littlejohns (U Leicester), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester),
T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report on behalf of the
Swift Team:

At 14:16:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120106A (trigger=511235).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 66.129, +64.028, which is 
   RA(J2000)  =  04h 24m 31s
   Dec(J2000) = +64d 01' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve show several overlapping peaks
starting ~T-8 sec with a total duration of about 20 sec.  The peak count rate
was ~2400 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 14:17:39.0 UT, 74.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 66.11105, 64.03810 which
is equivalent to:
   RA(J2000)  = 04h 24m 26.65s
   Dec(J2000) = +64d 02' 17.2"
with an uncertainty of 3.9 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.  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 (2.65 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4.8
(+4.97/-3.87) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.88e-09 erg cm^-2 s^-1 (0.2-10
keV). 

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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
Data from the list of sources generated on-board are not available at this
time. No correction has been made for the expected extinction corresponding to
E(B-V) of 1.19. 

Burst Advocate for this burst is S. Immler (stefan.immler 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: GRB120106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12811
SUBJECT: GRB 120106A: MASTER-Tunka optical observations
DATE:    12/01/06 15:36:39 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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



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


E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
  Blagoveschensk Educational State University, Blagoveschensk



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


MASTER II  robotic double telescope (MASTER-Net: http://observ.pereplet.ru) 
located at Tunka (Baykal) was pointed
to the  120106A (Immler et al., GCN Circ 12810) 19 s after notice time and 
46 sec after GRB time at 14:16:24.24 UT.

On our first (10s exposure) west telescope image (| polasizations) we 
haven't found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 15.8 mag.

On our first (10s exposure) east telescope image (- polasizations) we
haven't found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 15.9 mag.




The message may be cited.


GRB_name: GRB120106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12812
SUBJECT: GRB 120106A: TAROT Calern observatory optical observations
DATE:    12/01/06 18:08:30 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (OCA-CNRS), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120106A detected by SWIFT
(trigger 511235) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 169 min. after the GRB trigger,
just at the beginning of the night over Calern.
The elevation of the field increased from
52 degrees above horizon and weather conditions
were excellents.

We co-added a series of exposures. We did not found
any optical counterpart in the error box of the XRT
candidate (Immler et al. GCNC 12810):

Start    End       Rlim
169 min  212 min   19.3

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

This message may be cited.


GRB_name: GRB120106A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12813
SUBJECT: GRB 120106A: Enhanced Swift-XRT position
DATE:    12/01/06 21:47:32 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 3180 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 120106A, 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 = 66.10754, +64.03837 which is equivalent
to:

RA (J2000): 04h 24m 25.81s
Dec (J2000): +64d 02' 18.1"

with an uncertainty of 1.4 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: GRB120106A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12814
SUBJECT: GRB 120106A: MITSuME Okayama Optical upper limits
DATE:    12/01/06 23:03:34 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 120106A (Immler et al., GCNC 12810)
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 2012-01-06 14:17:12 UT (~48 sec after
the burst). We did not find any new point source within the enhanced
XRT circle (Evans et al., GCNC 12813) 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
------------------------------------------------------
0.00400    14:22:10     540.0   >19.3  >19.4  >18.7
0.04247    15:17:33    6420.0   >20.6  >20.2  >19.6
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120106A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12815
SUBJECT: GRB 120106A: Swift-BAT refined analysis
DATE:    12/01/06 23:27:37 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
S. Immler (CRESST/GSFC/UMD), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), 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-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120106A (trigger #511235)
(Immler, et al., GCN Circ. 12810).  The BAT ground-calculated position is
RA, Dec = 66.129, 64.050 deg, which is 
   RA(J2000)  =  04h 24m 30.9s 
   Dec(J2000) = +64d 03' 00.0" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
 
The mask-weighted light curve shows the first peak starting at ~T-7 sec,
peaking at ~T+1 sec, and ending at ~T+13 sec. There is a second, weaker peak
starting at ~T+50 sec and ending at ~T+65 (possibly T+85) sec. 
T90 (15-350 keV) is 61.6 +- 4.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.24 to T+60.24 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.53 +- 0.17.  The fluence in the 15-150 keV band is 9.7 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.46 sec in the 15-150 keV band
is 1.5 +- 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/511235/BA/


GRB_name: GRB120106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12817
SUBJECT: GRB 120106A: Swift-XRT refined Analysis
DATE:    12/01/07 02:26:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), V. Mangano (INAF-IASFPA),
J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), J.P. Osborne
(U. Leicester), K.L. Page (U. Leicester), C. Pagani (U. Leicester) and
S. Immler report on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 120106A (Immler  et al. GCN
Circ. 12810), from 64 s to 29.5 ks after the  BAT trigger. The data
comprise 273 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 12813).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.3 (+/-0.3), followed by a break at T+152 s to an alpha
of 0.91 (+0.05, -0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.15 (+0.12, -0.15). The
best-fitting absorption column is  7.6 (+6.8, -0.7) x 10^21 cm^-2,
consistent with the Galactic value of 7.0 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 4.8 x 10^-11 (1.0 x
10^-10) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.6 (+6.8, -0.7) x 10^21 cm^-2
Galactic foreground: 7.0 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.15 (+0.12, -0.15)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00511235.

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


GRB_name: GRB120106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12818
SUBJECT: GRB 120106A: MASTER Early OT marginally detection
DATE:    12/01/07 10:00:52 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk

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


MASTER II  robotic double telescope (MASTER-Net: 
http://observ.pereplet.ru) located at Tunka (Baykal) was pointed to the 
120106A (Immler et al., GCN  Circ 12810) 19 s after notice time and 46 sec 
after GRB trigger time at  14:16:24.24 UT (Ivanov et al., GCN CIRC 12811).

On our first (10s exposure) set  we haven't
found optical transient  within preliminary SWIFT XRT error-box (Immler
et al., GCN Circ 12810).

But we found marginally OT at East telescope (- polarizations) outside
preliminary X-ray  error box (Immler et al., GCN Circ 12810). The position
of this OT is coincided with enhanced Swift-XRT position (Evans et al.,
GCN CIRC 12813).

      UT               T-T_GRB  Exp      mag      Tel    Filter

2012-01-06 14:17:10     46      10   17.0+-0.3   East    P-
2012-01-06 14:17:10     46      10     >16.8     West    P|
2012-01-06 14:22:23    359      70     >18.0     East    P-
2012-01-06 14:22:23    359      70     >18.0     West    P|
2012-01-06 14:26:45    720     120     >18.2     East    P-
2012-01-06 14:26:45    720     120     >18.2     West    P|
2012-01-06 14:31:49   1024     180     >18.3     East    P-
2012-01-06 14:31:49   1024     180     >18.4     West    P|


The images will be available at 
http://observ.pereplet.ru/images/GRB120106A/grb.html  .
The message may be cited.


GRB_name: GRB120106A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12819
SUBJECT: GRB 120106A: MITSuME Okayama Ks-band upper limit
DATE:    12/01/07 12:15:37 GMT
FROM:    Kenshi Yanagisawa at OAO/NAOJ  <yanagi@oao.nao.ac.jp>

Kenshi Yanagisawa, Daisuke Kuroda, Yasuhiro Shimizu, Kiichi Okita
(OAO/NAOJ), Michitoshi Yoshida (Hiroshima-U), Kouji Ohta(Kyoto-U),
and Nobuyuki Kawai(Tokyo Tech.) report on behalf of the MITSuME
collaboration:

We observed the field of GRB120106A (Immler et al., GCNC 12810) in
Ks-band with a wide-field NIR camera at Okayama  Astrophysical
Observatory (Japan). The camera has an effective aperture of 0.91m.

Observations started from 15:19 UT on 5th January, 1.05 hours after
the BAT trigger, to 16:20 UT.  The total exposure of 49 min was
successfully obtained.

In our co-add image, we did not find any new point source within the
enhanced XRT error circle (Evans et al., GCNC 12813) down to limiting
magnitude of  Ks= 15.6(Vega, S/N=3). The photometric calibration was
made against 2MASS field stars.

T0+[min]    MID-UT     T-EXP[min]      Ks
---------------------------------------------------
  +93.6     15:50         49.0       >15.6 (S/N=3)
---------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12820
SUBJECT: GRB 120106A: Bassano Bresciano Observatory optical observations
DATE:    12/01/07 16:22:20 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:We imaged the field of GRB 120106A detected by SWIFT(trigger 511235) with the robotic telescopeof (565)Bassano Bresciano Observatory, Italy.The observations started 223 min. after the GRB trigger,with our schmidt telescope (320/400/1000).Weather conditions were excellents.We co-added a series of 15 exposures. We did not foundany optical counterpart in the error box of the XRTcandidate.Start    End       Vlim223 min  252 min   19.5Magnitudes were estimated with the UCAC-3 catalog.


GRB_name: GRB120106A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12821
SUBJECT: GRB 120106A: Swift/UVOT Upper Limits 
DATE:    12/01/09 14:10:13 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (CRESST/GSFC/UMD) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120106A
65 s after the BAT trigger (Immler et al., GCN Circ. 12810).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 12813) is detected in the initial
UVOT exposures. Preliminary 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
for coadded exposures are:

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

white              687         6326          451   >20.3
v                   65         11570         619   >20.0
b                  551         6736          452   >20.8
u                  296         6531          924   >20.8
w1                 678         6326          452   >20.3
m2                 652         6121          454   >20.2
w2                 603         11220         1239   >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.195 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120107A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12822
SUBJECT: GBM trigger 347620337 (GRB 120107A?) : High-energy photon emission in Fermi/LAT data
DATE:    12/01/09 22:43:53 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

Weikang Zheng and Carl Akerlof, report on behalf of the ROTSE
collaboration:

High-energy photon emission in Fermi/LAT data was found to be correlated
with GBM trigger 347620337 (probably GRB 120107A). Our LAT data
processing pipeline which uses the matched filter technique (Akerlof et
al, 2010, ApJ, 725, L15; 2011 ApJ, 726, 22; Zheng et al. 2012, ApJ
745,72), detected the high-energy photon emission from 09:12:15 UT on
Jan. 7, 2012 (MET = 347620337) as a follow-up of a routine search in GBM
trigger catalogs. The GBM trigger location (Ra = 223.1, Dec = -77.96)
was about 56 degree from the LAT boresight, and the zenith angle was
about 106 degrees. ~7 photons above 100 MeV were detected within 50 s
after the burst, with the highest energy of ~1.78 GeV at 1.18s after the
burst (note that class 1 photons are not included in the pipeline
analysis since it is not automatically available from LAT data server at
the moment). The new GRB location estimated by the matched filter
technique is Ra = 246.40, Dec = -69.93 with uncertainty ~0.5 degree,
this is ~10 degrees away from the GBM trigger location.

A likelihood analysis gives a TS value of 58.9 (duration of 50 s), and
the GRB location Ra = 246.31, Dec = -69.93, which is also consistent
with the location derived from the matched filter technique.

All the pipeline results can be found in the following link, including
the skymap and light curve figures:
http://www.rotse.net/LAT/GBMTriggers/347620337/347620337_res.html


GRB_name: GRB120107A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12823
SUBJECT: IPN Triangulation of GRB 120107A
DATE:    12/01/10 16:47:43 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,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team,

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

The long GRB 120107A, seen by Fermi/GBM (trigger 347620337) and 
localized by Fermi/LAT (Zheng and Akerlof, GCN 12822), was also detected 
by Konus-Wind, Suzaku (WAM), and MESSENGER (GRNS) at about 33135 s UT 
(09:12:15).

Triangulation gives a MESSENGER-GBM annulus centered at RA(2000)=268.419 
deg (17h 53m 40s) Dec(2000)=-23.372 deg (-23d 22' 18"), whose radius is 
48.611  0.094 deg (3 sigma); and a Konus-GBM annulus centered at 
RA(2000)=262.874 deg (17h 31m 30s)  Dec(2000)=-24.735 deg (-24d 44' 
05"), whose radius is 47.383  1.667 deg (3 sigma).  These annuli 
intersect at grazing incidence to form a very long box (an annulus 
segment). The Fermi/LAT position (Zheng and Akerlof, GCN 12822) is 
entirely contained within the Konus-GBM annulus, and intersected by the 
MESSENGER-GBM annulus resulting in the IPN/LAT error box area of ~600 
sq. arcmin.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB120107_T33132/IPN/
showing the LAT best-fit position (red star), and the IPN annuli (solid
lines with centers dot-dashed).

Follow-up observations of the LAT error box by the Swift satellite are 
in progress.


GRB_name: GRB120107A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12824
SUBJECT: Konus-Wind observation of GRB 120107A
DATE:    12/01/10 16:51:34 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 120107A (GBM trigger 347620337;
Fermi/LAT detection: Zheng and Akerlof, GCN 12822;
IPN triangulation: Hurley et al., GCN 12823)
triggered Konus-Wind at T0=33132.445s UT (09:12:12.445)

The light curve shows multiple partly overlapped pulses.
A total duration of the burst is ~25 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/GRB120107_T33132/

As observed by Konus-Wind the burst
had a fluence of 5.5(-1.0,+1.5)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.128 s,
of 1.2(-0.2,+0.3)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model, for which
alpha = -1.38 (-0.26, +0.33),
and Ep = 196(-54, +160) keV,
chi2 = 82.5/58 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.98 (-0.34, +0.41),
and Ep = 178(-37, +72) keV,
chi2 = 60.0/58 dof.

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


GRB_name: GRB120106A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12825
SUBJECT: GRB 120106A: MITSuME Okayama Optical Observation (update)
DATE:    12/01/10 17:05:24 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

We carried out a detailed analysis of GRB 120106A and found the optical
afterglow in only Ic-band. This results indicated the possibility of
a Rc-band dropout.
Although we reported the three sigma upper limits in the previous circular
(Kuroda et al., GCNC 12814), we updated our results as follows.

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

T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic  Ic_err
-----------------------------------------------------------
0.00400    14:22:10     540.0    >19.3  >19.4  19.1  0.3
-----------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120107A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12826
SUBJECT: GRB 120107A: Fermi GBM observation
DATE:    12/01/10 18:00:19 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

S. McBreen (UCD/MPE)
reports on behalf of the Fermi GBM Team:

"At 09:12:15.41 UT on 07 January 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120107A (trigger 347620337/120107384)
which was also detected by the Fermi/LAT
(Zheng and  Akerlof 2012, GCN 12822).

The GBM light curve consists of about six pulses
with a duration (T90) of about 23 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+23 s is
well fit by a Band function with
Epeak = 188.90 (+24.90/-22.20) keV,
alpha = -0.91 (+0.08/-0.07), and beta = -2.11 (+0.12/-0.19).

The event fluence (10-1000 keV) in this time interval is
(6.81 +/- 0.06)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.003 s in the 10-1000 keV band
is 5.55 +/- 0.24 ph/s/cm^2.

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


GRB_name: GRB110915B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12827
SUBJECT: GRB 110915B, the review of the sky area in plate archives
DATE:    12/01/11 17:56:57 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 110915B (P. D'Avanzo et al. GCN Circ.12348) 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 and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19820210/174605 GUA040C000008A 27.0 15.70 0900-01403360
19820210/174605 GUA040D000009 27.0 15.70 0900-01403360
19911011/014851 GUA040C001873 25.1 15.05 0900-01404372
19911012/015416 GUA040C001880A 18.2 15.05 0900-01408313
19920108/200727 GUA040C001916 23.0 16.45 0900-01406794
19920201/181314 GUA040C001929A 23.0 15.05 0900-01408313
Plates: - the plates archive identifier of DWA (D/F=400/2000, 
GUA040C, M=103"/mm) of the Ukrainian NAS Main Astro obs.
GUA040D  (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 17 minutes area around 
       the location given in GCN Circ.12348: 
       RA(J2000) = 05h 10m 13.13s, Dec(J2000) = +01d 55'57.9"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 17x17 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/110915B/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: GRB120107A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12828
SUBJECT: GRB 120107A: Suzaku WAM observation of the prompt emission
DATE:    12/01/12 04:23:47 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

W. Iwakiri, M. Tashiro, Y. Terada, T. Yasuda, K. Takahara, M. Asahina, 
S. Kobayashi, A. Sakamoto (Saitama U.) Y. Hanabata, T. Uehara, T. Kawano, 
K. Takaki, M. Mizuno, M. Ohno, Y. Fukazawa (Hiroshima U.), 
S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), M. Kokubun, 
T. Takahashi (ISAS/JAXA), Y. E. Nakagawa (Waseda U.), N. Ohmori, M. Akiyama, 
M. Yamauchi (Univ. of Miyazaki), C-J. Chuang, Y. Urata, P. Tsai (NCU), 
K. Nakazawa, K. Makishima (Univ. of Tokyo), 
on behalf of the Suzaku WAM team, report:

The long GRB 120107A (Fermi-GBM trigger 347620337; Fermi-LAT detection: 
Zheng & Akerlof, GCN 12822; IPN triangulation: Hurley et al., GCN 12823) 
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy 
range of 50 keV - 5 MeV at 09:12:15.352 UT (=T0). 

The observed light curve shows a multi-peaked structure starting at T0-2 s 
and ending at T0+24 s with a duration (T90) of about 22 seconds. The fluence 
in 100 - 1000 keV was 3.98 (-0.31, +0.28) x 10^-6 erg/cm^2. The 1-s peak flux 
measured from T0 s was 1.94 (-0.37, +0.22) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-2 s to T0+24 s 
is well fitted by a single power-law with a photon index of 2.43 (-0.23, +0.28) 
(chi^2/d.o.f = 20.5/25).

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 now available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB120106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12830
SUBJECT: GRB 120106A: optical upper limit
DATE:    12/01/12 14:38:43 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU), E. Litvinenko (UBAI), A. Pozanenko (IKI) on behalf of 
larger GRB follow up collaboration report:

We observed the field of the Swift GRB 120106A (Beardmore  et al., GCN 
12810) with ORI-40 telescope of Kitab ISON observatory on Jan. 6 starting on 
(UT) 18:49:24. We obtained several unfiltered images between (UT) 18:49:24 - 
19:20:20.  On the stacked image we do not detect any source within the 
enhanced XRT error box (Evans et al., GCN  12813). The photometry is based 
on nearby  reference stars of USNO-B1.0 (R2 magnitudes):

 Tstart UT, T0+,       Filter, Exposure, OT, UL (3 sigma)
                 (mid, d)             (s)

 18:49:24  0.2003    none  30*60       n/d  18.5


GRB_name: GRB111228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12832
SUBJECT: GRB 111228A: optical observations
DATE:    12/01/14 12:00:43 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (SAI MSU), L. Elenin (KIAM), A. Pozanenko (IKI) report on
behalf of larger GRB follow-up collaboration:

We observed the field of GRB 111228A (Ukwatta et al., GCN 12737) with
0.45-m telescope of ISON-NM observatory on Dec. 29 at 11:55 (UT,
middle of exposure) in R band with mean FWHM of about 4.9". We took
several unfiltered frames with exposure of 60 s. In a stacked image we
detect an optical counterpart (Ukwatta et al., GCN 12737; Xin et al.,
GCN 12738). The photometry is based on the USNO-B1.0 star 1415-0025726
(RA = 10:00:22.70 Dec = +18:19:23.4, J2000) assuming R2 = 17.28:

T0+,    Filter, Exposure,  OT
(mid, d)       (s)

0.84102  R     1800   19.27+/-0.12


GRB_name: GRB120114A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12833
SUBJECT: GRB 120114A found in ground analysis of BAT data
DATE:    12/01/15 14:56:28 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

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

Automated BAT ground analysis found a burst that occurred at 16:20:09 UT 
with a significance of 9.1 sigma (15-200 keV) from the failed event data 
of trigger #511739.  The event is temporally coincident with the Fermi GBM 
348250807.  The best BAT location is RA, Dec = 317.9043, +57.0358 deg, which is

  RA(J2000)  =  21h 11m 37.03s 
  Dec(J2000) = +57d 02' 08.9" 

with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.

