# GCN_circulars

GRB_name: GRB111005A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12419
SUBJECT: GRB 111005A:  EVLA Observations
DATE:    11/10/06 18:22:27 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger, A. M. Soderberg (Harvard), and D. A. Frail 
(NRAO) report:

"We observed the BAT error circle of GRB 111005A (GCN #12415) with the 
EVLA on 2011 October 5.98 UT (15.4 hours after the burst) at a frequency 
of 5 GHz.  We detect two sources within the error circle at the 
following coordinates (J2000):

EVLA-S1:
RA = 14:53:07.78
DEC = -19:44:12.2

EVLA-S2:
RA 14:53:11.64
DEC -19:43:30.8

EVLA-S1 coincides with the disk of the z=0.01326 galaxy ESO 580-49 
(Levan et al. GCN #12414), and is located about 2.5 arcsec from its 
bulge.  It is therefore a possible counterpart of GRB 111005A.  EVLA-S2 
is detected in the NVSS survey with a 1.4 GHz flux density of 5.7 mJy 
and is thus unlikely to be related to GRB 111005A.

Additional observations to check for variability of EVLA-S1 are in 
progress."


GRB_name: GRB111005A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12420
SUBJECT: GRB 111005A : miniTAO/ANIR NIR observations
DATE:    11/10/07 02:01:12 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

K. Motohara, M. Konishi, T. Tanabe, T. Kamizuka, K. Tateuchi,
T. Minezaki, and Y. Yoshii (University of Tokyo),
report on behalf of the TAO project team

We observed the field of GRB 111005A (Saxton et al., GCN 12413)
in Ks and J with the near-infrared camera ANIR mounted on the
miniTAO 1.0m telescope at the University of Tokyo Atacama
Observatory, located on the summit of Co. Chajnantor (5640m
altitude) in the northern Chile.

Observations started just after the sunset, at 22:59 UT in Ks
and at 23:17 UT in J, approximately 15 hours after the burst.
Exposure time is 720sec in Ks and 600sec in J, which result in
the 5 sigma limiting magnitude (AB system) of J < 19.4 and
Ks < 19.1 (3" aperture). All the magnitudes are calibrated
against the 2MASS field stars. The final seeing size is 1.2" in
Ks and 1.5" in J.

We find no new sources compared to the 2MASS catalog, consistent
with the report by Levan et al. (GCN 12416) and Nardini et al.
(GCN 12417). In addition, no point source is detected at the
position of the 5GHz source EVLA-S1 (Zauderer et al., GCN 12419).


GRB_name: GRB111005A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12421
SUBJECT: GRB 111005A: ATCA radio upper limit
DATE:    11/10/07 12:15:26 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), M. Michalowski (U. Edinburgh), J. Stevens, P. Edwards, D.
Bock, B. Hiscock, R. Wark (CSIRO) report on behalf of a larger
collaboration:

We observed the BAT field of GRB 111005A (Saxton et al., GCN 12413)
with the Australia Telescope Compact Array (ATCA), starting at 05:13
UT, 7th Oct. 2011 (i.e., 45.1 hours after the burst) at frequencies of
5.5/9 GHz.

The source of NVSS 145310-194331, or EVLA-S2 by Zauderer et al. (GCN
12419), in the field was clearly detected in our 5.5GHz image. But no
radio source was detected near or in the local galaxy, ESO 580-49 at
z=0.013 (Levan et al., GCN 12414), to a 3sigma upper limit of ~114
microJy at 5.5GHz.

Comparison with the earlier detection of a radio transient, EVLA-S1,
in the galaxy (GCN 12419; and typical EVLA 3sigma upper limit of
~60-100 microJy from previous GRB events) reveals that probably this
radio transient has been decaying over the past ~2 days.

Further ATCA observations of the field are underway.


GRB_name: GRB111005A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12422
SUBJECT: GRB 111005A: ATCA 18 GHz detection
DATE:    11/10/08 20:20:14 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

M. Michalowski (U. Edinburgh), D. Xu (WIS), J. Stevens, P. Edwards, D.
Bock, B. Hiscock, R. Wark (CSIRO) report:

We continued to observe the BAT field of GRB 111005A (Saxton et al.,
GCN 12413) with the Australia Telescope Compact Array (ATCA), starting
at 07:04 UT, 8th Oct. 2011 (i.e., 71 hours after the burst) at the
frequency of 18 GHz.

We detected a radio source with the coordinates

RA(J2000) = 14:53:07.74
Dec(J2000) = -19:44:08.9

coincident with the disk of the local galaxy ESO 580-49 at z=0.013
(M_B ~ -18.6 mag).

Together with our earlier upper limit at this position at 5.5 GHz (Xu
et al., GCN 12421), it would be difficult to ascribe the 18 GHz
detection to the contribution of the ESO 580-49 galaxy itself as this
would require the galaxy spectrum to fall with decreasing radio
frequency. Hence, we suggest the above source to be the radio
afterglow of GRB 111005A and thus an associated supernova is expected.

Our 18 GHz position is ~3.4 arcsec away from the 5 GHz source EVLA-S1
reported by Zauderer et al., (GCN 12419), well within the positional
uncertainties of the ATCA observation.

Further observations are planned.


GRB_name: GRB111008A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12423
SUBJECT: GRB 111008A: Swift detection of a burst
DATE:    11/10/08 22:22:55 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. J. Saxton (UCL-MSSL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), S. T. Holland (CRESST/USRA/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), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL) and C. A. Swenson (PSU)
report on behalf of the Swift Team:

At 22:12:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111008A (trigger=505054).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 60.454, -32.689, which is 
   RA(J2000)  =  04h 01m 49s
   Dec(J2000) = -32d 41' 18"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows 3 sets of peaks
with a total duration of about 70 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 22:14:29.8 UT, 91.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 60.4491, -32.7098 which is equivalent to:
   RA(J2000)  = 04h 01m 47.78s
   Dec(J2000) = -32d 42' 35.2"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 76 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 98 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.01. 

Burst Advocate for this burst is 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: GRB111008A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12424
SUBJECT: GRB 111008A, Swift-BAT refined analysis,
DATE:    11/10/09 01:01:29 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@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),
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-240 to T+302 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111008A (trigger #505054)
(Saxton, et al., GCN Circ. 12423).  The BAT ground-calculated position is
RA, Dec = 60.439, -32.708 deg which is
    RA(J2000)  =  04h 01m 45.3s
    Dec(J2000) = -32d 42' 29.3"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 9%.

The mask-tagged light curve shows three clusters of peaks, each containing at least
two subpeaks, and with returns to the baseline between clusters.  Each cluster
is softer and weaker than the one preceding it. The first cluster runs from
T-10 sec to T+10 sec, the second runs from T+28 sec to T+35 sec, and the third
from T+58 to T+65 sec.  We note that there is a gap in the telemetry from T+180
to T+240 sec, but there is no indication of any emission between the last peak
and the gap or after the gap. T90 (15-350 keV) is 63.46 +- 2.19 sec (estimated
error including systematics).

The time-averaged spectrum from T-2.64 to T+68.80 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.86 +- 0.09.  The fluence in the 15-150 keV band is 5.3 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV band
is 6.4 +- 0.7 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/505054/BA/


GRB_name: GRB111008A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12425
SUBJECT: GRB 111008A: Enhanced Swift-XRT position
DATE:    11/10/09 02:49:05 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 1125 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111008A, 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 = 60.45094, -32.70947 which is equivalent
to:

RA (J2000): 04h 01m 48.22s
Dec (J2000): -32d 42' 34.1"

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: GRB111008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12426
SUBJECT: GRB 111008A: Gemini optical counterpart
DATE:    11/10/09 05:21:05 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (Warwick), K. Wiersema, N.R. Tanvir (Leicester) report
on behalf of a larger collaboration:

"We observed the field of GRB 111008A (Saxton et al. GCN 12423)
with Gemini-South in the r-band. Observations began at 03:12 UT, 5
hours after the BAT trigger. Within the refined XRT error circle
(Beardmore GCN 12425) we locate a single object at

RA(J2000) 04:04:48.24 
DEC(J2000) -32:42:33.4

with an error of 0.5" in each axis. Preliminary photometry against
USNO-B1 suggests R~22.8.  We suggest this may be the afterglow of
GRB 111008A. Further spectroscopic observations are in progress.

We thank the Gemini staff for the rapid and efficient execution of
these observations."


GRB_name: GRB111008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12427
SUBJECT: GRB 111008A: NOT optical observation
DATE:    11/10/09 06:29:50 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), D. Malesani (DARK/NBI), L.A. Buchhave (NBI), S. Schulze,
P. Jakobsson (U. Iceland) report on behalf of a larger collaboration:

We observed the field of GRB 111008A (Saxton et al., GCN 12423) with
the 2.5m Nordic Optical Telescope (NOT) equipped with ALFOSC. We
obtained 2x600 s R-band images, starting at 04:40:07 UT 9th Oct. 2011
(i.e., 6.45 hr after the burst). The optical afterglow reported in
Levan et al. (GCN 12426) was detected at R ~ 22.3 mag, calibrated
against the #0572-0051383 star (R2=16.77) in the USNO-B1.0 catalog.


GRB_name: GRB111008A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12428
SUBJECT: GRB 111008A, GROND observations
DATE:    11/10/09 06:31:49 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

M. Nardini (Milano Bicocca), S. Klose (TLS Tautenburg), J. Greiner (MPE
Garching), and P. Afonso (MPE/American River College) report on behalf of
the GROND team:

We observed the field of GRB 111008A (Saxton et al., GCN #12423)  
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 4:30 UT on October 08, 6.3 hours after the GRB
trigger.

We detect a point source within the 1.7 arcsec enhanced Swift-XRT error
circle (Beardmore et al., GCN #12425) at coordinates RA, DEC (J2000) =
04:01:48.25, -32:42:33.2 (+/-0.5"), confirming the observations from
Gemini (Levan et al., GCN 12426).

Preliminary magnitudes at a meantime of 5:15 UT are (in the AB system):

g' > 24.0,
r' = 22.6 +/- 0.1,
i' = 20.9 +/- 0.1,
z' = 19.9 +/- 0.1,

indicating a cosmological g-band dropout.

Data are calibrated against GROND zeropoints. Observations are ongoing.


GRB_name: GRB111008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12429
SUBJECT: GRB 111008A: Gemini spectroscopic redshift
DATE:    11/10/09 06:31:58 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

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

"We obtained optical spectroscopy of the candidate counterpart of
GRB 111008A (Saxton et al. GCN 12423, Levan et al. GCN 12426),
with GMOS on Gemini-South. Observations were centred at 6000A, 
and cover the region from 3900-8100A. We see flux from the 
candidate afterglow down to ~5500A, and a broad absorption feature 
centred at ~7300A, with a brighter continuum red-ward of this.  If 
interpreted as a DLA then this suggests that the redshift of 
GRB 111008A is z~5. We also find weak absorption lines of 
Ly-beta, OI(1302), CII(1334) and SiII (1260.5), consistent with a 
common redshift of z=5.0.

We note that there was a typographical error in the co-ordinates
of GCN 12426, which should have read

RA(J2000) 04:01:48.24 
DEC(J2000) -32:42:33.4

We thank Javier Gorosabel for pointing this error out, and apologise
for any confusion."


GRB_name: GRB111008A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12430
SUBJECT: GRB 111008A: Swift-XRT refined Analysis
DATE:    11/10/09 08:52:45 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U Leicester) and C. J. Saxton (UCL-MSSL) report on behalf of
the Swift-XRT team:

We have analysed 5.1 ks of XRT data for GRB 111008A (Saxton  et al. GCN
Circ. 12423), from 81 s to 24.0 ks after the  BAT trigger. The data
comprise 223 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 12425).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=7.1 (+0.9, -1.0). At T+103 s  the decay
flattens to an alpha of 3.22 (+/-0.12). The light curve breaks again at
T+311 s to a decay with alpha=0.26 (+/-0.16),  before a final break at
T+4539 s s after which the decay index is 0.99 (+0.12, -0.11).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.64 (+0.11, -0.10). The
best-fitting absorption column is  8.3 (+1.7, -1.6) x 10^20 cm^-2, in
excess of the Galactic value of 9.8 x 10^19 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.02 (+/-0.11) and a
best-fitting absorption column of 4.3 (+2.1, -2.0) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.5 x 10^-11 (4.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.3 (+2.1, -2.0) x 10^20 cm^-2
Galactic foreground: 9.8 x 10^19 cm^-2
Excess significance: 3.6 sigma
Photon index:      2.02 (+/-0.11)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00505054.

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


GRB_name: GRB111008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12431
SUBJECT: GRB 111008A: VLT/X-shooter spectroscopy
DATE:    11/10/09 11:03:04 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

K. Wiersema (Univ. Leicester), H. Flores (GEPI/Obs. de Paris), V. D'Elia 
(ASI/ASDC & INAF/OAR), P. Goldoni (APC/Univ. Paris 7 & SAp/CEA), D. 
Malesani (DARK/NBI), S. D. Vergani (INAF/OABr), A. de Ugarte Postigo 
(IAA-CSIC), A. J. Levan (Univ. Warwick), B. Milvang-Jensen, J. P. U. 
Fynbo (DARK/NBI), report on behalf of a larger collaboration:

We observed the optical counterpart of GRB 111008A (Saxton et al., GCN 
12423; Levan et al., GCN 12426; Xu et al., GCN 12427; Nardini et al., 
GCN 12428), using the X-shooter spectrograph mounted on the ESO-VLT. 
Observations started on 2011 October 9.247 UT (7.71 hr after the GRB), 
with a total exposure time of 2 hr, covering the wavelength range 
3000-25000 AA.

Continuum is clearly detected  redwards of ~7600 AA, with several, 
strong superimposed absorption features, consistent with a commom 
redshift z = 4.9898. Among them, we note several Si II and Fe II 
transitions, the CIV doublet, the Mg II doublet (in the H band), and 
several fine-structure lines commonly observed in GRB afterglow spectra 
(such as Si II*, S II*, O I*). We also note the presence of an 
intervening Mg II system at z = 4.61. Our results are thus consistent 
with the redshift derived by Levan et al. (GCN 12429; see also Nardini 
et al., GCN 12428).

We acknowledge excellent support from the observing staff in Paranal, in 
particular Christophe Martayan, Claudio Melo, Leonel Rivas, and Sergio Vera.


GRB_name: GRB111008A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12432
SUBJECT: GRB 111008A: IAC80 I-band observations
DATE:    11/10/09 14:05:45 GMT
FROM:    RubÃ©n SÃ¡nchez-RamÃ­rez at IAA-CSIC  <ruben@iaa.es>

R. Sanchez-Ramirez (IAA-CSIC), J. Gorosabel (IAA-CSIC), M. Cebrian (IAC), A.
de Ugarte Postigo (IAA-CSIC, DARK/NBI), P. Montaes (IAC), A. Rodriguez
Anton (IAC), report on behalf of a larger collaboration:

"We observed the field of GRB 111008A (Saxton et al., GCN Circ 12423) with
the 82cm IAC80 telescope at the Observatorio del Teide, Tenerife, Spain. We
acquired 22 x 300s I-band images on Oct 9.12973 - Oct 9.21239 UT (average
epoch 5.90h after the trigger) . A preliminary analysis of the combined
frame shows the source reported by Levan et al. (GCN Circ 12426) with a
magnitude of I ~ 20.6 (calibrated against USNO-B1 stars)."


GRB_name: GRB111008A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12433
SUBJECT: Konus-Wind observation of GRB 111008A
DATE:    11/10/09 14:58:01 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 111008A (Swift-BAT trigger #505054:
Saxton et al., GCN 12433; Baumgartner et al., GCN 12434)
triggered Konus-Wind at T0=79981.676s UT (22:13:01.676)

The burst light curve shows an initial pulse which
peaked at T0+0.256s and a softer weaker pulse at ~T0+30s.
A total burst duration is ~40 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/GRB111008_T79981/

As observed by Konus-Wind the burst
had a fluence of (9.0  0.9)x10-6 erg/cm2,
and a 256-ms peak flux, measured from T0+0.256 s,
of (1.4  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+41.216 s) is best fitted
in the 20 keV - 2 MeV range by a simple
power-law model with index (2.02  0.09),
chi2 = 54.3/59 dof.

The spectrum of the initial pulse
(measured from T0 to T0+8.448 s) is best fitted
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = -1.36 (-0.21, +0.24),
and Ep = 149(-28, +52) keV,
chi2 = 38.4/58 dof.

Assuming the redshift z=5.0 (Levan et al., GCN 12429;
Wiersema et al., GCN 12431) 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 (4.1  0.4)x10^53 erg,
the isotropic peak luminosity L_iso_max is (3.8  0.7)x10^53 erg/s,
and Ep_rest is 894(-168,+312) keV (the initial pulse spectrum).

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


GRB_name: GRB111008A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12434
SUBJECT: GRB 111008A: Swift/UVOT Upper Limits
DATE:    11/10/09 18:37:31 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 111008A
99 s after the BAT trigger (Saxton et al., GCN Circ. 12423).
No optical afterglow consistent with the refined XRT position
(Beardmore et al., GCN 12425; see also Levan et al. GCN 12426,
Nardini et al. GCN 12428, and Wiersema et al. GCN 12431) is
detected in the initial UVOT exposures, consistent with the
redshift reported by Levan et al. and Wiersema et al..
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

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

white_FC            99          249          147         >21.3
u_FC               311          561          246         >20.5
white               99         1359          373         >21.8
v                  641         1409           97         >19.0
b                  566         1335           78         >19.7
u                  311         1310          304         >20.6
w1                 690         1457           77         >19.2
m2                 666         1433           97         >21.0
w2                 617         1385           97         >19.8

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


GRB_name: GRB111005A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12435
SUBJECT: GRB 111005A: ATCA 18 GHz decay
DATE:    11/10/10 10:55:05 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS), M. Michalowski (U. Edinburgh), J. Stevens, P. Edwards
(CSIRO) report:

GRB 111005A (Saxton et al., GCN 12413) was observed with the Australia
Telescope Compact Array (ATCA), starting at 02:43 UT, 10th Oct. 2011
(i.e., 4.8 days after the burst) at the frequencies of 18, 34 and 94
GHz. Compared with our earlier detection (Michalowski et al., GCN
12422) the afterglow has decayed by 0.5 mJy at 18 GHz.


GRB_name: GRB111008A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12436
SUBJECT: EVLA 22 GHz Detection of GRB 111008A
DATE:    11/10/13 15:29:15 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, E. Berger (Harvard), and D. Frail (NRAO) report:

"We observed the position of GRB 111008A (GCN 12423 ) with the EVLA 
beginning 2011 October 10.37 UT (1.4 days after the burst).  At 22 GHz, 
we detect a radio source consistent with the Swift-XRT error circle (GCN 
12425) and the candidate optical counterpart (GCN 12429) at a position of

RA:   04:01:48.24 (+/- 0.04)
Dec:  -32:42:32.7 (+/- 0.6)

Further observations are planned."


GRB_name: GRB111008A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12437
SUBJECT: GRB 111008A : miniTAO/ANIR NIR observations
DATE:    11/10/14 16:04:57 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

M. Konishi, K. Tateuchi, K. Motohara, T. Tanabe, T. Kamizuka,
A. Nakashima, T. Minezaki, and Y. Yoshii (University of Tokyo),
S. Komugi (NAOJ/ALMA), S. Manabe (Kobe University),
report on behalf of the TAO project team

We report the near-infrared (NIR) imaging observation of GRB111008A
(Saxton et al., GCN 12423) using NIR Camera ANIR mounted on the
miniTAO 1.0m telescope at the University of Tokyo Atacama Observatory,
located on the summit of Co. Chajnantor (5,640m altitude) in the
northern Chile. Observations started at 04:36 UT on October 09,
approximately 6 hours after the burst.

We detect a point source at the coordinate reported by Levan et al.
(GCN 12426) in the JHKs-bands. The preliminary magnitudes are

J = 19.79 +/- 0.18,
H = 19.47 +/- 0.19,
Ks = 19.38 +/- 0.17,

in AB system.


GRB_name: GRB110921A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12438
SUBJECT: GRB 110921A: optical observations
DATE:    11/10/16 01:25:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU), A. Pozanenko (IKI), E. Klunko (ISTP), V. Rumyantsev 
(CrAO),  N.Pit (CrAO) on behalf of  larger GRB follow up collaboration 
report:

We observed  the field of the Swift GRB 110921A (Baumgartner et al., GCN 
12373) with  AZT-33IK telescope of Sayan observatory (Mondy) on Sep. 21 
between (UT) 14:36:31 -- 16:05:00 and AZT-11 telescope of CrAO  on Sep. 21 
between (UT) 17:38:46 -- 19:00:15. In a combined image of a few first frames 
taken with AZT-33IK we detected a faint source which coincides with the 
optical counterpart of  GRB 110921A (Xin et al., GCN 12377; Xu et al., GCN 
12385).   A photometry  is based on the  star USNO B1.0 1263-0338839 (19 36 
21.52 +36 19 56.2) assuming R=16.13

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

0.03934 R 850  22.08 +/- 0.18  22.3    AZT-33IK
0.07558 R 1920 n/d                   22.5    AZT-33IK
0.18620 R 4860 n/d                   21.3    AZT-11

In a combined image of a total exposure of 3030 s taken with AZT-33IK 
telescope we clearly detected the SDSS object noted by Xu et al. (GCN 12385) 
and Vreeswijk et al. (GCN 12387). The photometry of the SDSS object against 
the above calibration star is R=22.8 +/- 0.3. 


GRB_name: GRB111016A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12439
SUBJECT: GRB 111016A: Swift detection of a burst
DATE:    11/10/16 19:13:07 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), C. Guidorzi (U Ferrara), J. A. Kennea (PSU),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA), C. J. Saxton (UCL-MSSL),
M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC) and
G. Tagliaferri (INAF-OAB) report on behalf of the Swift Team:

At 18:37:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111016A (trigger=505646).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 153.806, +27.476 which is 
   RA(J2000)  =  10h 15m 13s
   Dec(J2000) = +27d 28' 32"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows at least 7 well separated
peaks with a total duration of at least 230 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger, and another
equally bright peak at T+160 sec.  And there is a possible peak at T+600 sec. 

The XRT began observing the field at 18:40:03.2 UT, 180 seconds
after the BAT trigger. A bright source was present in the field, 
at the following location RA,Dec(J2000) = 153.8334, 27.4634, which 
is equivalent to:
   RA(J2000)  =  10h 15m 20.0s
   Dec(J2000) = +27d 27' 48.3"
with an estimated error of 5 arc-seconds radius (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White 
filter  starting 187 seconds after the BAT trigger. No credible 
afterglow candidate has been found in the initial data products. The
2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical
3-sigma upper limit has been about 19.6 mag. The 8'x8' region for
the list of sources generated on-board covers 100% of the XRT error
circle. The list of sources is typically complete to about 18 mag. No 
correction has been made for the expected extinction corresponding to
E(B-V) of 0.04. 

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


GRB_name: GRB111016A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12440
SUBJECT: GRB 111016A: Swift-XRT observations
DATE:    11/10/16 20:49:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne (U. Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU), G.
Cusumano (INAF-IASF PA), M. Perri (ASDC) and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 111016A at 18:40:03.2 UT,
178.7 seconds after the BAT trigger. XRT found a bright, uncatalogued
X-ray source located at RA, Dec 153.8334, +27.4634 which is equivalent
to:
   RA(J2000)  = 10h 15m 20.01s
   Dec(J2000) = +27d 27' 48.2"
with an uncertainty of 6.0 arcseconds (radius, 90% containment). This
location is 98 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 0.00e+00 erg cm^-2 s^-1 (0.2-10
keV).


GRB_name: GRB111016A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12441
SUBJECT: GRB 111016A: Enhanced Swift-XRT position
DATE:    11/10/17 01:26:25 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 5089 s of XRT Photon Counting mode data and 11 UVOT
images for GRB 111016A, 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 = 153.83400, +27.46235 which is equivalent
to:

RA (J2000): 10h 15m 20.16s
Dec (J2000): +27d 27' 44.5"

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

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

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


GRB_name: GRB111016A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12442
SUBJECT: GRB 111016A: Swift-XRT refined Analysis
DATE:    11/10/17 09:25:16 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF-IASFPA) reports on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 111016A (Mangano  et al. GCN
Circ. 12439), from 185 s to 23.8 ks after the  BAT trigger. The data
comprise 693 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 12441).

The late-time light curve (from T0+4.1 ks) can be modelled with an
initial power-law decay with an index of alpha=3.62 (+0.24, -0.98),
followed by a break at T+5533 s to an alpha of 1.06 (+0.15, -0.23).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.800 (+/-0.024). The
best-fitting absorption column is  1.85 (+/-0.07) x 10^21 cm^-2, in
excess of the Galactic value of 2.5 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.23 (+0.09, -0.14)
and a best-fitting absorption column of 7.3 (+2.2, -3.3) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.2 x 10^-11 (4.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.3 (+2.2, -3.3) x 10^20 cm^-2
Galactic foreground: 2.5 x 10^20 cm^-2
Excess significance: 3.6 sigma
Photon index:      2.23 (+0.09, -0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00505646.

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


GRB_name: GRB111016A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12443
SUBJECT: GRB 111016A: MITSuME Akeno Optical upper limits
DATE:    11/10/17 13:14:11 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

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

We observed GRB 111016A (Mangano et al., GCNC 12439) with an optical
three color (g, Rc, and Ic) CCD camera attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.
The follow-up observation was started at 18:52:46, ~15 min after the
BAT trigger.
We did not find any new point source within the enhanced XRT error
circle (Evans et al., GCNC 12441) in all the three bands.

Photometric results are listed below. We used GSC2.3 catalog for flux
calibration.

T0+[sec]      MID-UT     T-EXP[sec]      g'             Rc           Ic
---------------------------------------------------------------------------------
  +942        19:38:33        1380         >17.4      >17.3     >16.5
---------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111016A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12444
SUBJECT: GRB 111016A: P60 Afterglow Candidate
DATE:    11/10/17 13:50:42 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 GRB111016A (Mangano et al., GCN 12439) with
the robotic Palomar 60 inch telescope.  Observations began at 11:30 UT on
2011 October 17 (~ 16.9 hours after the initial Swift trigger) and were
obtained in the Sloan r', i', and z' filters.

Inside the revised localization of the X-ray afterglow (Evans et al., GCN
12441) we marginally detect a source in the i' filter with coordinates:

   RA: 10:15:20.23; Dec: +27:27:44.0 (J2000)

Compared with nearby point sources from the Sloan Digital Sky Survey, we
measure a magnitude of i' ~ 22.1 +/- 0.3 mag at this time.  No significant
emission is detected at this location in the r' filter to r' > 21.9 mag.

Given the modest significance of the detection in only a single filter, we
encourage further observations to confirm if this possible source is
indeed the afterglow of GRB111016A.


GRB_name: GRB111016A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12445
SUBJECT: GRB 111016A: Swift-BAT refined analysis
DATE:    11/10/17 17:23:05 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), V. Mangano (INAF-IASFPA), 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 111016A (trigger #505646)
(Mangano, et al., GCN Circ. 12439).  The BAT ground-calculated position is
RA, Dec = 153.826, 27.474 deg, which is 
   RA(J2000)  =  10h 15m 18.2s 
   Dec(J2000) = +27d 28' 26.7" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.
 
The mask-weighted light curve shows a series of slighlty overlapping peaks
starting at ~T-5 sec, peaking at T+58, T+118, T+160, T+210, T+255,
then returning to baseline, followed by smaller peaks at T+410, T+540, T+600,
and possible peaks at T+700 and T+800.  The burst location goes out
of the BAT FOV at T+960 sec.  T90 (15-350 keV) is 550 +- 105 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+35.41 to T+614.48 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.12.  The fluence in the 15-150 keV band is 4.0 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+115.23 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/505646/BA/


GRB_name: GRB111016A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12446
SUBJECT: GRB 111016A: Swift/UVOT Detection of a Source
DATE:    11/10/17 18:18:13 GMT
FROM:    Tyler Pritchard at PSU  <tapritchard@astro.psu.edu>

T. A. Pritchard (PSU) and V. Mangano (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111016A
188 s after the BAT trigger (Mangano et al., GCN Circ. 12439).
No optical afterglow consistent with the Enhanced Swift-XRT position
(Evans et al., GCN Circ 12441) is detected in the initial UVOT exposures,
however a marginal source is detected in followup observations in the
UVOT white filter.  This position is consistent with the source observed by
Cenko et all (GCN Circ 12444).  Preliminary 3-sigma upper limits and
magnitudes using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

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

white_FC           188          337          147 >20.3
u_FC               345          595          246 >19.3
white              188        23781         1926 >21.5
white            27360        45216         4662         21.56
v                 4468        16602         1278 >20.5
b                 5288        23264         1967 >21.6
u                  345        22351         1328 >20.4
w1                 724        18207         1095 >20.5
m2                 700        17507         1298 >20.8
w2                 651        12429         1135 >20.7

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: GRB111016A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12447
SUBJECT: GRB 111016A: Gemini Detection of the NIR Counterpart
DATE:    11/10/18 03:52:20 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), A. Cucchiara (UC Santa Cruz), N. R. Tanvir
(U. Leicester), A. J. Levan (U. Warwick), A. S. Fruchter (STScI), and E.
Berger (Harvard) report on behalf of a larger collaboration:

We have imaged the field of GRB111016A (Mangano et al., GCN 12439) with
the Near-Infrared Imager and Spectrometer (NIRI) mounted on the 8 m Gemini
North telescope.  Observations were obtained in the J, H, and K filters
beginning at 14:25 UT on 2011 October 17 (~ 19.8 hours after the initial
Swift trigger).

We detect a faint, unresolved source in all three filters coincident with
the optical afterglow candidate from P60 (Cenko et al., GCN 12444) and
UVOT (Pritchard et al., GCN 12446).  Having established the reality of
this object, pre-outburst limits from the Sloan Digital Sky Survey imply
some degree of variability and establish it as the optical counterpart of
GRB111016A.

Using the only two 2MASS sources within the NIRI field of view for
calibration, we measure K ~ 20.4 +/- 0.2 (Vega) at this time.  Assuming
limited evolution from the time of the P60 observations, the i' - K color
implies a relatively unusual blue SED (flat spectrum in fnu) when compared
with other GRB afterglows at this time, particularly given the presence of
a modest host galaxy dust column inferred from the X-ray spectrum (Mangano
et al., GCN 12442).  We caution however, that the photometric calibration
in the NIR remains somewhat uncertain due to the lack of reference sources
in the field.

We wish to thank the entire Gemini staff for the prompt execution
of these observations.  Further observations are encouraged.