The mask-weighted light curve created from the failed event data 
(available from 16:20:06 to 16:20:16 UT) shows a constant positive 
rate from the beginning.  And then, the rate increases by three times 
around 16:20:13 UT.  From the BAT raw light curve, the duration of 
the event is ~35 sec long.  

The spectrum extracted using the full event data is best fit by a simple 
power-law model.  The power law index of the spectrum is 1.4 +- 0.3 
(90% confidence). 

Since the GRB is too close to the Sun, no Swift ToO has been requested.


GRB_name: GRB120116A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12834
SUBJECT: GRB 120116A: Swift detection of a burst
DATE:    12/01/16 18:17:28 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), S. Campana (INAF-OAB),
P. D'Avanzo (INAF-OAB), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
A. Y. Lien (NASA/GSFC/ORAU), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester),
C. A. Swenson (PSU), T. N. Ukwatta (MSU), C. A. Wolf (PSU) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 18:06:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120116A (trigger=511866).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 16.248, +33.929, which is 
   RA(J2000)  =  01h 05m 00s
   Dec(J2000) = +33d 55' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows at least two
precursor peaks followed by a complex FRED peak with a total duration
of at least 50 sec.  The peak count rate was ~4000 counts/sec 
(15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 18:07:42.5 UT, 74.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 16.24183, 33.93034 which
is equivalent to:
   RA(J2000)  = 01h 04m 58.04s
   Dec(J2000) = +33d 55' 49.2"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 19 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 4.64
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 6.52e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 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
0.05. 

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.)


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12835
SUBJECT: GRB 120116A: MASTER Early optical limit
DATE:    12/01/16 18:33:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk

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



MASTER II  robotic double telescope (MASTER-Net: 
http://observ.pereplet.ru)  located in Tunka was pointed to the 
GRB120116A 10 sec s after notice time and 31 sec after GRB time
at 2012-01-16 18:06:59.889 UT.

On our first (10s exposure) set we haven't found optical transient
within SWIFT XRT error-box (Melandri et al, GCN Circ 12834) in both 
polarizations.

The 3-sigma unfiltered upper limit has been about 15.0 mag
This circular was generated automatically.

The message may be cited.


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12836
SUBJECT: GRB 120116A: Bassano Bresciano Observatory optical observations
DATE:    12/01/16 21:37:31 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

 U.Quadri, L.Strabla and R.Girelli report:
 We imaged the field of GRB 120116A detected
 by SWIFT(trigger 511866) with the robotic
 telescope of (IAU station 565) Bassano Bresciano
 Observatory, Italy.

 The observations started 3min 41sec. after the 
 GRB trigger,with our Schmidt telescope 
 D=320 mm F/D=3.1.

 Weather conditions were discrete.

 We co-added a series of 15 exposures of 120sec. 
 
 We did not found any optical counterpart  
 in the error box of the XRTcandidate 
 (Melandri et al, GCN Circ 12834). 
 
 Start      End       Vlim 
 03min      30min     17.0 
 
 Magnitudes were estimated with the UCAC-3 
 catalog and are not corrected for galactic 
 dust extinction.
 
 The message may be cited.


GRB_name: GRB120116A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12837
SUBJECT: GRB 120116A: IAC80 I-band observations
DATE:    12/01/16 22:49:38 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

R. Sanchez-Ramirez (IAA-CSIC), D. Jimenez Mejias (IAC), J.C. Tello (IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK), J. Gorosabel (IAA-CSIC), report on behalf of a larger collaboration: 

"We observed the field of GRB 120116A (Melandri et al., GCNC 12834) with the 82cm IAC80 telescope at the Observatorio del Teide, Tenerife, Spain. The observations were carried in the I-band on Jan 16.83154 -- 16.91640 UT (1.85-3.89 hours post burst) with a total exposure time of 22x300s. A preliminary analysis of the combined image shows no object brighter than I~21.8 inside the XRT error circle."


GRB_name: GRB120116A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12838
SUBJECT: GRB 120116A: NOT observations
DATE:    12/01/16 23:13:41 GMT
FROM:    Paul Vreeswijk at U of Iceland  <pmv@raunvis.hi.is>

Paul Vreeswijk (U. Iceland), Don Pollacco, David Armstrong, Paul
McDaid (Queens U. of Belfast), Dong Xu (WIS), A. De Cia and Pll 
Jakobsson (U. Iceland), report on behalf of a larger collaboration:

Using ALFOSC on the Nordic Optical Telescope (NOT) we have obtained
Sloan r'- (3 x 600 s) and z'-band (6 x 300 s) imaging of the field of
the Swift GRB 120116A (Melandri et al., GCN 12834), starting on 2012
January 16 at 19:59 UT, just under 2 hours after the burst. The
observations were performed in clear conditions, with a seeing of
about 1".

We do not detect any object within the XRT error circle, down to
approximate limiting magnitudes of r'>24.1 and z'>22.4 (calibrated
against the SDSS catalog).


GRB_name: GRB120116A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12839
SUBJECT: GRB 120116A: Swift-BAT refined analysis
DATE:    12/01/16 23:16:16 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), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB),
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-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120116A (trigger #511866)
(Melandri, et al., GCN Circ. 12834).  The BAT ground-calculated position is
RA, Dec = 16.240, 33.927 deg, which is 
   RA(J2000)  =  01h 04m 57.7s 
   Dec(J2000) = +33d 55' 36.3" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.
 
The mask-weighted light curve shows a couple small precursor peaks 
starting at ~T-30 sec.  The main peak has a fast rise starting around T-2 sec,
peaking at ~T+0 sec, and a roughly linear decay ending around T+30 sec.
T90 (15-350 keV) is 41.0 +- 5.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-33.44 to T+26.57 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.31 +- 0.41, 
and Epeak of 19.4 +- 6.3 keV (chi squared 55.4 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.9 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.00 sec in the 15-150 keV band is
4.1 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.70 +- 0.07 (chi squared 101.2 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/511866/BA/


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12840
SUBJECT: GRB 120116A: Optical observations at Crni Vrh
DATE:    12/01/16 23:33:02 GMT
FROM:    Bojan Dintinjana at OCV  <bojan.dintinjana@fmf.uni-lj.si>

S. Maticic, B. Dintinjana and H. Mikuz on behalf of PIKA observing 
program at Crni Vrh Observatory.

We observed the field of GRB 120116A (GCN 12834) from Crni Vrh 
Observatory with a 60 cm robotic telescope, R filter and CCD. Twenty 
consecutive exposures of 60 second duration were taken. First exposure 
started at 2012-01-16 18:07:47 UT, 79 seconds after the burst (60 
seconds after the SWIFT trigger).

No optical candidate was detected within the uncertainty radius on 
single exposures, having R limiting magnitude 20.0 +/-0.2. Also we found 
no optical candidate on 20 sumed R images with total exposure of 1200 
seconds and limiting R band magnitude 22.0 +/-0.2 (all magnitudes 
calibrated against the nearby USNO B1.0 R2 magnitude stars).


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12841
SUBJECT: GRB 120116A: WHT optical observations
DATE:    12/01/17 00:32:20 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan, S. Parsons (U. Warwick), N.R. Tanvir, K. Wiersema (U.
Leicester), T. R. Marsh (Warwick), S. Littlefair (Sheffield) report
on behalf of a larger collaboration:

We observed the field of GRB 120116A (Melandri et al. GCN 12834)
with ULTRACAM on the 4.2m William Herschel Telescope. Observations
began approximately 2 hours after the trigger, and 45, 60 second
exposures were obtained simultaneously in ug and r. In the XRT error
circle we do not locate any sources to preliminary limiting magnitudes
of g>25.4, r>24.8, calibrated against SDSS observations of the
field.


GRB_name: GRB120116A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12842
SUBJECT: GRB 120116A: EVLA observations
DATE:    12/01/17 09:00:04 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer and E. Berger (Harvard) report on behalf of a larger
collaboration:

"We observed the position of GRB 120116A (GCN 12834) beginning 2012 Jan 
17.06 (0.3 d after the burst) with the EVLA at a mean frequency of 5.8 
GHz.  We find no significant radio emission at the Swift-XRT position 
(http://www.swift.ac.uk/sper/) to a 3-sigma limit of 45 uJy."


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12843
SUBJECT: GRB 120116A: Gemini optical/IR candidate
DATE:    12/01/17 16:37:18 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

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

"We observed GRB 120116A (Melandri et al. GCN 12834) with Gemini
North beginning at Jan 17 04:54, approximately 11 hours after the
burst trigger. We obtained optical imaging in iz with GMOS and
near-IR imaging in JHK with GNIRS. Within the XRT localization of
the source we find a faint object at

RA(J2000) 01:04:57.84
DEC(J2000) 33:55:51.1

(error +/- 0.3") with preliminary magnitudes (calibrated against
SDSS and 2MASS) of

i=24.7 +/- 0.2
z=24.7 +/- 0.3
J> 23.0 (3-sigma)
H=22.8 +/- 0.4
K=21.6 +/- 0.3

This object is a plausible counterpart for GRB 120116A. However,
at present we cannot assess if the source is fading, as it is
significantly fainter than earlier optical limits (Quadri et al.
GCN 12836, Sanchez-Ramirez et al. GCN 12837, Vreeswijk et al. GCN
12838, Levan et al. GCN 12841). We further note that the probability
of a chance alignment of an object with this magnitude within a 2"
error XRT position is non-negligible.

We thank the staff of Gemini, in particular Richard McDermid for their
assistance in acquiring these data. "


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12844
SUBJECT: GRB 120116A: Mondy optical observations
DATE:    12/01/17 18:12:05 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (SAI MSU), I. Korobtsev, E. Klunko (ISTP), A.Pozanenko
(IKI) on behalf of larger GRB follow up collaboration report:

We observed the field of the Swift GRB 120116A (Melandri et al., GCN
12834) with AZT-33IK telescope of Sayan observatory (Mondy) on Jan, 16
between (UT) 18:49:24 - 19:20:20, i.e. starting 40 minutes after the
trigger. We took several series of 60 s exposures in R-filter. Within
the XRT error circle (Melandri et al., GCN 12834) we do not detect
any source, in particular we do not detect the source reported by
Levan and Tanvir (GCN 12843). The photometry is based on the USNO-B1.0
1239-0020213 star (RA=01 05 04.50, Dec=+33 55 37.7) assuming R2=16.36.

UT_start, T0+,    Filter, Exposure,  OT    uplim,
       d                            3 sigma
18:49:24  0.03815 R     29x60     n/d     19.5


GRB_name: GRB120116A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12846
SUBJECT: GRB 120116A: Enhanced Swift-XRT position
DATE:    12/01/17 20:13:49 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 1642 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 120116A, 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 = 16.24134, +33.93057 which is equivalent
to:

RA (J2000): 01h 04m 57.92s
Dec (J2000): +33d 55' 50.0"

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: GRB120116A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12847
SUBJECT: GRB 120116A: Swift-XRT refined Analysis
DATE:    12/01/17 22:47:37 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), S. Campana (INAF-OAB) and P. D'Avanzo
(INAF-OAB) report on behalf of the Swift-XRT team:

We have analysed 8.2 ks of XRT data for GRB 120116A (Melandri  et al.
GCN Circ. 12834), from 64 s to 35.1 ks after the  BAT trigger. The data
comprise 92 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 12846).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.9 (+0.9, -0.8). Centered at T+114 s
there is a small flare. The light curve breaks again at T+205 s to a
decay with alpha=0.42 (+0.09, -0.07),  before a final break at T+8394 s
s after which the decay index is 1.24 (+0.69, -0.24).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.93 (+0.33, -0.28). The
best-fitting absorption column is  2.5 (+/-0.6) x 10^21 cm^-2, in
excess of the Galactic value of 4.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.19 (+0.19, -0.18)
and a best-fitting absorption column of 1.9 (+/-0.5) 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 (5.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 4.6 x 10^20 cm^-2
Excess significance: 4.8 sigma
Photon index:      2.19 (+0.19, -0.18)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00511866.

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


GRB_name: GRB120116A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12848
SUBJECT: GRB 120116A: Swift/UVOT Upper Limits
DATE:    12/01/17 22:57:58 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120116A
83 s after the BAT trigger (Melandri et al., GCN Circ. 12834).
No optical afterglow consistent with the enhanced XRT position
Goad et al, GCN_Circ. 12846) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            83          233          147         >21.0
u_FC               296          546          246         >20.1
white               83          919          192         >21.1
v                 4479         4679          197         >19.1
u                  296         5173          324         >20.4
w1                4889         5089          197         >20.2
m2                4684         4884          197         >19.8
w2                4274         4474          197         >20.5

The magnitudes in the table 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: GRB120118B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12852
SUBJECT: GRB 120118B: Swift detection of a burst
DATE:    12/01/18 17:13:53 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

O. M. Littlejohns (U Leicester), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), S. Campana (INAF-OAB),
M. M. Chester (PSU), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU),
V. Mangano (INAF-IASFPA), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), T. Sakamoto (NASA/UMBC),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester),
C. A. Swenson (PSU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report
on behalf of the Swift Team:

At 17:00:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120118B (trigger=512003).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 124.866, -7.182, which is 
   RA(J2000)  =  08h 19m 28s
   Dec(J2000) = -07d 10' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows single peak
with a duration of about 30 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 17:02:13.2 UT, 112.1 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 115 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 25% of
the BAT 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
0.15. 

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: GRB120118B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12853
SUBJECT: GRB 120118B: MASTER optical observations
DATE:    12/01/18 19:39:46 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

O.Gres, O.Chuvalaev,K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev
  Irkutsk State University


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


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

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk

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 Tunka was pointed to the  GRB120118A (Littlejohns et al., 
GCN Circ 12852) 1417  s after notice time 
and 1437 sec after GRB time at 2012-01-18 17:24:53  UT in two 
polarizations. On our first (120s exposure) set we haven't found optical 
transient  within SWIFT error-box .
The delay is due to weather conditions.
  The 5-sigma upper limit has been about 17.0  mag

This circular was generated automatically.

The message may be cited.


GRB_name: GRB120118B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12854
SUBJECT: GRB 120118B: Swift-XRT position
DATE:    12/01/18 20:50:33 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O. M. Littlejohns, K. Page and P. A. Evans (U. Leicester) report on behalf of the Swift-XRT team:

Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec = 124.8713, -7.1848 (degrees) which is equivalent to:

RA (J2000) = 08h 19m 29.12s
DEC (J2000) = -07d 11' 05.2"

with an uncertainty of 2.2 arcsec (radius, 90% containment).

This location is 21.4 arcseconds from the BAT onboard position, inside the BAT
error circle.

This message may be cited.


GRB_name: GRB120118B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12856
SUBJECT: GRB 120118B: Faulkes Telescope South observations
DATE:    12/01/18 23:08:17 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), C. G. Mundell  (Liverpool JMU) and C. Guidorzi  
(U. Ferrara) report on behalf of a large collaboration:

The 2-m Faulkes Telescope South responded automatically to Swift GRB  
120118B (Littlejohns et al. GCN Circ. 12852) with observations  
beginning at 17:03 UT  2012 January 18th (~2.8 min after the BAT  
trigger time).

Within the XRT error circle (Littlejohns et al. GCN Circ. 12854) we do  
not find any source in the R and i' filters down to the following  
(3sigma) limiting magnitudes:

Mid time from  Total Exp   Filter    Magnitude
trigger (min)    (s)
-------------------------------------------------
   34.9            720         R    > 18.9
   39.2            700         i'     > 19.1
-------------------------------------------------

Magnitudes have been calibrated from R2 and I nominal values of nearby  
USNOB1.0 stars.


GRB_name: GRB120118B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12857
SUBJECT: GRB 120118B: Enhanced Swift-XRT position
DATE:    12/01/19 01:33:14 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 1411 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120118B, 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 = 124.87106, -7.18474 which is equivalent
to:

RA (J2000): 08h 19m 29.05s
Dec (J2000): -07d 11' 05.1"

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: GRB120118B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12858
SUBJECT: GRB 120118B: NOT observations
DATE:    12/01/19 01:33:52 GMT
FROM:    Paul Vreeswijk at U of Iceland  <pmv@raunvis.hi.is>

Paul Vreeswijk (U. Iceland), Tapio Pursimo (NOT) and Pll Jakobsson
(U. Iceland), report on behalf of a larger collaboration:

Using ALFOSC on the Nordic Optical Telescope (NOT) we have obtained
Sloan r'- (3 x 600 s) and z'-band (6 x 300 s) imaging of the field of
the Swift GRB 120118B (Littlejohns et al., GCN 12852), starting on
2012 January 18 at 22:48 UT, just under 6 hours after the burst. The
observations were performed in non-optimal seeing conditions (~3.5").

We do not detect any object within the XRT error circle (Littlejohns
et al., GCN 12854), down to approximate limiting magnitudes of r'>21.2
and z'>19.5 (calibrated against the SDSS catalog).


GRB_name: GRB120119A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12859
SUBJECT: GRB 120119A: Swift detection of a burst with an optical counterpart
DATE:    12/01/19 04:22:23 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. P. Beardmore (U Leicester), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), M. H. Siegel (PSU), C. A. Swenson (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 04:04:30.21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120119A (trigger=512035).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 120.027, -9.074, which is 
   RA(J2000)  =  08h 00m 07s
   Dec(J2000) = -09d 04' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows at least three peaks
with a total duration of at least 50 sec.  The peak count rate
was ~16,000 counts/sec (15-350 keV), at ~10 sec after the trigger. 

The XRT began observing the field at 04:05:23.4 UT, 53.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 120.0293, -9.0803 which is equivalent to:
   RA(J2000)  = +08h 00m 7.03s
   Dec(J2000) = -09d 04' 49.1"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 24 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. 

The initial flux in the 2.5 s image was 1.06e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 61 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 08:00:06.94 = 120.02890
  DEC(J2000) = -09:04:53.7  =  -9.08157
with a 90%-confidence error radius of about 0.66 arc sec. This position is 4.8
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.67 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.11. 

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: GRB120119A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12860
SUBJECT: GRB 120119A: PAIRITEL NIR Detection
DATE:    12/01/19 04:42:48 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

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

We observed the field of GRB 120119A (Beardmore et al., GCN 12859) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2012-Jan-19 04h05m23s UT, ~53 seconds after the Swift trigger.  In
 mosaics (effective exposure time of 560 seconds) taken simultaneously in
the J, H, and Ks filters, we detect a source at the position of the optical
afterglow.

The preliminary photometry yields:

post burst
t_mid (m)  exp.(s)  filt  mag    m_err
10.3       560      J     14.35  0.02
10.3       560      H     13.10  0.02
10.3       560      Ks    11.95  0.02

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.

[GCN OPS NOTE(19jan11): Per author's request, the start time in the 3rd line
was changed from "04h07m15s UT, ~2.7 minutes" to "04h05m23s UT, ~53 seconds".]


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12861
SUBJECT: GRB 120119A: Liverpool Telescope afterglow detection
DATE:    12/01/19 04:51:56 GMT
FROM:    Andreja Gomboc at LT,ARI,Liverpool JMU  <ag@astro.livjm.ac.uk>

A. Gomboc (University of Ljubljana, CE Space.si) reports on behalf of a large collaboration:
The 2-m Liverpool Telescope responded automatically to Swift trigger 512035. Following observations with RINGO-2 polarimeter, observations in r' i' and z' filter started at 14.5 min after the BAT trigger time. We clearly detect the afterglow in all three filters consistent with the UVOT position (Beardmore et al. GCN Circ. 12859).


GRB_name: GRB120118B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12862
SUBJECT: GRB 120118B: Swift/UVOT Upper Limits
DATE:    12/01/19 05:11:09 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester (PSU) and O. M. Littlejohns (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120118B
116 s after the BAT trigger (Littlejohns et al., GCN Circ. 12852).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al., GCN Circ. 12857) is detected in the initial UVOT data.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:

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

white_FC           116          265          147         >20.9
u_FC               328          577          246         >19.9
white              116         1528          392         >21.6
v                  657         1574          113         >19.1
b                  583         1504           97         >20.5
u                  328         1479          324         >20.2
w1                 708         1454           78         >19.0
m2                 682         1430           78         >19.9
w2                 633         1554          117         >19.8

The magnitudes in the table are not corrected for the Galactic  
extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120119A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12863
SUBJECT: GRB 120119A: GROND Detection of the Optical/NIR Afterglow
DATE:    12/01/19 05:27:34 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady, V. Sudilovsky, J. Greiner (all MPE Garching) and T.Kruehler  
(DARK/NBI) report on behalf of the GROND team:

We observed the field of GRB 120119A (Swift trigger 512035; Beardmore  
et al., GCN #12859) 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 04:08 UT, 3.5 min after the GRB trigger, and  
are continuing. They were performed at an average seeing of 0.9" and  
at an average airmass of 1.0.

We found a single point source consistent with the UVOT afterglow  
position.

Based on the first 2.4 min of total exposures in g'r'i'z' and 4 min in  
JHK, we estimate preliminary magnitudes (all in AB) of

g' = 18.8 +- 0.1 mag,
r' = 17.7 +- 0.1 mag,
i' = 16.8 +- 0.1 mag,
z' = 16.2 +- 0.1 mag,
J = 15.2 +- 0.1 mag,
H = 14.6 +- 0.1 mag and
K = 14.0 +- 0.1mag

Given magnitudes are calibrated against SDSS zeropoints as well as  
2MASS field stars and are not corrected for the expected Galactic  
foreground extinction corresponding to a reddening of E_(B-V)=0.11 mag  
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12864
SUBJECT: GRB 120119A: PROMPT optical observation of early afterglow
DATE:    12/01/19 05:29:06 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, J. Haislip, K. Ivarsen, D. Reichart, J. Moore, M. Nysewander, 
A. Trotter, R. Egger, A. Foster, A. Oza, T. Cromartie, E. Speckhard, and J. 
A. Crain report:

Skynet observed the field of GRB 120119A with the PROMPT telescopes located 
at CTIO in Chile. Observations in B, R, and I began at 04:05:08 UT, 38 
seconds after the burst. We detect an optical source consistent with the 
UVOT position reported by Beardmore et. al. (GCN 12859) in all three 
filters. The optical afterglow faded for the first ~2.3 minutes, then 
brightened until approximately minute 14, after which it resumed fading. 
The afterglow is red, with (I - R) ~ 1 mag and (R - B) ~ 2 mag. 

A preliminary light curve can be found at:
http://skynet.unc.edu/grb/grb120119a.png

Further observations are ongoing.


GRB_name: GRB120119A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12865
SUBJECT: GRB 120119A: Gemini-S redshift
DATE:    12/01/19 06:01:56 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara, J. X. Prochaska (UCSC/UCO Lick) 
report on behalf of a larger collaboration:

On January 19.20 UT (53 minutes after the BAT trigger) 
we observed the optical counterpart of GRB 120119A 
(Beardmore et al., GCN 12859) using GMOS-South on the 
Gemini-South 8-m telescope.  

Spectroscopic observation covering 4000-8000 Angstrom wavelength 
range reveals several absorption features, including AlIII1854, 
1862, FeII2586,2600, MnII2606, MgII2796,2803 at a common 
redshift of 1.728.
Also at least an intervening system is present at z=1.212
based on strong MgII2796 absorption features.

We therefore suggest this to be the redshift of GRB 120119A.

We thank the Gemini staff for performing this observation.


GRB_name: GRB120119A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12866
SUBJECT: GRB 120119A: Lick 3m Spectroscopy
DATE:    12/01/19 06:23:08 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

Anna Pancoast (UCSB), Rebecca Rosen (Cal Poly), Vardha Bennert 
(Cal Poly), A. Cucchiara (UCO) and J. Xavier Prochaska (UCO) 
on behalf of GRAASP report:

"We observed the afterglow of GRB 120119 with the Kast
dual spectrometer for 1800s total starting at UT 05:30
under fine conditions.  Analysis of the red side exposure
shows strong absorption from ZnII and FeII transitions
at a common redshift of z=1.73 confirming the reported
redshift of Cucciara & Prochaska (GCN 12865).  

Further analysis is in progress.

This GCN may be cited.


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12867
SUBJECT: GRB 120119A: MMT redshift confirmation
DATE:    12/01/19 06:24:14 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

D. Milisavljevic, M. Drout, and E. Berger (Harvard) report:

"We obtained an optical spectrum of GRB 120119A (GCN 12859) with the
Blue Channel spectrograph mounted on the MMT 6.5-m telescope.  In a
single 1800 sec exposure covering 3500-8500 Ang we find a wide range
of absorption features (from CII1335 to MgI2853) at a common redshift
of z=1.728, confirming the results of Cucchiara & Prochaska (GCN
12865)."


GRB_name: GRB120118B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12868
SUBJECT: GRB 120118B  : Lulin Optical limit 
DATE:    12/01/19 06:45:41 GMT
FROM:    Kuiyun Huang at ASIAA  <ljhuang@asiaa.sinica.edu.tw>

GRB 120118B  : Lulin Optical limit 

H.Y. Hsiao, Y. Urata (NCU), K.Y. Huang (ASIAA) on behalf the EAFON
cooperation:

The Lulin 1-m telescope at Taiwan started optical observations on 
GRB 120118B at 1.8 hours after the BAT trigger (Littlejohns et al. GCN
12852). No optical counterpart was found at the Swift-XRT position
(Osborne et al, GCN 12857). Our stacked images indicate 3-sigma
limiting magnitudes of g'~21.9, r'~ 21.4 and i'~ 20.9. The
calibrations were against two nearby sdss stars.

This message can be cited.


GRB_name: GRB120118B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12869
SUBJECT: GRB 120118B: Swift-XRT refined Analysis
DATE:    12/01/19 09:56:37 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O. M. Littlejohns (U Leicester) reports on behalf of the Swift-XRT
team:

We have analysed 8.6 ks of XRT data for GRB 120118B (Littlejohns  et
al. GCN Circ. 12852), from 96 s to 33.9 ks after the  BAT trigger. The
data comprise 19 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 12857).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.9 (+0.5, -0.4). At T+312 s  the decay
flattens to an alpha of -0.25 (+0.24, -0.21) before breaking again at
T+2735 s to a final decay with index alpha=0.99 (+/-0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.22 (+0.20, -0.18). The
best-fitting absorption column is  2.7 (+/-0.6) x 10^21 cm^-2, in
excess of the Galactic value of 6.9 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 (6.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 6.9 x 10^20 cm^-2
Excess significance: 6.0 sigma
Photon index:      2.22 (+0.20, -0.18)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00512003.

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


GRB_name: GRB120118B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12870
SUBJECT: GRB 120118B: TNG NIR observations
DATE:    12/01/19 11:53:27 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB) and E. Palazzi (INAF/IASF Bo) report on behalf of
the CIBO collaboration:

We observed the field of GRB 120118B (Littlejohns et al., GCN 12852) with
the 3.6m TNG telescope located in the Canary Islands. We secured 40 min
H-band and 40 min J-band imaging with the NICS instrument, carried out at
a mean t-t0=9.9 hr and t-t0=10.9 hr, respectively.

Within the UVOT-enhanced XRT error circle (Osborne et al., GCN 12857), we
detect no source down to the limiting magnitudes H > 20.3 and J > 20.5
(Vega, calibrated against the 2MASS catalog).

We note however, a hint for the presence of a faint, low-significance
object in the H-band image, at the following position (J2000):

RA: 08:19:29.02
Dec: -07:11:05.1

(+/- 0.3"), consistent with the UVOT-enhanced XRT position. At present we
cannot asses if the source is real or due to a background fluctuation.

We acknoledge the TNG staff for their support, in particular Avet
Harutyunyan and Gianni Mainella.

[GCN OPS NOTE(19jan12): Per author's request, "Gianni Tessicini" was changed
to "Gianni Mainella".]


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12871
SUBJECT: GRB 120119A: optical observations
DATE:    12/01/19 12:57:41 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  A. Volnova (SAI MSU),  A. Pozanenko (IKI)  report on 
behalf of  larger GRB follow-up collaboration:

We observed the field of the Swift GRB 120119A  (Beardmore  et al.,  GCN 
12859) with 0.45-m telescope  ISON-NM observatory on Jan. 19. We took 
several unfiltered images of  60 s exposure on Jan.19, starting (UT) 
05:19:52. We clearly detect the OT source (Beardmore  et al.,  GCN  12859). 
Coordinates of the source are (J2000) 08 00 06.96 -09 04 54.4 which is 
consistent with UVOT position (GCN  12859). Photometry of the source is 
based on SDSS star J080000.59-090624.3 (08:00:00.60 -09:06:24.4) assuming 
R=16.42:

t-t0             filter      Exp.        OT
(mid, days)             (s)

0.05234    none     600   18.97  +/-    0.09
0.06039    none     600   18.84  +/-    0.08
0.06837    none     600   19.13  +/-    0.11
0.08321    none    1500  19.51  +/-    0.07
0.10178    none    1500  19.70  +/-    0.08
0.12128    none    1500  19.99  +/-    0.08
0.13989    none    1500  19.86  +/-    0.08

Looking for the photometry result one can suggest either plateau phase or 
the start of a re-brightening episode at ~ 0.14d.


GRB_name: GRB120119A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12872
SUBJECT: Konus-Wind observation of GRB 120119A
DATE:    12/01/19 13:18:14 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 120119A (Swift-BAT trigger #512035:
Beardmore et al., GCN 12859)
triggered Konus-Wind at T0=14674.872s UT (04:01:34.872)

The burst light curve shows a multi-peaked pulse
with a total duration of ~61 s.
The emission is seen up to ~7 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120119_T14674/

As observed by Konus-Wind the burst
had a fluence of (4.7  0.6)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+16.384 s,
of (3.9  0.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+49.152 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.85 (-0.16, +0.20),
the high energy photon index beta = -2.34 (-0.22, +0.15),
the peak energy Ep = 153(-19, +21) keV,
chi2 = 73.5/84 dof.

The spectrum of the initial pulse
(measured from T0 to T0+16.384 s) is best fitted
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.92 (-0.13, +0.14),
the high energy photon index beta = -2.41 (-0.35, +0.16),
the peak energy Ep = 192(-21, +29) keV,
chi2 = 72.4/84 dof.

Assuming the redshift z=1.73 (Cucchiara & Prochaska, GCN 12865;
Pancoast et al., GCN 12866; Milisavljevic et al., GCN 12867)
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 (3.6  0.5)x10^53 erg,
the isotropic peak luminosity L_iso_max is (5.1  0.7)x10^52 erg/s,
and Ep_rest is (265  35) keV.

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


GRB_name: GRB120118B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12873
SUBJECT: GRB 120118B, Swift-BAT refined analysis
DATE:    12/01/19 14:48:38 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

T. Sakamoto (GSFC/UMBC), 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), O. M. Littlejohns (U Leicester),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), 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 120118B (trigger #512003)
(Littlejohns, et al., GCN Circ. 12852).  The BAT ground-calculated position is
RA, Dec = 124.862, -7.178 deg which is
     RA(J2000)  =  08h 19m 26.9s
     Dec(J2000) = -07d 10' 39.5"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 40%.

The mask-weighted light curve shows a single smooth FRED peak lasting from T-5
sec to T+25 sec.  T90 (15-350 keV) is 23.26 +- 4.02 sec (estimated error
including systematics).

The time-averaged spectrum from T-1.92 to T+30.51 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.08 +- 0.11.  The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+6.69 sec in the 15-150 keV band
is 2.2 +- 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/512003/BA/


GRB_name: GRB120119A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12874
SUBJECT: GRB 120119A: Fermi GBM observation
DATE:    12/01/19 15:24:03 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team:

"At 04:04:25.06 UT on 19 January 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120119A (trigger 348638667 / 120119170).
which was also detected by the Swift/BAT and Swift/XRT
(Beardmore et al. 2012, GCN 12859)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 31.4 degrees.

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

The GBM light curve shows several overlapping pulses
with a duration (T90) of about 55 s (50-300 keV).
The time-averaged spectrum from T0-1.5 s to T0+53.8 s is
best fit by a Band function with Epeak = 189.2 +/- 8.3 keV,
alpha = -0.98 +/- 0.03, and beta = -2.36 +/- 0.09.

The event fluence (10-1000 keV) in this time interval is
(3.87 +/- 0.01)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+14.5 s in the 10-1000 keV band
is 16.86 +/- 0.39 ph/s/cm^2.

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


GRB_name: GRB120102A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12875
SUBJECT: GRB 120102A, the review of the sky area in plate archive
DATE:    12/01/19 15:43:02 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V. V. Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120102A (A.P. Beardmore et al., GCN Circ.12795) 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 and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates--- Exp. LimM Star USNOA2 
19890629/211821 EAO040B001801 13.5 16.50 1125-09467284
19890708/212336 GUA040C001487 16.0 16.45 1125-09467782
19890803/192540 GUA040C001492A 16.0 16.00 1125-09466499
19890803/194958 GUA040C001493 16.0 16.00 1125-09466499
19890905/172315 EAO040B001991 13.5 16.50 1125-09467284
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) and 
EAO040B archive of DWAZ (D/F=400/2000, M=103"/mm) of the 
 Engelhardt South. St. Zelenchuk Russia 
 (Marsden's number - 114) [1]. 
Exp.   - Duration of the maximum exposure (minutes). 
LimM - Limited V mag, derived in the 8 minutes area around 
 the location given in GCN Circ.12795:  
 RA(J2000): 18h 24m 53.93s, Dec(J2000): +24d 42' 48.7"
Star USNOA2 - Comparison star. 
  The preview images of 5 areas together with  
the 8x8 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120102A/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: GRB120119A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12876
SUBJECT: GRB 120119A: Enhanced Swift-XRT position
DATE:    12/01/19 17:52:23 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 6070 s of XRT Photon Counting mode data and 12 UVOT
images for GRB 120119A, 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 = 120.02875, -9.08177 which is equivalent
to:

RA (J2000): 08h 00m 6.90s
Dec (J2000): -09d 04' 54.4"

with an uncertainty of 1.4 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: GRB120119A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12877
SUBJECT: GRB 120119A: Swift-XRT refined Analysis
DATE:    12/01/19 18:22:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

V. D'Elia (ASDC), V. Mangano (INAF-IASFPA), M.C. Stroh (PSU), D.N.
Burrows (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), C. Pagani
(U. Leicester), A. Melandri (INAF-OAB) and A.P. Beardmore report on
behalf of the Swift-XRT team:

We have analysed 9.1 ks of XRT data for GRB 120119A (Beardmore et al.
GCN Circ. 12859), from 59 s to 30.4 ks after the  BAT trigger. The data
comprise 332 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 12876).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.58 (+/-0.08), followed by a break at T+167 s to an
alpha of 1.008 (+0.017, -0.018).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.93 (+/-0.07). The
best-fitting absorption column is  2.18 (+0.22, -0.21) x 10^21 cm^-2,
in excess of the Galactic value of 7.9 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.68 (+0.13, -0.12)
and a best-fitting absorption column of 2.1 (+0.5, -0.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.7 x 10^-11 (6.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.1 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 7.9 x 10^20 cm^-2
Excess significance: 4.9 sigma
Photon index:      1.68 (+0.13, -0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00512035.

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


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12878
SUBJECT: GRB 120119A: SMARTS optical/IR afterglow observations
DATE:    12/01/19 19:46:55 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 120119A (GCN 12859,
Beardmore et al.) over several epochs, starting ~0.6 hours post-burst.
For the first epoch, several dithered images were obtained in each filter,
with total summed exposure times of 180s in each of BRIJK and 120s in each
of H and V.  For later epochs, total summed exposure times amounted to 15
minutes in I and V and 12 minutes in J and K.

At a mid-exposure time of 2012-01-19 04:43 UT (0.64 hrs post-burst), the
GRB afterglow (e.g. GCN 12859, Beardmore et al., GCN 12860, Morgan et
al., GCN 12863, Schady et al.) is detected with the following magnitudes:

B = 20.07 +/- 0.06
V = 18.91 +/- 0.05
R = 18.02 +/- 0.03
I = 16.96 +/- 0.03
J = 15.14 +/- 0.05
H = 14.02 +/- 0.06
K = 12.89 +/- 0.10

Between about 0.6 hrs and 3 hrs post-burst, the GRB afterglow fades with a
decay rate of approximately alpha = 1.6 (where afterglow flux is
proportional to t^-alpha).

time
post-burst      I-band magnitude
0.64 hrs        16.96 +/- 0.03
1.71 hrs        18.52 +/- 0.03
2.97 hrs        19.39 +/- 0.05

(Optical photometry is calibrated against Landolt standard stars
and IR photometry is calibrated against 2MASS stars in the field.)


GRB_name: GRB120118B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12879
SUBJECT: GRB 120118B: RTT150 optical observations
DATE:    12/01/19 19:47:54 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

I. Bikmaev, A.Galeev , N. Sakhibullin (Kazan University),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Khamitov, Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

The field of GRB 120118B (Littlejohns et al., GCN 12852) was observed
with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK
National Observatory, Turkey) in January 18/19, 2012, during UT 20:29
-- 01:01, i.e. starting approximately 3.5 hours after the burst. A
serie of 3 exposures by 900 sec and 10 exposures by 600 sec each in Rc
filter was obtained at moderate seeing conditions of 1.8-2.3 arcsec.