GRB_name: GRB111016A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12448
SUBJECT: GRB111016A: D50 optical limit
DATE:    11/10/18 15:08:32 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

M. Blazek (AsU AV), R. Hudec (AsU AV), M. Jelinek (IAA-CSIC), C. 
Polasek (AsU AV) and J. Strobl (AsU AV)

"We observed the field of GRB 111016A (Mangano et al., GCN
12439) with 0.5m robotic telescope D50 in Ondrejov observatory
(Czech Republic).  The observation started at 01:59:08 UT on
October 17, 2011, approx.  5.5 hours after the Swift trigger.
We report no detection of the optical counterpart on the
unfiltered images within the error circle given by SWIFT-XRT
(Evans et al., GCN 12441). The upper limit of 19.5 mag in
R-band was estimated using nearby sources from GSC2.2
catalogue."


GRB_name: GRB111017A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12449
SUBJECT: GRB 111017A: Fermi GBM Detection
DATE:    11/10/18 15:48:22 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

Peter Jenke (MSFC/NPP)
report on behalf of the Fermi GBM Team:

"At 15:45:23.72 UT on 10 17 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111017A (trigger 340559125 / 111017.657).
There was an independent SPI-ACS detection of this burst at 15:45:27 UT.

The on-ground calculated location, using the GBM trigger
data, is RA = 8.10, DEC = -7.01 (J2000 degrees,
equivalent to 00 h 32.4 m, -7 d 36 m), with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 39.00 degrees.

The GBM light curve shows one main peak with emission
extending to 1 MeV.  Moreover, this burst was
bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver.
The burst had a duration (T90) of about 11s (50-300 keV).
This single peak had an unusual symmetric form, unlike the
usual FRED-like light curve.  The time-averaged spectrum from
T0-0.512 s to T0+14.848 s is adequately fit by a Band function
 with Epeak =692.5 +/- 48.3 keV,
alpha = -0.91 +/- 0.02, and beta = -2.7 +/- 0.40
(CSTAT  1088.9 for 619 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(2.26 +/- 0.038)E-05 erg/cm^2. The peak photon flux measured
starting from T0+-0.512 s in the 10-1000 keV band
is 5.904 +/- 0.061 ph/s/cm^2.

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


GRB_name: GRB111018A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12450
SUBJECT: GRB 111018A: Swift detection of a burst
DATE:    11/10/18 17:43:51 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
M. M. Chester (PSU), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), V. Mangano (INAF-IASFPA),
D. M. Palmer (LANL), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester), C. A. Swenson (PSU),
G. Tagliaferri (INAF-OAB), E. Troja (NASA/GSFC/ORAU) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 17:26:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111018A (trigger=505801).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 271.500, -3.871 which is 
   RA(J2000)  =  18h 06m 00s
   Dec(J2000) = -03d 52' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two weak peaks
at T+0 and T+30 sec with a total duration of about 40 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 17:28:27.6 UT, 123.0 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find an uncatalogued X-ray source located at RA, Dec 271.48887,
-3.90719 which is equivalent to:
   RA(J2000)  = 18h 05m 57.33s
   Dec(J2000) = -03d 54' 25.9"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 135 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.54
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 132 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
2.16. 

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: GRB111016A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12451
SUBJECT: GRB111016A : WIYN 3.5m NIR observations
DATE:    11/10/18 21:52:37 GMT
FROM:    Atish Kamble at U. of Wisconsin  <atish@gravity.phys.uwm.edu>

Atish Kamble, Ralf Kotulla, David Kaplan (UW-Milwaukee), Nial Tanvir, 
K. Wiersema (U. Leicester) and A. Levan (U. Warwick) reports :

We observed the field of GRB 111016A (Mangano et al., GCN 12439) 
using the WIYN High Resolution Infrared Camera (WHIRC) on the WIYN 3.5m telescope, 
beginning at October 17.5 (UT), approximately 17 hours post-burst. 
Observations were carried out using J, H and Ks bands. We do not detect 
any source within the XRT error circle (Evans et al., GCN 12441).

The preliminary limiting magnitudes are J = 18.3, H = 17.8 and K = 19.0.

We acknowledge the support from the staff of WIYN-3.5m telescope, and 
especially from Andrew Schechtman-Rook in carrying out these observations.


GRB_name: GRB111016B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12452
SUBJECT: IPN Triangulation of GRB 111016B (long duration, intense)
DATE:    11/10/18 23:01:32 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, and W.
Hajdas, on behalf of the RHESSI GRB team,

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team, report:

The long-duration, intense GRB 111016B was observed by Konus-Wind, Mars 
Odyssey (HEND), MESSENGER (GRNS), RHESSI, and Swift (BAT) (outside the 
coded field of view) at 81700 s UT (22:41:40). We have triangulated it 
to a preliminary, 3 sigma error box whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   290.499 (19h 22m 00s)  -4.578 ( -4d 34' 39")
  Corners:
   290.322 (19h 21m 17s)  -4.416 ( -4d 24' 56")
   290.513 (19h 22m 03s)  -4.048 ( -4d 02' 53")
   290.676 (19h 22m 42s)  -4.740 ( -4d 44' 24")
   290.487 (19h 21m 57s)  -5.119 ( -5d 07' 09")
  ---------------------------------------------

The error box area is 696 sq. arcmin, and its maximum
dimension is 64 arcmin.

This box can be improved.

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


GRB_name: GRB111018A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12453
SUBJECT: GRB 111018A: Enhanced Swift-XRT position
DATE:    11/10/19 00:01:32 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 1590 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 111018A, 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 = 271.48854, -3.90728 which is equivalent
to:

RA (J2000): 18h 05m 57.25s
Dec (J2000): -03d 54' 26.2"

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: GRB111018A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12454
SUBJECT: GRB 111018A: GROND Upper Limits
DATE:    11/10/19 06:21:50 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

M. Nardini (Uni. Milano-Bicocca), J. Elliott and J. Greiner (both MPE  
Garching) report on behalf of the GROND team:

We observed the field of GRB111018A (Swift trigger 505801; Marhsal et  
al., GCN #12450) simultaneously in g'r'i'z'JHK with GROND (Greiner et  
al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La  
Silla Observatory (Chile).

Observations started at 23:47 UT on 18 October 2011, 6.35 hours after  
the trigger. They were performed at an average seeing of 2.8 and at 
an average airmass of 1.9.

Based on images with total exposures of 1500 s in g'r'i'z' and 1200 s  
in JHK, we do not detect a source within the Swift-XRT error circle  
reported by Goad et al. (GCN #12453) down to (all AB):

g' > 23.2,
r' > 23.5,
i' > 22.5,
z' > 22.2,
J  > 20.0,
H  > 18.9, 
K  > 18.6

Given magnitudes are calibrated against GROND zeropoints as well as  
2MASS field stars and are not corrected for the expected Galactic  
foreground extinction corresponding to the heavy reddening of 
E(B-V)=2.16 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB111018A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12455
SUBJECT: GRB 111018A: Swift-XRT refined Analysis
DATE:    11/10/19 07:53:17 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF IASFPA) and F. E. Marshall (NASA/GSFC) reports on
behalf of the Swift-XRT team:

We have analysed 11 ks of XRT data for GRB 111018A (Marshall  et al.
GCN Circ. 12450), from 115 s to 36.2 ks after the  BAT trigger. The
data comprise 37 s in Windowed Timing (WT) mode (the first 6 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 12453).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.01 (+0.15, -0.13).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+0.8, -0.7). The
best-fitting absorption column is  1.2 (+0.8, -0.6) x 10^22 cm^-2, in
excess of the Galactic value of 2.5 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 6.7 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.2 (+0.8, -0.6) x 10^22 cm^-2
Galactic foreground: 2.5 x 10^21 cm^-2
Excess significance: 3.4 sigma
Photon index:      1.8 (+0.8, -0.7)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00505801.

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


GRB_name: GRB111016B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12456
SUBJECT: Konus-Wind observation of GRB 111016B
DATE:    11/10/19 08:50:35 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long hard intense GRB 111016B
(localized by IPN: Hurley et al., GCN 12452)
triggered Konus-Wind at T0=81700.723s UT (22:41:40.723)

The light curve shows a multi-peaked complex with
a total duration of ~150 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/GRB111016_T81700/

As observed by Konus-Wind the burst
had a fluence of 1.37(-0.05,+0.05)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+1.792 s,
of 3.7(-0.3,+0.3)x10-6 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+145.408 s)
is best fitted in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.78 (-0.06, +0.06),
and Ep = 378(-19, +21) keV,
chi2 = 58.7/76 dof.
Fitting this spectrum by the GRB (Band) function yields
the same alpha and Ep with a high energy photon index
beta < -3.0 (chi2 = 58.7/75 dof).

The spectrum at the maximum count rate
(measured from T0 to T0+6.144 s)
is best fitted in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.72 (-0.10, +0.11),
and Ep = 327(-26, +30) keV,
chi2 = 86.4/76 dof.

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


GRB_name: GRB111018A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12457
SUBJECT: GRB 111018A: Swift-BAT refined analysis
DATE:    11/10/19 11:49:22 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), 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-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111018A (trigger #505801)
(Marshall, et al., GCN Circ. 12450).  The BAT ground-calculated position is
RA, Dec = 271.482, -3.880 deg, which is 
   RA(J2000)  =  18h 05m 55.6s 
   Dec(J2000) = -03d 52' 48.5" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 80%.
 
The mask-weighted light curve shows a couple overlapping peaks starting 
at ~T-4 sec, peaking at ~T-1 and ~T+22 sec, and ending at ~T+35 sec,
possibly out to T+75 sec.  T90 (15-350 keV) is 36 +- 5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-4.08 to T+37.30 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.18 +- 0.27.  The fluence in the 15-150 keV band is 4.0 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+21.71 sec in the 15-150 keV band
is 0.4 +- 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/505801/BA/


GRB_name: GRB110918A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12458
SUBJECT: GRB 110918A: Optical light curve for days 1.4 to 16.3
DATE:    11/10/19 12:14:28 GMT
FROM:    AAVSO GRB Network at AAVSO  <matthewt@aavso.org>

Arto Oksanen (Hankasalmi Obs., Hankasalmi, Finland), Bradley Schaefer 
(LSU), Caisey Harlingten (Harlingten Observatory, San Pedro de Atacama, 
Chile), and Matthew Templeton (AAVSO) report the following observations of 
GRB 110918A (Hurley et al., GCN Circ. #12357):

A. Oksanen (Hankasalmi Obs., Hankasalmi, Finland) reports observations of 
the optical transient associated with the intense, long GRB 110918A at 
z=0.982 (Hurley et al., GCNC #12357; Golonetskii, et al., GCNC #12362; 
Mangano et al. GCN 12364; Levan et al. GCN 12368) using the Harlingten 
Observatory 0.5-m Planewave telescope with Apogee Alta-U42D9 CCD located 
in San Pedro de Atacama, Chile.  The observations were made on 15 nights 
from 1.417 to 16.325 days after the burst, all without a filter so that 
the color sensitivity is like that of a broad R-band filter.  We have 
calibrated the optical transient magnitude with the five comparison stars 
used by Perley et al. (GCN 12388) for which they quote the R-band 
magnitudes from the USNO catalog.  Our magnitudes (plus two taken from the 
GCNs) are given in the following table:

JD              R(GRB)       T-T0 (days)
2455824.8105    19.18  0.04 1.417
2455825.5537    19.70  0.10 2.160 (Guidorzi et al. GCN 12382)
2455825.7625    19.97  0.05 2.369
2455826.6343    20.68  0.13 3.241 (Perley et al. GCN 12388)
2455826.7059    20.51  0.06 3.312
2455827.7137    20.85  0.07 4.320
2455828.7067    21.14  0.09 5.313
2455829.7193    21.26  0.09 6.326
2455830.7107    21.56  0.12 7.317
2455831.7025    21.34  0.09 8.309
2455832.7116    21.62  0.11 9.318
2455833.6930    21.90  0.12 10.299
2455834.7065    21.76  0.12 11.313
2455835.6894    21.58  0.10 12.296
2455836.7208    21.67  0.11 13.327
2455837.7159    21.94  0.12 14.322
2455839.7185    21.99  0.13 16.325

The flux up to 10 days after the burst is well fit by a power law with an 
index of -1.24.  After 10 days after the burst, the light curve appears to 
flatten (i.e., the opposite of a jet break), for which we expect that the 
underlying galaxy is appearing in the light curve.

There is certainly no jet break in the time interval from 1.417 to roughly 
10-16 days after the burst.  The index over this time interval is typical 
for the interval before the jet break, which implies that the jet break is 
at a time of greater than 10 days after the burst.  The previous 
suggestion of an early jet break was simply due to one group looking at 
only two magnitudes with relatively large uncertainty (not counting 
inconsistencies in the two calibrations) and closely spaced in time and 
seeing an apparently steep slope.  With our long interval with consistent 
magnitudes with small statistical uncertainty, we can be certain that the 
index is shallow and no jet break is present.

The light curve of this GRB may be viewed at the following URL:

http://www.aavso.org/sites/default/files/images/110918A_Oksanen.png


The AAVSO International High Energy Network was made possible through 
grants from the Charles Curry Foundation and from NASA, and is supported 
through the AAVSO Endowment.


GRB_name: GRB111018A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12459
SUBJECT: GRB 111018A: Swift/UVOT Upper Limits
DATE:    11/10/19 12:59:31 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 111018A 
132 s after the BAT trigger (Marshall et al., GCN Circ. 12450). No 
optical afterglow consistent with the refined XRT position (Goad et 
al., GCN Circ. 12453) is detected in the initial UVOT exposures. 
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC) 
exposure and subsequent exposures are:

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

white_FC           132          282          147         >21.1
white              132         7508          653         >21.8
v                  462        12028          673         >20.2
b                  388         6000          333         >20.9
u                  291         5794          329         >20.6
uvw1               512         5590          314         >20.4
uvm2               487         5384          333         >20.2
uvw2               438        11672         1040         >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 2.16 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111020A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12460
SUBJECT: GRB 111020A: Swift detection of a short burst
DATE:    11/10/20 06:46:03 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. Sakamoto (NASA/UMBC), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), V. Mangano (INAF-IASFPA),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
P. Romano (INAF-IASFPA) report on behalf of the Swift Team:

At 06:33:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111020A (trigger=505926).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 287.027, -37.985 which is 
   RA(J2000) = 19h 08m 06s
   Dec(J2000) = -37d 59' 05"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a short single peak
structure with a duration of about 0.5 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 06:35:01.8 UT, 72.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 287.05305, -38.01178 which is
equivalent to:
   RA(J2000)  = 19h 08m 12.73s
   Dec(J2000) = -38d 00' 42.4"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 121 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 6.89
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 79 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 0.43. 

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: GRB111020A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12461
SUBJECT: GRB 111020A: Planned XMM-Newton observation
DATE:    11/10/20 08:10:40 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.esac.esa.int>

XMM-Newton will observe GRB 111020A at location
(RA=19h 08m 12.73s, DEC=-38d 00' 42.4", J2000),
starting at 19:41:49 UT, on October 20, 2011,
for an exposure of 30,000 seconds.




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GRB_name: GRB111020A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12462
SUBJECT: GRB 111020A: BOOTES-3 Optical Upper Limit.
DATE:    11/10/20 15:07:24 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

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

We have observed the field of the short GRB 111020A, detected by Swift/BAT
(Palmer et al., GCNC 12460) with the 0.6m Yock-Allen telescope at the
BOOTES-3 station in Blenheim (New Zealand). Unfiltered images were obtained
starting 69.72 minutes after the burst (07:43:32 UT), no new source is
visible in the co-added image with total exposure 6900 sec (115 images
ending in 09:40:53 UT), the limiting magnitude for the combined image is R =
19.5 (calibrated against USNO B1.0).

USNO B1-0519-0893471, a catalogued R=18.7 magnitude source is at the edge of
the XRT circle but shows no evident variability.


GRB_name: GRB111020A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12463
SUBJECT: GRB 111020A: Enhanced Swift-XRT position
DATE:    11/10/20 15:32:42 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 2124 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 111020A, 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 = 287.05219, -38.01216 which is equivalent
to:

RA (J2000): 19h 08m 12.53s
Dec (J2000): -38d 00' 43.8"

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: GRB111020A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12464
SUBJECT: GRB 111020A: Swift-BAT refined analysis
DATE:    11/10/20 15:49:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), 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):
 
Using the data set from T-240 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111020A (trigger #505926)
(Sakamoto, et al., GCN Circ. 12460).  The BAT ground-calculated position is
RA, Dec = 287.029, -38.031 deg, which is 
   RA(J2000)  =  19h 08m 06.9s 
   Dec(J2000) = -38d 01' 50.3" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 74%.
 
The mask-weighted light curve shows a single spike starting at ~T+0.0, peaking
at ~T+0.1 sec, and ending at ~T+1.0 sec.  There is a hint (at the 2.5-sigma level)
of a soft tail out to ~T+10 sec.  T90 (15-350 keV) is 0.40 +- 0.09 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.04 to T+0.39 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.37 +- 0.26.  The fluence in the 15-150 keV band is 6.5 +- 1.0 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.32 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/505926/BA/


GRB_name: GRB111020A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12465
SUBJECT: GRB 111020A: Faulkes Telescope South observations
DATE:    11/10/20 16:07:13 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

C. Guidorzi (U. Ferrera), N. R. Tanvir (U. Leicester), C. Mottram,
D. Bersier (Liverpool JMU), report:

On 2011 October 20 at 11:02:37 UT the 2-m Faulkes Telescope
South began observing short GRB 111020A (Sakamoto et al., GCN Circ.
12460) using the Ri filters, corresponding to approximately 4.5 hours
after the burst trigger time.

We detect no uncatalogued sources, either inside or near the
enhanced XRT error circle (Osborne et al. GCN Circ. 12463),
to the following limiting magnitudes:

Mid time from Total Exp Filter Magnitude
trigger (hours) (s)
------------------------------------------------
4.75 6x300 R> 21.0
5.32 6x300 i> 21.7
------------------------------------------------

Magnitudes have been calibrated from nearby USNOB-1
stars using their R2 and I nominal values.


GRB_name: GRB111020A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12466
SUBJECT: GRB 111020A: Swift/UVOT Upper Limits
DATE:    11/10/20 19:47:57 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 111020A
80 s after the BAT trigger (Sakamoto et al., GCN Circ. 12460).
No optical afterglow consistent with the XRT position (Osborne et al., GCN Circ. 12463) 
is detected in the initial UVOT exposures. 

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

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

white_FC            80          230          147         >20.0
u_FC               292          542          246         >19.6
white               80         7160          766         >20.3
v                  622         6135          275         >18.8
b                  547         6956          471         >19.9
u                  292        18728         1973         >20.3
w1                 670        18066         2242         >21.0
m2                6140        22385         2310         >21.1
w2                1027         5930          216         >20.5

This photometry may be complicated by the presence of a catalogued source 
approximately 3'' away from the centre of the enhanced XRT error circle.
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.43 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111020A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12467
SUBJECT: GRB 111020A: Gemini-South i-band observations
DATE:    11/10/21 01:58:38 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong (Harvard), E. Berger (Harvard) and D. Fox (PSU) report:

We imaged the location of the short GRB 111020A (GCN 12460) with GMOS on the
Gemini-South 8-m telescope on 2011 October 21.01 UT (mid-time of 17.7 hours
post-burst).  We obtained 9x180s exposures in i-band with 0.8" seeing.

We find no sources within the enhanced XRT error circle (GCN 12463) to a
3-sigma limiting magnitude of i~25 mag.

However, we find two faint objects just outside of the XRT error circle with
coordinates (J2000):

S1:
RA = 19:08:12.501
Dec = -38:00:41.80

S2:
RA = 19:08:12.698
Dec = -38:00:44.46

S1 has a brightness of i~23.7 mag and appears to be point-like. S2 is
fainter, at the threshold of detectability with a brightness of i~25 mag.

The nearest galaxy is located at:

G1:
RA = 19:08:12.231
Dec = -38:00:48.80

with a magnitude of i~23.3 mag, and 6.2" from the center of the XRT error
circle.


GRB_name: GRB111020A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12468
SUBJECT: GRB 111020A: Swift-XRT refined Analysis
DATE:    11/10/21 07:36:44 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF IASFPA) and T. Sakamoto (NASA/UMBC) reports on behalf
of the Swift-XRT team:

We have analysed 20 ks of XRT data for GRB 111020A (Sakamoto  et al.
GCN Circ. 12460), from 59 s to 69.8 ks after the  BAT trigger. The data
comprise 7 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
12463).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.72 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.14 (+0.19, -0.41). The
best-fitting absorption column is  10.0 (+5.4, -1.8) 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 5.3 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      10.0 (+5.4, -1.8) x 10^21 cm^-2
Galactic foreground: 6.9 x 10^20 cm^-2
Excess significance: 8.9 sigma
Photon index:      2.14 (+0.19, -0.41)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00505926.

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


GRB_name: GRB111020A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12469
SUBJECT: GRB 111020A: EVLA observations
DATE:    11/10/21 14:26:47 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the position of GRB 111020A (GCN 12460) with the EVLA beginning
on 2011 October 20.98 UT (16.9 hours post-burst) at a mean frequency of 5.8
GHz.  In 1 hour of observations we do not detect any radio source within the
enhanced XRT error circle (GCN 12463) to a 3-sigma limit of ~50 microJy.
Further observations are in progress."


GRB_name: GRB111020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12470
SUBJECT: GRB 111020A: Gemini-South additional observations and limit on an optical afterglow
DATE:    11/10/22 02:47:44 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong and E. Berger (Harvard) report:

"We re-imaged the field of GRB 111020A (GCN 12640) with GMOS on the
Gemini-South telescope on 2011 October 22.01 UT (mid-time of 1.7 days
post-burst, and 23.1 hours after our initial observations; GCN 12467).  We
obtained 11x180s exposures in i-band in 0.73" seeing.

We still detect the two faint sources S1 and S2 from our previous GMOS
observation (GCN 12467), and neither source shows evidence for fading.
Digital image subtraction of the two epochs using the ISIS package reveals
no residuals inside or near the XRT error circle.  We therefore place a
limit on the optical afterglow of i~25 mag at 17.7 hours after the burst."


GRB_name: GRB111022A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12471
SUBJECT: GRB 111022A: Swift detection of a burst
DATE:    11/10/22 16:23:02 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

S. Immler (CRESST/GSFC/UMD), M. M. Chester (PSU), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester),
E. Sonbas (GSFC/USRA/Adiyaman Univ.), E. Troja (NASA/GSFC/ORAU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 16:07:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111022A (trigger=506070).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 275.872, -23.668 which is 
   RA(J2000) = 18h 23m 29s
   Dec(J2000) = -23d 40' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 15 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 16:08:21.1 UT, 76.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 275.8642, -23.6724 which is equivalent to:
   RA(J2000)  = 18h 23m 27.40s
   Dec(J2000) = -23d 40' 20.6"
with an uncertainty of 6.3 arcseconds (radius, 90% containment). This
location is 27 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. 

Swift entered the SAA shortly after detecting this burst, so there are
no prompt UVOT data products for this burst at this time. 

Burst Advocate for this burst is S. Immler (immler 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: GRB111022B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12472
SUBJECT: GRB 111022B: Swift detection of a burst
DATE:    11/10/22 17:31:34 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/USRA/GSFC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
M. M. Chester (PSU), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
C. Guidorzi (U Ferrara), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), A. Melandri (INAF-OAB),
K. L. Page (U Leicester) and G. Stratta (ASDC) report on behalf of the
Swift Team:

At 17:13:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111022B (trigger=506074).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 108.951, +49.666 which is 
   RA(J2000)  =  07h 15m 48s
   Dec(J2000) = +49d 39' 59"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows nothing which is typical
for an image trigger. 

The XRT began observing the field at 17:15:21.8 UT, 137.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
108.9646, 49.6835 which is equivalent to:
   RA(J2000)  = 07h 15m 51.49s
   Dec(J2000) = +49d 41' 00.4"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 69 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 7.32
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 8.17e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 144 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.07. 

Burst Advocate for this burst is S. T. Holland (Stephen.T.Holland 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: GRB111022A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12473
SUBJECT: GRB 111022A: MASTER-Net early limit
DATE:    11/10/22 17:51:33 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, P.V.Kortunov, A.Kuznetsov, 
D.Zimnukhov, M. Kornilov, A.Sankovich
Sternberg Astronomical Institute, Moscow State University

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

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

V.Krushinski, I.Zalozhnich, T.Kopytova, 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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB111022A 29 sec  after notice 
time and 47 sec after GRB time at 2011-10-22 16:07:52 UT. On our first 
(10s exposure) set we haven't found optical transient  within SWIFT 
error-box.
The 5-sigma upper limit has been about 16.6 mag. The object was observed 
on high (80 deg) zenit distance.
The message may be cited.


GRB_name: GRB111022A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12474
SUBJECT: GRB 111022A: Preliminary UVOT TDRSS Non-Detection
DATE:    11/10/22 17:54:31 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

S. T. Holland (CRESST/USRA/GSFC), and
S. Immler (CRESST/USRA/GSFC)
report on behalf of the Swift/UVOT team:

GRB 111022A: Swift/UVOT Non-Detection

UVOT took a finding chart exposure of 150 seconds with the white filter
starting 815 seconds after the BAT trigger.  This field is very crowded,
but no credible afterglow candidate has been found in the initial data
products.  The 2.7' x 2.7' sub-image covers 100% of the XRT error circle.
The estimated 3-sigma upper limit is white > 20.0 mag.  No correction has
been made for the expected Galactic extinction corresponding to a reddening
of E_{B-V} =  0.66 mag.  Due to the low Galactic latitude of this burst the
extinction is highly uncertain.


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12475
SUBJECT: GRB 111022B: MASTER-Net early limit
DATE:    11/10/22 18:07:27 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB111022B 22 sec after 
notice time and 583 sec after GRB time at 2011-10-22 17:22:48 UT in two 
polarization bands. On our first (120s exposure) set we haven't found 
optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 17.0 mag

MASTER II  robotic telescope located in Tunka(Siberia) was pointed to
GRB111022B 183 sec  after notice time and 748 sec after GRB time at
2011-10-22 17:25:32 UT in two polarization bands. On 
our first (150s exposure) set we haven't found optical transient  within 
SWIFT error-box. So long time of pointing in this site is caused by a 
mount problem.
The 5-sigma upper limit has been about 18.3 mag

The message may be cited.


GRB_name: GRB111022A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12476
SUBJECT: GRB 111022A: Swift-BAT refined analysis
DATE:    11/10/22 20:01:20 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), S. Immler (CRESST/GSFC/UMD),
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 recent telemetry downlinks,
we report further analysis of BAT GRB 111022A (trigger #506070)
(Immler, et al., GCN Circ. 12471).  The BAT ground-calculated position is
RA, Dec = 275.871, -23.666 deg, which is 
   RA(J2000)  =  18h 23m 29.1s 
   Dec(J2000) = -23d 39' 58.7" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 66%.
 
The mask-weighted light curve shows two peaks: a small peak starting
at ~T-18 sec, peaking at ~T-12 sec, merging into the main peak
at ~T-8 sec, peaking at ~T-2 sec, and ending at ~T+15 sec.
T90 (15-350 keV) is 24.7 +- 3.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-17.69 to T+18.57 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.01 +- 0.37, 
and Epeak of 64.7 +- 13.9 keV (chi squared 63.3 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.0 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T-1.46 sec in the 15-150 keV band is
2.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.73 +- 0.08 (chi squared 76.5 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/506070/BA/


GRB_name: GRB111020A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12477
SUBJECT: GRB 111020A Spectral lag analysis
DATE:    11/10/22 20:25:56 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), 
J. Norris (BSU), T. N. Ukwatta (MSU)

We report the spectral lag analysis for GRB 111020A (GCN Circ. 12460) 
based on the BAT data.  Using 64 ms binned light curves, the spectral 
lag for 15-25 keV to 50-100 keV is 124 +36/-38 msec.  This significant 
lag is due to a broader pulse in the 15-25 keV band comparing to that 
in the 50-100 keV band which indicates the strong pulse evolution from 
hard to soft.  Although the burst duration itself is short (T90 = 400 ms; 
GCN Circ. 12464), this positive lag argues against a "short" classification.  

However, there is a possibility that the broader pulse seen in the 
15-25 keV band is composed from two pulses instead of a single pulse.  
If this is the case, the lag result above could be confused by 
cross-correlating the 2nd pulse in the 15-25 keV and the 1st pulse 
in the 50-100 keV band.  Due to the limiting signal-to-noise in the 
light curve data, it is not possible to claim whether the broad pulse 
in the 15-25 keV has two pulses or just a single pulse.  

Give the large non-zero lag and the possible double peak interpretation
that could cause a false lag, we think it equally like that this burst 
is short or long. 

[GCN OPS NOTE(24oct11): Per author's request, the T90 value typo
was corrected to 400 ms.]


GRB_name: GRB111022B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12478
SUBJECT: GRB 111022B: Enhanced Swift-XRT position
DATE:    11/10/22 21:50:44 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 885 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111022B, 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 = 108.96498, +49.68362 which is equivalent
to:

RA (J2000): 07h 15m 51.59s
Dec (J2000): +49d 41' 01.0"

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: GRB111022B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12479
SUBJECT: GRB 111022B: NOT observations
DATE:    11/10/23 04:42:13 GMT
FROM:    Paul Vreeswijk at U of Iceland  <pmv@raunvis.hi.is>

Paul Vreeswijk, Annalisa De Cia (U. Iceland), Dong Xu (WIS), Daniele
Malesani (DARK), Pll Jakobsson (U. Iceland) report on behalf of a
larger collaboration:

Using ALFOSC on the Nordic Optical Telescope (NOT) we have obtained R
(3 x 300 s) and I-band (5 x 400 s) imaging of the field of the Swift
GRB 111022B (Holland et al., GCN 12472), starting on 2011 October
23.097 UT (roughly 9.3 hours after the burst). The seeing during the
observations was around 1".

We do not detect any object within the enhanced XRT error circle
(Beardmore et al., GCN 12478), down to limiting magnitudes of about
R>23.2 and I>21.9 (calibrated against the USNO-B1 catalog).

We are grateful to the NOT observer, Terese Hansen (U. Copenhagen),
for obtaining these observations.


GRB_name: GRB111022B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12480
SUBJECT: GRB 111022B: MITSuME Akeno Optical upper limits
DATE:    11/10/23 07:51:48 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

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

We observed GRB 111022B (S.T. Holland et al, GCN12472)
with the optical three color (g, Rc, and Ic) CCD camera attached
to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.
The follow-up observation was started at 18:09:58, ~ 57 min after the
BAT trigger because of bad weather.

We did not find any new point source within the enhanced XRT error
circle (A.P. Beardmore et al, GCN12478) in three bands.