We found no optical source within the 1.8" enhanced XRT error circle
(Osborne et al., GCN 12857) in our combined image at a limiting
magnitude of Rc ~ 23.2 mag.


GRB_name: GRB120119A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12880
SUBJECT: GRB 120119A:  Swift/UVOT Observations
DATE:    12/01/19 20:29:33 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 120119A
62 s after the BAT trigger (Beardmore et al., GCN Circ. 12859).
A source consistent with the XRT position (Beardmore et al., GCN Circ.
12876) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  08:00:06.93 = 120.02889 (deg.)
     Dec (J2000) = -09:04:53.7  =  -9.08159 (deg.)
with an estimated uncertainty of 0.59 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)  
are:

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

white_FC            62          211          147         19.5 +/- 0.1
white               62         1997          205         19.5 +/- 0.1
white             6130        30955         1112         21.9 +/- 0.4
v                 1682         2048           58        >19.1
v                 7810        12009          926        >20.8
b                 1608         1973           58         19.4 +/- 0.3
b                 5926        30829         1967        >22.0
u_FC               273          302           28        >18.7
u                  273         1948           66        >19.3
u                 5720        29917         1967        >21.7
w1                1731         1923           39        >19.1
w1               12921        25179         1511        >21.5
m2                1706         2073           58        >19.3
m2               12014        12914          885        >21.2
w2                1658         2022           58        >19.5
w2                6336         7804          242        >20.6

The magnitudes in the table are not corrected for the Galactic  
extinction
due to the reddening of E(B-V) = 0.11 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12881
SUBJECT: GRB 120119A: optical observations
DATE:    12/01/20 09:20:57 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  A. Volnova (SAI MSU),  A. Pozanenko (IKI)  report on 
behalf of  larger GRB follow-up collaboration:

We observed the field of the Swift GRB 120119A  (Beardmore  et al.,  GCN 
12859) with 0.45-m telescope  ISON-NM observatory on Jan. 20  between (UT) 
05:59:24 - 06:53:16. We do not detect the OT at the UVOT position reported 
in GCN 12880 (Chester et al.).

However we detect the source with coordiantes (J2000) 08 00 06.97 -09 04 
56.6 with uncertainties of 0.1" (in both coordinates) which is differ from 
OT coordinates calculated in the first epoch of our observations (Elenin et 
al, GCN  12871). This source coincide with SDSS source 
SDSSJ080006.97-090456.8 (r=21.05) and is also visible at DSS2 image (R).

Photometry of this source at 1.0987 days after burst (mean time) is 21.1 +/- 
0.2 and based on SDSS star J080005.86-090434.9   (J2000) 08 00 05.868 -09 04 
34.91 assuming R=18.05.We suggest that the source could be a host galaxy of 
GRB 120119A. All results are preliminary.


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12882
SUBJECT: GRB120119A: REM NIR observations
DATE:    12/01/20 09:36:12 GMT
FROM:    Dino Fugazza at INAF-OAB  <dino.fugazza@brera.inaf.it>

D. Fugazza, P. D'Avanzo, A. Melandri (INAF-OAB), L. A. Antonelli (INAF-OAR/ASI-ASDC) report on behalf of the CIBO collaboration:

We observed the field of GRB 120119A (Beardmore et al., GCN 12859) with the REMIR infrared camera, mounted on the 60-cm robotic REM telescope at
La Silla, starting 2.5 min after the burst.

The optical/NIR afterglow (Beardmore et al. GCN 12859; Morgan & Bloom GCN 12860; Gomboc GCN 12861; Schady et al. GCN 12863; Elenin et al. GCN 12871; Cobb GCN 12878) is clearly detected in the H-band. 
The light curve shows a plateau from about 4.5 min to 10 min after the burst with an observed magnitude of H~13.4, peaks at about T-T0=15 min with H~13.0 and then displays a significant decay. 
The last detection is at T-T0=3.8 hr with a magnitude of H~16.0.


The magnitudes are calibrated against the 2MASS catalogue.


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12883
SUBJECT: GRB 120119A: TAROT La Silla observatory optical observations
DATE:    12/01/20 09:47:40 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120119A detected by SWIFT
(trigger 512035) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 33.0s after the GRB trigger
(9.2s after the notice) using the trigger time origin
at 04:04:30.21 UT (Beardmore et al. GCNC 12859).
The elevation of the field increased from
67 degrees above horizon and weather conditions
were good. We observed during 4.35h until the
dawn allowing a continuous follow up of the afterglow
discovered by Beardmore et al. (GCNC 12859).

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
This image was obtained during the fading of the
gamma emission. We extracted three measurements from
the trail.

A first magnitude extraction is reported in the following
table. As noticed by LaCluyze et al. (GCNC 12864), the
optical emission decreased slowly in the range 33s to 200s,
then it increased to reach a maximum R=16.8 at 850 +/- 50s.
A decay phase alpha=1.3 occured between 10^3 and 10^4 seconds.
As noticed by Elenin et al. (GCNC 12871) the begining of a
plateau is suspected after 10^4 seconds. The end of the
night over Chile does not allow to conclude definitively.

Note that the GRB was also observed at TAROT Calern (France)
but data are poor due to the low elevation of the field.
However, the afterglow is also detected in the TAROT Calern
images.

------------------------------------------
  t1(min)    t2(min)     mag    dmag
------------------------------------------
     0.55       0.85    16.96    0.30
     0.85       1.15    17.15    0.30
     1.15       1.55    17.05    0.30
     1.67       2.17    17.32    0.16
     2.34       2.84    17.37    0.12
     3.01       3.51    17.58    0.22
     3.67       4.17    17.53    0.17
     4.34       4.84    17.27    0.17
    10.36      11.86    17.02    0.26
    12.03      13.53    16.87    0.20
    13.70      15.20    17.03    0.15
    15.37      16.87    16.94    0.18
    17.03      18.53    17.19    0.29
    18.70      20.20    17.19    0.11
    21.31      22.81    17.27    0.24
    22.97      24.47    17.37    0.16
    24.64      26.14    17.35    0.09
    26.31      27.81    17.32    0.19
    27.98      29.48    17.40    0.06
    29.64      31.14    17.59    0.05
    35.98      38.98    17.65    0.05
    39.15      42.15    18.00    0.21
    45.48      48.48    18.09    0.06
    48.65      51.65    18.31    0.25
    55.66      58.66    18.39    0.15
    58.83      61.83    18.58    0.26
    42.32      84.94    18.51    0.12
    65.16      91.28    19.10    0.15
    95.40     126.40    19.51    0.09
   129.73     195.34    19.78    0.12
   199.45     261.71    19.90    0.08


GRB_name: GRB120119A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12884
SUBJECT: GRB 120119A, Swift-BAT refined analysis
DATE:    12/01/20 22:42:20 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), 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),
J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+395 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120119A (trigger #512035)
(Beardmore, et al., GCN Circ. 12859).  The BAT ground-calculated position is
RA, Dec = 120.029, -9.076 deg which is
    RA(J2000)  =  08h 00m 06.9s
    Dec(J2000) = -09d 04' 35.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a series of three overlapping peaks running
from T-10 sec to T+220 sec, with the bulk of emission before T+60 sec.
T90 (15-350 keV) is 253.8 +- 24.5 sec (estimated error including systematics).
Swift started to enter the South Atlantic Anomaly at T+ ~200 sec and collection of
event data was terminated at T+395 sec.

The time-averaged spectrum from T-13.2 to T+361.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.38 +- 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+9.21 sec in the 15-150 keV band
is 10.3 +- 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/512035/BA/


GRB_name: GRB120121A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12885
SUBJECT: GRB 120121A: Swift detection of a burst
DATE:    12/01/21 10:00:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), A. P. Beardmore (U Leicester),
P. A. Evans (U Leicester), J. A. Kennea (PSU), D. M. Palmer (LANL),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 09:42:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120121A (trigger=512164).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 249.336, -23.954 which is 
   RA(J2000) = 16h 37m 21s
   Dec(J2000) = -23d 57' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
FRED structure with a duration of about 40 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 09:44:18.7 UT, 119.4 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 123 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 25% of
the BAT 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
0.84. 

Burst Advocate for this burst is K. L. Page (kpa 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: GRB120121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12886
SUBJECT: GRB 120121A: Swift-XRT position
DATE:    12/01/21 10:58:57 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT 
team:

Using promptly downlinked data we find an X-ray source with an enhanced 
position: RA,Dec = 249.3547, -23.9618 (degrees) which is equivalent to:

RA  (J2000) = 16 37 25.13
DEC (J2000) = -23 57 42.4

with an uncertainty of 3.2 arcsec (radius, 90% containment). This location 
is 67.6 arcseconds from the BAT onboard position, inside the BAT error 
circle. It is not yet possible to determine whether the source is fading.


GRB_name: GRB120121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12887
SUBJECT: GRB 120121A: ISON-NM optical observations
DATE:    12/01/21 13:16:52 GMT
FROM:    Leonid Elenin at ISON  <l.elenin@gmail.com>

L. Elenin (KIAM), A. Pozanenko (IKI), A. Volnova (SAI MSU), I. Molotov
(KIAM) report on behalf of larger GRB  follow-up collaboration:

We observed the field of the Swift GRB 120121A  (Page et al.,  GCN 12885)
with 0.45-m telescope ISON-NM observatory on Jan. 21. We took several
unfiltered images of  60 s exposure on Jan. 21, starting (UT) 12:29:25.  We
do not detect any object within the XRT error circle (Page et al., GCN 12886
), down to 19.7m (calibrated against the USNO B1.0 catalog).


GRB_name: GRB120121A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12888
SUBJECT: GRB 120121A: Enhanced Swift-XRT position
DATE:    12/01/21 16:34:19 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 1511 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120121A, 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 = 249.35428, -23.96156 which is equivalent
to:

RA (J2000): 16h 37m 25.03s
Dec (J2000): -23d 57' 41.6"

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: GRB120121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12889
SUBJECT: GRB 120121A: Swift-BAT refined analysis
DATE:    12/01/21 17:59:41 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),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), K. L. Page (U Leicester), 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 recent telemetry downlinks,
we report further analysis of BAT GRB 120121A (trigger #512164)
(Page, et al., GCN Circ. 12885).  The BAT ground-calculated position is
RA, Dec = 249.363, -23.963 deg which is 
   RA(J2000)  =  16h 37m 27.1s 
   Dec(J2000) = -23d 57' 45.9" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 70%.
 
The mask-weighted light curve shows several overlapping peaks starting at
~T-10 sec, peaking at ~T+2 sec, and ending at ~T+70 sec.
T90 (15-350 keV) is 26.1 +- 3.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-11.00 to T+18.33 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.23 +- 0.13.  The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.86 sec in the 15-150 keV band
is 0.7 +- 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/512164/BA/


GRB_name: GRB120121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12890
SUBJECT: GRB 120121A: Swift-XRT refined Analysis
DATE:    12/01/21 20:02:06 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K. L. Page (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 9.8 ks of XRT data for GRB 120121A (Page  et al. GCN
Circ. 12885), from 130 s to 23.1 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 12888).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.88 (+0.09, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+0.7, -0.6). The
best-fitting absorption column is  2.4 (+1.3, -0.9) x 10^22 cm^-2, in
excess of the Galactic value of 1.2 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 7.5 x 10^-11 (2.0 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.4 (+1.3, -0.9) x 10^22 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 4.3 sigma
Photon index:      2.0 (+0.7, -0.6)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00512164.

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


GRB_name: GRB120121A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12891
SUBJECT: GRB 120121A: Swift/UVOT Upper Limits
DATE:    12/01/21 20:11:24 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and K. L. Page (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120121A
124 s after the BAT trigger (Page et al., GCN Circ. 12885).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 12888)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           124          273          147         >20.2
u_FC               336          585          246         >19.7
white              124         6777          673         >21.1
v                  664         7188          510         >18.9
b                  591        13219         1160         >20.2
u                  336        18998         2078         >20.2
w1                 714        18281         2108         >20.4
m2               16474        17374          886         >20.1
w2                1020        23198         1298         >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.87 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120119A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12892
SUBJECT: GRB 120119A: optical upper limit
DATE:    12/01/21 22:00:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 120119A  (Beardmore  et al.,  GCN 
12859) with AZT-11 telescope  of CrAO observatory on Jan. 19. We took 
several  images in R-filter under poor seeing (FWHM ~ 4.4") on Jan.19, 
between (UT) 18:35 - 19:59. We do not detect the OT  (Beardmore et al. GCN 
12859).  Photometry  is  based on USNO-B1.0 star  0809-0167535  (08 00 
04.98 -09 03 55.5) assuming R=16.22:

t-t0             filter      Exp.       UpperLimit
(mid, days)             (s)

0.6347        R       28x180     21.1 


GRB_name: GRB111225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12893
SUBJECT: GRB 111225A: optical observations
DATE:    12/01/21 22:04:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.Volnova (SAI MSU),  E. Klunko (ISTP),  M. Andreev, A. Sergeev  (Terskol 
Branch of INASAN), A. Pozanenko (IKI) on behalf of  larger GRB follow up 
collaboration report:

We observed the field of GRB 111225A (Siegel et al., GCN 12720) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Dec. 25 between (UT) 
17:37:41 - 18:25:58 in R filter under mean seeing (FWHM) of about 2.0".

We also observed  the field with Zeiss-2000 telescope of Mt. Terskol 
observatory on Dec. 26 between (UT) 17:37:23-18:46:37 in BRI filters under 
poor seeing (FWHM) of about 4.4". On   stacked images of both epochs we did 
not find an optical counterpart (Siegel  et al., GCN 12720; Klotz et al., 
GCN 12722; Adria et al., GCN 12723; Wren et al., GCN 12803).

The photometry is based on the USNO-B1.0 star 1415-0025726 (J2000) 
00:52:35.11 +51:33:58.9, assuming B = 17.56, R =16.50, I = 16.20:

T0+,        Filter,  Exposure,   OT,   UL(3 sigma),    Telescope
(mid, d)             (s)
0.63278     R     24 x 120   n/d   22.5            AZT-33IK
1.58789     B     10 x 90     n/d   22.0            Zeiss-2000
1.60285     R     10 x 90     n/d   21.5            Zeiss-2000
1.61677     I      10 x 90     n/d   20.5            Zeiss-2000

Upper limits above are consistent with upper limits of R~22.5 reported by 
Sonbas et al. (GCN 12740) and observations of the afterglow at R ~ 23.2 on ~ 
1day  after burst trigger (Cenko et al., GCN 12733). Taking into account the 
positive detection of the afterglow on 3.7590 days at R~22.5 (Rumyantsev et 
al., GCN 12793) one can suggest a strong rebrightening of the afterglow 
which is a rare case of  late afterglow (3.7590 days) of an apparently 
nearby burst (cf. UVOT optical detection in uvw2 filter  (Siegel, GCN 
12735). 


GRB_name: GRB120119A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12894
SUBJECT: GRB 120119A: GRT detection of early afterglow
DATE:    12/01/22 02:16:11 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),
T. Okajima (GSFC), Y. Urata (NCU)

We observed the field of GRB 120119A detected by Swift
(trigger #512035; Beardmore et al., GCN Circ. 12859) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

A total 294 images of 5 sec (200 images), 30 sec (60 images) and 
60 sec (34 images) exposures were taken in the R filter starting 
from January 19 04:06:42 (UT), about 132 seconds after the trigger 
(114 seconds after the BAT position notice), and stopped on 
January 19 06:07:50 (UT).  

We detect the optical afterglow inside the XRT error circle (Beardmore 
et al., GCN Circ. 12876) in the stacked image of good quality 5 sec 
exposure images (total exposure of 985 sec).  The estimated magnitude is 
R = 17.24 +- 0.19 mag (start time: 04:06:42, stop time: 04:44:37).   We do 
not detected the afterglow in the stacked images of 30 sec exposure images 
(total exposure of 1560 sec) and 60 sec exposure images (total exposure of 
2040 sec).  The estimated five sigma upper limits of those stacked images 
are ~17.9 mag (start time: 04:44:55, stop time: 05:30:01) and ~18.0 mag 
(start time: 05:30:17, stop time: 06:07:50).  All the reported magnitudes 
are estimated using the USNO-B1 catalog.  


GRB_name: GRB120119A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12895
SUBJECT: GRB 120119A:  EVLA observations
DATE:    12/01/22 23:17:26 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer and E. Berger (Harvard) report on behalf of a larger
collaboration:

"We observed the position of GRB 120119A (GCN 12859) with the EVLA
beginning 2012 Jan 21.2 UT (2.0 days after the burst) at a mean
frequency of 5.8 GHz.  No significant radio emission is detected at the
enhanced Swift-XRT position (GCN 12876), the UVOT position (GCN 12859)
or optical position (e.g. GCN 12881), to a three-sigma upper limit of
34 uJy."


GRB_name: GRB120119A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12897
SUBJECT: GRB 120119A : SMA submm follow-up observation
DATE:    12/01/24 02:54:46 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Y. Urata (NCU), S. Takahashi, K.Y. Huang (ASIAA)
and G. Petitpas (SMA)

We observed the field of GRB120119A (Siegel et al., GCN 12720) with
the Sub-Millimeter Array (SMA). The observation in the 225 GHz band
was started at January 19 11.1 UT (7.1 hours after the trigger).
Our preliminary analysis show no counterpart brighter than 8.1 mJy (3-sigma).


GRB_name: GRB120119A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12898
SUBJECT: GRB 120119A : LOAO Optical Observations
DATE:    12/01/24 09:13:48 GMT
FROM:    Minsung Jang at Seoul National U  <rigel103@snu.ac.kr>

M. Jang, M. Im (SNU), and Y. Urata (NCU) on behalf of EAFON

We observed GRB 120119A (GCN 12859, Beardmore et al.) in B,V,R- bands
with a 1 m telescope at Mt. Lemmon, Arizona, US.
The observation began at 06:03:31 UT, ~ 2 hours after burst alert.
We took 3 frames for each filter with the exposure time, 300 secs

The afterglow candidate was detected in stacked images of all three filters
with a preliminary magnitude R ~ 20.3 +/- 0.2 mag.
The photometry calibration is based on two USNO B1.0 stars,
USNO-B1.0 0809-0167573 and 0808-0168858

We thank the LOAO operator, J. Yoon for his help with the observation. 


GRB_name: GRB120116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12899
SUBJECT: GRB 120116A: optical upper limit
DATE:    12/01/27 09:42:18 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

 A. Volnova (SAI MSU), E. Litvinenko (UBAI), I. Molotov (KIAM), A.
Pozanenko (IKI) on behalf of  larger GRB follow up collaboration
report:

 We observed the field of the Swift GRB 120116A (Melandri et al., GCN
12834) with ORI-40 telescope of Kitab ISON observatory on Jan. 16
 starting (UT) 18:12:48, i.e. ~6 min after burst trigger. We obtained
several unfiltered images with exposure of 60 seconds. On the stacked
image we do not detect any source within the enhanced XRT error box
(Goad et al., GCN 12846). The photometry is based on nearby reference
stars of USNO-B1.0
 (R2 magnitudes):

 Tstart UT,   T0+,      Filter,  Exposure, OT,   UL (3 sigma)
                (mid, d)             (s)

 18:12:48     0.01480 none    29x60      n/d   19.4


GRB_name: GRB120118B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12900
SUBJECT: GRB 120118B: optical upper limit
DATE:    12/01/27 09:43:39 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

 A. Volnova (SAI MSU), E. Litvinenko (UBAI), I. Molotov (KIAM), A.
Pozanenko (IKI) on behalf of  larger GRB follow up collaboration
report:

 We observed the field of the Swift GRB 120118B (Littlejohns et al.,
 GCNs 12852, 12854) with ORI-40 telescope of Kitab ISON observatory on
 Jan. 18 between (UT) 17:39:55 and 18:10:51. We obtained several
 unfiltered images with exposure of 60 seconds. On the stacked image we
 do not detect a source reported by D'Avanzo et al. (GCN 12870). The
 photometry is based on nearby reference stars of USNO-B1.0 (R2
 magnitudes):

 Tstart UT,   T0+,        Filter, Exposure, OT,   UL (3 sigma)
                 (mid, d)            (s)

 17:39:55     0.03127   none   26x60      n/d   19.5


GRB_name: GRB120127A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12901
SUBJECT: GRB 120127A: MAXI/GSC detection of a probable GRB
DATE:    12/01/27 11:53:36 GMT
FROM:    Mikio Morii at Tokyo Inst Tech  <morii@hp.phys.titech.ac.jp>

S. Song, M. Morii (Tokyo Tech), H. Negoro, F. Suwa (Nihon U.), M. Serino, S. Nakahira (RIKEN),
S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN), 
N. Kawai, K. Sugimori, R. Usui, T. Toizumi, Y. Aoki (Tokyo Tech),
A. Yoshida, K. Yamaoka (AGU),
H. Tsunemi, M. Kimura, H. Kitayama (Osaka U.), 
M. Nakajima, M. Asada, H. Sakakibara (Nihon U.), 
Y. Ueda, K. Hiroi, M. Shidatsu (Kyoto U.),
Y. Tsuboi, T. Matsumura, K. Yamazaki (Chuo U.)
M. Yamauchi, Y. Nishimura, T. Hanayama (Miyazaki U.) 
report on behalf of the MAXI team:

MAXI/GSC triggered at 2012-01-27 04:21:52 UT on an uncatalogued X-ray transient source.
The transient emission lasted for about 10 seconds
within the 50 second long triangular transit response of
MAXI/GSC. We identify this event as GRB 120127A.

Assuming that the source flux was constant over the transit,
we obtain a statistical 90% C.L. elliptical error region centered on

(R.A., Dec) = (139.14 deg, 15.88 deg) = (09 16 34, +15 52 51)(J2000)

with long and short radii of 0.74 deg and 0.52 deg, respectively.
The position angle of long axis is 53.7 deg.
There is additional systematic uncertainty of 0.1 deg (90% containment radius).

Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:

 (R.A., Dec) = (138.12 deg, 15.61 deg) = (09 12 29, +15 36 32)(J2000)
 (R.A., Dec) = (138.95 deg, 14.87 deg) = (09 15 47, +14 52 29)(J2000)
 (R.A., Dec) = (140.82 deg, 16.80 deg) = (09 23 16, +16 48 02)(J2000)
 (R.A., Dec) = (140.00 deg, 17.54 deg) = (09 20 01, +17 32 09)(J2000)

The X-ray flux averaged over the scan was 48 +- 21  mCrab (4-10 keV, 1 sigma error).

Follow-up observations are encouraged.


GRB_name: GRB120127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12902
SUBJECT: GRB 120127A: MASTER optical observations
DATE:    12/01/27 15:38:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


O.Gres, O.Chuvalaev,K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev
  Irkutsk State University

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

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk

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



  MASTER II  robotic double telescope (FOW=2x4 square degrees, 
http://observ.pereplet.ru) located 
in Tunka was pointed to the  GRB120127A (MAXI/GSC, Song et al., GCN Circ 
12901) 9h 30 min after GRB time at 2012-01-27 04:21:52 UT  in two polarizations. 
On our  images we haven't found optical transient
within error-box (Song et al., GCN Circ 12901).
The delay is due to the MAXI/GSC ground reduction.

    Date       UT         UT           Exp     Coadd      Limit
             Start     Mean Time
2012-01-27 13:51:59   13:53:29      180s       no         18.9
2012-01-27 13:51:59   13:58:40      900s       yes        19.9




This circular was generated automatically.

The message may be cited.


GRB_name: GRB120127A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12903
SUBJECT: GRB 120127A / P48 Imaging
DATE:    12/01/28 23:41:44 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), E. O. Ofek (Weizmann Institute), and P. E.
Nugent (LBNL/UC Berkeley) report on behalf of a larger collaboration:

We have imaged the location of the MAXI GRB120127A (Song et al., GCN
12901) with the Palomar 48 inch Oschin Schmidt telescope as part of the
Palomar Transient Factory.  Observations began at 3:41 UT on 28 January
2012 (~ 23.3 hours after the MAXI trigger) and cover ~ 90% of the MAXI
error localization.

By comparing sources detected in our images with the USNO-B1 catalog,
2MASS point source catalog, and the Digital Palomar Optical Sky Survey
archival images, we find no new sources within the MAXI error
localization (aside from a number of known minor planets).  The limiting
magnitude of our imaging is R >~ 19.5 mag (calculated with respect to
field stars from the USNO-B catalog).


GRB_name: GRB120129A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12904
SUBJECT: IPN Triangulation of GRB 120129A (long/intense)
DATE:    12/01/30 18:38:05 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi,
on behalf of the AGILE MCAL team, and

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, report:

The long-duration, very intense GRB 120129A was observed by Konus-Wind, 
MESSENGER (GRNS), AGILE (MCAL and SuperAGILE), Fermi (GBM), and Swift 
(BAT) at about 50146 s UT (13:55:46). The burst was outside the coded 
fields of view of the BAT and SuperAGILE.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    30.440 (02h 01m 46s) +59.282 (+59d 16' 55")
  Corners:
    23.362 (01h 33m 27s) +68.842 (+68d 50' 33")
    31.740 (02h 06m 58s) +56.353 (+56d 21' 09")
    34.401 (02h 17m 36s) +51.346 (+51d 20' 44")
    28.869 (01h 55m 29s) +62.399 (+62d 23' 58")
  ---------------------------------------------

The error box area is 2.7  sq. deg, and its maximum
dimension is 18.3 deg.

This box can be improved.

The time history and spectrum will be given in a forthcoming GCN Circular.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120129_T50148/IPN/


GRB_name: GRB120129A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12905
SUBJECT: Konus-Wind observation of GRB 120129A
DATE:    12/01/31 10:18:12 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 intense GRB 120129A
(localized by IPN: Golenetskii et al., GCN 12904)
triggered Konus-Wind at T0=50148.403s UT (13:55:48.403).
The observation is performed against very high and variable
background count rate caused by solar charged particles.

The burst light curve shows two bright partly overlapped pulses.
A total duration of the burst is ~4 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/GRB120129_T50148/

As observed by Konus-Wind the burst
had a fluence of (2.7  0.7)x10-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.672 s,
of (3.3  1.0)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+3.328 s)
is best fitted in the 20 keV - 5 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.76 (-0.09, +0.09),
the high energy photon index beta = -2.9 ( <-2.3),
the peak energy Ep = 326(-38, +52) keV,
chi2 = 66.5/76 dof.

The spectrum at the maximum count rate
(measured from T0+0.512 to T0+0.768 s) is best fitted
is best fitted in the 20 keV - 5 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.51 (-0.19, +0.21),
the high energy photon index beta = -2.3 (-1.4, +0.3),
the peak energy Ep = 317(-66, +92) keV,
chi2 = 54.2/61 dof.


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


GRB_name: GRB120116A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12906
SUBJECT: GRB 120116A, the review of the sky area in plate archives
DATE:    12/01/31 14:27:52 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120116A (M.R. Goad et al., GCN Circ.12846) 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 
and Epson Expression 10000XL flatbed scanners and have been 
placed into Golosiiv Plate Archive database DBGPA with open 
access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19770906/232931 GUA040C000721B 30.0 15.95 1200-00453119
19850919/225420 GUA040C000745A 16.0 15.95 1200-00453119
19860910/234443 GUA040C001009A 16.0 15.10 1200-00451448
19870917/232503 GUA040C001119A 16.0 15.55 1200-00452448
19871023/210844 GUA040C001139A 20.0 16.15 1200-00452199
19871024/204207 GUA040C001155A 17.0 15.10 1200-00451448
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C M=103"/mm) of the Ukrainian NAS Main Astro obs.
        (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 23 minutes area around 
       the location given in M.R. Goad et al. GCN Circ. 12846: 
       RA(J2000): 01h 04m 57.92s, Dec(J2000): +33d 55' 50.0"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 23x19 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120116A/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: GRB120129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12907
SUBJECT: GRB 120129A: MASTER optical observations 
DATE:    12/01/31 14:59:21 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


O.Gres, O.Chuvalaev,K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev
  Irkutsk State University

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

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk

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



  MASTER II  robotic double telescope (FOW=2x4 square degrees, 
http://observ.pereplet.ru) located in Tunka was observed  the 
GRB120129A (S. Golenetskii et al., GCN Circ 
12904) IPN triangulation error-box  using 9 diffent fields.
Observations  proceeded since 2012-01-30 20:50  to 2012-01-30 22:50 i.e 
aprox. 1.3 days after grbtime.
On our  images we haven't found an optical transient
within IPN error-box (S. Golenetskii et al., GCN Circ 12904).
Unfiltred upper limit is 18.5 on each image.

  There is a one strange OT MASTER022229.64+523924.9 
which seen only at one image.

      Date    time             Ra                Dec         Mag
  2012-01-30 22:50:52.423  02h 22m 29.64s , +52d 39m 24s.9 15.37

  The object is not seen on images given after (10 hours) and before (1 
hour) detection time.

A preview of this object  available here 
http://master.sai.msu.ru/static/OTMASTER022229_523924.png

  Our very wide fiels cameras (FOW=2x420 square degrees) synchronously 
with GRB have covered area directly under the errors-box.

  A coverage map available here http://master.sai.msu.ru/static/GRB120129A_MASTER_Cover.png

The message may be cited.


GRB_name: GRB111228A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12908
SUBJECT: GRB 111228A: Possible host detected by Swift/UVOT
DATE:    12/02/02 21:57:17 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

Paul Kuin (MSSL/UCL) and Tilan Ukwatta (MSU) reports on behalf of
the Swift UVOT Team:

Until recently, Swift UVOT continued observations in multiple filters
of GRB 111228A (Ukwatta et al., GCN Circ. 12737).

Based on the observations taken up to January 31, 2012 in the white filter,
a possible host is detected.

The UVOT position in decimal degrees of the GRB during the early and peak
emission period is:  RA=150.06684  DEC=+18.297834, J2000 (sexagesimal
10:00:16.04, +18:17:52.20),  consistent with the enhanced XRT position
reported in GCN Circ. 12747 by Goad et al..  The position of the late time
emission/possible host is:  RA=150.06643  DEC=+18.297903, J2000
(sexagesimal 10:00:15.94, +18:17:52.45).   The position of the late-time
emission is offset by 0.9" which is significantly larger than the
position error for a single uvot image of 0.5" (Breeveld et al., 2010,
MNRAS 406, 1587), and the unknown smaller position error when
comparing between summed UVOT images.  The offset suggests that
the late-time emission is due to a different source, possibly the host.

Other evidence comes from a late time flattening of the light curve.

The late time count-rate light curve decays with a power index of -1.3
in nearly all bands. Taking that as the decay rate, the light curves
in white and uvw2 deviate at times more than 800ks after the trigger.

Extrapolating the power law decay and subtracting from the late-time
white count rate, we estimate a host magnitude in white = 24.6 (+0.4/-0.6) mag,
which corresponds to a host flux in the broadband white filter of
(2.05+/-0.8)x10^-7 Jy (3471 A).


GRB_name: GRB120202A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12909
SUBJECT: GRB 120202A: A long GRB detected by INTEGRAL
DATE:    12/02/02 22:53:28 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, A.Taylor (ISDC, Versoix), on behalf of the 
IBAS Localization Team report:

a long gamma ray burst lasting about 100 s has been detected by IBAS in 
the IBIS/ISGRI data at 21:40:17 UT of February 2.

Its refined coordinates (J2000) are:

RA: 203.5065 [degrees], 
DEC: 22.7747 [degrees]

with an uncertainty of 2.5 arcmin (90% c.l.).

A preliminary analysis gives a 20-200 keV fluence of about 7e-7 erg/cm2 
and a peak flux of about 0.2 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

[GCN OPS NOTE(03feb12):  Per author's request, the typo on the exponent
of the fluence was changed from "-8" to "-7".]


GRB_name: GRB120202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12910
SUBJECT: GRB 120202A: TAROT Calern observatory optical observations
DATE:    12/02/03 00:13:09 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120202A detected by INTEGRAL
(trigger 6461) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 20s after the GRB trigger
(14s after the notice). The burst was still active.
The elevation of the field increased from 9 degrees
above horizon and weather conditions were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT with a limiting magnitude of:
t0+20s to t0+80s : R > 15.2

The second image is 30.0s exposure in tracking mode:
t0+96s to t0+126s : R > 15.9

We co-added a series of exposures:
t0+96s to t0+287s : R > 17.2

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

N.B. Galactic coordinates are lon=11.1564 lat=+79.4238
and the galactic extinction in R band is 0.05 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB120202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12911
SUBJECT: GRB 120202A: Swift/XRT and UVOT observations
DATE:    12/02/03 21:55:00 GMT
FROM:    Giulia Stratta at ASDC  <giulia.stratta@gmail.com>

S. Holland (NASA/GSFC), V. D'Elia (ASDC), G. Stratta (ASDC),
R. Starling (U. Leicester) report on behalf of the Swift team:

We have analysed 4.5 ks of XRT data for the INTEGRAL-detected burst:
GRB 120202A (Mereghetti et al., GCN Circ. 12909), from 33.9 ks to 58.6 ks
after the INTEGRAL trigger.
The data are entirely in Photon Counting (PC) mode.
An X-ray source is detected within the INTEGRAL error circle at:
RA, Dec = 203.503595, 22.773873 deg which is equivalent to:

RA (J2000): 13h 34m 00.86s
Dec(J2000): +22d 46' 25.94"

with an uncertainty of 4.8 arcsec (radius, 90% confidence).
The source count rate is 3.26E-03+/-1.1E-03 cts/s (1 sigma error).
This position is 10.1 arcsec from the INTEGRAL position.
We note that there is a bright SDSS galaxy at about 32 arcseconds
from the burst position, within the INTEGRAL error circle.
At the present time we can not assess whether the source is fading or not.

The Swift/UVOT observed the field of GRB 120202A starting 33,899 s
after the INTEGRAL/IBAS trigger.
We do not detect an optical afterglow inside the XRT error circle.
Preliminary 3-sigma upper limits for detecting a source in the the co-added
images are

Filter       TSTART       TSTOP  EXPOSURE       Mag
---------------------------------------------------
v            35,727      64,596       485     >20.0
u            33,899      64,484      2884     >22.0
white        34,522      64,580      1305     >22.4
---------------------------------------------------

The quoted magnitudes and upper limits have not been corrected for
the Galactic extinction along the line of sight to this burst of
E_{B-V} = 0.02 mag (Schlegel et al. 1998, ApJS, 500, 525).


GRB_name: GRB120202A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12912
SUBJECT: GRB 120202A: WHT, Gemini & UKIRT candidate afterglow
DATE:    12/02/03 22:14:28 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick),
L. DomÃ­nguez Palmero (ING), S. Leggett (Gemini) & T. Wold (JACH)
report on behalf of a larger collaboration:

We imaged the field of GRB120202A (Mereghetti et al. GCN12909) using the
WHT/ACAM and Gemini-N/GMOS.  At the location of the X-ray source identified
by Holland et al. (GCN12911) we find a faint source at position:

13:34:00.80  +22:46:24.3

with the following provisional magnitudes (both photometry and astrometry are
calibrated against SDSS DS8):

WHT
r= 25.00 +/- 0.15  (approx 7:40 hours post-burst)

Gemini-N
r=24.84 +/- 0.09 (approx 16:10 hours post-burst)

Thus there is no clear evidence for variability. 
There is however another point source close to the reported Swift XRT
source at position:

13:34:01.27 +22:46:29.0

slightly outside the reported 90% error circle, for which
we find magnitudes:

WHT:   
r=24.68 +/- 0.09,   z=22.93 +/- 0.18

Gemini:  
r=24.26 +/- 0.06,   z=22.64 +/- 0.08

Thus, there is evidence of brightening for this source by about
0.3-0.4 mag between the two epochs, making it likely associated with
the GRB, albeit with unusual afterglow behaviour.  For this source we also
have a K-band magnitude from UKIRT/WFCAM:

K=18.35 +/- 0.18  (calibrated against 2MASS, taken at 15:00 hours post-burst)

indicating a very red colour from the provisional photometry.


GRB_name: GRB120202A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12913
SUBJECT: GRB 120202A: GROND observations
DATE:    12/02/03 23:59:46 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady, J. Greiner (both MPE Garching), S. Schmidl and D.A. Kann  
(both TLS Tautenburg), J. Greiner (MPE Garching) and report on behalf  
of the GROND team:

We observed the field of the INTEGRAL burst GRB 120202A (Mereghetti et  
al., GCN #12909) 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 06:25 UT on February 3rd, 8.8 hrs after the  
GRB trigger. They were performed at an average seeing of 1arcsec and  
at high airmass.

Within a 1.5hrs of stacked data we detect a source within the Swift- 
XRT error circle (Holland et al., GCN #12911) consistent with the  
first position reported by Tanvir et al. (GCN #12912). We measure an  
r'(AB) magnitude of 24.8+/-0.2, in agreement with Tanvir et al.

In addition, we also detect the second source reported by Tanvir et  
al. in all the GROND optical and NIR bands, although we find that  
during our observations the source faded by 0.2-0.3 magnitudes. At a  
mid-time of 06:53 UT the source had an r'(AB) magnitude of 23.7+/-0.1,  
and at a mid-time of 08:11UT had faded to 24.0+/-0.1.

The above magnitude has been calibrated against SDSS and is not  
corrected for the expected Galactic foreground extinction  
corresponding to a reddening of E_(B-V)=0.02 mag in the direction of  
the burst (Schlegel et al. 1998).


GRB_name: GRB120202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12915
SUBJECT: GRB 120202A: D50 optical limits
DATE:    12/02/05 18:49:33 GMT
FROM:    Jan Strobl at AI AS CR,Ondrejov  <jan@strobl.cz>

M. Blazek, P. Skala, R. Hudec, C. Polasek and J. Strobl
Astronomical Institute of the Academy of Sciences of the Czech Republic

We observed the field of GRB 120202A (Mereghetti et al., GCN 12909) with 
0.5m robotic telescope D50 in Ondrejov observatory (Czech Republic). The 
observation started at 23:45:46 UT on February 02, 2012, approx. 2 hours 
after the INTEGRAL trigger. We report no detection of the optical 
counterpart on the unfiltered images within the error circle given by 
SWIFT/XRT (Holland et al., GCN 12911). The upper limit of 20.5 mag in R 
band was estiated using nearby sources from GSC2.2 catalogue.