Photometric results and are listed below. We used GSC2.3 catalog for
flux calibration.

T0+[s]      MID-UT     T-EXP[sec]      g'             Rc           Ic
---------------------------------------------------------------------------------
  +7317      19:54:13        540           >17.8       >17.7       ---
  +10426    20:12:52        360            ---             ---        >16.5
---------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12481
SUBJECT: GRB 111022B: Gemini infrared observations
DATE:    11/10/23 13:19:30 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

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

"We observed the localization of GRB 111022B (Holland et al. GCN
12472) with the Gemini-North telescope, equipped with NIRI.
Observations were obtained in poor conditions (2.5" seeing) and
began 17 hours after the burst in the YJHK filters.

We find a single source within the refined XRT error circle (Beardmore
et al. GCN 12478). The source is well detected in both H and K,
with K~19.0 +/- 0.2, but only very weakly in J. Given the earlier
non-detections in the optical (Vreeswijk et al. GCN 12479) the
inferred optical-IR colour is red (R-K > 4.2), coupled with the
lack of apparent excess N_H this could be indicative of a high
redshift burst.

Analysis is ongoing, and further observations are planned."


GRB_name: GRB111022A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12482
SUBJECT: GRB 111022A: Swift-XRT refined Analysis
DATE:    11/10/23 14:15:22 GMT
FROM:    Giulia Stratta at ASDC  <stratta@asdc.asi.it>

G. Stratta (ASDC), V. D'Elia (ASDC) and S. Immler (CRESST/GSFC/UMD)
report on behalf of the Swift-XRT team:

We have analysed 1.1 ks of XRT data for GRB 111022A (Immler  et al. GCN
Circ. 12471), from 775 s to 1.9 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The refined XRT position is RA,
Dec = 275.86481, -23.67325 which is equivalent to:

RA (J2000): 18 23 27.55
Dec(J2000): -23 40 23.7

with an uncertainty of 3.6 arcsec (radius, 90% confidence). The light
curve is consistent with a constant source of mean count rate 1.1e-01
ct/sec. A power-law fit gives an index of 0.2 (+0.6, -0.7).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.6, -0.5). The
best-fitting absorption column is  6.8 (+4.0, -2.7) x 10^21 cm^-2, in
excess of the Galactic value of 2.2 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.4 x 10^-11 (1.0 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.8 (+4.0, -2.7) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: 2.8 sigma
Photon index:      2.3 (+0.6, -0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00506070.

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


GRB_name: GRB111022A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12483
SUBJECT: GRB 111022A: RIzY Observation
DATE:    11/10/23 15:01:33 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im (CEOU/Seoul National Univ), and
Yuji Urata (NCU) on behalf of EAFON

We observed GRB 111022A (Holland et al., GCN 12472)
in R,I,z, and Y filters with a 1.0-m telescope at
Mt. Lemmon, Arizona. The observation started at
10-23-07:52:02 UT, or about 14.5 hrs after the BAT
alert, with total integraion of 10 min in each
filter. No credible afterglow candidate was found at
the enhanced XRT position (Beardmore et al. GCN 12478).

We thank the LOAO operator, J. Youn for his assistance
with the observation.


GRB_name: GRB111022B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12484
SUBJECT: GRB 111022B: Swift-XRT refined Analysis
DATE:    11/10/23 15:38:04 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia, G. Stratta (ASDC), S. T. Holland (CRESST/USRA/GSFC) report
on behalf of the Swift-XRT team:

We have analysed 8.5 ks of XRT data for GRB 111022B (Holland  et al.
GCN Circ. 12472), from 127 s to 18.5 ks after the  BAT trigger. The
data comprise 134 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
Beardmore et al. (GCN. Circ 12478).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.7 (+/-0.9). At T+176 s  the decay
steepens to an alpha of 3.64 (+0.26, -0.22) before breaking again at
T+404 s to a final decay with index alpha=2.05 (+0.26, -0.21).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.41 (+0.14, -0.13). The
best-fitting absorption column is  1.46 (+0.27, -0.26) x 10^21 cm^-2,
in excess of the Galactic value of 7.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.59 (+0.15, -0.12)
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 (5.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+2.7, -0) x 10^20 cm^-2
Galactic foreground: 7.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.59 (+0.15, -0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00506074.

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


GRB_name: GRB111022B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12485
SUBJECT: GRB 111022B, Swift-BAT refined analysis
DATE:    11/10/23 18:40:50 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

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),
S. T. Holland (CRESST/USRA/GSFC), H. A. Krimm (GSFC/USRA),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 111022B (trigger #506074)
(Holland, et al., GCN Circ. 12472). The BAT ground-calculated position is
RA, Dec = 108.927, 49.663 deg which is
   RA(J2000)  =  07h 15m 42.4s
   Dec(J2000) = +49d 39' 45.9"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.

The mask-weighted light curve shows a multi-peak structure starting at
~T-50 sec and ending at ~T+60 sec. T90 (15-350 keV) is 79.1 +/- 13.5
sec (estimated error including systematics).

The time-averaged spectrum from T-47.84 to T+53.80 sec is best fit by a
simple
power-law model. The power law index of the time-averaged spectrum is
1.59 +/- 0.20.  The fluence in the 15-150 keV band is 9.0 +/- 1.2 x 10^-07
erg/cm2.
The 1-sec peak photon flux measured from T+49.54 sec in the 15-150 keV band
is 0.4 +/- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/506074/BA/


GRB_name: GRB111016A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12486
SUBJECT: GRB 111016A: optical upper limit
DATE:    11/10/23 19:32:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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 111016A (Mangano  et al., GCN  12439) 
with 40-cm telescope ORI-40 of Kitab ISON observatory on Oct. 16 starting on 
(UT) 22:07:26. On the stacked image we do not detect any source within the 
enhanced XRT error box (Evans et al., GCN  12441). The photometry is based 
on the reference star SDSS  101516.54+272642.0 assuming (after recalibration 
gri->R) R=17.77:

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

 22:07:26   0.15905  none  36*60       n/d  19.2
 


GRB_name: GRB111022A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12487
SUBJECT: GRB 111022A: Swift/UVOT Upper Limits
DATE:    11/10/23 21:15:38 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and S. Immler (CRESST/GSFC/UMD)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111022A
815 s after the BAT trigger (Immler et al., GCN Circ. 12471).
No optical afterglow consistent with the XRT position (Stratta et
al, GCN Circ. 12482) is detected in the initial UVOT exposures.

The field is very crowded and the detection limits may be affected
in the white filter by the coincidence loss pattern from a
neighboring star.

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

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

white_FC           815          965          147         >21.3
white              815         1287          186         >21.5
v                  972         1859          117         >18.7
b                 1071         1957          117         >19.9
u                 1046         1932          114         >18.9
w1                1021         1908          117         >19.5
m2                 996         1883          117         >21.0
w2                1120         1833           97         >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.66 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111022B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12488
SUBJECT: GRB 111022B: Swift/UVOT upper limits
DATE:    11/10/23 21:29:31 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (MSSL-UCL) and S. T. Holland (CRESST/USRA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111022B
145 s after the BAT trigger (Holland et al., GCN Circ. 12472).
The upper limit of detection was determined at the enhanced XRT position
(Beardmore et al., GCN 12478).

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

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

white_FC           145          294          147         >20.8
u_FC               303          552          246         >20.0
v                  635         6091          452         >19.8
b                  559         6912          452         >20.3
u                  302         6707          678         >20.4
uvw1               685         6501          432         >20.3
uvm2               659         6296          452         >20.3
uvw2               608         5886          255         >20.1
white              145         6975          606         >21.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111024A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12489
SUBJECT: GRB 111024A: MAXI/GSC detection of a burst
DATE:    11/10/24 12:17:51 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

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

MAXI/GSC triggered at UT 2011-10-24T07:21:27 on a bright uncatalogued X-ray 
transient source.  Judging from its location and spectral hardness ratio, 
this transient is probably a gamma-ray burst. 
Assuming that the source flux was constant over the transit, 
we obtain the source position at

(R.A., Dec) = (+222.18 deg, +25.84 deg) = (14 48 42, +25 50 40)(J2000)  

with a rectangular error box (90%C.L.) with the following corners: 

(R.A., Dec) = (+222.22 deg, +25.74 deg) = (14 48 54, +25 44 11)(J2000) 
(R.A., Dec) = (+222.32 deg, +25.86 deg) = (14 49 16, +25 51 37)(J2000) 
(R.A., Dec) = (+222.13 deg, +25.95 deg) = (14 48 31, +25 57 15)(J2000) 
(R.A., Dec) = (+222.04 deg, +25.83 deg) = (14 48  9, +25 49 49)(J2000) 

There is additional systematic uncertainty of 0.2 deg (90% containment radius).
The preliminary flux of the transient source was 700 mCrab (4-10 keV).
There was no significant detection at the transit location in the
previous orbit (92 min before the detection) with an upper limit of 20 mCrab.  
There is no known bright X-ray source at the detected position. 

Follow-up observations are encouraged.


GRB_name: GRB111022A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12490
SUBJECT: GRB 111022A: MITSuME Akeno Optical upper limits
DATE:    11/10/24 12:25:42 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

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

We observed GRB 111022A (S. Immler et al, GCN12471)
with the optical three color (g, Rc, and Ic) CCD camera attached
to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2011-10-23 9:16:56 UT (~16.8 h after the burst).
We did not find any new point source within the Swift XRT error
circle (G. Stratta et al, GCN12482) in 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
---------------------------------------------------------------------------------
 0.71519     9:47:22        3060         >18.4       >16.5       >16.5
---------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12491
SUBJECT: GRB 111022B: BTA Optical Observations
DATE:    11/10/24 19:37:43 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. S. Moskvitin, V. N. Komarova, V. V. Sokolov and T. N. Sokolova
(SAO RAS GRB follow-up team) report:

The field of GRB 111022B (Holland et al., GCN#12472) was observed
with the 6-m BTA/Scorpio on October, 23, 2011. We obtained 3 x 180 sec.
frames in the Rc band and 25 x 120 sec. in the Ic band.
Observations in Rc began at 00:40:10 (7.5 hours after the trigger),
ended at 00:50:21 UT; in Ic began at 01:23:11 UT (8.2 hours after the
trigger), ended at 02:22:40 UT. Conditions were clear with a seeing
of about 1".2 (FWHM of stellar objects in the Ic co-added image).

The possible optical counterpart is clearly detected in the Ic band
within the 1".5 XRT error circle (according to
http://www.swift.ac.uk/xrt_positions/) at the coordinates:
R.A.  (J2000) = 07:15:51.56
Decl. (J2000) = +49:41:01.7
with the uncertainty 0".2.

The object magnitude is I = 23.6 +/- 0.3 as compared to USNO-B1.0 Imag
of six nearby stars. The high error is due to calibration, the 3-sigma
limit of the Ic co-added image is about 24.7. We do not detect the object
in the Rc-band down to the 3-sigma level limiting magnitude of about 24.3.
The Ic image can be found at
ftp://ftp.sao.ru/pub/grb/GRB111022B/GRB111022B_BTA.jpg

Our results are in agreement with the previously reported NOT observations
(Vreeswijk et al., GCN#12479) and do not contradict the idea of a high
redshift burst according to Gemini infrared observations (Levan et al.,
GCN#12481).

We are grateful to T. A. Fatkhullin
and the BTA staff for the help in observations.


GRB_name: GRB111020A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12492
SUBJECT: GRB 111020A: Chandra Observation
DATE:    11/10/24 20:28:14 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger, R. Margutti, and W. Fong (Harvard) report:

"We observed the field of the short GRB 111020A (GCN 12640) with the Chandra
X-ray Observatory + ACIS-S starting on 2011 October 23.14 UT (2.86 days
after the burst) for a total of 19.8 ksec.  We clearly detect a source in
coincidence with the enhanced XRT error circle (GCN 12463) at the following
coordinates (J2000):

RA = 19:08:12.502
DEC = -38:00:42.58

with an uncertainty of about 0.5".  The position includes a minor correction
to the Chandra astrometry using two X-ray sources with stellar counterparts
in our Gemini i-band images (which were astrometrically matched to the 2MASS
catalog; GCNs 12467, 12470).  The Chandra position is offset by 1.2" from
the centroid of the most recent XRT position (which has a 90% containment
uncertainty of 1.6").  Further analysis of the Chandra data is on-going.

We thank Harvey Tananbaum and the CXO scheduling staff for rapidly approving
and executing this observation."


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12493
SUBJECT: GRB111022B: D50 optical limit
DATE:    11/10/25 02:58:35 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

M. Blazek (AsU AV), R. Hudec (AsU AV), M. Jelinek (IAA-CSIC),
C. Polasek (AsU AV) and J. Strobl (AsU AV)


"We observed the field of GRB 111022B (Holland et al., GCN
12472) with 0.5m robotic telescope D50 in Ondrejov observatory
(Czech Republic). The observation started at 23:55:06 UT on
October 22, 2011, approx. 6.5 hours after the Swift trigger.

We report no detection of the optical counterpart on the
unfiltered images within the error circle given by SWIFT-XRT
(Beardmore et al., GCN 12478). The limiting magnitude of about
R>20.0 mag in R-band was estimated using nearby sources from
GSC2.2 catalogue."


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12494
SUBJECT: GRB 111022B: 10.4m GTC z'-band observations
DATE:    11/10/25 10:15:40 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC), A. Cabrera Lavers (GTC), R. Sanchez-Ramirez  
(IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), A.J. Levan (U.  
Warwick), C.C. Thoene (IAA-CSIC), N.R. Tanvir (U. Leicester), A.J.  
Castro-Tirado (IAA-CSIC), P. Kubanek (IAA-CSIC, U. Valencia), report  
on behalf of a larger collaboration:

We acquired z'-band images of the GRB 111022B field (Holland et al.,  
GCNC 12472; Beardmore et al., GCNC 12478) with the 10.4m GTC(+OSIRIS)  
telescope. The observations were carried out on Oct 24.1105--24.1453  
UT (33.4--34.3 hours post GRB) with a total exposure time of  
31x60s=1860s and a seeing of 1.0-1.5". A faint object is detected  
coincident with the near-IR and optical candidate (Levan et al.  GCNC  
12481; Moskvitin et al. GCNC 12491). This source has a very  
preliminary AB magnitude of  z'~25.5. In the XRT error circle  
(Beardmore et al., GCNC 12478) we note the presence of an additional  
object with a similar magnitude located 1.5" eastwards from the  
afterglow candidate.


GRB_name: GRB111022B
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12495
SUBJECT: GRB 111022B:  EVLA observations
DATE:    11/10/26 03:49:15 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer and E. Berger (Harvard) report:

"We observed the position of GRB 111022B (GCN 12472) with the EVLA at
5.8 and 22 GHz beginning on 2011 Oct 23.64 UT (0.92 days after the
burst).  No radio source is detected at 5.8 GHz to a 3-sigma upper limit 
of 30 uJy.  At 22 GHz, a potential radio counterpart was detected with a 
flux of 45+/-14 uJy, consistent with the most up-to-date 1.5'' Swift-XRT 
position (GCN 12478, http://www.swift.ac.uk/xrt_positions).  The 
potential radio source centroid is (J2000):

RA  =  07:15:51.53 +/- 0.05
Dec = 09:41:01.18 +/- 0.37

Follow-up observations at 22 GHz are planned."


GRB_name: GRB111022B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12496
SUBJECT: GRB 111022B:  EVLA observations - correction to GCN 12495
DATE:    11/10/26 04:35:32 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer and E. Berger (Harvard) report:

The declination given in GCN 12495 was incorrect.

"We observed the position of GRB 111022B (GCN 12472) with the EVLA at
5.8 and 22 GHz beginning on 2011 Oct 23.64 UT (0.92 days after the
burst).  No radio source is detected at 5.8 GHz to a 3-sigma upper limit 
of 30 uJy.  At 22 GHz, a potential radio counterpart was detected with a 
flux of 45+/-14 uJy, consistent with the most up-to-date 1.5'' Swift-XRT 
position (GCN 12478, http://www.swift.ac.uk/xrt_positions).  The 
potential radio source centroid is (J2000):

RA  =   07:15:51.53 +/- 0.05
Dec =  +49:41:01.18 +/- 0.37

Follow-up observations at 22 GHz are planned."


GRB_name: GRB111026A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12497
SUBJECT: GRB 111026A: Swift detection of a burst
DATE:    11/10/26 07:04:53 GMT
FROM:    Wayne Baumgartner at GSFC  <wayne@milkyway.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC),
P. A. Evans (U Leicester), C. Guidorzi (U Ferrara),
O. M. Littlejohns (U Leicester), C. J. Mountford (U Leicester) and
K. L. Page (U Leicester) report on behalf of the Swift Team:

At 06:47:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111026A (trigger=506291).  A pointing constraint prevented 
Swift from slewing immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 244.275, -47.495 which is 
   RA(J2000) = 16h 17m 06s
   Dec(J2000) = -47d 29' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked 
structure with a duration of about 1.5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 14:29 UT on 2012 January 12. There will thus be no XRT
or UVOT data for this trigger before this time. 

This burst is only two degrees off the Galactic plane and could be 
a Galactic transient. 

Burst Advocate for this burst is W. H. Baumgartner (wayne 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: GRB111029A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12498
SUBJECT: GRB 111029A: Swift detection of a burst
DATE:    11/10/29 10:02:02 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

E. Troja (NASA/GSFC/ORAU), S. Campana (INAF-OAB),
P. A. Evans (U Leicester), C. Guidorzi (U Ferrara),
E. A. Hoversten (PSU), V. Mangano (INAF-IASFPA),
C. J. Mountford (U Leicester), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 09:44:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111029A (trigger=506519).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 44.691, +57.085 which is 
   RA(J2000) = 02h 58m 46s
   Dec(J2000) = +57d 05' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of at least 20 sec from T+20 to T+40. 
The peak count rate was ~1500 counts/sec (15-350 keV), at ~23 sec
after the trigger. 

The XRT began observing the field at 09:47:39.0 UT, 178.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 44.78260, 57.11024 which is equivalent
to:
   RA(J2000)  = 02h 59m 7.82s
   Dec(J2000) = +57d 06' 36.9"
with an uncertainty of 4.4 arcseconds (radius, 90% containment). This
location is 200 arcseconds from the BAT onboard position. 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. As this position is
significantly outside the BAT error circle, it is probably unrelated to
the trigger. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 6.27
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of  71 seconds with the White filter
starting 163 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 large, but
uncertain extinction expected. 

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


GRB_name: GRB111029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12499
SUBJECT: GRB 111029A: ROTSE-III Optical Limits
DATE:    11/10/29 10:11:34 GMT
FROM:    Wiphu Rujopakarn at U AZ/Steward  <rujopakarn@gmail.com>

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

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
111029A (Swift trigger 506519; Troja, GCN 12498), producing images
beginning 7.7 s after the GCN notice time. An automated response took
the first image at 09:46:34.7 UT, 114.2 s after the burst, under
excellent conditions. We took 10 5-sec, 10 20-sec and 20 60-sec
exposures. These unfiltered images are calibrated relative to USNO
A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle or the XRT error circle, for both
single images and coadding into sets of 10; the field is not crowded.
Individual images have limiting magnitudes ranging from 16.9-17.6; we
set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
09:46:34.7   09:46:39.7         5     17.2          114.2       N
09:46:34.7   09:48:21.8       107     18.0          114.2       Y


GRB_name: GRB111029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12500
SUBJECT: GRB 111029A: optical upper limit  
DATE:    11/10/29 12:04:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (ISON),  A. Pozanenko (IKI), I. Molotov (KIAM) report on behalf of 
larger GRB  follow-up collaboration:

We observed the field of  GRB 111029A (Swift trigger 506519; Troja et al., 
GCN 12498) with 0.45-m telescope f ISON-NM observatory  starting in 
automatic response mode on  Oct. 29 (UT) 09:47:47, i.e. 187 s after burst 
trigger.  We took 31 unfiltered images.  We do not detect any source within 
XRT error circle.   The photometry of a single and co-added frames is based 
on the USNO-B1.0  nearby stars (R magnitudes):

T_start,   T0+,       Exposure, OT,  Upper Limit (3sigma)
(UT)        (mid, s)   (s)

09:47:47    216.5        60       n/d    18.3
09:47:47   1101.5  15x60       n/d    19.5
09:47:47   1385.0  31x60       n/d    20.3

 


GRB_name: GRB111029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12501
SUBJECT: GRB 111029A: Faulkes Telescope North observations
DATE:    11/10/29 12:14:50 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara) reports on behalf of a
large collaboration:

The 2-m Faulkes Telescope North robotically followed
up Swift GRB 111029A (Troja et al. GCN Circ. 12498)
from 09:49:03 UT, corresponding to 263 s after the
BAT trigger time.
Within the XRT error circle we do not find any source
in the R and i' filters down to the following magnitudes:

Mid time from  Total Exp   Filter    Magnitude
trigger (s)    (s)
-------------------------------------------------
  908            120         R > 21.8
1118            100         i' > 20.5
-------------------------------------------------

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


GRB_name: GRB111029A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12502
SUBJECT: GRB 111029A: Enhanced Swift-XRT position
DATE:    11/10/29 13:10:48 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 57 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111029A, 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 = 44.78376, +57.11122 which is equivalent
to:

RA (J2000): 02h 59m 8.10s
Dec (J2000): +57d 06' 40.4"

with an uncertainty of 2.5 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB111029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12503
SUBJECT: GRB 111029A: TNT optical upper limit
DATE:    11/10/29 13:30:29 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 111029A (Troja  al., GCN 12498)
with Xinglong TNT telescope at 10:35:49 (UT), about 51 min  after 
the burst.  15 R-band images were obtained under a bad seeing. 
No new source was detected in the combined R band image within 
the errorbox of XRT position. The upper limit was estimated 
to be about 19.6 mag derived from USNO B1.0 R2mag. 

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

[GCN OPS NOTE(30oct11): The "110929A" was corrected to "111029A";
see correction Circ 12510.]


GRB_name: GRB111029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12504
SUBJECT: GRB 111029A: Swift-BAT refined analysis 
DATE:    11/10/29 16:11:50 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
E. Troja (NASA/GSFC/ORAU), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111029A (trigger #506519)
(Troja, et al., GCN Circ. 12498).  The BAT ground-calculated position is
RA, Dec = 44.785, 57.101 deg, which is 
   RA(J2000)  =  02h 59m 08.4s 
   Dec(J2000) = +57d 06' 02.9" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
 
The mask-weighted light curve shows 2 or 3 overlapping peaks starting
at ~T+15 and ending at ~T=35 sec.  T90 (15-350 keV) is 7.6 +- 1.1 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+19.60 to T+28.92 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.77 +- 0.71, 
and Epeak of 36.2 +- 5.7 keV (chi squared 39.5 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.9 +- 0.4 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+23.62 sec in the 15-150 keV band is
1.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.11 +- 0.13 (chi squared 53.6 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/506519/BA/


GRB_name: GRB111029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12505
SUBJECT: GRB 111029A: KAIT optical limits
DATE:    11/10/29 18:03:13 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li and A. V. Filippenko, University of California
at Berkeley, on behalf of the KAIT GRB team, report:

The robotic 0.8-m KAIT located at Lick Observatory responded to
GRB 111029A (Swift trigger 506519; Troja et al. GCN 12498) automatically
and started the first image at 09:47:15 UT (154.5 seconds after the burst).
A series of images were taken in the V, I, and clear filters.
No new sources were detected within the Swift/XRT error circle
in the KAIT images (single or stacked frames) when compared to
the DSS II. We set the following specific limits (calibrated
to USNO B1): 

start UT       end UT      t_exp(s)   mlim (unfilt.)  coadd?
---------------------------------------------------------------
09:47:15.0   09:47:17.0        2      18.0            N 
09:47:15.0   09:47:46.0       20      19.0            Y (2s x 10) 


GRB_name: GRB111029A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12506
SUBJECT: GRB 111029A: Swift/UVOT Upper Limits
DATE:    11/10/29 18:32:13 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 111029A
164 s after the BAT trigger (Troja et al., GCN Circ. 12498).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 12502) is detected in the initial UVOT  
exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the initial exposures are:

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

white (FC)         164          235           70         >20.5
white              164         5606          463         >21.6
v                 4381         6010          387         >19.6
b                 3765         5401          393         >21.0
u                 3560         5196          393         >20.9
w1                4791         4991          197         >20.0
m2                4586         4786          197         >20.6
w2                4177         5812          393         >21.0

The magnitudes in the table are not corrected for the Galactic  
extinction
due to the reddening of E(B-V) = 1.55 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111026A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12507
SUBJECT: GRB 111026A: Swift-BAT refined analysis
DATE:    11/10/29 20:00:17 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+963 sec from telemetry downlinks,
we report further analysis of BAT GRB 111026A (trigger #506291)
(Baumgartner, et al., GCN Circ. 12497).  The BAT ground-calculated position is
RA, Dec = 244.256, -47.435 deg, which is 
   RA(J2000)  =  16h 17m 01.5s 
   Dec(J2000) = -47d 26' 05.1" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a couple overlapping pulses starting
at ~T-0.5 and ending at ~T+4 sec.  T90 (15-350 keV) is 3.62 +- 1.11 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.09 to T+4.07 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.69 +- 0.21.  The fluence in the 15-150 keV band is 1.7 +- 0.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band
is 1.1 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/506291/BA/


GRB_name: GRB111029A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12508
SUBJECT: GRB 111029A: PAIRITEL NIR Upper Limits
DATE:    11/10/29 22:49:08 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 111029A (Troja et al., GCN 12498) with
the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began
at 2011-10-29 09h47m33 UT, ~2.9 minutes after the Swift Trigger.  In
mosaics taken simultaneously in the J, H, and Ks filters, we do not
detect any source within the enhanced XRT error circle (Evans et al.,
GCN 12502) in the coaddition of the first few minutes of data nor the
first hour.

The preliminary photometry yields:

post burst
t_mid(s) exp.(s) filt  U. Limit (3 sig)
551      351     J     > 17.9
551      351     H     > 16.6
551      351     Ks    > 15.7
1837.5   1919    J     > 18.5
1837.5   1919    H     > 17.5
1837.5   1919    Ks    > 16.6


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: GRB111029A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12509
SUBJECT: GRB 111029A: Swift-XRT refined Analysis
DATE:    11/10/30 10:03:23 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@le.ac.uk>

O. M. Littlejohns (U. Leicester) and E. Troja (NASA/GSFC/ORAU) report
on behalf of the Swift-XRT team:

We have analysed 19 ks of XRT data for GRB 111029A (Troja  et al. GCN
Circ. 12498), from 163 s to 58.0 ks after the  BAT trigger. The data
comprise 25 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 12502).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.06 (+0.07, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.6 (+0.7, -0.5). The
best-fitting absorption column is  1.5 (+0.6, -0.3) x 10^22 cm^-2, in
excess of the Galactic value of 6.3 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 5.0 x 10^-11 (2.1 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.5 (+0.6, -0.3) x 10^22 cm^-2
Galactic foreground: 6.3 x 10^21 cm^-2
Excess significance: 3.9 sigma
Photon index:      2.6 (+0.7, -0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00506519.

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


GRB_name: GRB111029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12510
SUBJECT: GRB 111029A: TNT optical upper limit, Correction to GCN 12503
DATE:    11/10/30 13:09:44 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:

The burst given in GCN 12503 should be GRB111029A, 
but not  GRB 110929A. We apologize for this typo. 

"We began to observe GRB 111029A (Troja  al., GCN 12498)
with Xinglong TNT telescope at 10:35:49 (UT), about 51 min  after 
the burst.  15 R-band images were obtained under a bad seeing. 
No new source was detected in the combined R band image within 
the errorbox of XRT position. The upper limit was estimated 
to be about 19.6 mag derived from USNO B1.0 R2 mag. 

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: GRB111029A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12511
SUBJECT: GRB111029A: MITSuME Ishigakijima Optical Upper Limits
DATE:    11/10/30 13:25:56 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 111029A (Troja et al., GCNC 12498)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2011-10-29 15:49:45 UT, (~6.1 h after the burst).
We did not find any new point source within the enhanced XRT error
circle (Evans et al., GCNC 12502) in all the three 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    Ic
-----------------------------------------------------
0.30785    17:07:59   13140.0   >22.6  >22.0  >20.7
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111026A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12512
SUBJECT: GRB 111026A: spectral lag value inconclusive for a short burst
DATE:    11/10/30 18:13:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. Norris (BSU), N. Gehrels (GSFC):

We report the spectral lag analysis for GRB 111026A (GCN Circ. 12497) 
based on the BAT data.  Using 64 ms binned light curves, the spectral 
lag for 15-25 keV to 50-100 keV is 27 +32/-40 msec.  This value
is not very constraining towards the shortness of this burst.  
And further, the fact that the burst is longer in the 15-25 keV band
than in the higher energy band argues for a long burst assignment.


GRB_name: GRB111029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12514
SUBJECT: GRB 111029A: Super-LOTIS early limits
DATE:    11/10/30 19:34:42 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 111029A (Troja et al., GCN 12498) with the
robotic Super-LOTIS telescope under good conditions beginning 142 seconds
after the BAT trigger.  Our observations consisted of 5 10-sec images, 5
20-sec images, and 30 60-sec images in the R band.

Stacked images reveal no new sources in the XRT enhanced error circle
(Evans et al., GCN 12502) brighter than 19.5 magnitudes in R as calibrated
relative to the USNO B1.0 catalog.

This message may be cited.


GRB_name: GRB111029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12515
SUBJECT: GRB 111029A: SAO RAS optical limits
DATE:    11/10/31 18:53:30 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. S. Moskvitin and V. V. Sokolov report on behalf of larger collaboration:

The field of GRB 111029A (Troja et al., GCN#12498) was observed
with the Zeiss-1000 telescope of SAO RAS (Russia) on October 29/30 night.
12 x 300 sec. in Rc and 12 x 300 sec. in Ic images were obtained
under the good conditions and the seeing 2" (FWHM of stellar-like objects
at the co-added images). The observation started at 21:31:21 October 29
(since 11.8 hours after the trigger), finished at 00:33:51 October, 30 UT.

No optical counterpart was detected within the XRT 1".9 error circle
(according to http://www.swift.ac.uk/xrt_positions/ ) up to the 3 sigma
limiting magnitudes R_lim = 24.6 and I_lim = 23.3. The calibration was done
against R2 and I magnitudes of nearby USNO B-1.0 stars. The Rc and Ic images
can be found at ftp://ftp.sao.ru/pub/grb/GRB111029A/GRB111029A.jpg

The closest object is located 4".65 South-West from the center of XRT
error circle. The brightness of this object is R = 22.99 +/- 0.32,
I = 21.79 +/- 0.28 (the high error is due to calibration) and the
coordinates are R.A.(J2000) = 02:59:07.71, Dec.(J2000) = +57:06:35.5,
with the uncertainty 0".21. Due to cosmological nature of GRBs
this object probably can not be related to the GRB 111029A.