This message may be cited.

This research was made on behalf of larger cooperation and used RTS2 
system.


GRB_name: GRB120202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12917
SUBJECT: GRB 120202A: MASTER early optical observations 
DATE:    12/02/06 16:13:53 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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


O.Gres, O.Chuvalaev,K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev
  Irkutsk State University

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

E. Sinykov, V.Yurkov, Yu.Sergienko, D.Varda,
Blagoveschensk Educational State University, Blagoveschensk


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the INTEGRAL GRB120202A  (Mereghetti 
et al.,  GCN Circ No 12909) 73 sec s after 
notice time and 81 sec after GRB time at 2012-02-02 21:41:38.354 UT. On 
our first (20s exposure) set we haven't found optical transient  within 
INTEGRAL error-box. Some delay was due to non format socket alert.
The 5-sigma upper limit has been about 18.0 mag
The message may be cited.


GRB_name: GRB111228A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12918
SUBJECT: GRB 111228A, the review of the sky area in plate archives
DATE:    12/02/08 09:52:41 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 111228 (M.R. Goad et al. GCN Circ.12747) 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 and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19900323/192716 GUA040C003372 14.5 15.05 1050-06177767
19920228/213449 GUA040C001967A 20.0 15.60 1050-06179692
19921201/032302 GUA040C002052A 18.0 15.05 1050-06177767
19921218/022500 GUA040C002075A 21.0 15.05 1050-06177767
19930211/220606 GUA040C002118 22.0 15.60 1050-06179692
19930314/204336 GUA040C002155 20.0 15.60 1050-06179692
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C M=103"/mm) of the Ukrainian NAS Main Astro obs.
        (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 23 minutes area around 
       the location given in M.R. Goad et al. GCN Circ. 12747: 
       RA(J2000) = 10h 00m 16.08s, Dec(J2000) = +18d 17'52.1"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 23x23 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/111228A/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: GRB120202A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12919
SUBJECT: GRB 120202A, the review of the sky area in plate archives
DATE:    12/02/10 08:50:58 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120202 (S. Holland et al. GCN Circ.12911) 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 and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT --Plates-- Exp. LimMag Star USNOA2 
19820324/220009 GUA040C000042A 22.5 15.6 1125-06747907
19820324/220009 GUA040D000043A 22.5 15.6 1125-06747907
19880514/200727 GUA040C001241A 18.0 15.6 1125-06747907
19890205/022521 GUA040C001421A 18.0 15.6 1125-06747907
19900223/005820 GUA040C001583A 19.0 15.6 1125-06747907
Plates: the plates archive identifier of DWA (D/F=400/2000, 
GUA040C, M=103"/mm) of the Ukrainian NAS Main Astro obs.
GUA040D (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimM   - Limited V mag, derived in the 23 minutes area around 
       the location given in Holland et al. GCN Circ. 12911: 
       RA(J2000)= 13h 34m 00.86s, Dec(J2000)= +22d 46'25.94"
Star USNOA2 - Comparison star.
  The preview images of 5 areas together with  
the 23x23 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120202A/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: GRB120211A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12920
SUBJECT: GRB 120211A: Swift detection of a burst
DATE:    12/02/11 12:10:51 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
V. Mangano (INAF-IASFPA), C. Pagani (U Leicester),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 11:58:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120211A (trigger=514586).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 87.751, -24.759 which is 
   RA(J2000) = 05h 51m 00s
   Dec(J2000) = -24d 45' 32"
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 30 sec.  The peak count rate
was ~300 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 12:00:27.6 UT, 119.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 87.75354, -24.77477 which
is equivalent to:
   RA(J2000)  = 05h 51m 00.85s
   Dec(J2000) = -24d 46' 29.2"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 57 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 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 123 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
0.03. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.com). 
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: GRB120211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12921
SUBJECT: GRB 120211A - Faulkes Telescope South Observations
DATE:    12/02/11 15:02:33 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

F. J. Virgili, C.G. Mundell, I.A. Steele, R.J. Smith, C.J. Mottram, D.F. 
Bersier, S. Kobayashi (Liverpool, JMU), A. Gomboc, J. Japelj, D. Kopac 
(U. Ljubljana), C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB) report:

"The 2-m Faulkes Telescope South responded robotically to followup 
GRB120211A
(SWIFT trigger 514586; Sonbas et al. GCN 12920) 3.77 min after the GRB 
trigger time.
No optical counterpart within the XRT error circle is detected to the 
following conservative limits:

R > 21.5 mag (vs USNOB1) at 0.51 hrs from BAT trigger (total exposure = 
720 s)
i' > 20.4 mag (vs USNOB1) at 0.58 hrs from BAT trigger (total exposure = 
700 s)

We also note the presence of a USNOB-1 object lying on the XRT error 
circle border:
05:51:00.786, -24:46:23.86, with R2=20.19 and I=18.74 mag

This message may be cited"


GRB_name: GRB120211A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12922
SUBJECT: GRB 120211A: Enhanced Swift-XRT position
DATE:    12/02/11 15:52:16 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 1401 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120211A, 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 = 87.75371, -24.77521 which is equivalent
to:

RA (J2000): 05h 51m 0.89s
Dec (J2000): -24d 46' 30.8"

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: GRB120211A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12923
SUBJECT: GRB 120211A: MITSuME Okayama Ks-band upper limit
DATE:    12/02/11 16:11:45 GMT
FROM:    Kenshi Yanagisawa at OAO/NAOJ  <yanagi@oao.nao.ac.jp>

Kenshi Yanagisawa, Daisuke Kuroda, Yasuhiro Shimizu, Kiichi Okita
(OAO/NAOJ), Michitoshi Yoshida (Hiroshima-U), Kouji Ohta(Kyoto-U),
and Nobuyuki Kawai(Tokyo Tech.) report on behalf of the MITSuME
collaboration:

We observed the field of GRB120211A (Sonbas et al., GCNC 12920) in
Ks-band with a wide-field NIR camera at Okayama  Astrophysical
Observatory (Japan). The camera has an effective aperture of 0.91m.

Observations started from 12:08 UT on 11th Feburuary, 10.1 min after
the BAT trigger, to 13:22 UT.  The total exposure of 60 min was
successfully obtained.

In our co-add image, we did not find any new point source within the
enhanced XRT error circle (Goad et al., GCNC 12922) down to limiting
magnitude of  Ks= 15.5(Vega, S/N=3). The photometric calibration was
made against 2MASS field stars.

T0+[min]    MID-UT     T-EXP[min]      Ks
---------------------------------------------------
  +47.1     12:45        60.0       >15.5 (S/N=3)
---------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12924
SUBJECT: GRB 120211A: Swift-BAT refined analysis
DATE:    12/02/11 16:37:40 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU) 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), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), E. Sonbas (NASA/GSFC/Adiyaman U), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC)
(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 120211A (trigger #514586)
(Sonbas, et al., GCN Circ. 12920).  The BAT ground-calculated position is
RA, Dec = 87.781, -24.795 deg, which is 
   RA(J2000)  =  05h 51m 07.5s 
   Dec(J2000) = -24d 47' 43.6" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.
 
The mask-weighted light curve shows 2 or 3 overlapping peaks starting
at ~T-10 sec, peaking at ~T+42 sec, and ending at ~T+140 sec.
T90 (15-350 keV) is 61.7 +- 6.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.34 to T+64.10 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.50 +- 0.22.  The fluence in the 15-150 keV band is 8.1 +- 1.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+40.97 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/514586/BA/


GRB_name: GRB120211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12925
SUBJECT: GRB 120211A: MASTER early optical observations
DATE:    12/02/11 19:13:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

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

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

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

H.Levato, C.Mallamaci, C.Saffe
ICATE (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio), 
San Juan, San Juan University, Felix Aguilar Observatory, Argentina



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB120211A (SWIFT trigger 
514586; Sonbas et al. GCN 12920) 77 sec after GRB 
time at 2012-02-11 11:59:45.629 UT. On our first (20s exposure) set we 
haven't found optical transient  within SWIFT error-box (ra=05 51 00 
dec=-24 45 36 ).
The 5-sigma upper limit has been about 16.3 mag.

The message may be cited.


GRB_name: GRB120211A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12926
SUBJECT: GRB 120211A: Swift/UVOT Upper Limits
DATE:    12/02/11 19:42:47 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and E. Sonbas (NASA/GSFC/
Adiyaman_Univ.) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120211A
123 s after the BAT trigger (Sonbas et al., GCN Circ. 12920).
No optical afterglow consistent with the XRT enhanced position
(Goad et al., GCN Circ. 12922) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           123          273          147         >21.1
u_FC               281          531          246         >20.9
white              123         1528          392         >21.6
v                  612         1577          117         >19.7
b                  537         1503           97         >20.3
u                  281         1478          324         >20.9
w1                 662         1626          117         >20.2
m2                 637         1602          117         >20.1
w2                 588         1553          117         >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12927
SUBJECT: GRB 120211A: Swift-XRT refined Analysis
DATE:    12/02/12 00:11:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

V. Mangano (INAF-IASFPA), D.N. Burrows (PSU), J.A. Kennea (PSU), M.C.
Stroh (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU) and E. Sonbas report on behalf of the Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 120211A (Sonbas  et al. GCN
Circ. 12920), from 133 s to 13.2 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 12922).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.47 (+0.33, -0.22). At T+1267 s  the
decay flattens to an alpha of -0.14 (+0.20, -1.36) before breaking
again at T+11.0 ks to a final decay with index alpha=6.6 (+1.4, -4.1).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.29 (+0.21, -0.20). The
best-fitting absorption column is  6.5 (+6.5, -4.8) x 10^20 cm^-2,
consistent with the Galactic value of 1.7 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 5.4 x 10^-11 (5.8 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.5 (+6.5, -4.8) x 10^20 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.29 (+0.21, -0.20)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00514586.

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


GRB_name: GRB120211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12928
SUBJECT: GRB 120211A, optical observations
DATE:    12/02/12 05:01:42 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Vijay Bhatt and S. B. Pandey (ARIES Nainital, India, on
behalf
of larger Indian GRB collaboration).

The swift GRB 120211A (trigger =514586, Sonbas et al., GCN 12920) was
observed 
with the 104-cm telescope at ARIES Nainital. We took a sequence of images
starting at 13:31:26 UT on 11 Feb in R_c and I_c pass-bands with an
exposure
time of 300 sec each.

Photometry of the co-added R_c frame (300 sec x 4), in comparison to the
nearby
USNO- B1 stars, did not detect any new source within the XRT error-box down
to
a limiting magnitude of ~ 20 mag.

This massage may be cited.


GRB_name: GRB120211A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12929
SUBJECT: GRB 120211A: MITSuME Okayama and Ishigakijima Optical upper limits
DATE:    12/02/12 08:25:15 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, (OAO, NAOJ), H. Hanayama (IAO, NAOJ), K. Yanagisawa,
Y. Shimizu, H. Toda (OAO, NAOJ), T. Miyaji J. Watanabe, (IAO, 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 120211A (Sonbas et al., GCNC 12920)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory
and the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

We did not find any new point source within the enhanced XRT error
circle (Goad et al., GCNC 12922) in all the three bands.

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

Okayama Astrophysical Observatory:
The observation started on 012-02-11 11:59:56 UT (~1.5 min after
the burst).
T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.00444    12:04:52     540.0    >19.5  >19.5  >19.0
0.04267    12:59:55    6360.0    >20.3  >20.2  >19.7
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


Ishigakijima Astronomical Observatory:
The observation started on 2012-02-11 12:43:55 UT (~45 min after
the burst).
T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.04104    12:57:34    1260.0    >20.8  >20.5  >19.0
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120212A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12930
SUBJECT: GRB 120212A: Swift detection of a burst
DATE:    12/02/12 09:19:47 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), C. Guidorzi (U Ferrara),
A. Y. Lien (NASA/GSFC/ORAU), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 09:11:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120212A (trigger=514709).  Swift slewed to the burst location
at T+44 min due to an Earth limb observing constraint.
The BAT on-board calculated location is 
RA, Dec 43.105, -18.025 which is 
   RA(J2000) = 02h 52m 25s
   Dec(J2000) = -18d 01' 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 8 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+44.6
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.com). 
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.)

[GCN OPS NOTE(12feb12): Per author's request, the auto-generated
"slewed immediately" sentence was corrected to reflect the delayed slew.]


GRB_name: GRB120211A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12931
SUBJECT: GRB 120211A: GROND Upper limits
DATE:    12/02/12 09:30:37 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

J. Elliott, V. Sudilovsky and J. Greiner (all MPE Garching) report on
behalf of the GROND team:
  
We observed the field of GRB 120211A (Swift trigger 514586; Sonbas et
al., GCN 12920) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).
  
Observations started at 00:27 UT on 12 February 2012, 12.5 hours after the
GRB trigger. They were performed at an average seeing of 1.3" and at an
average airmass of 1.0. A total integration time of 90 minutes and 76
minutes was obtained in g'r'i'z' and JHK respectively.
  
We do not detect a source within the Swift-XRT error circle reported by
Goad et al. (GCN 12922) down to the following 3-sigma limits (all AB):
  
g' > 25.8
r' > 25.7
i' > 25.0
z' > 24.1
J  > 21.7
H  > 21.0
K  > 19.9
  
The given limits are derived based on calibrating the images against GROND
zeropoints and 2MASS field stars and are not corrected for the Galactic
foreground extinction corresponding to a reddening of E(B-V) = 0.03 in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB120212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12932
SUBJECT: GRB 120212A: Faulkes Telescope South afterglow candidate
DATE:    12/02/12 10:14:11 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), C.G. Mundell, F. Virgili, I.A. Steele
(LJMU), A. Melandri (INAF-OAB) report on behalf of a larger
collaboration:

The 2-m Faulkes Telescope South automatically began observing
GRB 120212A (Sonbas et al. GCN Circ. 12930) on February 2012,
09:25:18 UT corresponding to 14 minutes post burst
with BVRi' filters. We found the following uncatalogued source,

R.A. = 02:52:24.06
Dec = -18:01:14.2   (J2000)

with an uncertainty of about 1" with a magnitude of R=16.3 at
22 minutes, calibrated against USNOB-1 stars.
Presently, we cannot determine whether the source is fading.


GRB_name: GRB120212A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12933
SUBJECT: GRB 120212A: Swift/UVOT detection
DATE:    12/02/12 10:59:39 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and E. Sonbas (NASA/GSFC/Adiyaman Univ.) report on behalf of the Swift team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 2885 seconds after the BAT trigger. The source identified by 
Guidorzi et al. (GCN Circ. 12932) is detected in the rapidly available 
2.7'x2.7' sub-image at

RA(J2000) = 02:52:24.06 = 43.10025
DEC(J2000) = -18:01:14.1 = -18.02057

with a 90%-confidence error radius of about 0.76 arc sec. This position is 5.21
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.31 with a 1-sigma error of about 0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03. 


GRB_name: GRB120212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12934
SUBJECT: GRB 120212A: Swift-XRT observations
DATE:    12/02/12 11:03:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M. Perri (ASDC), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU) and G. Cusumano
(INAF-IASF PA) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 120212A at 09:59:24.6 UT,
2881.9 seconds after the BAT trigger. Using promptly downlinked data we
find a fading, uncatalogued X-ray source located at RA, Dec 43.10208,
-18.02125 which is equivalent to:
   RA(J2000)  = 02h 52m 24.50s
   Dec(J2000) = -18d 01' 16.5"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 16 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 (2.99 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 1.6
(+1.23/-1.13) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB120212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12935
SUBJECT: GRB 120212A: Kanata/HOWPol optical observation
DATE:    12/02/12 13:06:41 GMT
FROM:    Koji Kawabata at HASC,Hiroshima U  <kawabtkj@hiroshima-u.ac.jp>

K. S. Kawabata, H. Akitaya, M. Yamanaka, K. Takaki, T. Uehara, and
M. Yoshida (Hiroshima Univ.) report on behalf of Kanata team:

We performed a series of optical imaging polarimetry for the optical 
afterglow of GRB 120212A (Guidorzi et al.; GCN 12932) using HOWPol attached 
to the 1.5-m Kanata telescope at Higashi-Hiroshima Observatory, Japan. 

Our first exposure began at t=74 sec since Swift/BAT trigger (Sonbas 
et al.; GCN 12930), but the bright twilight sky shaded the afterglow 
until t=22 min. Our quick-look analysis indicates that Rc magnitude of 
the afterglow was 16.5 at t=23 min and faded to 17.6 at t=58 min. 
Further analysis is ongoing.


GRB_name: GRB120212A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12936
SUBJECT: GRB 120211A: MITSuME Okayama Ks-band Observation
DATE:    12/02/12 13:28:43 GMT
FROM:    Kenshi Yanagisawa at OAO/NAOJ  <yanagi@oao.nao.ac.jp>

Kenshi Yanagisawa, Daisuke Kuroda, Yasuhiro Shimizu, Kiichi Okita
(OAO/NAOJ), Michitoshi Yoshida (Hiroshima-U), Kouji Ohta(Kyoto-U),
and Nobuyuki Kawai(Tokyo Tech.) report on behalf of the MITSuME
collaboration:

We observed the field of GRB120212A (Sonbas et al., GCNC 12930,
Perri et al., GCNC 12934) in Ks-band with a wide-field NIR camera
at Okayama  Astrophysical Observatory (Japan). The camera has an
effective aperture of 0.91m.

Observations started from 10:01 UT on 12th February, 49.6 min after
the BAT trigger, to 10:44 UT.  The total exposure of 35 min was
successfully obtained.

In our co-add image, we found a single point source at
  R.A.(J2000) = 02:52:24.08
  DEC (J2000) = -18:01:14.8
with an uncertainty of of about 2 arcsec.
The position is consistent with the report by Guidorzi et al. (GCNC 12929)

We estimate the magnitude Ks = 15.13 +/- 0.19 (Vega).
The calibration was made against 2MASS field stars.

T0+[min]    MID-UT     T-EXP[min]    Ks
------------------------------------------------------------
  +71.2     10:22:     35.0          15.13 +/- 0.19 (Vega)
------------------------------------------------------------
T0+ : Elapsed time after the burst [min]
T-EXP: Total Exposure time [min]


GRB_name: GRB120212A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12937
SUBJECT: GRB 120212A: Enhanced Swift-XRT position
DATE:    12/02/12 13:59:38 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 2484 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 120212A, 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 = 43.10025, -18.02079 which is equivalent
to:

RA (J2000): 02h 52m 24.06s
Dec (J2000): -18d 01' 14.8"

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: GRB120212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12939
SUBJECT: GRB 120212A: Swift-BAT refined analysis
DATE:    12/02/12 16:14:22 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),
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), E. Sonbas (NASA/GSFC/Adiyaman U), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 120212A (trigger #514709)
(Sonbas, et al., GCN Circ. 12930).  The BAT ground-calculated position is
RA, Dec = 43.086, -18.043 deg, which is 
   RA(J2000)  =  02h 52m 20.6s 
   Dec(J2000) = -18d 02' 33.0" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 22%.
 
The mask-weighted light curve shows a single FRED pulse starting at ~T-0.7.
peaking at ~T+1, and ending at ~T+6 sec.
T90 (15-350 keV) is 5.52 +- 1.04 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.76 to T+6.09 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.05 +- 0.19.  The fluence in the 15-150 keV band is 5.1 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.02 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/514709/BA/


GRB_name: GRB120212A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12940
SUBJECT: GRB 120212A: Swift/UVOT Detection
DATE:    12/02/12 20:17:41 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and E. Sonbas (NASA/GSFC / Adiyaman_Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120212A
2885 s after the BAT trigger (Sonbas et al., GCN Circ. 12930).
A source consistent with the enhanced XRT position (Osborne et al.,
GCN Circ. 12937) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  02:52:24.05 =  43.10020 (deg.)
   Dec (J2000) = -18:01:14.2  = -18.02062 (deg.)
with an estimated uncertainty of 0.53 arc sec. (radius, 90% confidence).

The source is in the extended emission of a bright star (HD 17932) at
a distance
of 31", so the background was sampled at the same distance of that bright star
as the GRB is.

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

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

white             2885         3035          147         18.48 +/- 0.08
white             2885         5088          688         18.69 +/- 0.05
v                 2867         5379          286         18.12 +/- 0.12
b                 3249         4883          393         18.66 +/- 0.08
u                 3044         4678          393         18.47 +/- 0.10
w1                4274        11156          765        >21.0
m2                4069        10572         1082        >21.3
w2                3659         5294          393        >20.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12941
SUBJECT: GRB 120212A: NOT optical observation
DATE:    12/02/12 21:37:27 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), D. Malesani (DARK), G. Barisevicius (NOT), B. Nordstrom,
J. Andersen (NBI), P. Jakobsson (U. Iceland) report on
behalf of a larger collaboration:

We observed the field of GRB 120212A (Sonbas et al., GCN 12930) using
the 2.5m Nordic Optical Telescope (NOT) equipped with the ALFSOC
camera. We obtained 4x200s R-band images with a median time 19:52:24
UT on 2012-02-12, i.e., 10.7 hrs after the BAT trigger.

The optical afterglow of this burst (Guidorzi et al., GCN 12932;
Hoversten et al., GCN 12933; Kawabata et al., GCN 12935; Kuin et al.,
GCN 12940) was clearly detected in our stacked image and had R ~ 20.1
mag calibrated with nearby stars in the USNO B1 catalog.


GRB_name: GRB120213A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12942
SUBJECT: GRB 120213A: Swift detection of a burst
DATE:    12/02/13 00:40:47 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),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
M. C. Stroh (PSU) report on behalf of the Swift Team:

At 00:27:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120213A (trigger=514767).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 301.032, +65.397, which is 
   RA(J2000)  =  20h 04m 08s
   Dec(J2000) = +65d 23' 51"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single FRED pulse
with a duration of about 40 sec.  The peak count rate
was ~3200 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 00:28:09.0 UT, 49.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued, fading  X-ray source 
located at RA, Dec 301.0105, 65.4092 which is equivalent to:
   RA(J2000)  = +20h 04m 2.52s
   Dec(J2000) = +65d 24' 33.1"
with an uncertainty of 5.2 arcseconds (radius, 90% containment). This
location is 54 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. 

The initial flux in the 0.1 s image was 4.08e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 58 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
0.22. 

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: GRB120212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12943
SUBJECT: GRB 120212A: Swift-XRT refined Analysis
DATE:    12/02/13 00:45:14 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) and E. Sonbas (NASA/GSFC/Adiyaman Univ.)
report on behalf of the Swift-XRT team:

We have analysed 16 ks of XRT data for GRB 120212A (Sonbas  et al. GCN
Circ. 12930), from 2.9 ks to 44.6 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Osborne et al. (GCN. Circ 12937).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.25 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.11 (+0.16, -0.15). The
best-fitting absorption column is  7.5 (+3.3, -3.0) x 10^20 cm^-2, in
excess of the Galactic value of 3.0 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 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.5 (+3.3, -3.0) x 10^20 cm^-2
Galactic foreground: 3.0 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      2.11 (+0.16, -0.15)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00514709.

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


GRB_name: GRB120213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12944
SUBJECT: GRB 120213A: Prompt enhanced Swift-XRT position
DATE:    12/02/13 01:28:23 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:

Using  promptly downlinked XRT event data for GRB 120213A, we find an
enhanced XRT position of the afterglow: RA, Dec: 301.0128, 65.4110
which is equivalent to:
   RA (J2000)  = 20 04 03.07
   Dec (J2000) = +65 24 39.6
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/514767.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB120213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12945
SUBJECT: GRB 120213A: MASTER-NET early optical observations
DATE:    12/02/13 03:39:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

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

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

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

H.Levato, C.Mallamaci, C.Saffe
ICATE (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio), San 
Juan, San Juan University, Felix Aguilar Observatory, Argentina

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB120213A 26 sec. after  notice 
time and 49 sec. after GRB time at 2012-02-13 00:28:08.528 UT in two 
polarizations.
  On our first (10s exposure) set we haven't found optical transient 
within SWIFT  error-box (ra=20 04 07 dec=+65 23 59 r=0.050000).
The 5-sigma upper limit has been about 16.15mag
The message may be cited.


GRB_name: GRB120213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12946
SUBJECT: GRB 120213A: Swift-BAT refined analysis
DATE:    12/02/13 04:19:01 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),
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+841 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120213A (trigger #514767)
(Sakamoto, et al., GCN Circ. 12942).  The BAT ground-calculated position is
RA, Dec = 300.987, 65.413 deg, which is 
   RA(J2000)  =  20h 03m 56.8s 
   Dec(J2000) = +65d 24' 48.0" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a single FRED-like pulse starting
at ~T-7 sec, peaking at ~T+5 sec, and ending at ~T+75 sec.  T90 (15-350 keV) is
48.9 +- 12.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.31 to T+74.46 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.37 +- 0.09.  The fluence in the 15-150 keV band is 1.9 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+5.44 sec in the 15-150 keV band
is 1.7 +- 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/514767/BA/


GRB_name: GRB120212A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12947
SUBJECT: GRB 120212A:  MITSuME Ishigakijima Optical Observation
DATE:    12/02/13 04:58:31 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), 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 120212A (Sonbas et al., GCNC 12230)
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 2012-02-12 12:27:12 UT (~3.3 h after the burst).
We detected the previously reported afterglow (Guidorzi et al.,GCNC 12932;
Kawabata et al., GCNC 12935; Yanagisawa et al., GCNC 12936) in Rc and Ic
bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'    Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.14653    12:42:22    780.0    >20.2  18.7 0.2     18.4 0.3
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120213A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12948
SUBJECT: GRB 120213A: Enhanced Swift-XRT position
DATE:    12/02/13 06:29:22 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 2431 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 120213A, 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 = 301.01211, +65.41135 which is equivalent
to:

RA (J2000): 20h 04m 2.91s
Dec (J2000): +65d 24' 40.9"

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: GRB120212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12949
SUBJECT: GRB 120212A: GMG optical observation
DATE:    12/02/13 07:36:53 GMT
FROM:    Xiao-hong Zhao at Yunnan Obs  <zhaoxiaohong78@gmail.com>

 X.-H. Zhao (YNAO), D. Xu (WIS), J.-R. Mao (KASI/YNAO), J.-M. Bai 
(YNAO) report on behalf of a larger collaboration:

We observed the field of GRB 120212A (Sonbas et al., GCN 12930) with 2.4m Gao-Mei-Gu (GMG) telescope. Observations
started at 12:11:45 UT on 2012-02-12 (i.e., ~3 hrs after the burst) and 3x600s R-band images were obtained. The optical afterglow of this burst (Guidorzi et al., GCN 12932;
Hoversten et al., GCN 12933; Kawabata et al., GCN 12935; Kuin et al.,
GCN 12940; Xu et al., GCN 12941; Kuroda et al., GCN 12947) was detected. The results are as follows:

Comparison star: USNO-B Catalog 0720-0030593, R=18.31
UT(start time)    Mag.    Err.    Exposure time (second)
12:11:45.283      18.77   0.05      600
12:23:51.293      18.64   0.05      600
12:35:30.413      18.96   0.05      600
   
We thank the GMG staff, especially Ju-Jia Zhang, Jian-Quan He, and De-Qing Wang for
performing these observations.


GRB_name: GRB120212A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12950
SUBJECT: GRB 120212A: Fermi GBM observation
DATE:    12/02/13 09:19:34 GMT
FROM:    Arne Rau at MPE  <arau@mpe.mpg.de>

Arne Rau (MPE) reports on behalf of the Fermi GBM Team:

"At 09:11:23.50 UT on 12 February 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 120212A (trigger 350730685 / 120212383) which
was also detected by the Swift/BAT (Sonbas et al. 2012, GCN 12930).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 53 degrees.

The GBM light curve shows/consists of a single peak
with a duration (T90) of about 9.2 s (50-300 keV).
The time-averaged spectrum from T0-3.1 s to T0+6.1 s is
best fit by a simple power law function with index -1.83  0.06

The event fluence (10-1000 keV) in this time interval is
(1.407  0.120)E-07 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.64 s in the 10-1000 keV band
is 3.3  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: GRB120213A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12951
SUBJECT: GRB 120213A: Swift/UVOT Upper Limits
DATE:    12/02/13 12:35:20 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and T. Sakamoto (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120213A
59 s after the BAT trigger (Sakamoto et al., GCN Circ. 12942).
No optical afterglow consistent with the XRT position
(Beardmore et al., GCN Circ. 12948) is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            59          209          147         >19.8
u_FC               271          521          246         >19.7
white               59        12944         1454         >21.6
v                  602         6546          294         >20.4
b                  527        12032         1219         >20.5
u                  271         7161          717         >20.6
w1                 653         6956          471         >19.8
m2                6551         6751          197         >19.8
w2                 578        13010          332         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.22 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12952
SUBJECT: GRB 120213A: Swift-XRT refined Analysis
DATE:    12/02/13 12:40:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), O.M. Littlejohns (U.
Leicester), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), G.
Stratta (ASDC) and T. Sakamoto report on behalf of the Swift-XRT team:

We have analysed 6.5 ks of XRT data for GRB 120213A (Sakamoto  et al.
GCN Circ. 12942), from 53 s to 22.8 ks after the  BAT trigger. The data
comprise 886 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 12944).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=3.02 (+0.19, -0.18).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.28 (+/-0.07). The
best-fitting absorption column is  3.52 (+0.15, -0.14) x 10^21 cm^-2,
in excess of the Galactic value of 1.0 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.22 (+/-0.15) and a
best-fitting absorption column of 1.7 (+/-0.4) x 10^21 cm^-2. 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:      1.7 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 1.0 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      2.22 (+/-0.15)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00514767.

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


GRB_name: GRB120211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12953
SUBJECT: GRB 120211A : LOAO optical observations
DATE:    12/02/13 15:45:18 GMT
FROM:    Minsung Jang at Seoul National U  <rigel103@snu.ac.kr>

Jang, M., Im, M. (SNU), & Urata, Y. (NCU)

We observed GRB 120211A (Sonbas et al., GCN 12920) in SDSS i,z-bands with a 1 m telescope at Mt. Lemmon, Arizona, U.S.
The obsevation started at 04:03:00 2012-02-12 UT, ~ 17 hours after the burst alert.
We took 4 frames for each filter alternatively with the exposure time 300s.
No afterglow candidate was found in the enhanced XRT position (Goad et al., GCN12922) in stacked images of both i and z.

We thank the LOAO operator, J. Yoon for this observation. 


GRB_name: GRB120215A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12954
SUBJECT: GRB 120215A: Swift detection of a burst
DATE:    12/02/15 00:51:33 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. A. Hoversten (PSU), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC),
A. Y. Lien (NASA/GSFC/ORAU), V. Mangano (INAF-IASFPA),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), T. N. Ukwatta (MSU)
and B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 00:41:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120215A (trigger=515015).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 30.032, +8.792 which is 
   RA(J2000) = 02h 00m 08s
   Dec(J2000) = +08d 47' 30"
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 15 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 00:43:01.8 UT, 106.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 30.04753, 8.80220 which is
equivalent to:
   RA(J2000)  = 02h 00m 11.41s
   Dec(J2000) = +08d 48' 07.9"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 66 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 5.40
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 110 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
0.08. 

Burst Advocate for this burst is E. A. Hoversten (hoversten 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: GRB120215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12955
SUBJECT: GRB 120215A: Swift-BAT refined analysis
DATE:    12/02/15 05:06:22 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), E. A. Hoversten (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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120215A (trigger #515015)
(Hoversten, et al., GCN Circ. 12954).  The BAT ground-calculated position is
RA, Dec = 30.057, 8.790 deg, which is 
   RA(J2000)  =  02h 00m 13.7s 
   Dec(J2000) = +08d 47' 25.4" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.
 
The mask-weighted light curve shows 2 or 3 overlapping peaks starting at ~T-2 sec,
peaking at ~T+4 sec, and ending at ~T+35 sec.  T90 (15-350 keV) is 26.5 +- 8.9 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.36 to T+29.27 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.62 +- 0.22.  The fluence in the 15-150 keV band is 4.0 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+4.87 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/515015/BA/


GRB_name: GRB120215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12956
SUBJECT: Skynet/PROMPT observations of GRB120215A
DATE:    12/02/15 06:54:17 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, J. Haislip, K. Ivarsen, D. Reichart, J. Moore, M. Nysewander, 
A. Trotter, R. Egger, A. Foster, A. Oza, H. T. Cromartie, E. Speckhard, and 
J. A. Crain report:

Skynet observed the field of GRB 120215A with the PROMPT telescopes located 
at CTIO in Chile. Observations in B, R, and I began at 00:42:24 UT, 69 
seconds after the burst. While no source is detected in early images, 
stacks of later images do find an optical source of roughly 20th magnitude 
consistent with the XRT position reported by Hoversten et. al. (GCN 12954).


mean-t #exp  explen filt mag +(1sig) -(1sig)
19.27m 4 80s I 19.095 0.287 0.228
20.88m  6 80s B 20.320 0.361 0.274

Analysis is ongoing, although no further observations are planned as the 
field has set in Chile.

A preliminary light curve can be found at: 
http://skynet.unc.edu/grb/grb120215a.png


GRB_name: GRB120215A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12957
SUBJECT: GRB 120215A: Enhanced Swift-XRT position
DATE:    12/02/15 08:31:38 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 1619 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 120215A, 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 = 30.04752, +8.80178 which is equivalent
to:

RA (J2000): 02h 00m 11.41s
Dec (J2000): +08d 48' 06.4"

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: GRB120215A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12959
SUBJECT: GRB 120215A: Swift-XRT refined Analysis
DATE:    12/02/15 12:51:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.C. Stroh (PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester), O.M.
Littlejohns (U. Leicester), J.P. Osborne (U. Leicester), B. Sbarufatti
(INAF-OAB/PSU), G. Stratta (ASDC), P. D'Avanzo (INAF-OAB), J.A. Kennea
(PSU) and E.A. Hoversten report on behalf of the Swift-XRT team:

We have analysed 9.4 ks of XRT data for GRB 120215A (Hoversten et al.
GCN Circ. 12954), from 110 s to 19.3 ks after the  BAT trigger. The
data comprise 36 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 12957).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.38 (+0.26, -0.23), followed by a break at T+699 s to
an alpha of -0.28 (+0.15, -0.18).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.10 (+0.24, -0.22). The
best-fitting absorption column is  8.4 (+5.1, -3.0) x 10^20 cm^-2,
consistent with the Galactic value of 5.4 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 3.4 x 10^-11 (4.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.4 (+5.1, -3.0) x 10^20 cm^-2
Galactic foreground: 5.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.10 (+0.24, -0.22)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00515015.

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


GRB_name: GRB120215A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12960
SUBJECT: GRB 120215A: MITSuME Okayama Optical upper limits
DATE:    12/02/15 16:43:39 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 120215A (Hoversten et al., GCNC 12954)
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 2012-02-15 10:16:42 UT (9.6 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Evans et al., GCNC 12957) in all the three bands.
We also could not detect the previously reported afterglow (LaCluyze et al.,
GCNC 12956).


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
------------------------------------------------------
0.40591    10:25:46    1140.0   >19.1  >19.0  >18.5
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120215A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12961
SUBJECT: GRB 120215A: Swift/UVOT Upper Limits
DATE:    12/02/15 17:30:15 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120215A
110 s after the BAT trigger (Hoversten et al., GCN Circ. 12954).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 12957) is detected in the initial UVOT  
exposures.
The optical source reported by LaCluyze et al. (GCN Circ. 12956) was not
seen in the first orbit of observations, however our upper limits are  
higher than
their detections. Preliminary 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)  
for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           110          260          147         >20.5
u_FC               322          572          246         >20.3
white              110          795          186         >20.8
v                  652          672           19         >17.6
b                  578          771           39         >19.2
u                  322          746          265         >20.3
w1                 702          721           19         >18.9
m2                 677          869           39         >19.6

The magnitudes in the table 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: GRB120218A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12962
SUBJECT: GRB 120218A: Swift detection of a burst
DATE:    12/02/18 00:59:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. A. Wolf (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), C. B. Markwardt (NASA/GSFC), D. M. Palmer (LANL),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/PSU),
C. A. Swenson (PSU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report
on behalf of the Swift Team:

At 00:49:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120218A (trigger=515277).  Swift did not slew due to a 
Sun constraint. The BAT on-board calculated location is 
RA, Dec 319.758, -25.450, which is 
   RA(J2000) = 21h 19m 02s
   Dec(J2000) = -25d 27' 00"
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 30 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 19:14 UT on 2012 March 20. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is C. A. Wolf (cwolf AT swift.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: GRB120218A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12963
SUBJECT: GRB 120218A: Swift-BAT refined analysis
DATE:    12/02/18 14:51:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), 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), D. M. Palmer (LANL),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU), C. A. Wolf (PSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+303 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 120218A (trigger #515277)
(Wolf, et al., GCN Circ. 12962).  The BAT ground-calculated position is
RA, Dec = 319.7641, -25.4626 deg which is
   RA(J2000)  =  21h 19m 03.4s
   Dec(J2000) = -25d 27' 45.4"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 4%.

The mask-weighted light curve shows 3 or 4 overlapping peaks starting
at ~T-28 sec, with the highest peak is at ~T+3 sec, and ending at ~T+15 sec.
T90 (15-350 keV) is 27.5 +- 1.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-20.6 to T+8.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.75 +- 0.11.  The fluence in the 15-150 keV band is 5.3 +- 0.4 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.33 sec in the 15-150 keV band
is 9.1 +- 1.2 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/515277/BA/


GRB_name: GRB120219A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12964
SUBJECT: GRB 120219A: Swift detection of a burst
DATE:    12/02/19 14:40:43 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. A. Swenson (PSU), D. N. Burrows (PSU), N. Gehrels (NASA/GSFC),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), C. J. Saxton (UCL-MSSL),
B. Sbarufatti (INAF-OAB/PSU), G. Tagliaferri (INAF-OAB) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 14:30:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120219A (trigger=515375).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 129.793, +51.025 which is 
   RA(J2000) = 08h 39m 10s
   Dec(J2000) = +51d 01' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for an image trigger, there is no
obvious variation in the immediately available lightcurve. 