GRB_name: GRB111029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12516
SUBJECT: GRB 111029A: RAPTOR Limits During the Gamma-ray Emitting Interval
DATE:    11/10/31 23:17:42 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 wide-field optical monitors made observations of Swift trigger 506519 (Troja et al., GCN 12498) during the gamma-ray emitting interval.  These systems began 10 s exposures at 09:44:40 UTC, coincident with the BAT trigger time, and 09:45:00, coincident with the primary interval in which BAT observed the most prominent gamma-ray emission.  No counterpart was detected in any of the unfiltered images taken by the sky monitoring systems with 3-sigma limiting magntiudes of 10.7 when compared with the Tycho-2 V-band.


GRB_name: GRB111103A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12518
SUBJECT: GRB 111103A: Swift detection of a burst
DATE:    11/11/03 10:54:18 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. C. Stroh (PSU), W. H. Baumgartner (GSFC/UMBC),
S. Campana (INAF-OAB), P. A. Evans (U Leicester),
E. A. Hoversten (PSU), V. Mangano (INAF-IASFPA),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/IASFPA) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift Team:

At 10:35:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111103A (trigger=506902). 
The BAT on-board calculated location is 
RA, Dec 327.122, -10.547 which is 
   RA(J2000) = 21h 48m 29s
   Dec(J2000) = -10d 32' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiple-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~4800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 20:12 UT on 2011 November 05. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is M. C. Stroh (stroh AT astroh.org). 
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: GRB111103B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12519
SUBJECT: GRB 111103B: Swift detection of a strong burst from a GRB or Galactic source
DATE:    11/11/03 11:22:49 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Grupe (PSU), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), A. Melandri (INAF-OAB),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), M. C. Stroh (PSU) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:

At 10:59:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111103B (trigger=506903).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 265.704, +1.590 which is 
   RA(J2000) = 17h 42m 49s
   Dec(J2000) = +01d 35' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a bright main peak from T+0 to T+20 s and continued
activity to a duration of at least 150 sec.  The peak count rate
was ~15000 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 11:00:03.1 UT, 59.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 265.6955, +1.6107 which is equivalent to:
   RA(J2000)  = 17h 42m 46.91s
   Dec(J2000) = +01d 36' 38.5"
with an uncertainty of 5.1 arcseconds (radius, 90% containment). This
location is 79 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 102 seconds with the U filter starting
281 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. 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
0.29. 

We note that this location is in a crowded field 30 degrees from the
Galactic center.  In particular the XRT position is near (7.4 arcseconds)
the high proper motion star G 20-10.  Thus this burst may be from a
Galactic source.  We will require data from the Malindi ground link
to make this determination. 

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


GRB_name: GRB111103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12520
SUBJECT: GRB 111103B: optical observations 
DATE:    11/11/03 11:44:11 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, 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
  Kislovodsk Solar Station of the Pulkovo Observatory

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

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

  MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka(Siberia) was pointed to the  GRB111103.46 19 sec s after 
notice time and 42 sec after GRB time at 2011-11-03 10:59:45.246 UT. On 
our first unfiltered 10s exposure set we haven't found optical transient 
within  SWIFT error-box (Grupe et al, GCN Circ 12519).

  The 5-sigma upper limit has been about 14.7mag

  The message may be cited.


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12521
SUBJECT: GRB 111022B: MASTER OT observations
DATE:    11/11/03 11:46:35 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


  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, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. 
Kornilov,A.Sankovich
  Sternberg Astronomical Institute, Moscow State University


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

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


MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in 
Tunka(Siberia) was pointed to the GRB110801A 101 sec after GRB time at 
2011-08-01 19:51:23 UT. Unfortunatelly the objects was not in focus  because 
recently photometer modification.  On our first (20s
exposure) set we haven't found optical transient within SWIFT error-box
(De Pasquale et al., GCN 12228).
The 3-sigma upper limit has been about 14.0 mag (white+polarizator).


MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located 
near Kislovodsk (Caucasus Mountains)  closed roof 20 min before trigger due to 
cloudy condidtions. The telescope was repointed to the
GRB110901A  only 47 min 40 sec after trigger time at 2011-08-01 20:37:22 UT.
We found OT at UVOT postion (De Pasquale et al., GCN 12228).
The results of our photometry are:

Time_Start    T_mean-T_trig  exp time       m        error      Band UT 
s          s 20:37:22          2950        180         16.13       0.06 
R
20:44:29          3377        180         16.12       0.06        R 20:48:01 
3589        180         16.29       0.08        R
20:48:01          3589        180         16.03       0.06     White 20:51:24 
3792        180         16.43       0.06        R
20:51:24          3792        180         16.19       0.06     White
23:20:14         12722        180         17.75       0.10        R

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).

The power low index (F~t^-aplha) apha ~1.0+-0.1     during this observations in 
R-band.

The message may be cited.


GRB_name: GRB111103A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12523
SUBJECT: GRB 111103A: Swift-BAT refined analysis
DATE:    11/11/03 15:18:22 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), M. Stamatikos (OSU),
M. C. Stroh (PSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+358 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111103A (trigger #506902)
(Stroh, et al., GCN Circ. 12518).  The BAT ground-calculated position is
RA, Dec = 327.111, -10.532 deg, which is 
   RA(J2000)  =  21h 48m 26.7s 
   Dec(J2000) = -10d 31' 54.3" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 31%.
 
The mask-weighted light curve shows 4 almost overlapping peaks with the
first starting at ~T-0.5 sec, peaks at T+1, +4, +6, and +12 sec,
and the last peak ending at ~T+20 sec.  T90 (15-350 keV) is 11.6 +- 0.5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.42 to T+12.14 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.30 +- 0.10.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+6.04 sec in the 15-150 keV band
is 3.1 +- 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/506902/BA/


GRB_name: GRB111103B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12524
SUBJECT: GRB 111103B: Swift-BAT refined analysis
DATE:    11/11/03 15:45:44 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), D. Grupe (PSU), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+418 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111103B (trigger #506903)
(Grupe, et al., GCN Circ. 12519).  The BAT ground-calculated position is
RA, Dec = 265.691, 1.605 deg which is 
   RA(J2000)  =  17h 42m 45.8s 
   Dec(J2000) = +01d 36' 19.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.
 
The mask-weighted light curve shows at least 4 overlapping peaks in the first
group: starting at ~T-25 sec, with the brightest peak at ~T+8 sec, and ending
at ~T+90 sec.  The second group of peaks starts at ~T+100 sec and ends
at ~T+250 sec.  T90 (15-350 keV) is 167 +- 35 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-6.55 to T+250.78 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.41 +- 0.05.  The fluence in the 15-150 keV band is 8.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+5.48 sec in the 15-150 keV band
is 7.2 +- 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/506903/BA/


GRB_name: GRB111103B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12525
SUBJECT: GRB 111103B: Enhanced Swift-XRT position
DATE:    11/11/03 16:12:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1541 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 111103B, 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 = 265.69322, +1.61007 which is equivalent
to:

RA (J2000): 17h 42m 46.37s
Dec (J2000): +01d 36' 36.3"

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

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

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


GRB_name: GRB111103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12527
SUBJECT: GRB 111103B: optical observations from TAU, Ka-Dar
DATE:    11/11/03 17:52:12 GMT
FROM:    Denis Denissenko at IKI, Moscow  <d.v.denisenko@gmail.com>

D. Denisenko (IKI, Moscow), V. Gerke and S. Korotkiy (Ka-Dar
observatory, Russia) report:

Position of GRB 111103B (Grupe et al., GCN 12519; Barthelmy et al.,
GCN 12524; Goad et al., GCN 12525) was observed by 40-cm Djigit
telescope of Ka-Dar observatory's TAU station (Nizhniy Arkhyz,
Karachay-Cherkessia) equipped with SBIG STL-11K CCD from 15:35 UT to
16:04 UT on 2011 Nov. 03 (4.6-5.1 hr after the burst trigger). In
total, 10 unfiltered 120-sec exposures were taken.

There are no new sources detected in the error box of GRB 111103B on
the combined image, as compared to Red DSS plate of similar depth. The
limiting magnitude of the combined image (SNR=3) is R~20.2. The sum of
nine best frames (effective exposure of 18 minutes centered at 15:50
UT) is available at http://pics.livejournal.com/bigdenru/pic/000ak676/
(5'x5' crop).

We have also measured the light curve of the nearby star G 20-10 =
2MASS 17424702+0136326 (J=11.060+/-0.023, K=10.232+/-0.023) to check
for its variability. The star has remained constant within 0.01 mag
during our 0.5 hr observations. It is far from saturation with no more
than 13000 ADU on the individual images.

This message can be cited.


GRB_name: GRB111103B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12528
SUBJECT: GRB111103B Swift/UVOT Upper Limits
DATE:    11/11/03 21:26:25 GMT
FROM:    Patricia Schady at MPE/Swift  <msslba@googlemail.com>

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

The Swift/UVOT began settled observations of the field of GRB 111103B
68 s after the BAT trigger (Grupe et al., GCN Circ. 12519).
No optical afterglow consistent with the XRT position (Goad et al., GCN Circ. 12525)
is detected in the initial UVOT exposures.  The lack of an optical detection at the XRT 
refined position excludes the possibility that the trigger is associated with the high proper 
motion star (v~15mag) mentioned in Grupe et al. (GCN Circ. 12519) confirming that 
the BAT trigger 506903 is a GRB.

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

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

white_FC            68          218          147         >20.6
white               68         5055          344         >21.1
v                 5266         5466          197         >19.1
b                 4650         6161          270         >20.0
u                  281         6081          297         >20.2
w1                5677         5876          197         >19.9
m2                5471         5670          197         >19.8
w2                5061         5261          197         >20.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.29 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111103A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12529
SUBJECT: GRB 111103A: Fermi GBM observation
DATE:    11/11/03 21:56:48 GMT
FROM:    David Tierney at UCD  <david.tierney@ucd.ie>

D. Tierney (UCD)
reports on behalf of the Fermi GBM Team:

At 10:35:13.39 UT on 03 November 2011, the Fermi Gamma-Ray Burst Monitor
triggered and observed GRB 111103A (trigger 342009315/111103441),
which was detected by the Swift/BAT (Stroh et al. 2011, GCN 12518).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of multiple peaks
with a duration (T90) of 11.78 +/- 1.18 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+13.7 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.43 (+0.16/-0.15) and
the cutoff energy, parameterized as Epeak, is 152.2 (+16.1/-12.8) keV.

The event fluence (10-1000 keV) in this time interval is
(3.20 +/- 0.19)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.13 s in the 10-1000 keV band is 5.2 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB111103B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12530
SUBJECT: GRB 111103B: Swift-XRT refined Analysis
DATE:    11/11/04 02:24:06 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

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

We have analysed 5.1 ks of XRT data for GRB 111103B (Grupe  et al. GCN
Circ. 12519), from 49 s to 33.3 ks after the  BAT trigger. The data
comprise 335 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 12525).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.1 (+0.4, -0.3). At T+94.2 s  the decay
flattens to an alpha of 0.59 (+0.05, -0.07) before breaking again at
T+8356 s to a final decay with index alpha=1.32 (+0.13, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.97 (+0.05, -0.04). The
best-fitting absorption column is  2.90 (+0.16, -0.15) x 10^21 cm^-2,
in excess of the Galactic value of 9.1 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.85 (+0.13, -0.12)
and a best-fitting absorption column of 2.7 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.4 x 10^-11 (6.3 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 9.1 x 10^20 cm^-2
Excess significance: 9.8 sigma
Photon index:      1.85 (+0.13, -0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00506903.

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


GRB_name: GRB111103B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12531
SUBJECT: GRB 111103B : WIYN 3.5m NIR observations
DATE:    11/11/05 00:57:24 GMT
FROM:    Atish Kamble at U. of Wisconsin  <atish@gravity.phys.uwm.edu>

Ralf Kotulla, Atish Kamble, David Kaplan (UW-Milwaukee) and Nial Tanvir (U.
Leicester) report :

We observed the field of strong GRB 111103B (Palmer et al., GCN 12519)
using the WIYN High Resolution Infrared Camera (WHIRC) on the WIYN 3.5m
telescope,  beginning at November 4.08 (UT), approximately 15 hours after
the burst.  Observations were carried out using the Ks filter, and the seeing
was about 1 arcsec.

We detect a faint object within the improved XRT error circle (Goad et al.,
GCN 12525).  The preliminary magnitude of this source is K = 18.6 +/- 0.4,
but our observations do not allow us to make any statement about variability.
The source appears point-like, but the poor signal-to-noise means we could
not rule out it being slightly extended.

Further deep observations are encouraged for variability check and possible
association with the GRB.

The combined WIYN image of the field is available at :
http://members.galev.org/shared/GRB_111103B/whirc_zoom.jpg

We acknowledge the support from the staff of WIYN-3.5m telescope, and
especially from Greg Mosby in carrying out these observations.


GRB_name: GRB111103B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12532
SUBJECT: Konus-Wind observation of GRB 111103B
DATE:    11/11/05 13:12:31 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 GRB 111103B (Swift-BAT trigger #505054:
Grupe et al., GCN 12519; Barthelmy et al., GCN 12524)
triggered Konus-Wind at T0=39541.020s UT (10:59:01.020)

The light curve shows a ~15 s long pulse followed by
a weaker activity continuing till ~(T0+40)s. The second group
of peaks observed by Swift/BAT after T0+100
is poorly determined in the Konus-Wind light curves
against the background of a rising M2.5 Solar flare.
The emission in the initial peak complex is seen up to ~4 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111103_T39541/

As observed by Konus-Wind the burst
had a fluence of (2.0 +/-0.3)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+5.120 s,
of (2.7 +/-0.4)x10-6 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+41.216 s)
is best fitted in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.97 (-0.18, +0.19),
and Ep = 372(-69, +109) keV,
chi2 = 77.2/77 dof.
Fitting this spectrum by the GRB (Band) function yields
the same alpha and Ep with a high energy photon index
beta < -2.2 (chi2 = 77.1/76 dof).

The spectrum at the maximum count rate
(measured from T0 to T0+6.144 s)
is best fitted in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.97 (-0.12, +0.14),
and Ep = 393(-55, +76) keV,
chi2 = 70.2/77 dof.

All the observed properties are typical for a moderately intense
long gamma-ray burst and don't argue for a Galactic transient hypothesis.

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


GRB_name: GRB111103B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12533
SUBJECT: GRB 111103B: MITSuME Akeno Optical upper limits
DATE:    11/11/05 13:40:02 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

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

We observed GRB 111103B (D. Grupe et al, GCN12519) with the
optical three color (g, Rc, and Ic) CCD camera attached to the MITSuME
50 cm telescope of Akeno Observatory, Yamanashi, Japan.

We started the observation about ~10.5 hour after the BAT trigger
from 2011-11-04 9:35:15 UT.  And we did not find any new point source
within the XRT error circle (S. D. Barthelmy  et al, GCN12524) in three bands.
The results of photometry (3sigma upper limits) are listed below.

#The photon flux were calibrated against GSC2.3 catalog.

T0+[day]      MID-UT     T-EXP[sec]      g'             Rc           Ic
---------------------------------------------------------------------------------

 3.710^4     9:44:05        1020       -----       >17.9       >18.0
---------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111107A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12534
SUBJECT: GRB 111107A: Swift detection of a burst with an optical counterpart
DATE:    11/11/07 01:00:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. H. Siegel (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), C. A. Swenson (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 00:50:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111107A (trigger=507185).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 129.484, -66.506 which is 
   RA(J2000)  =  08h 37m 56s
   Dec(J2000) = -66d 30' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single FRED-like
peak with a duration of about 15 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 00:51:28.8 UT, 64.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 129.47682,
-66.52012 which is equivalent to:
   RA(J2000)  = 08h 37m 54.44s
   Dec(J2000) = -66d 31' 12.4"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 51 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 (8.93 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.6
(+2.29/-1.97) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.37e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 73 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 08:37:54.66 = 129.47775
  DEC(J2000) = -66:31:12.3  = -66.52009
with a 90%-confidence error radius of about 0.65 arc sec. This position is 1.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.21 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.14. 

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: GRB111107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12535
SUBJECT: Skynet observations of GRB 111107A
DATE:    11/11/07 03:33:45 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

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

Skynet observed the field of GRB 111107A, Swift trigger 507185, with the
PROMPT telescopes located at CTIO in Chile.  We detect a fading optical
source within the error circle.  Preliminary calibration to USNO catalog
stars yields the follow initial detections:


Tmean(min) Tmean(day) Tel      Exp     Filt Mag     S/N
14.75 m    0.01024    Prompt4  5 x 80 s  R  19.467  2.892
15.22 m    0.01057    Prompt5  4 x 80 s  I  18.444  4.363

Further observations are ongoing. This message may be cited.


GRB_name: GRB111107A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12536
SUBJECT: GRB 111107A: GROND observations
DATE:    11/11/07 04:36:54 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (DARK/NBI), 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 the Swift GRB 111107A (Siegel et al., GCN 12534) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPI/ESO telescope at La Silla Observatory (Chile).

Observations started on November 7, 2011, 03:28 UT as soon as the field of GRB 111107A rose above the pointing constraints of the telescope. This is roughly 2.6 hrs after the trigger.

We detect the afterglow candidate reported by Siegel et al. (GCN 12534) and LaCluyze et al. (GCN 12535). Based on an exposure time of 460 s, we estimate a preliminary r'-band magnitude (in the AB system) of:

r' = 21.3 +/- 0.1
 
at a midtime of 03:41 UT. The r' band magnitude has been calibrated against the GROND zeropoint.


GRB_name: GRB111107A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12537
SUBJECT: GRB 111107A: Gemini-South Redshift
DATE:    11/11/07 06:31:01 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock, E. Berger (Harvard), and D. Fox (Penn St.) report:

We obtained spectroscopy of the optical afterglow of GRB 111107A (Siegel 
et al., GCN 12534; LaCluyze et al., GCN 12535; Kruehler et al., GCN 
12536) using GMOS-South on the Gemini-South 8-m telescope.  Observations 
began at 05:05 UT (4.2 hrs after the BAT trigger).  Inspection of the 
first two exposures (range 4160-8140 Angstroms) reveals a damped 
Lyman-alpha absorber as well as narrow absorption lines of C IV, Al II, 
and C II at a common redshift of 2.893.


GRB_name: GRB111107A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12538
SUBJECT: GRB 111107A: Enhanced Swift-XRT position
DATE:    11/11/07 06:51:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 1642 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 111107A, 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 = 129.47666, -66.51988 which is equivalent
to:

RA (J2000): 08h 37m 54.40s
Dec (J2000): -66d 31' 11.6"

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: GRB111107A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12539
SUBJECT: GRB 111107A: Swift-BAT refined analysis
DATE:    11/11/07 13:02:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. 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 recent telemetry downlinks,
we report further analysis of BAT GRB 111107A (trigger #507185)
(Siegel, et al., GCN Circ. 12534).  The BAT ground-calculated position is
RA, Dec = 129.487, -66.520 deg, which is 
   RA(J2000)  =  08h 37m 56.8s 
   Dec(J2000) = -66d 31' 12.0" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.
 
The mask-weighted light curve shows a FRED peak starting at ~T-1 sec,
peaking at ~T+2 sec, and returning to baseline at ~T+55 sec.  At the 2-sigma
level, there is a possible peak from T+130 to T+180 sec.  There is no hint
of a peak in the T+250 to T+400 sec range corresponding to the flare seen
in the XRT afterglow lightcurve.  T90 (15-350 keV) is 26.6 +- 6.6 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.06 to T+32.83 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.49 +- 0.14.  The fluence in the 15-150 keV band is 8.8 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+2.16 sec in the 15-150 keV band
is 1.2 +- 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/507185/BA/


GRB_name: GRB111107A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12540
SUBJECT: GRB 111107A: Swift/UVOT Afterglow Analysis
DATE:    11/11/07 14:21:50 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of
GRB 111107A  73 s after the BAT trigger (Siegel et al.,
GCN Circ. 12534).

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Poole et al. 2008, MNRAS, 383, 627)
for the early exposures are:

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

white               73          223          147         19.45 +/- 0.10
v                  615         1755          136        >18.7
b                  540         1681          117        >20.0
u                  285         1656          343        >19.9
w1                 664         1631          117        >19.2
m2                 639         5231          299        >19.7
w2                 590         1730          136        >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.14 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB111107A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12541
SUBJECT: GRB 111107A: APEX submm observation
DATE:    11/11/07 15:30:22 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), R. J. Cumming, A. O. Henrik Olofsson,  P. Bergman (OSO), Felipe McAuliffe, M. Martinez (ESO) and A. Lundgren (ESO/ALMA) report on behalf of a larger collaboration:

We have observed the field of GRB 111107A (Siegel et al., GCN 12534) using LABOCA/APEX at Chajnantor (Chile) in the 345 GHz band. The observation consisted of 241 min on source, observed between 3:41 and 10:08 UT (between 2.85 and 9.3 hr after the burst) using the imaging mode. Weather conditions were good, with precipitable water vapour ranging between 0.5 and 0.8. In a preliminary reduction we do not detect any source at the position of the afterglow. The r.m.s. of the image is ~6 mJy, giving a 3-sigma detection limit of 18 mJy.


GRB_name: GRB111107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12542
SUBJECT: GRB 111107A: VLT/X-shooter spectroscopy
DATE:    11/11/07 16:32:22 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), S. D. Vergani (INAF-OAB), H. Flores (GEPI/Obs. de
Paris), D. Malesani, D. Watson (DARK/NBI), A. J. Levan (Univ. Warwick), J. P. U.
Fynbo (DARK/NBI), report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 111107A (Siegel et al., GCN
12534; LaCluyze et al., GCN 12535; Kruehler et al., GCN 12536; Kuin et
al., GCN 12540), using the X-shooter spectrograph mounted on the ESO-VLT.
Observations started on 2011 November 7.254 UT (5.26 hr after the GRB),
with a total exposure time of 1.3 hr, covering the wavelength range
3000-25000 AA.

In the spectra (reduced with archival calibration files) we detect several
absorption lines, like Ly-alpha, CIV, FeII and MgII, and the correspondent
Lyman limit absorption, at a redshift consistent with that reported by
Chornock et al. (GCN 12537).

We also note the presence of a strong intervening Mg II system at z = 1.998.

We acknowledge excellent support from the observing staff in Paranal, in
particular Valentin Ivanov, Petr Kabath, Jonathan Smoker, Claudia Cid,
Sergio Vera, Christophe Martayan and Roger Wesson.

[GCN OPS NOTE(07nov11): The afilliation of DM and DW was changed.]


GRB_name: GRB111107A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12543
SUBJECT: GRB 111107A: Swift-XRT refined Analysis
DATE:    11/11/07 17:40:49 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

Bin-Bin Zhang (PSU) reports on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 111107A (Siegel  et al. GCN
Circ. 12534), from 55 s to 30.6 ks after the  BAT trigger. The data
comprise 42 s in Windowed Timing (WT) mode (the first 7 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 12538).

The late-time light curve (from T0+5.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.12 (+0.29, -0.27).

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, -0.16). The
best-fitting absorption column is  3.5 (+6.0, -3.5) x 10^21 cm^-2, at a
redshift of 2.893, in addition to the Galactic value of 8.9 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 3.3 x
10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 8.9 x 10^20 cm^-2
Intrinsic column:    3.5 (+6.0, -3.5) x 10^21 cm^-2 at z=2.893
Photon index:      2.15 (+0.12, -0.16)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00507185.

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


GRB_name: GRB111107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12544
SUBJECT: Continued Skynet observations of GRB111107A
DATE:    11/11/07 22:21:48 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

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

Skynet continued observing the field of GRB 111107A (Swift trigger 507185, 
Siegel et al., GCN 12534; LaCluyze et al., GCN 12535; Kruehler et al., GCN 
12536; Kuin et al., GCN 12540) with the PROMPT telescopes located at CTIO 
in Chile in B, R, and I.  We detect the fading optical counterpart in R and 
I, with limits in B.  The fading is consistent with a power-law index of 
~-0.7.

Preliminary light curve can be found at the following link:
http://skynet.unc.edu/grb/grb111107a.png


Prompt4, R-band, calibrated to 12 USNO B1.0 stars

T(mean) Tmean(days) Exps     Mag     1-sig MagErr
14.75 m  0.01024  5 x 80 s   19.467  +0.427/-0.311
30.93 m  0.02148  13 x 80 s  19.883  +0.360/-0.273
61.87 m  0.04296  24 x 80 s  20.319  +0.337/-0.259
118.57 m 0.08234  43 x 80 s  20.818  +0.404/-0.298
3.815 h  0.15895  94 x 80 s  21.206  +0.243/-0.200
6.619 h  0.27579  102 x 80 s 21.837  +0.357/-0.271


Prompt5, I-band, calibrated to 15 USNO B1.0 stars

T(mean) Tmean(days) Exps     Mag     1-sig MagErr
15.22 m  0.01057  4 x 80 s   18.443  +0.274/-0.220
24.77 m  0.01720  5 x 80 s   18.520  +0.263/-0.212
49.60 m  0.03444  24 x 80 s  19.474  +0.262/-0.212
112.45 m 0.07809  49 x 80 s  19.898  +0.300/-0.237
3.139 h  0.13081  43 x 80 s  20.297  +0.390/-0.291
6.189 h  0.25788  130 x 80 s 20.650  +0.273/-0.220


Prompt3, B-band, calibrated to 14 USNO B1.0 stars

T(mean) Tmean(days) Exps   3-SigLimMag
88.62 m  0.06154  47 x 80 s  20.3
4.738 h  0.19743  159 x 80 s 21.6


Further observations are planned.  This message may be cited.


GRB_name: GRB111107A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12545
SUBJECT: GRB 111107A: Fermi GBM observation
DATE:    11/11/08 21:37:43 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa (UAH) reports on behalf of the Fermi GBM Team:

"At 00:50:25.48 UT on 07 November 2011, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 111107A (trigger 342319827 /
111107035) which was also detected by the Swift/BAT (Siegel et al.
2011, GCN 12534). The GBM on-ground location is consistent with the
Swift position. The angle from the Fermi LAT boresight is 119 degrees.

The GBM light curve consists of a FRED-like pulse with a duration
(T90) of about 12 s (50-300 keV). The time-averaged spectrum from
T0-1.024 s to T0+11.264 s is well fit by a power law function with an
exponential high-energy cutoff. The power law index is -1.38 +/- 0.21
and the cutoff energy, parameterized as Epeak, is 108 +/- 32 keV
(Castor statistics 318.55 for 365 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(1.392 +/- 0.197)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.96 s in the 10-1000 keV band is
2.6 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB111103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12546
SUBJECT: GRB 111103B: optical upper limit of Mt. Terskol observatory   
DATE:    11/11/08 22:20:22 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 Swift  GRB 111103B  (Grupe  et al. GCN  12519) with
Zeiss-600 telescope of Mt.Terskol observatory in R filter between Nov. 3
(UT) 15:07:44 - 15:17:50.   We took 10 images of 60 exposure under good
weather conditions and mean seeing (FWHW) of about 1.6". We do not detect
any source within enhanced XRT  position (Goad et al., GCN 12525). A
photometry is based on the USNO B1.0 nearby stars.

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

0.17619  R         10x60       n/d   17.5


GRB_name: GRB111103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12547
SUBJECT: GRB 111103B: optical upper limit of CrAO 
DATE:    11/11/08 22:24:22 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev, N. Pit (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
AZT-11 telescope of CrAO in R filter between Nov. 3 (UT) 16:12:05  -
17:00:21.   We took several images of 180 exposure under unfavorable weather
conditions and mean seeing (FWHW) of about 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 nearby stars.

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

 0.2352  R         16x180       n/d   19.4


GRB_name: GRB111109A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12548
SUBJECT: GRB 111109A: Swift detection of a burst
DATE:    11/11/09 03:07:17 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. Pagani (U Leicester), S. D. Barthelmy (GSFC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 02:57:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111109A (trigger=507342).  Swift did not slew due an
observing constraint.  The BAT on-board calculated location is 
RA, Dec 118.196, -41.599, which is 
   RA(J2000)  =  07h 52m 47s
   Dec(J2000) = -41d 35' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a few peaks with a
total duration of about 20 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until 
T0+49.2 minutes. There will be no XRT or UVOT data until
this time. 

Burst Advocate for this burst is C. Pagani (cp232 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: GRB111109A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12549
SUBJECT: GRB 111109A: Swift-XRT observations
DATE:    11/11/09 04:24:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J.A. Kennea (PSU), M. Perri (ASDC), G. Tagliaferri
(INAF-OAB), P.A. Evans (U. Leicester) and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 111109A at 03:49:14.9 UT,
3088.9 seconds after the BAT trigger. No source was detected in 922 s
of promptly downlinked data. We are waiting for the full dataset to
detect and localise the XRT counterpart.


GRB_name: GRB111109A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12550
SUBJECT: GRB 111109A: Enhanced Swift-XRT position
DATE:    11/11/09 08:36:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2557 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111109A, 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 = 118.20283, -41.58413 which is equivalent
to:

RA (J2000): 07h 52m 48.68s
Dec (J2000): -41d 35' 02.9"

with an uncertainty of 2.4 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: GRB111109A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12551
SUBJECT: GRB 111109A: Swift-BAT refined analysis
DATE:    11/11/09 14:14:55 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
C. Pagani (U Leicester), 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-240 to T+645 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111109A (trigger #507342)
(Pagani, et al., GCN Circ. 12548).  The BAT ground-calculated position is
RA, Dec = 118.248, -41.588 deg, which is 
   RA(J2000)  =  07h 52m 59.5s 
   Dec(J2000) = -41d 35' 18.3" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 91%.
 
The mask-weighted light curve shows a couple overlapping peaks starting
at ~T-5 sec, peaking at ~T+2 sec, and ending at ~T+20 sec.  There is a
hint of possible precursor activity (~2 sigma) at ~T-110 sec.  We note
that the burst location went out of the BAT FoV at ~T+120 sec (a slew
due to an observing constraint).  T90 (15-350 keV) is 13.0 +- 3.2 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-5.60 to T+8.40 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.86 +- 0.26.  The fluence in the 15-150 keV band is 2.4 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.40 sec in the 15-150 keV band
is 0.5 +- 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/507342/BA/


GRB_name: GRB111109A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12552
SUBJECT: GRB 111109A: Swift/UVOT Photometry 
DATE:    11/11/09 20:13:32 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

S. T. Holland (CRESST/USRA/GSFC) and
C. Pagani (U Leicester)
report on behalf of the Swift/UVOT team:

     The Swift/UVOT observed the field of GRB 111109A starting 3074 s
after the BAT trigger (Pagani et al., 2011, GCNC 12548).  Settled
observations started at 3095 s.  The USNO-B1.0 source 0484-0114145 is
seen in the UVOT-enhanced XRT error circle (Beardmore et al., 2011,
GCNC 12550).  Our preliminary photometry suggests that this source
did not vary during the UVOT observations.  We note that the
position listed in the GCN/SWIFT_POSITION_NOTICE dated Wed 09 Nov 11
03:56:21 UT is incorrect due to it being inconsistent with the XRT
position, and the presence of a nearby high proper motion star.