The XRT began observing the field at 14:32:16.4 UT, 128.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 129.79218, 51.03194 which
is equivalent to:
   RA(J2000)  = 08h 39m 10.12s
   Dec(J2000) = +51d 01' 55.0"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 25 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 3.48
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 2.37e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 139 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
0.03. 

Burst Advocate for this burst is C. A. Swenson (cswenson 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: GRB120219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12965
SUBJECT: GRB 120219A: MASTER-NET prompt and early optical observations 
DATE:    12/02/19 17:14:39 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


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


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

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

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

H.Levato, C.Mallamaci, C.Saffe
ICATE (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio), San 
Juan, San Juan University, Felix Aguilar Observatory, Argentina

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the  GRB120219A (Swenson et
al., GCN Circ 12964) 22 sec s after notice
time and 105 sec after GRB time at 2012-02-19 14:31:54 UT. On our
first (20s exposure, two "ra" and "dec"  polarisation
orientations) set we haven't found optical
transient  within SWIFT XRT error-box.
The 5-sigma upper limit in two polarizations has been about 17.3mag and
17.0 correspondingly.


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kourovka (Ural)  was pointed to the  GRB120219A (Swenson et 
al., GCN Circ 12964) 26 sec s after notice
time and 109 sec after GRB time at 2012-02-19 14:31:58 UT. On our
first (20s exposure, diagonal polarisation) set we haven't found optical
transient  within  SWIFT XRT error-box.
The 5-sigma upper limit has been about 17.0 mag


One   MASTER Very Wide Field Camera located at Tunka
(D=68 mm, 420 square degrees, 11 Mpx) was observed  GRB error box
with 5 s exposure  befoure, during and after GRB Trigger Time
without time gap between images.

Our unfiltered images are calibrated relative to Tycho stars (V).
The magnitude limit of the each emage is  11.5 m at the edge of FOW.
We do not detect OT.
But we need the duration and beginning time of the GRB.
The redaction is continuated.

The message may be cited.


GRB_name: GRB120219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12966
SUBJECT: GRB120219A: TNT optical afterglow candidates
DATE:    12/02/19 17:28:20 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB120219A (Swenso et al. GCN 12964 ) 
with Xinglong TNT telescope at 14:32:15 (UT), 127 sec after 
the burst. A serveral white and  R-band were obtained.

After combining 11*300s R-band images, a new marginal source was 
found within the errorbox  of X-ray counterpart  ( Swenso et al. GCN 12964). 
Its coordinates ( RA and Dec ) are  08:39:09.55 51:01:56.5  (J2000)
with an uncertainty of  about 1 arcsecond.
The brightness of the source is estimated to be about 
21.5 +/- 0.3 mag relatively to  USNO B1.0 R2 mag 
at the mean time of 37 min 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/

We thank ChunLan Lu for performing these observations.


GRB_name: GRB120219A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12967
SUBJECT: GRB 120219A: Enhanced Swift-XRT position
DATE:    12/02/19 23:12:00 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 1088 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120219A, 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 = 129.79026, +51.03174 which is equivalent
to:

RA (J2000): 08h 39m 9.66s
Dec (J2000): +51d 01' 54.2"

with an uncertainty of 1.6 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: GRB120219A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12968
SUBJECT: GRB 120219A: Swift-BAT refined analysis
DATE:    12/02/20 02:31:54 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),
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), C. A. Swenson (PSU),
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 recent telemetry downlinks,
we report further analysis of BAT GRB 120219A (trigger #515375)
(Swenson, et al., GCN Circ. 12964).  The BAT ground-calculated position is
RA, Dec = 129.862, 51.006 deg, which is 
   RA(J2000)  =  08h 39m 26.8s 
   Dec(J2000) = +51d 00' 21.4" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.
 
The mask-weighted light curve shows two slightly overlapping peaks starting
at ~T-15 sec, peaking at T+0 and T+70 sec, and returning to baseline
at ~T+140 sec.  T90 (15-350 keV) is 90.5 +- 10.9 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-7.83 to T+90.06 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index -0.60 +- 1.69, 
and Epeak of 51.6 +- 14.2 keV (chi squared 54.9 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.4 +- 1.4 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T-2.30 sec in the 15-150 keV band is
0.3 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.56 +- 0.23 (chi squared 63.9 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/515375/BA/


GRB_name: GRB120219A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12969
SUBJECT: GRB 120219A: MITSuME Okayama Optical upper limits
DATE:    12/02/20 02:45:29 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 120219A (Swenson et al., GCNC 12964)
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 2012-02-19 14:31:47 UT (~99 sec after the burst)
We did not find any new point source within the enhanced XRT circle
(Goad et al., GCNC 12967) in all the three bands.
We also could not detect the previously reported afterglow (Xin et al.,
GCNC 12966).


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
------------------------------------------------------
0.00458    14:36:44     540.0   >20.5  >20.4  >19.6
0.04314    15:32:16    6300.0   >21.4  >21.2  >20.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120219A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12970
SUBJECT: GRB 120219A: Swift/UVOT Upper Limits
DATE:    12/02/20 04:01:47 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120219A
139 s after the BAT trigger (Swenson et al., GCN Circ. 12964).
No optical afterglow consistent with the XRT position (Goad et al.,
GCN Circ. 12967) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           139          289          147>21.2
u_FC               298          547          246>20.5
white              139          598          167>21.2
v                 3846         4045          197>19.3
b                  553          573           19>19.6
u                  298         4614          397>20.7
w1                4255         4455          197>21.5
m2                4050         4250          197>19.9
w2                 603          623           19>19.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB120219A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12971
SUBJECT: GRB 120219A: Swift-XRT refined Analysis
DATE:    12/02/20 07:40:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

D.N. Burrows (PSU), O.M. Littlejohns (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), G. Stratta (ASDC), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), J.A. Kennea (PSU), M.C. Stroh (PSU) and
C.A. Swenson report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 120219A (Swenson  et al.
GCN Circ. 12964), from 118 s to 51.3 ks after the  BAT trigger. The
data comprise 667 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 12967).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.25 (+0.11, -0.10), followed by a break at T+444 s to
an alpha of 1.64 (+0.15, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.25 (+0.16, -0.14). The
best-fitting absorption column is  2.25 (+0.26, -0.24) x 10^21 cm^-2,
in excess of the Galactic value of 3.5 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.11 (+0.14, -0.11)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (3.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+3.4, -0) x 10^20 cm^-2
Galactic foreground: 3.5 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.11 (+0.14, -0.11)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00515375.

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


GRB_name: GRB120215A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12972
SUBJECT: GRB 120215A: MITSuME Akeno Optical upper limits
DATE:    12/02/20 08:16:23 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

Y. Saito, Y. Aoki, S. Song, M. Hayashi, K. Kawakami, K. Tokoyoda,
R. Usui, Y. Yatsu, and N. Kawai (Tokyo Tech)  report on behalf of
the MITSuME collaboration:

We observed GRB 120219A (Swenson et al., GCNC 12964) with the
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME
50 cm telescope of Akeno Observatory, Yamanashi, Japan.

We started the observation 134 sec after the BAT trigger
from 2012-02-19 14:32:22 UT.  And we did not find any new point source
within the XRT error circle (Goad et al., GCNC 12967) in the three bands.
The results of photometry (3sigma upper limits) are listed below.

The photon flux were calibrated against GSC2.3 catalog.

T0+[sec]      MID-UT     T-EXP[sec]       g'              Rc           Ic
----------------------------------------------------------------------------------------
   275      14:34:43       240         > 19.5        > 19.5       > 18.2
 12005     17:54:41     18060         > 21.5        > 21.4       > 20.5
----------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB120219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12973
SUBJECT: GRB120219A: Keck Observations
DATE:    12/02/20 12:22:23 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley and E. Bellm (Caltech) report:

We imaged the location of GRB 120219A (Swenson et al., GCN 12964) with 
the Keck I telescope (+ LRIS) on 2012-02-20 (UT) between 10:22-10:41 UT. 
  Observations suffered from strong attenuation due to clouds and poor 
seeing (>2 arcsec).  In a stack of our two deepest individual 200 second 
R-band frames (at 10:27 and 10:32) UT, we detect no source to a limiting 
magnitude of R > 24.0 mag.  The afterglow is also not detected in our 
g-band or I-band images.  If the reported object of Xin et al. (GCN 
12966) represents a real source, this apparent fading confirms it as the 
afterglow of GRB 120219A.


GRB_name: GRB120219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12974
SUBJECT: GRB 120219A, optical observations
DATE:    12/02/20 14:36:12 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Vijay Kumar Bhatt and S. B. Pandey (ARIES, Nainital, India, 
on behalf of larger Indian GRB collaboration).

We observed the Swift GRB120219A (trigger=515375, Swenson et al. GCN 12964)
with the 104cm telescope at ARIES Nainital starting ~ 22 minutes after the 
burst i.e. at 14:52:46 UT and onwards. Several images were taken in  R_c 
and I_c pass-bands.

In the co-added R_c frame (200sec + 2*300sec), we did not detect the 
optical transient reported by Xin et al. (GCN 12966) down to a 
limiting magnitude of ~ 20.5 mag. The photometry was performed 
in comparison to nearby USNO- B1 stars.

This massage may be cited.

[GCN OPS NOTE(20feb12): Per author's request, the typo n the Subject line
was corrected (110219A -- > 120219A).]


GRB_name: GRB120219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12976
SUBJECT: GRB 120219A: 1.23m CAHA optical observations
DATE:    12/02/20 19:16:49 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), P. Kubanek (IAA-CSIC & U. Valencia), R. Sanchez-Ramirez (IAA-CSIC), report on behalf of a larger collaboration:

"We imaged the field of the Swift GRB 120219A (Swenson et al., GCN Circ. 12964) with the 1.23m Calar Alto telescope. The observations were carried out in the R and V-bands on Feb 19.89829--20.03333 UT and 20.03396--20.15466 UT, respectively (7.1--13.2 hours post burst).  We detect a faint source at RA(J2000)=08:39:09.61 Dec(J2000)=+51:01:55.5 present in both bands (with a +/-0.9" error in each coordinate), consistent with the enhanced XRT error circle (Goad et al., GCN Circ. 12967) and the candidate reported by Xin et al. (GCN Circ. 12966). Preliminary photometry yields an R-band magnitude of ~22.8 with respect to the USNO B1.0 catalogue."


GRB_name: GRB120219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12977
SUBJECT: GRB 120219A: MASTER prompt and early optical limit and OT discussion
DATE:    12/02/21 09:04:00 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

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

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

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

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

MASTER II  robotic telescope (Global MASTER-Net: 
http://observ.pereplet.ru)
located in Tunka and Ural  was pointed to the  GRB120219A (Swenson et
al., GCN Circ 12964; Ivanov et al., GCN Circ 12965).

One   MASTER Very Wide Field Camera located at Tunka
(D=68 mm, 420 square degrees, 11 Mpx) was observed  GRB error box
with 5 s exposure  before, during and after GRB Trigger Time
without time gap between images.
Our unfiltered images are calibrated relative to Tycho stars (V).

We haven't found optical transient  within enhanced SWIFT XRT error-box 
(Goad et al., GCN Circ 12967).

Our results:

T_start-T_trig    T_mean-T_trig   Limit  Coadd  Telescope   Filter   Site
      (s)                   (s)

      -9                -6.5       11.5     No    VWFC (E)   Unfilt   Tunka
      -4                -1.5       11.5     No    VWFC (E)   Unfilt   Tunka
      -9                33.5       13.0     18    VWFC (E)   Unfilt   Tunka
     105                115        17.3     No   MASTERII(E)    P|    Tunka
     105                115        17.0     No   MASTERII(W)    P-    Tunka
     105                772        19.5     22   MASTERII(E+W)Unfilt  Tunka
     109                119        17.0     No   MASTERII(W)    P/     Ural
     109                552        19.0     11   MASTERII(W)    P/     Ural

There is some marginal object at Xin et al.(GCN 12966) OT candidate 
position in Ural and Tunka added images with ~19 and ~20 mag 
correspondingly (see images). The some marginal object appear on Very Wide 
Field Camera at -1.5 s (mean time) and +3.5s images with 12 mag (pixel is equal 22"). 
But the signal/noice level is 2-3 sigma and we can not confirm or reject 
this candidate.

The images and video are available at 
http://master.sai.msu.ru/static/GRB120219A/GRB120219A.html .

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).




The message may be cited.


GRB_name: GRB120219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12978
SUBJECT: GRB 1202019A: optical observation in Mondy observatory
DATE:    12/02/21 15:05:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.Volnova (SAI MSU),  E. Klunko (ISTP), A. Pozanenko (IKI) on behalf of 
larger GRB follow up  collaboration report:

We observed the field of GRB 120219A (Swenson et al., GCN 12964) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Feb. 19 between (UT) 
15:14:55 - 16:25:47  in R filter under mean seeing (FWHM) of 2.2". In a 
combined image we marginally detect the afterglow (Xin et al., GCN 12966; 
Gorosabel et al., GCN 12976). Preliminary photometry is based on the 
USNO-B1.0 field stars:

T0+,        Filter,  Exposure,   OT,
(mid, d)             (s)
0.05571    R     70 x 60      22.5 +/-0.3 


GRB_name: GRB120215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12979
SUBJECT: GRB_120215, the_review_of_the_sky_area_in_plate_archives
DATE:    12/02/22 14:14:53 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V.Golovnya (Main Astro Obs, Kyiv)
report: 
We have undertaken the review of the sky area in vicinity of 
GRB 120215 (P.A. Evans et al. GCN Circ.12957) 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 and Epson Expression 10000XL flatbed 
scanners and have been placed into Golosiiv Plate Archive 
database DBGPA with open access to them.
  The list of plates is given in the table:
YYYYMMDD/TimeUT Plates Exp.  LimMag Star USNOA2 
19881013/222653 0075 16.0 15.80 0975-00450083
19901011/221607 1722A 22.0 16.10 0975-00449483
19901013/222637 1727 16.0 16.10 0975-00449483
19911010/224551 1867 18.0 15.05 0975-00448648
19911011/223546 1875 16.0 15.80 0975-00450083
19911102/204815 1894 18.0 15.80 0975-00450083
Plates: the plates archive identifier of DWA (D/F=400/2000,
GUA040C M=103"/mm) of the Ukrainian NAS Main Astro obs.
        (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 26 minutes area around 
       the location given in P.A. Evans et al. GCN Circ.12957:
       RA(J2000) = 02h 00m 11.41s, Dec(J2000) = +08d 48'06.4"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 26x26 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/120215A/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: GRB120224A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12980
SUBJECT: GRB 120224A: Swift detection of a burst
DATE:    12/02/24 04:51:10 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. J. Saxton (UCL-MSSL), J. R. Cummings (NASA/UMBC),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
S. R. Oates (UCL-MSSL), K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), C. A. Swenson (PSU)
and T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 04:39:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120224A (trigger=515976).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 40.975, -17.793 which is 
   RA(J2000) = 02h 43m 54s
   Dec(J2000) = -17d 47' 32"
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 ~1200 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 04:41:45.6 UT, 109.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 40.94380, -17.75959 which is equivalent
to:
   RA(J2000)  = 02h 43m 46.51s
   Dec(J2000) = -17d 45' 34.5"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 160 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 (2.45 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.6
(+4.34/-3.51) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 114 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 0.04. 

Burst Advocate for this burst is C. J. Saxton (cjs2 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: GRB120224A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12981
SUBJECT: GRB 120224A: Enhanced Swift-XRT position
DATE:    12/02/24 08:48:09 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 1421 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120224A, 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 = 40.94221, -17.76130 which is equivalent
to:

RA (J2000): 02h 43m 46.13s
Dec (J2000): -17d 45' 40.7"

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: GRB120224A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12982
SUBJECT: GRB 120224A: FTN optical observations
DATE:    12/02/24 10:11:35 GMT
FROM:    Jure Japelj at U. of Ljubljana,Slovenia  <jure.japelj@fmf.uni-lj.si>

J. Japelj, D. Kopac (U. Ljubljana) and C. Guidorzi (U. Ferrara) report on
behalf of a larger collaboration:

The 2-m Faulkes Telescope North automatically began observing GRB 120224A
(Saxton et al., GCN 12980), starting at 04:44:40 UT on 2012 February 24.
We do not detect any optical counterpart inside the enhanced Swift-XRT
error circle (Osborne et al., GCN 12981) down to the following limiting
magnitudes:

Mid time from   Exp    Filter   Mag limit
trigger (min)   (sec)
-------------------------------------------
44.5            600    R        > 19.3
39.3            480    i'       > 18.6
-------------------------------------------

The magnitudes are calibrated against nearby USNO-B1.0 stars.


GRB_name: GRB120224A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12983
SUBJECT: GRB 120224A: Swift-BAT refined analysis
DATE:    12/02/24 13:26:41 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),
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), C. J. Saxton (UCL-MSSL), 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+326 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120224A (trigger #515976)
(Saxton, et al., GCN Circ. 12980).  The BAT ground-calculated position is
RA, Dec = 40.937, -17.779 deg, which is 
   RA(J2000)  =  02h 43m 44.8s 
   Dec(J2000) = -17d 46' 42.6" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 29%.
 
The mask-weighted light curve shows two peaks, the first starting
at ~T-20 sec, peaking at ~T-6 sec.  The second (and stronger peak) 
starts at ~T-3 sec, peaks at ~T+1 sec, and ends at ~T+13 sec.
T90 (15-350 keV) is 8.13 +- 1.99 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.08 to T+8.26 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.25 +- 0.36.  The fluence in the 15-150 keV band is 2.4 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.24 sec in the 15-150 keV band
is 0.9 +- 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/515976/BA/


GRB_name: GRB120224A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12984
SUBJECT: GRB 120224A: Swift/UVOT Upper Limits
DATE:    12/02/24 16:39:22 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 120224A
115 s after the BAT trigger (Saxton et al., GCN Circ. 12980).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al., GCN Circ. 12981) is detected in the initial UVOT
exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           115          264          147         >20.7
u_FC               273          522          246         >20.5
white              115         1547          392         >21.2
v                  602         1424           97         >19.4
b                  529         1522           97         >20.2
u                  273         1497          304         >20.4
w1                1107         1127           19         >19.6
m2                1254         1448           39         >19.8

The magnitudes in the table 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: GRB120224A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12986
SUBJECT: GRB 120224A: Swift-XRT refined Analysis
DATE:    12/02/24 19:51:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani (U.
Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. Maselli 
(INAF-IASFPA), J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU)
and C.J. Saxton report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 120224A (Saxton  et al. GCN
Circ. 12980), from 95 s to 34.0 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 enhanced
XRT position for this burst was given by Osborne et al. (GCN. Circ
12981).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.99 (+/-0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.22 (+0.16, -0.15). The
best-fitting absorption column is  3.0 (+/-0.5) 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 3.7 x 10^-11 (6.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.0 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 9.3 sigma
Photon index:      2.22 (+0.16, -0.15)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00515976.

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