GRB_name: GRB111109A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12553
SUBJECT: GRB 111109A: Swift-XRT refined Analysis
DATE:    11/11/09 23:04:22 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 111109A (Pagani  et al. GCN
Circ. 12548), from 3.1 ks to 51.8 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN. Circ 12550).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.5 (+/-0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.0 (+0.8, -0.7). The
best-fitting absorption column is  6.1 (+3.1, -2.9) x 10^21 cm^-2, in
excess of the Galactic value of 3.2 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 3.1 x 10^-11 (1.5 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.1 (+3.1, -2.9) x 10^21 cm^-2
Galactic foreground: 3.2 x 10^21 cm^-2
Excess significance: 3.5 sigma
Photon index:      3.0 (+0.8, -0.7)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00507342.

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


GRB_name: GRB111113A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12556
SUBJECT: IPN Triangulation of GRB 111113A (short/hard/intense)
DATE:    11/11/15 11:24:23 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,

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

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

The short-duration, hard, intense GRB 111113A has been observed by 
INTEGRAL (SPI-ACS), Konus-Wind, MESSENGER (GRNS), and Swift (BAT) 
(outside the coded field of view) so far, at about 18618 s UT (05:10:18).
We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   225.390 (15h 01m 34s)  +2.185 ( +2d 11' 05")
  Corners:
   224.649 (14h 58m 36s)  +1.899 ( +1d 53' 57")
   225.195 (15h 00m 47s)  +2.382 ( +2d 22' 56")
   226.104 (15h 04m 25s)  +2.430 ( +2d 25' 47")
   225.583 (15h 02m 20s)  +1.985 ( +1d 59' 05")
  ---------------------------------------------

The error box area is 1408 sq. arcmin, and its maximum dimension is 93 
arcmin.

This box can be improved.

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


GRB_name: GRB111113A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12557
SUBJECT: Konus-Wind observation of GRB 111113A
DATE:    11/11/15 14:06:16 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 111113A
(localized by IPN: Golenetskii et al., GCN 12556)
triggered Konus-Wind at T0=18613.625s UT (05:10:13.625)

The light curve consists of a single hard peak with
a total duration of ~160 ms. There is a hint of a weaker
emission starting ~200 ms before the main pulse
and extending to ~T0+500ms;
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111113_T18613/

As observed by Konus-Wind the burst
had a fluence of (7.7  1.0)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.016 s,
of (9.2  1.8)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.128 s)
is best fitted in the 40 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.53 (-0.16, +0.18),
and Ep = 1480(-226, +265) keV,
chi2 = 20.7/23 dof.
Also, a noticeable counts excess over this model spectrum
is observed in the 20-40 keV range.


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


GRB_name: GRB111107A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12558
SUBJECT: GRB111107A: ATCA observations - upper limit and a possible detection
DATE:    11/11/17 09:28:48 GMT
FROM:    Paul Hancock at U of Sydney  <hancock@physics.usyd.edu.au>

Paul J. Hancock, Tara Murphy (U of Sydney)
We observed GRB111107A (GCN12534) with the Australian Telescope
Compact Array (ATCA) on Nov 07 at 12 UT (~11 hours after the GRB
trigger). At 9GHz there is no sign of any emission from the GRB above
a 3 limit of 200uJy. At 5.5GHz there appears to be a 4 source at
300+/-40uJy at the UVOT location of the GRB (GCN 12538). In both cases
the measurement of the possible GRB flux is complicated by the
presence of one or more confusing radio sources in the field of view.
Further observations are planned. We thank the observatory staff for
scheduling and supporting these observations.


GRB_name: GRB111117A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12559
SUBJECT: GRB 111117A: Swift detection of a short hard burst
DATE:    11/11/17 12:27:17 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

V. Mangano (INAF-IASFPA), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), H. A. Krimm (CRESST/GSFC/USRA),
O. M. Littlejohns (U Leicester), F. E. Marshall (NASA/GSFC),
P. T. O'Brien (U Leicester), S. R. Oates (UCL-MSSL),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
R. L. C. Starling (U Leicester), C. A. Swenson (PSU) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 12:13:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111117A (trigger=507901).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 12.702, +23.021 which is 
   RA(J2000) = 00h 50m 49s
   Dec(J2000) = +23d 01' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 0.6 sec.  The peak count rate
was ~6140 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 12:14:58.7 UT, 76.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 12.6925, 23.0103 which
is equivalent to:
   RA(J2000)  = 00h 50m 46.19s
   Dec(J2000) = +23d 00' 36.9"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 50 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  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 (3.70 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3
(+2.73/-2.30) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
136 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. The
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 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03. 

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


GRB_name: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12560
SUBJECT: GRB 111117A: GMG upper limit
DATE:    11/11/17 16:54:52 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

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

We observed the field of GRB 111117A (Mangano et al., GCN 12559) at
the 2.4m Gao-Mei-Gu telescope (GMG) equipped with YFOSC. The weather
was not optimistic but 1x600s R-band and 3x600s z-band images were
obtained, starting at 14:11:16 UT, 17 Nov. 2011 (i..e, 1.960 hrs after
the burst). No afterglow was detected within the XRT error circle for
both filters, to a 3sigma upper limit of R~22.2 mag, calibrated with
the USNO B1 catalog.

We thank Gui-Hua He, Jian-Quan He, and Yu-Xin Xin for performing these
observations.


GRB_name: GRB111117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12561
SUBJECT: GRB 111117A: Swift-BAT refined analysis of a short hard burst
DATE:    11/11/17 20:12:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), V. Mangano (INAF-IASFPA),
J. Norris (BSU), 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+395 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111117A (trigger #507901)
(Mangano, et al., GCN Circ. 12559).  The BAT ground-calculated position is
RA, Dec = 12.702, 23.021 deg, which is 
   RA(J2000)  =   00h 50m 49.9s
   Dec(J2000) =  +23d 00' 11.0"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows two peaks, the first starts at ~T+0.00,
peaks at ~T+0.15 and ends at ~T+0.30 sec.  The second starts at ~T+0.35,
peaks at ~T+0.50, and ends at ~T+0.60 sec.  T90 (15-350 keV) is 0.47 +- 0.09 sec
(estimated error including systematics).

The spectral lag is 0.6 +/- 2.4 msec using the 100-350 and 25-50 keV bands
with 4-ms binning of the raw lightcurves.  This clearly indicates a short burst.
 
The time-averaged spectrum from T-0.016 to T+0.520 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.65 +- 0.22.  The fluence in the 15-150 keV band is 1.40 +- 0.18 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band
is 1.35 +- 0.20 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/507901/BA/

[GCN OPS NOTE(17nov11):  Per author's request, the missing position uncertainty
was added (1.7 arcmin).]


GRB_name: GRB111117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12562
SUBJECT: GRB 111117A: Chandra ToO observation scheduled
DATE:    11/11/17 21:07:23 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), N. Gehrels (GSFC), E. Troja (NASA/GSFC/ORAU), 
J. Norris (BSU), S. D. Barthelmy (GSFC), J. L. Racusin (GSFC), 
N. Kawai (Tokyo Tech), A. Fruchter (STScI)

The Chandra ToO observation has been approved for GRB 111117A 
(Mangano et al., GCN Circ. 12559; Sakamoto et al., GCN Circ. 12561).  
The observation has been tentatively scheduled on November 20 12:48 UT 
for 20 ksec.  

This is the approved ToO program in AO-13 to identify a Swift short GRB 
afterglow in X-rays by a sub-arcsecond position from Chandra 
(PI: Sakamoto, #501616).  The main goal is to identify the host galaxy 
of GRB 111117A by the sub-arcsecond X-ray position which is very likely 
to be able to obtain from the Chandra observation.  Therefore, we strongly 
encourage deep optical observations of the field.  


GRB_name: GRB111117A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12563
SUBJECT: GRB 111117A: NOT observations
DATE:    11/11/17 22:57:59 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

Michael I. Andersen (DARK), Antonio de Ugarte Postigo (IAA-CSIC and DARK),
Giorgos Leloudas (DARK), Johan P. U. Fynbo (DARK) report on behalf of a
larger collaboration:

Using ALFOSC on the Nordic Optical Telescope (NOT) we have obtained R-band
(6 x 300 s) imaging of the field of the Swift GRB 111117A (Mangano et
al., GCN 12559), starting on 2011 November 20:49:50 UT (mean epoch 7.88
hours after the burst trigger). The seeing during the observations was
around 0.9".

In a preliminary reduction we detect a source with a magnitude of R=23.1 +/- 0.3 
(based on USNO-B1.0 photometry) at the coordinates (J2000 +/- 1"):

R.A.: 00:50:46.28
Dec.: +23:00:40.3

This is formally 3.6" from the XRT position and thus outside the
XRTerror circle reported in GCN 12559. However we note that it is
within the automatically generated SPER error box
(http://www.swift.ac.uk/sper/507901/).
We therefore suggest that this object is the host galaxy or afterglow of
GRB 111117A.

We are grateful to the NOT observers, Kristian Vida (Konkoly Observatory) and
Heidi Korhonen (U. Copenhagen) for obtaining these observations.


GRB_name: GRB111107A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12564
SUBJECT: GRB111107A: Further ATCA observations - no detection
DATE:    11/11/18 00:25:22 GMT
FROM:    Paul Hancock at U of Sydney  <hancock@physics.usyd.edu.au>

Paul J. Hancock, Tara Murphy (U of Sydney)

Following the possible detection reported in GCN12558 we again
observed GRB111107A (GCN12534) with the Australian Telescope Compact
Array (ATCA) on Nov 14 from 16:54UT to 18:43UT (~7.5 days after the
GRB trigger). We detect no emission from the GRB with a 3sigma limit
of 180 uJy and 150 uJy at 5.5GHz and 9 GHz respectively. Given that
the 5.5 GHz radio luminosity of the GRB is expected to increase over
at least the first 7.5 days post burst, we conclude that the possible
4sigma detection reported in GCN12558 is a result of the nearby source
SUMSS J083735-663107. No further observations are planned. We thank
the observatory staff for scheduling and supporting these
observations.


GRB_name: GRB111117A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12565
SUBJECT: GRB 111117A: Swift-XRT refined Analysis
DATE:    11/11/18 01:27:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/IASFPA), G. Stratta
(ASDC), 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) and V. Mangano report on behalf of the Swift-XRT team:

We have analysed 7.0 ks of XRT data for GRB 111117A (Mangano  et al.
GCN Circ. 12559), from 89 s to 30.1 ks after the  BAT trigger. The data
comprise 18 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The best available XRT position  (using the
promptly downlinked event data, the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue) is RA, Dec = 12.6926,
23.0109 which is equivalent to:

RA (J2000): 00 50 46.22
Dec(J2000): +23 00 39.2

with an uncertainty of 2.1 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.33 (+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 2.2 (+/-0.4). The
best-fitting absorption column is  2.2 (+1.1, -1.0) x 10^21 cm^-2, in
excess of the Galactic value of 3.7 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (5.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+1.1, -1.0) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: 3.4 sigma
Photon index:      2.2 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00507901.

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


GRB_name: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12566
SUBJECT: GRB111117A: Magellan IMACS observations
DATE:    11/11/18 04:35:38 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, N. Sanders, D. Milisavljevic and E. Berger (Harvard) report:

We imaged the location of the short GRB 111117A (GCN 12559) with IMACS on
the Magellan/Baade 6.5-m telescope starting on 2011 November 18.07 UT (13.5
hrs post-burst) in 1.0" seeing. In a stack of 4x300 sec r-band exposures,
we detect an extended source at the edge of the enhanced XRT error circle
(GCN 12565) at a position of:

RA = 00:50:46.24
Dec = +23:00:41.04
(J2000)

with an uncertainty of ~0.5" in each coordinate. This is consistent with
the source position reported by Andersen et al. (GCN 12563, R = 23.1 +/-
0.3).

We calculate the extended source to have a magnitude of r = 23.9 +/- 0.15.
The fainter magnitude implies that the source reported by Andersen et al.
has faded between 7.9 and 13.5 hours post-burst.


GRB_name: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12567
SUBJECT: GRB 111117A: Gemini host observation
DATE:    11/11/18 05:36:11 GMT
FROM:    Antonino Cucchiara at LBNL  <acucchiara@lbl.gov>

A. Cucchiara (UCSC/UCO Lick) and S. B. Cenko (UC Berkeley) report
on behalf of a large collaboration:

On November 18.07 UT we observed the field of the short-hard 
GRB 111117A (Mangano et al., GCN 12559) with the Gemini-South 
telescope equipped with the GMOS instrument.

In our 30 minutes co-added image in r' band we clearly detect the 
source identified by Andersen et al. and Fong et al.(GCN 12563, 
12566): this object appear to be elongated in the SW-NE direction, 
suggesting it is indeed the host of GRB 111117A.

Using several SDSS (DR8) objects in the field we obtain a value of 
r' = 23.99 +/- 0.11 for this galaxy brightness, consistent 
with the one reported by the Magellan Telescope. 

We thank the Gemini-South staff for performing these observations,
in particular Pascale Hibon.


GRB_name: GRB111117A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12568
SUBJECT: GRB 111117A: GROND observations
DATE:    11/11/18 11:02:44 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed the field of GRB 111117A (Swift trigger #507901, Mangano et al.,
GCN 12559) 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 02:01 UT on November 18, 13.8 hr after the GRB
trigger. They were performed at an average seeing of 1".8 and an average
airmass of 1.7 .

We detect the afterglow/host candidate that was reported by Andersen et
al. (GCN 12563, R = 23.1  0.3), Fong et al. (GCN 12566, r = 23.9  0.15)
and Cucchiara et al. (GCN 12567, r' = 23.99  0.11) in the g' and r' band.

Based on the first 75 min of total exposures in g'r'i'z' and 60 min in
JHK, we estimate preliminary magnitudes (all in AB system) of

g' = 24.08  0.15,

r' = 24.08  0.16,

i' > 23.9,

z' > 23.4,

J  > 21.7,

H  > 21.3 and

K  > 19.5.

Our r'-band magnitude is in agreement with Fong et al. and Cucchiara et al.

Magnitudes are calibrated against SDSS as well as 2MASS field stars
and are not corrected for the expected Galactic foreground extinction
corresponding to a reddening of E_(B-V)=0.03 mag in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB111117A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12569
SUBJECT: GRB 111117A: Swift/UVOT Upper Limits
DATE:    11/11/18 11:04:27 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and V. Mangano (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111117A
137 s after the BAT trigger (Mangano et al., GCN Circ. 12559).
No optical afterglow consistent with the XRT position
(Melandri et al., GCN Circ. 12565) or the optical position 
(Andersen et al., GCN Circ. 12563 & Fong et al., GCN Circ. 12566) 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

u_FC               137          387          246         >20.4
v                  443         1241           97         >19.3
b                  392         1191          117         >20.0
u                  137         1315          490         >20.7
w1                 493         1290           97         >20.4
m2                 468         1117           78         >19.5
w2                 419         1217           97         >21.5

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: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12570
SUBJECT: GRB 111117A: TNG observations
DATE:    11/11/18 11:32:21 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri, D. Fugazza, S. Covino (INAF-OAB) and E. Palazzi (INAF- 
IASFBo)
on behalf of a larger collaboration report:

We observed the field of GRB 111117A (Mangano et al. GCN 12559) with  
the 3.6m TNG equipped with the Dolores camera. A sequence of 6x300s  
images were acquired starting on Nov 17.801 UT (i.e. ~7 hours after  
the burst event).

No obvious fading object is detected inside the refined XRT error  
circle (Melandri et al. GCN 12565), while the extended object  
previously reported by Andersen et al. (GCN 12563), Fong et al. (GCN  
12566), Cucchiara et al. (GCN 12567) and Schmidl et al. (GCN 12568) is  
clearly visible in our coadded image.

Calibrating against a set of USNO-B1 stars of the field we find R =  
23.1 +/- 0.2, consistent with the value found by Andersen et al. (GCN  
12563). We caution about the possible fading of this object, as  
reported by Fong et al. (GCN 12566), because the apparent difference  
of magnitude could be related to the different calibration system.  
Since this object is extended also in our image and it does not seem  
to vary, it is more likely the host galaxy of GRB 111117A.

We thank the TNG staff for their support, in particular Aldo Fiorenzano.


GRB_name: GRB111117A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12571
SUBJECT: GRB 111117A: EVLA observations
DATE:    11/11/19 01:10:01 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the position of the short GRB 111117A (GCN 12559) with the
EVLA beginning 2011 November 18.0 UT (11.8 hours post-burst) at a mean
frequency of 5.8 GHz. In two hours of observations, we do not detect any
radio source within the enhanced XRT position (GCN 12565) down to a 3-sigma
limit of ~34 microJy."


GRB_name: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12572
SUBJECT: GRB 111117A: further NOT observations
DATE:    11/11/19 10:35:25 GMT
FROM:    Giorgos Leloudas at Dark Cosmology Centre  <giorgos@dark-cosmology.dk>

Giorgos Leloudas, Daniele Malesani (DARK) and Dong Xu (WIS) report on behalf of a larger collaboration:

We have continued observing GRB 111117A (Mangano et al., GCN 12559) using ALFOSC on the Nordic Optical Telescope (NOT).
In addition, we have made a more careful analysis of the data reported in Andersen et al. (GCN  12563).
Our R-band photometry, calibrated to USNO B1, can be summarized in the following table:

Stack    mid-time  R   
5x300 s    7.93 hr  23.36+-0.15 
5x300 s    9.88 hr  23.98+-0.24 
8x300 s    36.38 hr  23.74+-0.20  

If we instead stack all the images obtained during the first night (10x300s, mid-time 8.91 hr after the GRB), we obtain R = 23.81+-0.17.

Based on the NOT observations only, we suggest that there is some evidence of fading (albeit at low significance) between the observations obtained at 7.93 hr and later, indicating that at that time there was some contribution from the GRB afterglow to the underlying host galaxy light.

We are grateful to the NOT observers, Kristian Vida (Konkoly Observatory) and
Heidi Korhonen (U. Copenhagen) for obtaining these observations.


GRB_name: GRB111117A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12573
SUBJECT: GRB 111117A: Fermi GBM observation
DATE:    11/11/19 15:35:22 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (MPE) and P. Jenke (UAH)
report on behalf of the Fermi GBM Team:

"At 12:13:42.03 UT on 17 November 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111117A (trigger 343224824 / 111117510)
which was also detected by the Swift/BAT
(Mangano et al. 2011, GCN 12559).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 12 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver.

The GBM light curve consists of two pulses
with a duration (T90) of about 0.5 s (50-300 keV).
The time-averaged spectrum from T0-0.128 s to T0+0.384 s is
well fit by a power law function with an exponential high-energy cutoff.
The power law index is -0.69 (+0.17/- 0.15) and the lower limit on
the cutoff energy, parameterized as Epeak, is 370 keV.

The event fluence (10-1000 keV) in this time interval is
(6.7 +/- 0.2)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.128 s in the 10-1000 keV band
is 2.8 +/- 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: GRB111117A
Detection_method: Fermi GBM Det
Circular_text:
This is a duplicate of 12573.



TITLE:   GCN CIRCULAR
NUMBER:  12574
SUBJECT: GRB 111117A: Fermi GBM observation
DATE:    11/11/19 15:35:30 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (MPE) and P. Jenke (UAH)
report on behalf of the Fermi GBM Team:

"At 12:13:42.03 UT on 17 November 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111117A (trigger 343224824 / 111117510)
which was also detected by the Swift/BAT
(Mangano et al. 2011, GCN 12559).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 12 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver.

The GBM light curve consists of two pulses
with a duration (T90) of about 0.5 s (50-300 keV).
The time-averaged spectrum from T0-0.128 s to T0+0.384 s is
well fit by a power law function with an exponential high-energy cutoff.
The power law index is -0.69 (+0.17/- 0.15) and the lower limit on
the cutoff energy, parameterized as Epeak, is 370 keV.

The event fluence (10-1000 keV) in this time interval is
(6.7 +/- 0.2)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.128 s in the 10-1000 keV band
is 2.8 +/- 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: GRB111117A
Detection_method: Fermi GBM Det
Circular_text:
This is a duplicate of 12573.



TITLE:   GCN CIRCULAR
NUMBER:  12575
SUBJECT: GRB 111117A: Fermi GBM observation
DATE:    11/11/19 15:35:52 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (MPE) and P. Jenke (UAH)
report on behalf of the Fermi GBM Team:

"At 12:13:42.03 UT on 17 November 2011, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 111117A (trigger 343224824 / 111117510)
which was also detected by the Swift/BAT
(Mangano et al. 2011, GCN 12559).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 12 degrees.
Moreover, this burst was bright enough to result in a Fermi spacecraft
autonomous rapid repoint (ARR) maneuver.

The GBM light curve consists of two pulses
with a duration (T90) of about 0.5 s (50-300 keV).
The time-averaged spectrum from T0-0.128 s to T0+0.384 s is
well fit by a power law function with an exponential high-energy cutoff.
The power law index is -0.69 (+0.17/- 0.15) and the lower limit on
the cutoff energy, parameterized as Epeak, is 370 keV.

The event fluence (10-1000 keV) in this time interval is
(6.7 +/- 0.2)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.128 s in the 10-1000 keV band
is 2.8 +/- 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: GRB111117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12576
SUBJECT: GRB 111117A: optical upper limit in CrAO 
DATE:    11/11/20 15:51:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed field of the Swift  GRB 111117A  (Mangano  et al. GCN 12559) 
with AZT-11 telescope of CrAO in R filter between Nov. 17 (UT) 16:11:05 - 
17:14:24, i.e. starting ~ 4 h after burst trigger. We took several images of 
180 exposure under variable weather conditions and mean seeing (FWHM) of 
about 2.7". We do not detect any source within XRT  position (Melandri  et 
al. GCN 12565). A photometry is based on the USNO B1.0  1130-0013895 star 
(00:50:46.48 +23:01:28.8) assuming R=16.98:

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

0.1879   R         22x180       n/d   20.6


GRB_name: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12577
SUBJECT: GRB 111117A: Gemini Afterglow Limits
DATE:    11/11/21 10:02:31 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley) and A. Cucchiara (UC Santa Cruz / UCO Lick)
report on behalf of a larger collaboration:

We obtained a second epoch of imaging of the X-ray afterglow error circle
of the short-hard GRB111117A (Mangano et al., GCN 12559) with the Gemini
Multi-Object Spectrograph mounted on the 8-m Gemini South telescope.
Observations were taken in the r' filter beginning at 1:18 UT on 2011 Nov
20 (~ 2.5 days after the Swift trigger).

The host galaxy candidate (Andersen et al., GCN 12563; Fong et al., GCN
12566) is well detected in our stacked image, and has maintained a
constant brightness (within uncertainties) when compared with our first
epoch of GMOS imaging (Cucchiara et al., GCN 12567).  Using the HOTPANTS
image subtraction software package, we have differenced the two images and
estimate a limit on the afterglow flux of r' > 25.5 mag at our first epoch
(calculated with respect to several SDSS stars in the field).


GRB_name: GRB111121A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12578
SUBJECT: GRB 111121A: Swift detection of a short hard burst
DATE:    11/11/21 16:43:39 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), M. M. Chester (PSU), N. Gehrels (NASA/GSFC),
B. Gendre (ASDC), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
J. P. Osborne (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), R. L. C. Starling (U Leicester),
G. Stratta (ASDC), C. A. Swenson (PSU), E. Troja (NASA/GSFC/ORAU),
T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report on behalf of the
Swift Team:

At 16:26:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111121A (trigger=508161).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 154.751, -46.637 which is 
   RA(J2000)  =  10h 19m 00s
   Dec(J2000) = -46d 38' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 1 sec.  The peak count rate
was ~38000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 16:27:41.3 UT, 76.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
154.7612, -46.6709 which is equivalent to:
   RA(J2000)  = 10h 19m 2.68s
   Dec(J2000) = -46d 40' 15.1"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 124 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 (1.20 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4
(+2.62/-2.25) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.58e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White 
filter  starting 85 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  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
18.0 mag.No  correction has been made  for the expected extinction
corresponding to  E(B-V) of 0.26. We note that the XRT centroid is
close to a known 14th  magnitude star, which may complicate the
analysis. 

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


GRB_name: GRB111121A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12579
SUBJECT: GRB 111121A: Enhanced Swift-XRT position
DATE:    11/11/21 21:22:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2196 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 111121A, 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 = 154.76137, -46.67064 which is equivalent
to:

RA (J2000): 10h 19m 2.73s
Dec (J2000): -46d 40' 14.3"

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: GRB111117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12580
SUBJECT: GRB 111117A: Chandra detection of the afterglow
DATE:    11/11/21 21:40:47 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), E. Troja (NASA/GSFC/ORAU), N. Gehrels (GSFC), 
J. Norris (BSU), S. D. Barthelmy (GSFC), J. L. Racusin (GSFC), 
N. Kawai (Tokyo Tech), A. Fruchter (STScI)

A Chandra ToO observation of GRB 111117A (Mangano et al., GCN Circ. 12559; 
Sakamoto et al., GCN Circ. 12561) started on November 20 12:39 UT (~3 days 
after the GRB trigger) for a total of 19.8 ksec.  The X-ray afterglow of the 
burst in the 0.3-8 keV band was detected at a position RA, Dec 12.69286, +23.01108
which is equivalent to:

RA (J2000) = 00 50 46.29 
Dec(J2000) = 23 00 39.9

The 1-sigma statistical error is 0.09 and 0.15 arcsec on RA and Dec respectively.  
The systematic error of the Chandra aspect solution is 0.6 arcsec (radius, 90% 
containment; i.e, http://cxc.harvard.edu/cal/ASPECT/celmon/) which dominates  
the localization uncertainty.  The detection significance is 3.9 sigma (7.8 net source 
counts and 0.2 estimated background counts) by the ciao wavdetect software.   

The Chandra location is consistent with the enhanced XRT error circle (Melandri et al., 
GCN Circ. 12565) and the reported optical afterglow/host galaxy candidate from the NOT 
observation (Andersen et al., GCN Circ. 12563).  However, we note that the optical 
candidate reported from the Magellan observation (Fong et al., GCN Circ 12566) is 
offset by 1.3 arcsec from the Chandra location.  

We would like to thank Harvey Tananbaum and the Chandra operation team for rapidly 
approving and making this observation.  


GRB_name: GRB111121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12581
SUBJECT: GRB 111121A: Swift-BAT refined analysis
DATE:    11/11/22 01:15:03 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
V. D'Elia (ASDC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), J. Norris (BSU), 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 recent telemetry downlinks,
we report further analysis of BAT GRB 111121A (trigger #508161)
(D'Elia, et al., GCN Circ. 12578).  The BAT ground-calculated position is
RA, Dec = 154.746, -46.670 deg, which is 
   RA(J2000)  =  10h 18m 59.1s 
   Dec(J2000) = -46d 40' 10.7" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.
 
The mask-weighted light curve shows an inital strong pulse composed 
of two overlapping peaks, the first starting at ~T-0.3 sec and 
peaking at ~T+0.17 sec (at 2.6 cnts/det/sec). The second peaks
at ~T+0.3 sec and is done by ~T+0.6 sec.  This is followed by
two episodes of extended emission.  The first is roughly constant
(~0.02 to 0.03 cnts/det/sec) out to ~T+65sec.  The second episode
is ~0.006 cnts/det/sec out to ~T+130 sec.  T90 (15-350 keV)
is 119 +- 16 sec (estimated error including systematics).
This T90 includes the extended emission.

The spectral lag is 10.2 ms +2.6-1.8 ms (for the 100-350 to 25-50 keV band)
and 12.7 ms +6.8-8.7 ms (for the 50-100 to 15-25 keV band).  This puts it
on the long end of the distribution for spectral lag for short GRBs.
 
The time-averaged spectrum from T-0.34 to T+141.08 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.66 +- 0.12.  The fluence in the 15-150 keV band is 2.2 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.26 sec in the 15-150 keV band
is 7.1 +- 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/508161/BA/


GRB_name: GRB111121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12582
SUBJECT: GRB 111121A: Swift-XRT refined Analysis
DATE:    11/11/22 04:43:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 111121A (D'Elia  et al. GCN
Circ. 12578), from 66 s to 24.1 ks after the  BAT trigger. The data
comprise 180 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 12579).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.85 (+/-0.09). At T+217 s  the decay
steepens to an alpha of 3.7 (+1.2, -0.7). The light curve breaks again
at T+378 s to a decay with alpha=0.93 (+0.07, -0.08),  before a final
break at T+9772 s s after which the decay index is 2.1 (+0.5, -0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.71 (+/-0.08). The
best-fitting absorption column is  4.2 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.88 (+0.15, -0.17)
and a best-fitting absorption column of 3.4 (+/-0.7) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.6 x 10^-11 (6.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.4 (+/-0.7) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 8.0 sigma
Photon index:      1.88 (+0.15, -0.17)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00508161.

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


GRB_name: GRB111121A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12583
SUBJECT: GRB 111121A: Magellan/Megacam observations
DATE:    11/11/22 12:58:18 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

W. Fong (Harvard), A. Seth (U. Utah), R. Chornock and E. Berger (Harvard)
report:

"We imaged the field of the short GRB 111121A (GCN 12578) with Megacam on
the Magellan/Clay 6.5-m telescope at a mid-time of 2011 November 22.27 UT
(13.9 hours post-burst).  We obtained 25x30-sec exposures in r-band at an
airmass of 1.7 in ~0.7" seeing.

The location of the latest enhanced XRT error circle (improved from GCN
12579 at http://www.swift.ac.uk/xrt_positions/ with RA(J2000) =
10:19:02.71, Dec(J2000) = -46:40:14.5, 1.4" uncertainty) is contaminated by
emission from a nearby bright (R~12.5) star.  However, we find a faint
source on the southern edge of the XRT circle at (J2000):

RA = 10:19:02.7
Dec = -46:40:15.6,

with an uncertainty of ~0.5" in each coordinate that includes contributions
from the centroiding error of the source and a 0.27" rms uncertainty from
the astrometric tie to USNO-B.

Due to the location of the source near a diffraction spike from the bright
star, it is unclear at present whether it is extended or point-like.
Additional analysis to extract a magnitude for the source is on-going, and
additional observations to check for variability are planned."


GRB_name: GRB111121A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12584
SUBJECT: GRB 111121A: Swift/UVOT Upper Limits
DATE:    11/11/22 14:39:55 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin, S. Oates (MSSL-UCL) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111121A
86 s after the BAT trigger (D'Elia et al., GCN Circ. 12578).
No optical afterglow consistent with the XRT position
(Evans et al, GCN Circ. 12579) is detected in the initial UVOT exposures.

The XRT enhanced position falls within the PSF wings of a B~13.6
magnitude star. Inspection of the event mode data after correction
for a slight wander in attitude shows no evidence for any transient
source.

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 dominated
by the nearly star and are:

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

white_FC            86          235          147         >14.8
u_FC               298          548          246         >15.5
white               86          990          296         >14.7
v                  629          822           39         >13.1
b                  554          748           39         >14.2
u                  298          723          265         >15.5
w1                 678          873           39         >16.5
m2                 653          847           39         >18.5
w2                 604          797           39         >17.9

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: GRB111121A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12585
SUBJECT: Konus-Wind observation of GRB 111121A
DATE:    11/11/23 12:26:06 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 111121A (Swift-BAT trigger #508161:
D'Elia et al., GCN 12578; Cummings et al., GCN 12581)
triggered Konus-Wind at T0=59182.640s UT (16:26:22.640)

The light curve shows of a hard bright pulse with
a total duration of ~600 ms followed by a tail
of a weak soft extended emission for at 20 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111121_T59182/

As observed by Konus-Wind the burst
had a fluence of (2.3  0.3)x10-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.160 s,
of (8.4  1.5)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.256 s)
is best fitted in the 20 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -0.44 (-0.07, +0.07),
the high energy photon index beta = -3.0 (<-2.4),
the peak energy Ep = 1780(-290, +310) keV,
chi2 = 59.7/51 dof.

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


GRB_name: GRB111117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12586
SUBJECT: GRB 111117A, the review of the sky area in plate archives
DATE:    11/11/23 14:21:21 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

V.V. Golovnya, L.M. Kizyun (Main Astro Obs, Kyiv) report:
 
We have undertaken the review of the sky area of GRB 111117A
(W. Fong et al. GCN Circ.12566) on astronegatives, collected 
in Ukrainian NAS Main astronomical observatory plate archive 
(1976-1996). All the plates with the possible object 
appearance are digitized using Microtek ScanMaker 9800XL TMA
flatbed scanner and have been placed into Golosiiv Plate 
Archive database DBGPA with open access to them. 
 The list of plates is given in the table:
YYYYMMDD TimeUT --Plates-- Exp. LimMag USNOA2 
19860910 231743 GUA040C001009 16.0 15.20 1125-00304111
19860927 221901 GUA040C001012B 14.0 15.20 1125-00304111
19870917 230117 GUA040C001118A 16.0 15.20 1125-00304111
19880821 010032 GUA040C001325A 16.0 13.70 1125-00304597
19911009 205736 GUA040C001853A 15.5 15.20 1125-00304111
Plates-the plate's identifier in GUA040C archives
        of DWA (D/F=400/2000, M=103"/mm) of the Ukrainian NAS 
        Main Astro obs in Kyiv (Marsden's number - 83)[1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 10 minutes area around 
       the location given in W. Fong et al. GCN Circ.12566: 
       RA(J2000): 00h 50m 46.24s, Dec(J2000): +23d 00' 41.04"
USNOA2 - Comparison star.
  The preview images of 11 areas together with  
the 10x10 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/111117A/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: GRB111123A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12587
SUBJECT: GRB 111123A: Swift detection of a burst
DATE:    11/11/23 18:33:53 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. Stamatikos (OSU/NASA/GSFC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), M. M. Chester (PSU), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB),
P. T. O'Brien (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), T. Sakamoto (NASA/UMBC),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester),
G. Stratta (ASDC), G. Tagliaferri (INAF-OAB),
E. Troja (NASA/GSFC/ORAU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:

At 18:13:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111123A (trigger=508319).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 154.851, -20.642 which is 
   RA(J2000)  =  10h 19m 24s
   Dec(J2000) = -20d 38' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a few overlapping peaks
from T-10 to T+30 sec and then a strong peak from T+60 to T+160 sec,
with a total duration of about 170 sec.  The peak count rate was ~1400 counts/sec
(15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 18:15:00.5 UT, 99.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 154.8464,
-20.6453 which is equivalent to:
   RA(J2000)  = 10h 19m 23.14s
   Dec(J2000) = -20d 38' 43.1"
with an uncertainty of 3.3 arcseconds (radius, 90% containment). This
location is 20 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. The XRT
light curve shows correlated activity with BAT, rising to peak followed 
by fading. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.78
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 8.48e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 109 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
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 M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB111117A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12588
SUBJECT: GRB 111117A: Refined Chandra Astrometry
DATE:    11/11/23 20:58:42 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger, W. Fong (Harvard), T. Sakamoto (GSFC/UMBC), and E. Troja
(NASA/GSFC/ORAU) report:

"We re-analyzed the Chandra observation of the short GRB 111117A (Sakamoto
et al. GCN 12580) for the purpose of clarifying and refining the astrometry
relative to the location of the host galaxy (using an optical image from
Magellan/IMACS:  Fong et al. GCN 12566).  Using 4 objects in common to the
Chandra data and the IMACS image (which is itself tied to USNO-B with 0.25"
rms) we find a correction to the native Chandra astrometry of:

dRA = -0.54+/-0.17"
dDEC = +0.34+/-0.14"

substantially improved relative to the 0.6" systematic uncertainty of the
native Chandra astrometry (Sakamoto et al. GCN 12580).  With this
correction, the position of the X-ray counterpart of GRB 111117A is (J2000):

RA = 00:50:46.257
DEC = +23:00:40.01

with a statistical uncertainty of about 0.13" in each coordinate.

Relative astrometry compared to the centroid of the host galaxy indicates a
projected angular offset of 1.0".  Although the redshift of the host galaxy
is not known at the present, this roughly corresponds to 6-8 kpc at
redshifts of z>0.5 (typical of short GRB offsets: Fong et al. 2010, ApJ,
708, 9)."


GRB_name: GRB111123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12589
SUBJECT: GRB 111123A: GMG optical observation
DATE:    11/11/24 02:23:25 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

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

We observed the field of GRB 111123A (Stamatikos et al., GCN 12587)
with the 2.4m Gao-Mei-Gu (GMG) telescope equipped with YFOSC, and
obtained 3x600s R-band and 3x600s I-band images, starting at 21:00:56
UT on Nov. 23rd (i.e., 2.793 hrs after the burst).

Within the XRT SPER error circle (http://www.swift.ac.uk/sper/), no
optical source was detected in the stacked I-band image, and a weak
and compact source was found in the stacked R-band image at
coordinates

RA(J2000)  =  10:19:23.10
Dec(J2000) = -20:38:41.72

with an uncertainty of ~1" in each coordinate. We caution that the
above source may be ascribed to background fluctuation. In this sense,
we derive R>~23.7 mag, calibrated with the #0693-0243590 star
(R1=17.95 and R2=17.60) in the USNO B1 catalog.

Deeper and NIR observations are encouraged.

We are grateful to Chuan-Jun Wang, De-Qing Wang, and Yan-Dong Lang for
performing these observations.

[GCN OPS NOTE(24nov11): Per author's request, Mao was added to the author list.]


GRB_name: GRB111123A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12590
SUBJECT: GRB 111123A: Enhanced Swift-XRT position
DATE:    11/11/24 05:02:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 2720 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 111123A, 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 = 154.84638, -20.64469 which is equivalent
to:

RA (J2000): 10h 19m 23.13s
Dec (J2000): -20d 38' 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: GRB111123A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12591
SUBJECT: GRB 111123A: MITSuME Okayama Optical upper limits
DATE:    11/11/24 05:49:35 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 111123A (Stamatikos et al., GCNC 12587)
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 2011-11-23 18:30:27 UT (~17 min after
the burst). We did not find any new point source within the enhanced
XRT circle (Goad, et al., GCNC 12590) 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
------------------------------------------------------
0.01541    18:35:32     540.0    >18.9 >18.9  >18.3
0.04573    19:19:12    5820.0    >20.4 >20.2  >19.6
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12592
SUBJECT: GRB 111123A: Swift-XRT refined Analysis
DATE:    11/11/24 09:34:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 11 ks of XRT data for GRB 111123A (Stamatikos et al.
GCN Circ. 12587), from 88 s to 35.6 ks after the  BAT trigger. The data
comprise 656 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 12590).

The late-time light curve (from T0+4.2 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.86 (+/-0.10).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.715 (+/-0.026). The
best-fitting absorption column is  2.62 (+0.10, -0.09) x 10^21 cm^-2,
in excess of the Galactic value of 5.8 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.43 (+0.19, -0.18)
and a best-fitting absorption column of 2.0 (+/-0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.1 x 10^-11 (5.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.0 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 5.8 x 10^20 cm^-2
Excess significance: 7.4 sigma
Photon index:      2.43 (+0.19, -0.18)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00508319.

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


GRB_name: GRB111123A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12593
SUBJECT: GRB 111123A: TNG NIR detection of the afterglow candidate
DATE:    11/11/24 12:33:57 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

D. Fugazza (INAF-OAB), V. D'Elia (INAF-OAR), P. D'Avanzo, A. Melandri
(INAF-OAB) and E. Palazzi (INAF-IASFBo) on behalf of a larger
collaboration report:

We observed the field of GRB 111123A (Stamatikos et al. GCN 12587) with
the 3.6m TNG equipped with the NICS near-infrared camera. A sequence of
JHK band images were acquired starting on Nov 24.238 UT (i.e. ~11.5 hours
after the burst event).

An object is detected in a stacked 20 min exposure image inside the
enhaced XRT error circle (Goad et al. GCN 12590) at the following
coordinates (J2000):

R.A. = 10:19:23.14
Dec. = -20:38:41.0

with an uncertainty of ~ 0.3", consistent with the position of the object
reported by Xu et al. (GCN 12589). The source has a magnitude K=19.4 +/-
0.3 (calibrated against the 2MASS catalogue). The source is not detected
in the shorter exposures (10 min) J and H-band images down to the
following 3sigma upper limits: J>19.7, H>20.5. At the present stage, it is
not possible to say anything about source variability.

We thank the TNG staff for their support, in particular Luca Di Fabrizio.


GRB_name: GRB111123A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12594
SUBJECT: GRB 111123A: correction to GCN 12593
DATE:    11/11/24 13:58:56 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB) on behalf of a larger collaboration report:

The TNG NIR 3sigma upper limits of GRB 111123A reported in Fugazza et al.
(GCN 12593) has been written in the wrong order. The correct values are:

J>20.5
H>19.7

(calibrated against the 2MASS catalogue). We confirm the K-band detection.

We apologize for the confusion that our previous report may have caused.


GRB_name: GRB111123A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12595
SUBJECT: GRB 111123A, GROND observations
DATE:    11/11/24 16:04:07 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

A. Rossi, A. Nicuesa Guelbenzu, S. Klose (all Tautenburg), P. Afonso
(American River College), and J. Greiner (MPE) report on behalf of the
GROND team:

We observed the field of GRB 111123A (Stamatikos, GCN 12587)
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 on La Silla. Observations
started at 6:30 UT on November 24, about 12 hr after the burst, and
continued for about 1.5 hr. They were performed at an average seeing of 1
arcsec and an average airmass of 1.5.

We do not detect the source discovered by Xu et al. (GCN 12589; see
also Fugazza et al. GCN 12593). At a mean time of November 24, 7:10 UT,
we measure the following preliminary upper limits (AB magnitudes):

  g' > 24.5,
  r' > 24.6,
  i' > 23.7,
  J  > 21.2,
  H  > 20.9,
  K  > 19.9.

The data are calibrated against GROND zeropoints and 2MASS field stars.


GRB_name: GRB111123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12596
SUBJECT: GRB 111123A - NOT optical observations
DATE:    11/11/24 17:38:19 GMT
FROM:    Annalisa De Cia at U of Iceland  <annalisa@raunvis.hi.is>

A. De Cia (U. of Iceland), D. Xu (WIS), N.R. Tanvir (U. of Leicester), G. Leloudas, D. Malesani (DARK), G. Maciejewski (U. Nicolaus Copernicus), A. de Ugarte Postigo (IAA/CSIC), J.P.U. Fynbo (DARK) and P. Jakobsson (U. of Iceland) report:

We observed the field of GRB 111123A (Stamatikos et al., GCN 12587, Fugazza et al. 12593) with the NOT equipped with ALFOSC at the end of the night in La Palma, when the humidity dropped below the observability threshold. Observations were carried out in the R filter for 30 minutes, starting at 5:59 UT, with a mean time of 12.02 hours after the GRB trigger.

No significant source was detected at the position of the candidate optical afterglow (Xu et al., GCN 12589) down to R>~24.4 mag, calibrated against USNO-B1stars.


GRB_name: GRB111123A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12597
SUBJECT: GRB 111123A: Swift/UVOT Upper Limits  
DATE:    11/11/24 20:37:04 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

S. T. Holland (CRESST/USRA/GSFC) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift/UVOT team:

     The Swift/UVOT observed the field of GRB 111123A starting 90 s
after the BAT trigger (Stamatikos et al., 2011, GCNC 12587).  Settled
observations started at 110 s.  We do not detect an optical afterglow
at the location of the optical and near-infrared afterglow (Xu et al.,
2011, GCNC 12589; Fugazza et al., 2011, GCNC 12593) in any of the UVOT
filters.  Preliminary 3-sigma upper limits for detecting a source in
the finding charts and in the co-added images, are

Filter       TSTART       TSTOP  EXPOSURE       Mag 
---------------------------------------------------
white (FC)      110         260       147     >21.2
    u (FC)      268         518       246     >20.3
white (FC)      871         934        62     >20.1
---------------------------------------------------
   v            598        5999       430     >20.2
   b            524        6711       325     >20.7
   u            268        6614       678     >20.8
uvw1            647        6409       432     >20.6
uvm2            622        6204       432     >20.6
uvw2            573        5795       432     >20.9
white           110        5589       445     >21.7
---------------------------------------------------

    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} = 0.05 mag (Schlegel et al. 1998, ApJS, 500, 525).


GRB_name: GRB111123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12598
SUBJECT: GRB 111123A, Swift-BAT refined analysis
DATE:    11/11/26 00:24:19 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.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),
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-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111123A (trigger #508319)
(Stamatikos, et al., GCN Circ. 12587).  The BAT ground-calculated position is 
RA, Dec = 154.845, -20.639 deg which is 
  RA(J2000)  =  10h 19m 22.9s 
  Dec(J2000) = -20d 38' 19.9" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.

The mask-weighted light curve shows two episodes.  The first episode is starting 
at T-10 sec, and peaking at T+10 sec with possible two or three overlapping pulses.  
The second episode shows a gradual increases after the end of the initial episode, 
peaks at T+150 sec, and ends at T+170 sec.  The low level emission continues 
up to T+~300 sec.  T90 (15-350 keV) is 290.0 +- 88.1 sec (estimated error including 
systematics).

The time-averaged spectrum from T-8.7 to T+481.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.68 +- 0.07.  The fluence in the 15-150 keV band is 7.3 +- 0.3 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+146.30 sec in the 15-150 keV band
is 0.9 +- 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/508319/BA/


GRB_name: GRB111126A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12599
SUBJECT: GRB 111126A found in ground analysis of BAT data
DATE:    11/11/29 02:12:02 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (NASA/UMBC/CRESST), D. M. Palmer (LANL)
on behalf of the Swift-BAT team

At 18:57:42 UTC, on November 26, 2011, BAT count rates spiked during
a pre-planned slew maneuver.  In a mosaic of images from slew event data,
a significant source was found at RA, Dec 276.057, +51.461, which is

RA (J2000) 18h 24m 13.6s
Dec (J2000) 51d 27' 38"

with an estimated uncertainty of 3 arcmin radius.  This location is
currently about 29 degrees from the Sun.  No Swift followup is anticipated.

It was a short, hard GRB with multiple peaks.  T90 was 0.8 +/- 0.1 seconds.

The BAT spectrum is best fit by a simple powerlaw with a photon index of
1.1 +/- 0.3.  The fluence in 0.8 seconds was 7 +/- 2 ergs/cm^2.  The peak
flux was 1.2 +/- 0.4 photons/cm^2/s.  The uncertainties are 90% estimated
including systematics.


GRB_name: GRB111129A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12600
SUBJECT: GRB 111129A: Swift detection of a burst with an optical counterpart
DATE:    11/11/29 16:27:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. L. Racusin (NASA/GSFC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), P. A. Evans (U Leicester),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), O. M. Littlejohns (U Leicester),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), M. C. Stroh (PSU), C. A. Swenson (PSU),
E. Troja (NASA/GSFC/ORAU) and B.-B. Zhang (PSU) report on behalf of
the Swift Team:

At 16:18:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111129A (trigger=508712).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 307.441, -52.724, which is 
   RA(J2000)  =  20h 29m 46s
   Dec(J2000) = -52d 43' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a few weak peaks
with a total duration of about 20 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 16:19:46.5 UT, 92.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 307.43460, -52.71300 which is
equivalent to:
   RA(J2000)  = 20h 29m 44.30s
   Dec(J2000) = -52d 42' 46.8"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 42 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 3.24
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White 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)  = 20:29:44.15 = 307.43395
  DEC(J2000) = -52:42:46.5  = -52.71291
with a 90%-confidence error radius of about 0.64 arc sec. This position is 1.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.06 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.04. 

Burst Advocate for this burst is J. L. Racusin (judith.racusin 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: GRB111129A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12601
SUBJECT: GRB 111129A: Enhanced Swift-XRT position
DATE:    11/11/29 20:10:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 809 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111129A, 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 = 307.43385, -52.71297 which is equivalent
to:

RA (J2000): 20h 29m 44.12s
Dec (J2000): -52d 42' 46.7"

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: GRB111129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12602
SUBJECT: GRB 111129A: Swift-BAT refined analysis
DATE:    11/11/30 00:47:25 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111129A (trigger #508712)
(Racusin, et al., GCN Circ. 12600).  The BAT ground-calculated position is
RA, Dec = 307.415, -52.722 deg, which is 
   RA(J2000)  =  20h 29m 39.5s 
   Dec(J2000) = -52d 43' 20.9" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 61%.
 
The mask-weighted light curve shows two slightly overlapping peaks
starting at ~T-7 sec, peaking at ~T-5 and T+1 sec, and ending at ~T+10 sec.
T90 (15-350 keV) is 7.6 +- 1.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.29 to T+2.88 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.56 +- 0.38.  The fluence in the 15-150 keV band is 1.8 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.41 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/508712/BA/


GRB_name: GRB111126A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12603
SUBJECT: GRB 111126A Circular #12599 erratum
DATE:    11/11/30 02:16:56 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

The magnitude of the fluence was omitted in the circular, it should
have been (7 +/- 2) x 10^-8 ergs/cm^2.  We thank Kevin Hurley for
pointing out the error.


GRB_name: GRB111129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12604
SUBJECT: GRB 111129A: Swift-XRT refined Analysis
DATE:    11/11/30 05:27:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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), P.
D'Avanzo (INAF-OAB), V. D'Elia (ASDC), V. Mangano (INAF-IASFPA) and
J.L. Racusin report on behalf of the Swift-XRT team:

We have analysed 9.2 ks of XRT data for GRB 111129A (Racusin  et al.
GCN Circ. 12600), from 77 s to 34.7 ks after the  BAT trigger. The data
comprise 26 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 12601).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.57 (+0.16, -0.17), followed by a break at T+3006 s to
an alpha of 1.19 (+0.12, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.93 (+/-0.08). The
best-fitting absorption column is  1.72 (+0.40, -0.24) x 10^21 cm^-2,
in excess of the Galactic value of 3.2 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (5.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.72 (+0.40, -0.24) x 10^21 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: 11.6 sigma
Photon index:      1.93 (+/-0.08)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00508712.

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


GRB_name: GRB111129A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12605
SUBJECT: GRB 111129A, GROND afterglow observations
DATE:    11/11/30 09:34:58 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

A. Rossi, A. Nicuesa Guelbenzu (all Tautenburg)
and J. Greiner (MPE) report on behalf of the GROND team:

We observed the field of GRB 111129A (Racusin, GCN 12600)
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 on La Silla.

Observations started at 00:30 UT on November 30, about 8.2 hr after the 
burst,
and continued for about 2 hrs. They were performed at an average seeing of 1
arcsec and an average airmass of 1.8.

We detect the afterglow discovered by Racusin et al. (GCN 12600) in the
optical/NIR. At a mean time of November 30, 01:31 UT
(9.25 hours after the trigger)
with exporures times of 24.3 minutes in griz and 20 min in JHK,
we measure the following preliminary magnitudes (AB system):

   g' = 22.9  +/- 0.1,
   r' = 22.3  +/- 0.1,
   i' = 21.8  +/- 0.1,
   z  = 21.3  +/- 0.1,
   J  = 20.5  +/- 0.2,
   H  = 19.8  +/- 0.2,
   K  = 19.1  +/- 0.3

Optical data are calibrated against GROND zeropoints and
NIR against 2MASS field stars.


GRB_name: GRB111129A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12606
SUBJECT: GRB 111129A: Swift/UVOT Detection
DATE:    11/11/30 10:47:24 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and J. L. Racusin (NASA/GSFC) report on behalf 
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111129A
96 s after the BAT trigger (Racusin et al., GCN Circ. 12600).
A source consistent with the XRT position (Osborne et al., GCN Circ. 
12601) is detected in the initial UVOT exposures in the white and u 
filters. The source had already faded by the time the other filters were 
used.

The preliminary UVOT position is:
     RA  (J2000) =  20:29:44.15 = 307.43396 (deg.)
     Dec (J2000) = -52:42:46.5  = -52.71293 (deg.)
with an estimated uncertainty of 0.54 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               96          245          147         19.11  0.1
white              534          726           39        >20.32
v                  584        12305          524        >19.9
b                  509        16631         1223        >21.3
u                  254          503          246         19.10  0.16
w1                 633        22753         1296        >21.2
m2                 608         6008          413        >20.4
w2                 559        12186         1120        >21.5

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: GRB111121A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12607
SUBJECT: GRB 111121A: Suzaku WAM observation of the prompt emission
DATE:    11/12/01 10:39:34 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

C-J. Chuang, Y. Urata, P. Tsai (NCU), Y. Hanabata, T. Uehara,
T. Takahashi, M. Mizuno, M. Ohno, Y. Fukazawa (Hiroshima U.),
T. Yasuda, Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, M. Asahina,
S. Kobayashi, A. Sakamoto (Saitama 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), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The bright short GRB 111121A (Swift/BAT trigger 508161 ; D'Elia et
al., GCN 12578) was detected by the the Suzaku Wide-band All-sky
Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at
16:26:24.488 UT (=T0).

The observed light curve shows a single peak structure starting at T0,
ending at T0+1 s with a duration (T90) of about 0.45 seconds. The
fluence in 100 - 1000 keV was 4.29(-0.41, 0.23) x 10^-6 erg/cm^2. The
1-s peak flux measured from T0+1 s was 20.26 photons/cm^2/s in the
same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+1 s is well fitted by a power-law with exponential cutoff model:

  dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha   0.58 (-0.19, 0.18), and
  Epeak   1678.97 (-210.66, 300.31) keV (chi^2/d.o.f. = 60.1/47).

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


GRB_name: GRB111201A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12608
SUBJECT: GRB 111201A found in ground analysis of BAT data
DATE:    11/12/01 21:33:27 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.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), 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 14:22:45 UT 
with a significance of 10.8 sigma (15-200 keV) from the failed event data 
of trigger #508800.  The event is temporary coincident with the Fermi GBM 
344442167.  The best BAT location is RA, Dec = 190.4854, 32.9935 deg, which is

  RA(J2000)  =  12h 41m 56.5s 
  Dec(J2000) = +32d 59' 36.6" 

with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 32%.

The mask-weighted light curve created from the failed event data 
(available from 14:22:41 to 14:22:51 UT) shows an increase in the rate ~1 sec 
after the event data start time.  The count rate stays constant until the 
end of the event data.  From the BAT raw light curve, the duration of the 
event is ~20 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 1.6 +- 0.3.  The 
fluence in 15-150 keV band measured from the 10 sec long event data is 
4.6 +- 0.8 x 10^-7 erg/cm2.  The 1-sec peak photon flux measured from 
14:22:46 UT is 1.1 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 
90% confidence level.  

Swift ToO observation of this burst has been scheduled.  


GRB_name: GRB111201A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12609
SUBJECT: GRB111201A: Swift-XRT observations
DATE:    11/12/02 03:44:03 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU) and T. Sakamoto (GSFC/UMBC) report on behalf of the
Swift-XRT team:

We have analysed 3.0 ks of XRT data for the GBM/BAT-detected burst:
GRB111201A (Sakamoto et al. et al. GCN Circ. 12608), from 26.5 ks to
32.7 ks after the  GBM/BAT trigger. The data are entirely in Photon
Counting (PC) mode.  An X-ray source is detected within the GBM/BAT
error circle. The refined XRT position is RA, Dec = 190.47701,
+32.98791 which is equivalent to:

RA (J2000): 12 41 54.48
Dec(J2000): +32 59 16.5

with an uncertainty of 3.6 arcsec (radius, 90% confidence). This
position is 32 arcsec from the BAT position. 

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+/-0.4). The
best-fitting absorption column is  3.6 (+1.7, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.3 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.7 x 10^-11 (7.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.6 (+1.7, -1.4) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^20 cm^-2
Excess significance: 4.1 sigma
Photon index:      2.3 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020188.

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


GRB_name: GRB111201A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12610
SUBJECT: GRB 111201A: Swift/UVOT Upper Limits
DATE:    11/12/02 14:45:05 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (MSSL/UCL) and  T. Sakamoto (GSFC/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111201A
26513 s after the BAT trigger (Sakamoto et al., GCN Circ. 12608).
No optical afterglow consistent with the XRT position  (Kennea and
Sakamoto, GCN Circ. 12609) 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

white            26513        32667         2746         >22.6

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: GRB111201A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12611
SUBJECT: GRB 111201A: Confirmation of the X-ray afterglow
DATE:    11/12/04 08:05:14 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) and T. Sakamoto (GSFC/UMBC) report on behalf of 
the Swift-XRT team:

Swift performed a second follow-up observation of the GBM/BAT-detected 
burst, GRB 111201A (Sakamoto et al., GCN Circ. 12608; Kennea & Sakamoto, 
GCN Circ. 12609), collecting a further 3 ks of data between 92.2 and 97.6 
ks after the trigger. This additional observation shows the source to be 
fading with a power-law decay of alpha = 0.55 (+0.22, -0.20), confirming 
it is, indeed, the X-ray afterglow of the burst.

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


GRB_name: GRB111204A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12612
SUBJECT: GRB 111204A: Swift detection of a burst
DATE:    11/12/04 13:50:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (GSFC/USRA/Adiyaman Univ.), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU),
C. A. Swenson (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 13:37:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111204A (trigger=509018).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 336.641, -31.395 which is 
   RA(J2000) = 22h 26m 34s
   Dec(J2000) = -31d 23' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 80 sec.  The peak count rate
was ~400 counts/sec (15-350 keV), at ~50 sec after the trigger. 

The XRT began observing the field at 13:40:08.0 UT, 159.7 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 336.62912, -31.37514 which is
equivalent to:
   RA(J2000)  = 22h 26m 30.99s
   Dec(J2000) = -31d 22' 30.5"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 80 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 1.08
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 143 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 34% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.01. 

Burst Advocate for this burst is 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(04dec11): Per author's request, the contact address for ES
has been changed to edasonbas@yahoo.com .]


GRB_name: GRB111123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12613
SUBJECT: GRB 111123A: optical upper limit in CrAO
DATE:    11/12/04 16:11:41 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

We observed the field of GRB 111123A (Stamatikos et al. GCN 12587) with 
Shajn telescope of CrAO observatory on Nov. 25 between (UT) 02:48 and 03:44 
under a mean seeing of 2.0 arsces and large airmass. We took several frames 
with exposure of 60 s in I-band. Within enhanced Swift-XRT position (Goad et 
al. GCN 12590) we do not detected the optical counterpart (Xu et al., GCN 
12589; Fugazza et al., GCN 12593). A photometry is based on the USNO B1.0 
star 0693-0243552 (10 19 20.57, -20 39 18.7, J2000) assuming I=16.85.

T_start UT  T0+        Filter, Exposure, OT,  uplim (3 sigma)
                  (mid, d)            (s)
02:48:33     1.89584   I       49x60      n/d    22.2


GRB_name: GRB111204A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12614
SUBJECT: GRB 111204A: Enhanced Swift-XRT position
DATE:    11/12/04 16:40:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.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 175 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111204A, 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 = 336.62848, -31.37479 which is equivalent
to:

RA (J2000): 22h 26m 30.84s
Dec (J2000): -31d 22' 29.3"

with an uncertainty of 2.1 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: GRB111123A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12615
SUBJECT: GRB 111123A: optical upper limit in CrAO: correction to the GCN circ. 12613
DATE:    11/12/04 16:57:12 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

The text of the GCN circular  #12613 should be corrected as following. I 
apologize for possible inconvenience.

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

We observed the field of GRB 111123A (Stamatikos et al. GCN 12587) with
Shajn telescope of CrAO observatory on Nov. 25 between (UT) 02:48 and 03:44
under a mean seeing of 2.0 arsces and large airmass. We took several frames
with exposure of 60 s in I-band. Within enhanced Swift-XRT position (Goad et
al. GCN 12590) we do not detected the optical counterpart (Xu et al., GCN
12589; Fugazza et al., GCN 12593). A photometry is based on the USNO B1.0
star 0693-0243552 (10 19 20.57, -20 39 18.7, J2000) assuming I=16.85.

T_start UT  T0+        Filter, Exposure, OT,  uplim (3 sigma)
                  (mid, d)            (s)
02:48:33     1.89584   I       49x60      n/d    22.2


GRB_name: GRB111204A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12616
SUBJECT: GRB 111204A: MASTER optical observations 
DATE:    11/12/04 18:06:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


  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, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. 
Kornilov,A.Sankovich
  Sternberg Astronomical Institute, Moscow State University


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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB111204A (Sonbas et al., GCN 
Circ 12612) 115 sec after GRB trigger time  after sunset.
Unfortunately our first (20s exposure) images are saturated.

The first unsaturated  images was 2828 sec after GRB 
time at 2011-12-04 14:24:36.065 UT. On our 180s exposure white+polarizator 
set we  haven't found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 15.0  mag.

Our coaded image (started at 2011-12-04 15:00:58 UT, 3240s effective 
exposition) has limit 19.2 mag.

  The message may be cited.


GRB_name: GRB110921A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12617
SUBJECT: GRB 110921A: optical observations in Maidanak observatory
DATE:    11/12/04 20:50:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We update results of Maidanak observations preliminary reported in GCN 
12380.
We observed  the field of the Swift GRB 110921A (Baumgartner  et al., GCN 
12373) with AZT-22 telescope of Maidanak observatory starting  Sep. 21 (UT) 
17:45:30.  Several images in R-filter of 300 s exposure were taken under 
moderate seeing (FWHM ~ 1.7"). We detect a source in coordinates (J2000) 19 
36 23.363 +36 19 43.02 with uncertainty of 0.2" and brightness of R = 22.0 
+/- 0.15. This source is rather consistent  both in position and brightness, 
with the SDSS object   (Xu et al. GCN 12385; Vreeswijk  et al. GCN 12387). 
So we do not detect afterglow reported by (Xu et al. GCN 12385; Breeveld et 
al. GCN 12389; Tokoyoda et al. GCN 12410; Volnova et al. GCN 12438).

Tstart UT, T0+,       Filter, Exposure, OT, Upper Limit (3 sigma)
                (mid, d)            (s)
17:45:30  0.17895  R       8*300        n/d   22.5


GRB_name: GRB111204A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12618
SUBJECT: GRB 111204A: Swift/UVOT Upper Limits
DATE:    11/12/04 21:19:05 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and E. Sonbas (GSFC/USRA/Adiyaman_Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111204A
143 s after the BAT trigger (Sonbas et al., GCN Circ. 12612).
No optical afterglow consistent with the XRT position 
(Beardmore et al., GCN Circ. 12614) 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           143          293          147         >20.4
white              143         5439          541         >21.6
v                 4214         5851          393         >19.6
b                 3599        11889         1054         >20.8
u                  302        11204         1116         >21.3
w1                4624        10291         1133         >20.7
m2                4419        15631          869         >21.1
w2                4009         5646          393         >20.8

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


GRB_name: GRB111022B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12619
SUBJECT: GRB 111022B: CrAO optical limit
DATE:    11/12/04 22:27:27 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  111022B (Holland  et al. GCN 12472) with Shajn 
telescope of CrAO observatory starting on Oct. 22  (UT) 20:44:36  under a 
mean seeing (FWHM) of 3.2 arsces. We took several frames  with exposure of 
60 s in R-band. Within enhanced Swift-XRT position (Beardmore et al. GCN 
12478) we do not detected any optical source. A photometry is based on the 
USNO B1.0  star 1396-0186811  (07 15 51.05 +49 40 13.0) assuming R=17.07
.
T_start UT  T0+        Filter, Exposure, OT,  uplim (3 sigma)
                  (mid, d)            (s)
20:44:36    0.1711     R       64x60       n/d   22.8 


GRB_name: GRB111204A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12620
SUBJECT: GRB 111204A, Swift-BAT refined analysis
DATE:    11/12/04 23:02:55 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <tilan.ukwatta@gmail.com>

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), D. M. Palmer (LANL), A. M. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
E. Sonbas (GSFC/USRA/Adiyaman Univ.), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 111204A (trigger #509018) (Sonbas, et al., GCN Circ. 12612).
The BAT ground-calculated position is RA, Dec = 336.651, -31.414 deg
which is
   RA(J2000)  =  22h 26m 36.2s
   Dec(J2000) = -31d 24' 49.4"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90%
containment). The partial coding was 75%.

The mask-weighted light curve shows two peaks. Initial peak starts
at the trigger time and last until ~T+10 sec. The second broad peak
starts at ~T+43 sec, peaks at ~T+48 sec, and ends at ~T+90 sec.
T90 (15-350 keV) is 48.0 +/- 22.6 sec (estimated error including
systematics).

The time-averaged spectrum from T+33.0 to T+81.0 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.83 +/- 0.30.  The fluence in the 15-150 keV band is
4.7 +/- 0.9 x 10^-07 erg/cm2. The 1-sec peak photon flux measured
from T+56.50 sec in the 15-150 keV band is 0.3 +/- 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/509018/BA/


GRB_name: GRB111204A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12621
SUBJECT: GRB 111204A: Swift-XRT refined Analysis
DATE:    11/12/05 01:50:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.4 ks of XRT data for GRB 111204A (Sonbas  et al. GCN
Circ. 12612), from 157 s to 27.3 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN. Circ 12614).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.86 (+0.31, -0.17).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.2 (+/-0.4). The
best-fitting absorption column is  9 (+16, -8) x 10^20 cm^-2,
consistent with the Galactic value of 1.1 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 6.0 x 10^-11 (6.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9 (+16, -8) x 10^20 cm^-2
Galactic foreground: 1.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.2 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00509018.

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


GRB_name: GRB111204A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12622
SUBJECT: GRB 111204A: GROND Observations
DATE:    11/12/05 08:13:42 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (Tautenburg Observatory), F. Olivares E., and J. Greiner,
(both MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 111204A (Swift trigger 509018; Sonbas et
al., GCN #12612) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP, 120, 405) mounted at the 2.2 m ESO/MPI telescope at La
Silla Observatory (Chile). Observations started on December 5, 2011,
at 00:38 UT, 11 hours after the GRB trigger, during twilight. They were
performed at an average seeing of 1".1 and at an airmass of 1.2 - 2.2.

Based on co-added images of 5900 s integration time in g'r'i'z' and
4800 s in JHK, centered 0.5253 days after the trigger, no new sources
within the enhanced 1".9 XRT error circle (RA = 22:26:30.81, Dec. =
-31:22:29.3; Beardmore et al., GCN #12614, updated version from the
Enhanced XRT Position page) are detected, and the following specific upper
limits (all in the AB magnitude system) are found:

g' > 24.5
r' > 24.9
i' > 24.4
z' > 24.0
J > 22.3
H > 21.6
K > 20.5

Magnitudes were calibrated against GROND zeropoints in g'r'i'z' and 2MASS
field stars in JHK. No corrections for the expected Galactic foreground
extinction were made, which correspond to a reddening of E(B-V)=0.012 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB111201A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12623
SUBJECT: GRB 111201A: GMG optical observation
DATE:    11/12/05 14:00:31 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

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

We observed the field of GRB 111201A (Sakamoto et al., GCN 12608) with
the 2.4m Gao-Mei-Gu (GMG) telescope equipped with YFOSC. Observation
were carried out in a very poor seeing of ~3.6" and 6x600s R-band
images were obtained starting at 21:38:32 UT on 2nd Dec. 2011 (i.e.,
31.27hrs after the burst).

We found a faint and apparently extended source on the southern border
of the XRT error circle (Kennea et al., GCN 12609) at coordinates

RA(J2000)=12:41:54.6
Dec(J2000)=+32:59:12.7

with a circle error radius of ~4 arcsec. The source had R~22.7 mag,
calibrated with nearby USNO B1 stars.

We thank W.-M. Yi, H.-Y. Gao and F. He for performing these observations.


GRB_name: GRB111204A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12624
SUBJECT: GRB 111204A: TNG NIR observations
DATE:    11/12/05 20:51:16 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

D. Fugazza, S. Covino, A. Melandri (INAF-OAB), V. D'Elia (INAF-OAR), P.
D'Avanzo, S. Campana, G. Tagliaferri (INAF-OAB) and E. Palazzi
(INAF-IASFBo) on behalf of a larger collaboration report:

We observed the field of GRB 111204A (Sonbas et al. GCN 12612) with the
3.6m TNG equipped with the NICS near-infrared camera. A sequence of JHK
band images were acquired starting on Dec 04.792 UT (i.e. ~5.4 hours after
the burst event) lasting 15, 10 and 20 minutes, respectively.

We do not detect any object inside the enhanced XRT position (Beardmore et
al. GCN 12614) down to the following limiting magnitudes (3sigma c.l.,
calibrated against the 2MASS catalogue):

J > 19.7
H > 18.8
Ks > 18.8

We thank the TNG staff for their support, in particular Luca di Fabrizio
and Gianni Tessicini.


GRB_name: GRB111117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12625
SUBJECT: GRB 111117A: Refined GMG observation
DATE:    11/12/07 12:48:44 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

D. Xu (WIS) reports on behalf of a larger collaboration:

We re-processed 1x600s R-band and 3x600s z-band images (Zhao et al.,
GCN 12560), starting 1.960 hrs post-burst,  with calibration frames
available later on. The R-band non-detection remains unchanged.

However, in the stacked z-band image an optical source was weakly
detected, with its position consistent with the NOT position (Andersen
et al., GCN 12563), the refined XRT position (Melandri et al., GCN
12565), as well as the refined Chandra position (Berger et al., GCN
12588), and to the magnitude of z=22.9+/-0.3, calibrated with nearby
SDSS stars. The z-band afterglow faded and was not detected by
following GROND observation (Schmidl et al., GCN 12568).


GRB_name: GRB111205A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12626
SUBJECT: IPN Triangulation of GRB 111205A (long/hard/intense)
DATE:    11/12/07 18:00:09 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,

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

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

The long-duration, intense GRB 111205A has been observed by
INTEGRAL (SPI-ACS), Konus-Wind, and Mars Odyssey (HEND) so far, at about 
47450 s UT (13:10:50).
We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ----------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   134.486 (08h 57m 57s) -31.972 (-31d 58' 20")
  Corners:
   134.668 (08h 58m 40s) -32.260 (-32d 15' 37")
   134.190 (08h 56m 46s) -31.944 (-31d 56' 38")
   134.306 (08h 57m 13s) -31.682 (-31d 40' 57")
   134.782 (08h 59m 08s) -31.999 (-31d 59' 57")
  ---------------------------------------------

The error box area is 492 sq. arcmin, and its maximum
dimension is 39 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: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12627
SUBJECT: Konus-Wind observation of GRB 111205A
DATE:    11/12/07 18:48:42 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 hard intense GRB 111205A (localized by IPN: Hurley et al., GCN 
12626) triggered Konus-Wind at T0=47450.301 s UT (13:10:50.301)

The light curve starts with a hard bright ~20 s long pulse
followed by a weaker tail of softer emission.
A total duration of the burst is ~85 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/GRB111205_T47450/

As observed by Konus-Wind the burst
had a fluence of (1.7  0.1)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+1.024 s,
of (2.2  0.25)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+80.384 
s) is best fitted in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.82 (-0.04, +0.04),
and Ep = 998 (-70, +77) keV,
chi2 = 98.0/85 dof.
Fitting by GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.86 (chi2 = 97.2/84 dof).

The spectrum at the maximum count rate (measured from T0 to T0+4.352 s)
is best fitted in the 20 keV - 10 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.35 (-0.05, +0.05),
and Ep = 1120 (-57, +60) keV,
chi2 = 68.8/85 dof.


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


GRB_name: GRB111208A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12628
SUBJECT: GRB 111208A found in ground analysis of BAT data
DATE:    11/12/08 16:35:58 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.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 08:28:11 UT 
with a significance of 10.1 sigma (15-200 keV) from the failed event data 
of trigger #509285.  The event is temporally coincident with the Fermi GBM 
345025692.  The best BAT location is RA, Dec = 290.2151, +40.6686 deg, which is

  RA(J2000)  =  19h 20m 51.6s 
  Dec(J2000) = +40d 40' 07.0" 

with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 10%.

The mask-weighted light curve created from the failed event data 
(available from 08:28:12 to 08:28:22 UT) shows a constant positive 
rate from the beginning of the data and then decaying at 08:28:20 UT.  
From the BAT raw light curve, the duration of the event is ~20 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 1.5 +- 0.3.  The 
fluence in 15-150 keV band measured from the 10 sec long event data is 
9.8 +- 1.8 x 10^-7 erg/cm2.  The 1-sec peak photon flux measured from 
08:28:19 UT is 1.3 +- 0.7 ph/cm2/sec.  All the quoted errors are at the 
90% confidence level.  

Swift ToO observation of this burst has been scheduled.  


GRB_name: GRB111207A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12629
SUBJECT: GRB 111207A found in ground analysis of BAT data
DATE:    11/12/08 18:14:33 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC-CRESST), D. M. Palmer (LANL), 
T. Sakamoto (NASA/UMBC-CRESST) and C. Wolf (PSU) on behalf of the BAT team.

At 14:16:59 on December 7, 2011, Swift-BAT detected a rate increase. The source
was not detected at high enough significance onboard to trigger a GRB response.
In ground analysis, a significant source was found at RA, Dec, 92.924 -39.504,
which is,

RA (J2000) 06h 11m 41.7s
Dec (J2000)  -39d 30' 16" 

The burst was a single pulse, T90 = 3 +/- 1 second. The maximum count
rate in BAT was 1000 +- 200 counts/second.  

A Swift followup TOO has been requested.


GRB_name: GRB111205A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12630
SUBJECT: GRB 111205A:  Swift XRT Observations
DATE:    11/12/08 19:40:46 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

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

We have analysed 5.0 ks of XRT data for the IPN-detected burst: GRB  
111205A
(Hurley et al.  GCN Circ. 12626), from 198.4 ks to 210.7 ks after the   
IPN trigger.
The data are entirely in Photon Counting (PC) mode. The XRT field-of- 
view does
not cover the entire IPN error region. However, an uncataloged X-ray  
source is
detected within the observed XRT field which is potentially the  
afterglow of
GRB 111205A. The refined XRT position is RA, Dec = 134.6793, -31.94327
which is equivalent to:

RA (J2000): 08 58 43.03
Dec(J2000): -31 56 35.8

with an uncertainty of 4.3 arcsec (radius, 90% confidence). This  
position is inside
the IPN error box. We cannot determine at the present time whether the  
source is
fading.  A follow-up Swift observation is planned in several days to  
confirm fading
of the source.  The XRT position is outside of the UVOT field of  
view.  However,
archival DSS imaging reveals a faint optical source within the XRT  
error circle.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020189.


GRB_name: GRB111208A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12631
SUBJECT: GRB 111208A: Swift XRT/UVOT observations
DATE:    11/12/08 22:00:03 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

C. A. Wolf (PSU), E. A. Hoversten (PSU), and T. Sakamoto (GSFC/UMBC)  
report on behalf of the Swift team:

We have analyzed 2.85 ks of XRT data for the BAT ground-detected  
burst: GRB 111208A (Sakamoto et. al. GCN Circ. 12628), from 24.3 ks to  
34.9 ks after the burst. The data are entirely in Photon Counting (PC)  
mode. An uncataloged X-ray source is detected within the BAT error  
circle and is potentially the afterglow of GRB 111208A. The refined  
XRT position is RA, Dec = 290.2251, +40.6766 which is equivalent to:

RA (J2000); 19 20 54.0
Dec(J2000): +40 40 35.8

with an uncertainty of 4.1 arcsec (radius, 90% confidence). This  
position is 39.7 arcsec from the BAT position, within the BAT error  
circle. This position may be improved as more data are received. We  
cannot determine whether the source is fading at the present time.
The Swift/UVOT began settled observations of the field of GRB 111208A  
24.3 ks after the BAT trigger. No optical afterglow consistent with  
the XRT position is detected in the initial UVOT exposures.   
Preliminary 3-sigma upper limits using the UVOT photometric system  
(Poole et al. 2008, MNRAS, 383, 627) for the initial exposures are:

Filter         T_start(ks)   T_stop(ks)      Exp(s)         Mag
white             24.3          34.9          2100         >22.0
The magnitude in the table is not corrected for the Galactic  
extinction due to the reddening of E(B-V) = 0.12 in the direction of  
the burst (Schlegel et al. 1998).  We note that this is a crowded  
field and that there is a source a few arcseconds outside the XRT  
error circle.  However, this source is clearly visible in archival  
optical imaging.


GRB_name: GRB111209A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12632
SUBJECT: GRB 111209A: Swift detection of a long burst with an optical counterpart
DATE:    11/12/09 07:42:40 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. A. Hoversten (PSU), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), A. Y. Lien (NASA/GSFC/ORAU),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
M. C. Stroh (PSU), G. Tagliaferri (INAF-OAB) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:

At 07:12:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111209A (trigger=509336).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 14.360, -46.788 which is 
   RA(J2000) = 00h 57m 26s
   Dec(J2000) = -46d 47' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  After the original 320 second long image 
trigger, the source caused a second trigger (#509337) over the
64 second time interval starting at T+424s, at much higher intensity. 

The XRT began observing the field at 07:19:07.2 UT, 418.9 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 14.3462, -46.8005 which is equivalent to:
   RA(J2000)  = 00h 57m 23.08s
   Dec(J2000) = -46d 48' 01.7"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 56 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 1.20e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 427 seconds after the BAT trigger.  There is a
candidate afterglow in  the rapidly available 2.7'x2.7' sub-image at
approximately the same position as the XRT source with a magnitude of
18.1.  No correction has been made  for the expected extinction
corresponding to E(B-V) of 0.02. 

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: GRB111209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12633
SUBJECT: GRB 111209A: TAROT La Silla observatory optical detection
DATE:    11/12/09 07:58:01 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 111209A detected by SWIFT
(trigger 509336) with the TAROT robotic
telescope (D=25cm) located at the European Southern
Observatory, La Silla observatory, Chile.

The observations started 358s after the GRB trigger.
The elevation of the field decreased from
13 degrees above horizon and weather conditions
were good.

We detected the candidate couterpart mentioned
by Hoversten et al. (GCNC 12632)
at the following position (+/- 1 arcsec):

RA(J2000) = 00h 57m 22.7s
DEC(J2000) -46d 48' 05"

OT peaked at R~16.2 about 680s after GRB.

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

This message may be cited.


GRB_name: GRB111209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12634
SUBJECT: GRB 111209A: REM NIR detection
DATE:    11/12/09 08:05:21 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@brera.inaf.it>

D. Fugazza, S. Covino (INAF/OAB), E. Palazzi (INAF/IASF-Bo), L.A. Antonelli (INAF/Rome),
on behalf of a larger collaboration, report:


The robotic 60-cm REM telescope located at La Silla (Chile) observed automatically
the field of GRB 111209A (Hoversten et al. GCN 12632) with the ROSS optical
and REMIR near-infrared cameras in imaging mode.

Observations started about 30 s after the Swift alert (about 5 min after the reported burst time)
when the field was only 13 deg on the local horizon. 

Summing H band images from 7 to 13 min after the burst a weak counterpart is visible
at coordinates RA=00:57:22.78 DEC=-46:48:04.2 (error approximately 0.5 arcsec on both axes)
and with magnitude H = 14.7 +- 0.2, calibrated against the 2MASS catalogue.
The source is coincident with the optical counterpart reported by Klotz et al. (GCN 12633).

Further observations are in progress.

[GCN OPS NOTE(09dec11):  Per author's request, LA was added to the author list.]


GRB_name: GRB111209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12635
SUBJECT: GRB 111209A: Faulkes Telescope North observations
DATE:    11/12/09 10:29:53 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB),
S. Kobayashi, C.G. Mundell (LJMU), A. Gomboc (U. Ljubljana)
report on behalf of the LJMU GRB group:

The 2-m Faulkes Telescope North robotically followed
up Swift GRB 111209A (Hoversten et al. GCN Circ. 12632)
from 07:20:00 UT, corresponding to 7.9 minutes after the
BAT trigger time.
Within the XRT error circle we clearly detect the optical
afterglow in the i' filter reported by Klotz et al. (GCN 12633)
and Fugazza et al. (GCN 12634) with the following magnitude:

Mid time from  Total Exp   Filter    Magnitude
trigger (s)    (s)
-------------------------------------------------
697            30           i'       18.3 +- 0.2
-------------------------------------------------

Magnitude has been calibrated from I nominal
values of nearby USNOB1.0 stars.


GRB_name: GRB111205A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12636
SUBJECT: GRB 111205A: GROND observations
DATE:    11/12/09 12:59:15 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

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

We observed the field of the possible X-ray afterglow (Wolf & Hoversten,
GCN #12630) of the intense IPN GRB 111205A (Hurley et al., GCN #12626,
Golenetskii et al., GCN #12627) simultaneously in g'r'i'z'JHK with GROND
(Greiner et al. 2008, PASP, 120, 405) mounted at the 2.2 m ESO/MPI
telescope at La Silla Observatory (Chile).

Observations were obtained at a
mid-time of 07:35 UT on December 9, 2011, 4.87 days after the GRB trigger,
under excellent conditions. They were performed at an average seeing of
0".7 in the optical bands and at an airmass of 1. The integration time was
1475 sec in g'r'i'z' and 1200 sec in JHK.

The DSS source mentioned by Wolf & Hoversten in the XRT error circle is
detected and is revealed to be a double star separated by about 1".2, both
components clearly resolved due to the excellent seeing. The r'-band
magnitudes of the stars (calibrated against an SDSS standard field) are
16.33 (south-east, edge of error circle) and 16.85 (north-west, in error
circle) with negligible errors.

We therefore posit that this source is not associated with GRB 111205A,
and the X-ray source detected by XRT is not the X-ray afterglow of the
GRB. We note that such a faint X-ray source, at 6E-3 cts/s, would be
untypical for an X-ray afterglow of an intense GRB, even several days
after the GRB.


GRB_name: GRB111209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12637
SUBJECT: GRB 111209A: TAROT La Silla observatory optical light curve analysis
DATE:    11/12/09 13:59:58 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We obtained an optical follow-up until 4500 seconds
after the trigger of GRB 111209A detected by SWIFT
(trigger 509336-7) using the TAROT robotic telescope
(D=25cm) located at the European Southern Observatory,
La Silla observatory, Chile.

In this GCN circular we describe the behaviour of the
optical transcient discovered by Hoversten et al.
(GCNC 12632).

 From 470s to 2000s, we observe a fluctuating
optical emission at a mean level R~17.5 that reaches
sometimes R=16.6.

 From 2100s to 2550s we recorded an optical flash
that reached R=15.4. This peak is followed by
a plateau R=16.3 between 2700s to 3700s.

After 3700s the flux seems begin to decrease but
the low elevation 5 degrees above horizon does
not allow to conclude definitively about the
phase decay.

All the magnitudes are based on the assumption
that the color index of the GRB in optical
wavelengths is the same as the reference star
NOMAD1 0431-0011481 (V-R=0.34).

This message may be cited.


GRB_name: GRB111209A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12638
SUBJECT: GRB111209A : planned XMM-Newton observation
DATE:    11/12/09 16:05:56 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@asdc.asi.it>

B. Gendre (ASDC/INAF-OAR), J.L. Atteia (IRAP-OMP), M. Bor (OHP-OAMP),
A. Klotz (IRAP-OMP), L. Piro (INAF-IASF-Roma), G. Stratta
(ASDC/INAF-OAR), on behaf of a larger collaboration, report :

Following the trigger of the exceptionally long and bright GRB 111209A,
we have activated a 50 ks (net) TOO on XMM-Newton starting on
2011-12-09:22:12:58 UT. We encourage any simultaneous follow-up of this
event at any wavelength.

This message can be quoted.


GRB_name: GRB111209A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12639
SUBJECT: GRB 111209A: Enhanced Swift-XRT position
DATE:    11/12/09 17:10:26 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 2386 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 111209A, 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 = 14.34424, -46.80112 which is equivalent
to:

RA (J2000): 00h 57m 22.62s
Dec (J2000): -46d 48' 04.0"

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: GRB111209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12640
SUBJECT: GRB 111209A, Swift-BAT refined analysis
DATE:    11/12/09 18:58:12 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.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), 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 the recent telemetry downlink, we report further 
analysis of BAT GRB 111209A (trigger #509336 and #509337) 
(Hoversten, et al., GCN Circ. 12632).  The BAT ground-calculated position 
using the event data of trigger #509337 (on-axis observation) 
is RA, Dec = 14.350, -46.799 deg which is 

 RA(J2000)  =  00h 57m 24.1s 
 Dec(J2000) = -46d 47' 57.1" 

with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows an excess rate already around T-150 s 
when the spacecraft settled to the pre-planned target (T is the BAT trigger 
time of #509336, which is 07:12:08.3 UT).  A gradual increase in the rate 
continues up to T+850s.  And then, the rate started to decay.  The positive 
rate is still seen at T+1400 s where the end of the event data.  Further 
analysis using the BAT survey data is on-going to address the duration of 
this event detected by BAT.   

The time-averaged spectrum from 358 to 1337 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.48 +- 0.03.  The fluence in the 15-150 keV band measured during this 
time interval is 3.6 +- 0.1 x 10^-05 erg/cm2.  The 1-sec peak photon flux 
measured from T+824 sec in the 15-150 keV band is 0.5 +- 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/509336/BA/
http://gcn.gsfc.nasa.gov/notices_s/509337/BA/


GRB_name: GRB111209A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12641
SUBJECT: GRB 111209A: Swift Burst of Interest
DATE:    11/12/09 19:04:03 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU), D.N. Burrows (PSU), S. Campana (INAF-OAB), P.  
A. Evans (U Leicester), N. Gehrels (GSFC), D. Grupe (PSU), M. H.  
Siegel (PSU), report on behalf of the Swift team:

We report an update on Swift observations of the unusual event GRB  
111209A.  BAT triggered twice and is saw extended duration emission  
from this event.  It peaked at 900s and decreased in flux after 1100s,  
but continued well beyond that to >10ks.

We have analyzed 11.9 ks of XRT data for GRB 111209A (Hoversten  et  
al. GCN Circ. 12632), from 425 s to 25.16 ks after the  BAT trigger.  
The data contain 9.4 ks in Windowed Timing (WT) mode data and the  
remainder in photon counting (pc) mode.

The light curve is highly complicated showing multiple flares. The  
afterglow is very bright and XRT remained in WT mode through 4 orbits  
(20ks after the trigger). The light curve after the fourth orbit  
suggests a sharp drop in the count rate from about 14 counts s^-1 at  
the end of the forth orbit to 5 counts s^-1 at the beginning of
the fifth orbit. The data of the 5th orbit were entirely taken in  
photon counting (pc) mode and the decay slope steepens significantly.

The Swift/UVOT began settled observations of the field of GRB 111209A  
427 s after the BAT trigger.  The afterglow is clearly detected in all  
seven UVOT filters.  We find a refined UVOT position of

      RA (J2000)  00:57:22.63  =  14.34429 (deg)
     Dec (J2000) -46:48:03.8   =  -46.80106 (deg)

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence,  
statistical + systematic).  This position is 0.25 arcseconds from the  
UVOT-enhanced XRT position, which is within the errors.

The white, v, and b filter show a fading source over the first orbit,  
however at the end of the first orbit the white magnitude increases  
abruptly by 0.6 magnitudes corresponding with a significant flare in  
the X-rays.  The v, b, u, uvw1, and uvm2 magnitudes show a  
rebrightening between 5.4 and 7 ks after the burst of 0.3 to 1.1  
magnitudes.

The data from all three instrument is similar is several ways to GRB  
060218, the long event associated with SN2006aj, and to GRB 101225A,  
the Christmas burst.  The detection in all UVOT filters implies a low  
redshift of z < 1.6.  We note that at 18 ks after the burst the source  
is still at 18th magnitude in the white filter which is extremely  
unusual.  Given the rare behavior exhibited by GRB 111209A we advocate  
for additional observations at all wavelengths.


GRB_name: GRB111209A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12642
SUBJECT: GRB 111209A: Swift UVOT refined analysis
DATE:    11/12/09 19:22:04 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and M. H. Siegel (PSU), report on behalf of the  
UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111209A  
427 s after the BAT trigger (Hoversten et al., GCN Circ. 12632).  The  
afterglow is clearly detected in all seven UVOT filters.  We find a  
refined UVOT position of

      RA (J2000)  00:57:22.63  =  14.34429 (deg)
     Dec (J2000) -46:48:03.8   =  -46.80106 (deg)

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence,  
statistical + systematic).  This position is 0.25 arcseconds from the  
UVOT-enhanced XRT position (Evans et al., GCN Circ. 12639), which is  
within the errors.

The white, v, and b filters show a fading source over the first orbit,  
however at the end of the first orbit the white magnitude increases  
abruptly by 0.6 magnitudes corresponding with a significant flare in  
the X-rays.  The v, b, u, uvw1, and uvm2 magnitudes show a  
rebrightening between 5.4 and 7 ks after the burst of 0.3 to 1.1  
magnitudes. Preliminary magnitudes 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     Err

white_FC     427         577      147   17.94    0.04
white        855        1005      147   17.73    0.04
white       1856        1876       19   18.01    0.11
white       2030        2050       19   17.40    0.08
v            584         603       19   17.25    0.24
b           1134        1154       19   18.16    0.21
u           6064        6264      196   18.11    0.09
w1           633         653       19   17.16    0.24
m2          5653        5853      196   18.23    0.17
w2          5244        5443      196   17.96    0.12

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).

The data from all three instrument is similar is several ways to GRB  
060218, the long event associated with SN2006aj, and to GRB 101225A,  
the Christmas burst.  The detection in all UVOT filters implies a low  
redshift of z < 1.6.  We note that at 18 ks after the burst the source  
is still at 18th magnitude in the white filter which is extremely  
unusual.  Given the rare behavior exhibited by GRB 111209A we advocate  
for additional observations at all wavelengths.


GRB_name: GRB111209A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12643
SUBJECT: GRB 111209A: Swift-XRT refined Analysis
DATE:    11/12/09 19:34:18 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

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

We have analyzed 11 ks of XRT data for GRB 111209A (Hoversten  et al.
GCN Circ. 12632), from 425 s to 25.2 ks after the  BAT trigger. The
data comprise 9.4 ks 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 12639).

The light curve can be modeled with a series of power-law decays. The
light curve initially rises, with an index alpha=-0.21 (+/-0.04). At
T+864 s it breaks to an alpha of 7.3 (+0.7, -2.6). The light curve
breaks again at T+899 s to a decay with alpha=0.679 (+0.012, -0.087), 
and  again at T+5807 s s to alpha=1.179 (+/-0.016),  before a final
break at T+19.4 ks s after which the decay index is 6.3 (+1.2, -0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.333 (+/-0.012). The
best-fitting absorption column is  1.38 (+/-0.04) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.83 (+0.17, -0.16)
and a best-fitting absorption column of 1.3 (+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 4.1 x 10^-11 (5.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: 4.4 sigma
Photon index:      1.83 (+0.17, -0.16)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00509336.

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


GRB_name: GRB111208A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12644
SUBJECT: GRB 111208A: Lightbuckets Optical Observations
DATE:    11/12/09 20:35:17 GMT
FROM:    Tilan Ukwatta at GSFC/GWU  <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 111208A
(Sakamoto et al., GCN 12628) 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
2011-12-08 at 17:04:45 UT (~ 31 ks after the GRB trigger).
This observation is in temporal coincidence with the Swift
XRT TOO observation which spanned from 24.3 ks to 34.9 ks
(Wolf et al., GCN 12631).

In the stacked R band image, we do not detect an optical
afterglow at the XRT location. Our upper-limit based on the
observation is given below.

Time after trigger       Exposure (s)   Filter     Magnitude
  8.61 hours             600               R         > 19


GRB_name: GRB111209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12645
SUBJECT: GRB 111209A: PROMPT optical observations of early afterglow
DATE:    11/12/09 22:54:13 GMT
FROM:    Melissa Nysewander at UNC-Chapel Hill  <mnysewan@unc.edu>

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

Skynet observed the field of GRB 111209A with the PROMPT telescopes located at CTIO in Chile.  Observations began in VRI at 378 sec (34 sec after the alert) and lasted for 13.2 min before the source set below PROMPT's elevation constraints.

We detect the fading afterglow discovered by Hoversten et al. (GCN 12632).  Preliminary calibration to USNO B1.0 catalog stars yields the follow initial detections:

Start Time    t - t0      Exp     Telescope      Filter       Mag      Err
07:18:28      380s      40s      Prompt5        I             18.0      0.20
07:18:31      383s      40s      Prompt4        R            18.3      0.30


GRB_name: GRB111209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12646
SUBJECT: GRB 111209A optical limit by "Pi of the Sky"
DATE:    11/12/09 23:59:27 GMT
FROM:    Marcin Sokolowski at Soltan Inst. Nuc Studies,Warsaw  <marcin.sokolowski@fuw.edu.pl>

M.Sokolowski,A.Majcher,T.Batsch,A.Majczyna,K.Nawrocki,G.Wrochna (NCNR,Swierk),
M.Cwiok,W.Dominik,L.W.Piotrowski,A.F.Zarnecki (University of Warsaw),
K.Malek,L.Mankiewicz,R.Opiela,M.Siudek,V.Repei (CFT PAN),
G.Kasprowicz,M.Zaremba (Warsaw University of Technology),
from the "Pi of the Sky" collaboration (http://grb.fuw.edu.pl).

The wide field "Pi of the Sky South" apparatus, installed in the private
observatory of Alain Maury in San Pedro de Atacama
(http://grb.fuw.edu.pl/pi/index.html#spda_site.htm) observed the position
of GRB 111209A ( SWIFT trigger #590336 ).
Three 10s images of this field have been taken at 01:59:03 - 01:59:51 UT
( 5 hours 13 min 5 sec before the first BAT alert ). No new object can be
  seen within the error box and the limit on 3 coadded images is 12.7 mag.
After receiving the trigger from SWIFT, the field was observed 480 seconds
after the GRB. The field has been observed in time period from 7:20:09 to
7:44:25 UT, no new object brighter than 10.2 mag was observed on 10s 
images. The limit on 20 coadded images is 10.7 mag.
Limits are based on the reference star magnitudo in V filter.

We acknowladge great support received from Alain Maury at SPdA Observatory.


GRB_name: GRB111209A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12647
SUBJECT: GRB 111209A: GROND Afterglow observations
DATE:    11/12/10 05:52:24 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, S. Klose (TLS Tautenburg), T. Kruehler (DARK/NBI) and J.
Greiner, (MPE Garching) report on behalf of the GROND team:

We observed the field of the "Swift Burst of Interest" GRB 111209A (Swift
trigger 509336 and 509337; Hoversten et al., GCN #12612) simultaneously in
g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP, 120, 405) mounted at
the 2.2 m ESO/MPG telescope at La Silla Observatory (Chile). Observations
started on December 10, 2011, at 00:56 UT, 0.74 days after the GRB
trigger, during twilight. They were performed at an average seeing of 0".9
and at an airmass of 1.

At the position of the optical afterglow (Klotz et al., GCN #12633;
Fugazza et al., GCN #12634; Guidorzi et al., GCN #12635; Hoversten &
Siegel, GCN #12642; Nysewander et al., GCN #12645), we clearly detect a
source in single 35 second integrations in g'r'i'z'.

Based on co-added images of 142 s integration time in g'r'i'z' and 240 s
in JHK, centered 0.74144 days after the trigger, the following magnitudes
(AB magnitude system) have been derived:

g' = 20.3 +/- 0.1
r' = 20.1 +/- 0.1
i' = 19.9 +/- 0.1
z' = 19.8 +/- 0.1
J = 19.3 +/ 0.2
H = 19.0 +/- 0.2
K = 18.6 +/- 0.4

The spectral slope is found to be beta ~0.8, which is typical for a GRB
afterglow, and dissimilar to thermally dominated emission.

Magnitudes were calibrated against an SDSS standard field in g'r'i'z' and
2MASS field stars in JHK.

Observations have continued at high cadence under excellent conditions. We
note these observations are contemporaneous to the planned XMM-Newton
observation (Gendre et al., GCN #12638).


GRB_name: GRB111209A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12648
SUBJECT: GRB 111209A: VLT/X-shooter redshift
DATE:    11/12/10 06:05:55 GMT
FROM:    Paul Vreeswijk at U of Iceland  <pmv@raunvis.hi.is>

Paul Vreeswijk (U. Iceland), Johan Fynbo (DARK), Andrea Melandri
(INAF-OAB) report on behalf of the X-shooter GTO GRB afterglow
collaboration:

The afterglow of Swift GRB 111209A (Hoversten et al., GCN 12632, Klotz
et al., GCN 12633, Fugazza et al., GCN 12634) was observed with the
X-shooter spectrograph mounted at the Kueyen unit of the VLT on Cerro
Paranal, Chile. Starting around 1 UT on 10 December 2011 (0.75 days
after the burst), a series of four spectra of 1200s each were secured,
covering the approximate wavelength range 0.3-2.5 micron. The slit
width was set to 1", resulting in a resolving power range of
4500-7500.

Preliminary reduction of the ultraviolet and visual parts of the
spectra shows a smooth continuum with several absorption features that
we can identify with resonance absorption lines of FeII, MgII, MgI,
CaII H and K at a redshift of z=0.677; this is the likely redshift of
GRB 111209A.

We acknowledge the excellent support from the Paranal Observatory staff,
in particular Willem-Jan de Wit, Dimitri Gadotti and Marcelo Lopez.
We are also very grateful for the flexibility and willingness of the
VLT-I visiting astronomer, Stefan Kraus, to shift his observations
to the end of the night, which have made these X-shooter observations possible.

[GCN OPS NOTE(10dec11): Per author's request, the last paragraph was expanded.]


GRB_name: GRB111209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12649
SUBJECT: GRB 111209A: IRTF NIR Imaging/Spectroscopy
DATE:    11/12/10 11:59:38 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Hyunsung Jun, and Dohyeong Kim (CEOU/Seoul National Univ)

We observed GRB 111209A (Hoversten et al., GCN 12632) using SpeX
on IRTF. The observation started at 12-09-07:42:13 UT, or about 0.5 hrs 
after the BAT alert. H-band images were taken using a guider camera
revealing a bright NIR counterpart with its flux at H~12 mag.
Note that calibration is done by an observation of a standard star 
next night and needs a further refinement.
NIR spectra were taken at 0.8-2.5 micron with R=750 for 
about 24 min, starting at ~35 min after the BAT alert,
showing good S/N but no obvious features in raw spectra. 
Analysis of the spectral/imaging data is onging.


GRB_name: GRB111210A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12650
SUBJECT: GRB 111210A: Swift detection of a burst
DATE:    11/12/10 14:49:33 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU), V. D'Elia (ASDC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU),
E. Troja (NASA/GSFC/ORAU) and B.-B. Zhang (PSU) report on behalf of
the Swift Team:

At 14:37:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111210A (trigger=509419).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 191.488, -7.167 which is 
   RA(J2000) = 12h 45m 57s
   Dec(J2000) = -07d 10' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 2.5 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 14:38:04.0 UT, 60.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 191.47507, -7.16565 which is equivalent
to:
   RA(J2000)  = 12h 45m 54.02s
   Dec(J2000) = -07d 09' 56.3"
with an uncertainty of 3.8 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 consistent with the Galactic value of 1.92
x 10^20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 64 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. No correction has been
made for the expected extinction corresponding to E(B-V) of 0.03. 

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: GRB111210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12651
SUBJECT: GRB 111210A: Swift-BAT refined analysis
DATE:    11/12/10 18:48:50 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. H. Siegel (PSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+178 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111210A (trigger #509419)
(Siegel, et al., GCN Circ. 12650).  The BAT ground-calculated position is
RA, Dec = 191.493, -7.173 deg, which is 
   RA(J2000)  =  12h 45m 58.3s 
   Dec(J2000) = -07d 10' 21.8" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows two peaks; the first starting at ~T-2.3 sec
and ending at ~T-1.6 sec, and the second starting at ~T-0.2 sec, peaking
at ~T+0.1 sec, and ending at ~T+0.4 sec.  T90 (15-350 keV) is 2.52 +- 0.13 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-2.33 to T+0.36 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.30 +- 0.19.  The fluence in the 15-150 keV band is 1.6 +- 0.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-2.33 sec in the 15-150 keV band
is 1.0 +- 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/509419/BA/


GRB_name: GRB111210A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12652
SUBJECT: GRB 111210A: Enhanced Swift-XRT position
DATE:    11/12/10 20:11:21 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 1316 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 111210A, 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 = 191.47684, -7.16593 which is equivalent
to:

RA (J2000): 12h 45m 54.44s
Dec (J2000): -07d 09' 57.4"

with an uncertainty of 2.1 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: GRB111210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12653
SUBJECT: GRB 111210A:  Spectral lag analysis
DATE:    11/12/10 21:06:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. Norris (BSU) for the BAT Team:

We report the spectral lag analysis for GRB 111210A (GCN Circ. 12632 & 12640) 
based on the BAT data.  Using 16-ms binned light curves, the spectral lag
for the 15-25 keV to 50-100 keV bands is 38 +26/-33 msec, and 36 +16/-18 msec
for the 25-50 keV to 100-350 keV bands for both peaks combined.  For just
the second peak, the lag for 15-25 keV to 50-100 keV bands is 97 +52/-40 msec.
These lag values place this burst in the long burst category.


GRB_name: GRB111210A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12654
SUBJECT: GRB 111210A: Swift/UVOT Upper Limits
DATE:    11/12/10 22:03:51 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 111210A
65 s after the BAT trigger (Siegel et al., GCN Circ. 12650).
No optical afterglow consistent with the XRT position (Goad et al., 
GCN Circ. 12652) 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)          65          214          147         >20.3
u (FC)             276          526          246         >19.5
white               65         6160          569         >20.5
v                  606         6570          471         >19.3
b                  532         7315          397         >20.0
u                  276         7185          659         >19.9
uvw1               657         6980          471         >20.1
uvm2              1062         1082           19         >18.1
uvw2               582         6365          216         >20.5

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: GRB111210A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12655
SUBJECT: GRB111210A: MITSuME Okayama J-band  upper-limit
DATE:    11/12/10 22:48:20 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 GRB111210A (Siegel et al, GCN12650, Stamatikos
et al, GCN12651) in J-band with a wide-field NIR camera at Okayama
Astrophysical Observatory (Japan). The camera has an effective aperture
of 0.91m.

Observations started from 17:59 UT on 10th December, 3.37 hours after
the BAT trigger, to 19:35 UT.  The total exposure of 73 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 12652) down to limiting
magnitude of  J=16.0 (Vega, S/N=10). The photometric calibration was
made against 2MASS field stars.

T0+[s]      MID-UT     T-EXP[sec]      J
---------------------------------------------------
 +15,000   18:47          4,380       >16.0(S/N=10)
---------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111209A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12656
SUBJECT: GRB 111209A: Rebrightening seen by GROND
DATE:    11/12/10 23:45:21 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We have analyzed the J-band observations (Kann et al., GCN #12647)
obtained with GROND over a total of five hours (0.74 to 0.93 days after
the trigger) of GRB 111209A (Hoversten et al., GCN #12632). Astrometry and
calibration were obtained against the 2MASS catalog.

We find the afterglow experiences a strong rise during our observations,
rising from J ~ 19.3 to J ~ 18.8 (AB Magnitudes). The slope of the rise is
alpha < -2 (assuming F(t) propto t^-alpha). This behavior may be due to a
strong energy injection.

Highly variable behavior in the first hours has already been reported by
Klotz et al. (GCN #12637) and Hoversten & Siegel (GCN #12642).

Dense photometric follow-up is strongly encouraged.


GRB_name: GRB111210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12657
SUBJECT: GRB 111210A: Gemini-North candidate counterpart
DATE:    11/12/11 00:42:50 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

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

We obtained short exposures of the field of GRB 111210A (Siegel et
al. GCN 12650) with Gemini-North using the GMOS instrument,
beginning at 2011-Dec-10 15:16UT, approximately 39 minutes post-burst. 
Within the refined XRT position (Goad et al. GCN12652) we find a faint
source which is visible in both z and r filters.  Calibrated against nearby
USNO stars we find a magnitude of r~23, with an estimated error
of +/-0.2 random and +/-0.3 calibration.

Our astrometry gives a position (conservative uncertainty of 0.5 arcsec) of:

RA(2000)= 12 45 54.40
dec(2000)= -07 09 57.4

We thank the Gemini staff, particularly Kristin Chiboucas and
Rachel Mason, for assistance with these observations.


GRB_name: GRB111208A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12658
SUBJECT: GRB 111208A: Swift-XRT refined analysis
DATE:    11/12/11 01:25:02 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

C. A. Wolf (PSU) reports on behalf of the Swift-XRT team:

We have analysed 4.5 ks of XRT data for the Swift/BAT ground-detected
burst: GRB 111208A (Sakamoto et al. GCN Circ. 12628), from 24.3 ks to
40.8 ks after the burst. The data are entirely in Photon Counting (PC)
mode.  An X-ray source is detected within the Swift/BAT error circle.
Using 4204 s of PC mode data and 6 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 = 290.22434, +40.67616 which is
equivalent to:

RA (J2000): 19h 20m 53.84s
Dec(J2000): +40d 40' 34.2"

with an uncertainty of 1.6 arcsec (radius, 90% confidence). This
position is 37 arcsec from the Swift/BAT position. 

The light curve can be modelled with  a power-law decay with a decay
index of alpha=3.14 (+0.23, -0.90).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.14 (+0.25, -0.37). The
best-fitting absorption column is  1.7 (+1.1, -0.9) x 10^21 cm^-2,
consistent with the Galactic value of 8.4 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 3.5 x 10^-11 (5.3 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+1.1, -0.9) x 10^21 cm^-2
Galactic foreground: 8.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.14 (+0.25, -0.37)

The results of the XRT-team automatic analysis are available at

http://www.swift.ac.uk/xrt_products/00020190
.

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


GRB_name: GRB111210A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12659
SUBJECT: GRB 111210A: MITSuME Okayama Optical upper limits
DATE:    11/12/11 02:24:18 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 111123A (Siegel et al., GCNC 12650)
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 2011-12-10 17:54:08 UT (~3.3 h after
the burst). We did not find any new point source within the enhanced
XRT circle (Goad, et al., GCNC 12652) in all the three bands.


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

T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.17952    18:55:34    5640.0    >18.9  >19.3  >18.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111210A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12660
SUBJECT: GRB 111210A: Swift-XRT refined Analysis
DATE:    11/12/11 02:49:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

D.N. Burrows (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), V. Mangano (INAF-IASFPA), A.
Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), J.A. Kennea (PSU),
M.C. Stroh (PSU) and M.H. Siegel report on behalf of the Swift-XRT
team:

We have analysed 6.8 ks of XRT data for GRB 111210A (Siegel  et al. GCN
Circ. 12650), from 69 s to 30.5 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 12652).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=3.7 (+/-0.4).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+0.6, -0.3). The
best-fitting absorption column is  consistent with the Galactic value
of 1.9 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 4.7 x 10^-11 (4.9 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+1.1, -0) x 10^21 cm^-2
Galactic foreground: 1.9 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.6 (+0.6, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00509419.

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


GRB_name: GRB111210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12661
SUBJECT: GRB 111210A: SDSS prior imaging
DATE:    11/12/11 11:58:43 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester) and D. Malesani (DARK) report:

We have analysed images of the field of GRB 111210A available in SDSS
DR8.  The source detected in the Gemini imaging (Tanvir et al. GCN
12657) is also visible at low S/N in the gri and z filter images.  Our
photometry gives magnitudes g=23.9, r=23.0, i=22.9 and z=23.0, with
errors around 0.3 mag in each case.  Since these are consistent with
the Gemini magnitudes, this suggests that the source is a candidate
host galaxy, with little if any afterglow contributing to the Gemini images.
The detection in the g-band, and indeed its brightness, mean this
source is likely to be at redshift z<4.


GRB_name: GRB111210A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12662
SUBJECT: GRB 111210A: GROND observations
DATE:    11/12/11 12:31:25 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of the Swift GRB 111210A (Swift trigger 509419; 
Siegel et al., GCN #12650) simultaneously in g'r'i'z'JHK with GROND 
(Greiner et al. 2008, PASP, 120, 405) mounted at the 2.2 m ESO/MPG 
telescope at La Silla Observatory (Chile). Observations started on 
December 11, 2011, at 08:06 UT, 0.73 days after the GRB trigger, during 
morning twilight and were partially performed only in the NIR. They were 
taken at an average seeing of 1".1 and at an airmass of 2 to 1.5.

At the position of the X-ray afterglow (Goad et al., GCN #12652) as well 
as the optical candidate (Tanvir et al., GCN #12657), we tentatively 
detect a source in the redder filters.

Based on co-added images of 743 s integration time in g'r'i'z' (centered 
0.7396 days after the trigger) and 2160 s in JHK (centered 0.7520 days 
after the trigger), the following magnitudes and limits (3 sigma, AB 
magnitude system) have been derived:

g' > 22.6,
r' > 23.2,
i' = 22.8 +/- 0.4,
z' = 22.4 +/- 0.3,
J =  21.4 +/ 0.3,
H =  21.4 +/- 0.4,
K >  20.5.

Our r'-band upper limit is not deep enough to check fading against the 
Gemini North candidate. If the faint detections actually represents a real 
object, this is likely the host galaxy of this GRB (Tanvir & Malesani, GCN 
12661).

Magnitudes were calibrated against the SDSS catalog in g'r'i'z' and 2MASS
field stars in JHK.


GRB_name: GRB111209A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12663
SUBJECT: Konus-Wind observation of GRB 111209A
DATE:    11/12/11 14:10:38 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The exceptionally long GRB 111209A (Swift-BAT trigger #509336: Hoversten 
  et al., GCN 12632; Palmer et al., GCN 12640) was detected by 
Konus-Wind in the waiting mode.

The burst light curve shows the main multipeaked episode of emission 
started at ~T0(BAT)-1900 s and lasted until ~T0(BAT)+4400 s (the 
duration is ~6300 s; T0(BAT)=25928 s UT (07:12:08)). There is also a 
weaker broad pulse of emission seen before the main pulse from 
~T0(BAT)-5400 s to ~T0(BAT)-2600 s and a hint of an additional episode 
of emission after the main pulse from ~T0(BAT)+5000 s to ~T0(BAT)+10000 
s. Both these episodes might be related to GRB 111209A (they were 
detected by the same KW detector, and the KW ecliptic latitude responses 
for them are consistent with the common origin with the main episode). 
The most intense peak in the Konus-Wind light curve, (which started at 
~T0+1740 s, peaked at ~T0+2040 s, and ended at ~T0+2300 s), corresponds 
to a significant raise in the XRT lc 
(http://www.swift.ac.uk/xrt_curves/00509336/ - Grupe & Hoversten GCN 
12643) and a bright optical flash (Klotz et al., GCN 12637).

As observed by Konus-Wind, the burst (the main episode) had a fluence of 
(4.86  0.61)x10^-4 erg/cm2 (in the 20 - 1400 keV energy range).

Modeling the KW 3-channel time-integrated spectrum (from T0-1890 s to
T0+4400 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.31  0.09, and Ep = 310  53 keV.

Assuming z = 0.677 (Vreeswijk, Fynbo, & Melandri GCN 12648) and a 
standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27,
Omega_Lambda = 0.73, the isotropic energy release, E_iso, is (5.82  
0.73)x10^53 erg, and Ep_rest is 520   89 keV.

Thus, the prompt gamma-ray emission properties of this GRB: fluence, Ep, 
and E_iso are similar to those observed in other long energetic GRBs. 
The only exceptional feature of the prompt gamma-ray emission is the 
huge duration.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB111209A/


GRB_name: GRB111209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12664
SUBJECT: GRB 111209A - ATCA 34GHz upper limit
DATE:    11/12/12 03:58:18 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)

On the 11th December 04:44-05:50UT (T=+1.9days) we observed GRB 111209A 
(GCN12632) with the Australia Telescope Compact Array (ATCA) at 34GHz. 
We do not detect any radio emission consistent with the GRB optical 
position (GCN12642). We place a 3sigma upper limit of 132uJy on the flux 
of the afterglow. Further observations are planned.

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


GRB_name: GRB111210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12665
SUBJECT: GRB 111210A: Xinglong TNT upper limit
DATE:    11/12/12 04:04:48 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 111210A (Siegel  et al., GCN 12650)
with Xinglong TNT telescope at 21:16:27 (UT), about 6.67 h  after 
the burst.  14 R-band images were obtained. 
No new source was detected in the combined R band image within 
the errorbox of XRT position. The upper limit was estimated 
to be about 19.5 mag derived from USNO B1.0 R2 mag. 

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: GRB111211A
Detection_method: superAGILE
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12666
SUBJECT: GRB 111211A: SuperAGILE localization of a long GRB
DATE:    11/12/12 07:34:30 GMT
FROM:    Marco Feroci at IASF/INAF  <sa.grb@iasf-roma.inaf.it>

F. Lazzarotto, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci,
L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda
(INAF/IASF Rome), G. Barbiellini, F. Longo, E. Moretti (INFN Trieste),
A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti,
F. Fuschino, M. Marisaldi, M. Galli (INAF/IASF Bologna),
A. Giuliani, A. Chen, S. Mereghetti, F. Perotti, P. Caraveo (INAF/IASF
Milan), M. Tavani, G. Pucella, V. Vittorini, A. Argan, A. Trois,
G. Piano, S. Sabatini, M. Cardillo (INAF/IASF Rome), A. Pellizzoni, M. Pilia
(INAF/OA Cagliari), S. Vercellone, F. D'Ammando (INAF/IASF Palermo),
P. W. Cattaneo, A. Rappoldi (INFN Pavia), P. Picozza, A. Morselli,
E. Striani, (INFN Roma-2), M. Prest, E. Vallazza (Universita'
dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1),
P. Giommi, C. Pittori, F. Lucarelli, P. Santolamazza, F. Verrecchia
(ASDC) and L. Salotti (ASI), on behalf of the AGILE Team, report:

"SuperAGILE detected a gamma ray burst on 11 December 2011, at 22:17:33 UT.
The event had a duration of about 15 s in the 20-60 keV energy range,
with a double peak (with internal structure). Assuming a
crab-like energy spectrum, the peak flux on 1-s timescale was 1.50E-06  
erg/cm2/s.
The burst position was reconstructed  as (RA, Dec)
(153.091, 11.182) deg, which is:

RA(J2000)  = 10h 12m 21.84s
Dec(J2000) = 11d 10' 55.52"

with an uncertainty of 3' radius. The given uncertainty accounts
for both the statistical and systematic errors.

An analysis of the AGILE Gamma Ray Imager (GRID) data is in progress."

This message may be cited.


GRB_name: GRB111212A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12667
SUBJECT: GRB 111212A: Swift detection of a burst
DATE:    11/12/12 09:41:19 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Campana (INAF-OAB), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
P. A. Evans (U Leicester), B. Gendre (ASDC), C. Guidorzi (U Ferrara),
O. M. Littlejohns (U Leicester), A. Melandri (INAF-OAB),
P. T. O'Brien (U Leicester), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU),
C. A. Swenson (PSU), E. Troja (NASA/GSFC/ORAU) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:

At 09:23:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111212A (trigger=509543).  Swift could not slew immediately
to the burst due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 310.404, -68.617 which is 
   RA(J2000) = 20h 41m 37s
   Dec(J2000) = -68d 37' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a weak emission
with a duration of at least 20 sec, but a more detailed description 
will require the ground-linked data.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+47.6
minutes. There will be no XRT or UVOT data until this time. 

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: GRB111211A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12668
SUBJECT: GRB 111211A: GROND afterglow candidate
DATE:    11/12/12 09:43:14 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

D.A. Kann (TLS Tautenburg), J. Greiner (MPE Garching), 
T. Kruehler (DARK/NBI) and S. Klose (TLS Tautenburg) 
report on behalf of the GROND team:

We observed the field of the SuperAGILE burst GRB 111211A (Feroci 
et al. 2011, GCN #12666) simultaneously in g'r'i'z'JHK with GROND 
(Greiner et al. 2008, PASP, 120, 405) mounted at the 2.2 m ESO/MPG 
telescope at La Silla Observatory (Chile). Observations
started on December 12, 2011, at 07:50 UT, 8.5 hrs after the GRB. 
They were performed at an average seeing of 1".1 and at an airmass 
of 1.4

Within the 3 arcmin error circle we find one source brighter
than the DSS limit, and not seen on the DSS2-red plate or SDSS-r,
at the following coordinate:

RA (2000.0) = 10:12:21.7
Decl. (2000.0) = 11:12:30

with a conservative error of 0.7 arcsec. This is 1.6 arcmin from the 
center of the SuperAGILE error circle. We propose this source as the 
afterglow of GRB 111211A.

We estimate a rough r-band magnitude (calibrated against the SDSS) of 

r'(AB) = 19.0

No obvious fading is detected, though this is not constraining
given the short GROND coverage and the time after the GRB.
Further observations are encouraged to check for the expected fading.


GRB_name: GRB111212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12669
SUBJECT: GRB 111212A: Swift-XRT observations
DATE:    11/12/12 11:24:01 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.A. Kennea (PSU), G. Tagliaferri (INAF-OAB), S. Campana (INAF-OAB),
P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and D.N. Burrows
(PSU) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 111212A at 10:17:35.0 UT,
3267.9 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 310.43423,
-68.61205 which is equivalent to:
   RA(J2000)  = 20h 41m 44.22s
   Dec(J2000) = -68d 36' 43.4"
with an uncertainty of 3.5 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.07 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2
(+0.94/-0.88) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB111212A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12670
SUBJECT: GRB 111212A: Enhanced Swift-XRT position
DATE:    11/12/12 14:11:53 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 2469 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 111212A, 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 = 310.43132, -68.61251 which is equivalent
to:

RA (J2000): 20h 41m 43.52s
Dec (J2000): -68d 36' 45.0"

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

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

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


GRB_name: GRB111212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12671
SUBJECT: GRB 111212A: Swift-BAT refined analysis
DATE:    11/12/12 14:55:22 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),
S. Campana (INAF-OAB), 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), (i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 111212A (trigger #509543)
(Campana, et al., GCN Circ. 12667).  The BAT ground-calculated position is
RA, Dec = 310.442, -68.585 deg, which is 
   RA(J2000)  =  20h 41m 46.0s 
   Dec(J2000) = -68d 35' 04.5" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
 
The mask-weighted light curve shows a FRED-like pulse starting at ~T-2 sec,
peaking at ~T+6 sec, and returning to background around T+60 sec.  Since
Swift slewed due to an observing constraint, the burst location left
the BAT FoV at ~T+70 sec, so we can not say if there was further actitivty
in the lightcurve.
 
The time-averaged spectrum from T-5.77 to T+62.74 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.67 +- 0.18.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.76 sec in the 15-150 keV band
is 0.8 +- 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/509543/BA/


GRB_name: GRB111212A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12672
SUBJECT: GRB 111212A: Swift/UVOT Upper Limits
DATE:    11/12/12 15:55:48 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 111212A
3272 s after the BAT trigger (Campana et al., GCN Circ. 12667).
No optical afterglow consistent with the XRT position
(Osborne et al., GCN Circ. 12670) 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          3272         3422          147 >20.3
white             3272         5481          541 >21.3
v                 4255         5751          255 >19.2
b                 3637         5276          393 >20.1
u                 3432         5071          393 >20.1
w1                4665         4865          197 >20.1
m2                4460         4660          197 >20.3
w2                4050         5687          393 >21.0

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: GRB111211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12673
SUBJECT: GRB 111211A:  Swift/XRT target of opportunity observation
DATE:    11/12/12 22:16:39 GMT
FROM:    Binbin Zhang at PSU  <buz12@psu.edu>

B.-B. Zhang (PSU) report on behalf of the Swift Team:

Swift began a target of opportunity observation of GRB 111211A on
December 12, 2011 at 15:53 UT, approximately 0.74 days after the burst
was detected by SuperAGILE. Swift data for these observations utilize
Target ID 20192.

We have analysed 2.5 ks of XRT data for the SuperAGILE-detected burst:
GRB 111211A (Lazzarotto et al. et al. GCN Circ. 12666), from 63.5 ks to
66.0 ks after the  SuperAGILE trigger. The data are entirely in Photon
Counting (PC) mode.  An X-ray source is detected within the SuperAGILE
error circle. Using 2512 s of PC mode data and 3 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 = 153.09040,
+11.20789 which is equivalent to:

RA (J2000): 10h 12m 21.70s
Dec(J2000): +11d 12' 28.4"

with an uncertainty of 1.8 arcsec (radius, 90% confidence). This
position is 93 arcsec from the SuperAGILE position and 1.6 arcsec from
the GROND afterglow candidate position (Kann et al. GCN Circ. 12668),
which confirms it is the X-ray afterglow of GRB 111211A. The light
curve is consistent with a constant source of mean count rate 1.3e-01
ct/sec. A power-law fit gives an index of -1.309 (+4.183, -0.020).


A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.02 (+0.18, -0.26). The
best-fitting absorption column is  1.3 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 3.4 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 (4.9 x 10^-11) erg
cm^-2 count^-1. 


A summary of the PC-mode spectrum is thus:

Total column:      1.3 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 3.4 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      2.02 (+0.18, -0.26)


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020192.

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


GRB_name: GRB111212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12674
SUBJECT: GRB 111212A: Swift-XRT refined Analysis
DATE:    11/12/12 22:19:20 GMT
FROM:    Binbin Zhang at PSU  <buz12@psu.edu>

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

We have analysed 6.5 ks of XRT data for GRB 111212A (Campana  et al.
GCN Circ. 12667), from 3.3 ks to 17.3 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 12670).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.39 (+0.11, -0.10).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.05 (+0.13, -0.07). The
best-fitting absorption column is  9.5 (+3.0, -1.6) x 10^20 cm^-2, in
excess of the Galactic value of 3.1 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (4.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.5 (+3.0, -1.6) x 10^20 cm^-2
Galactic foreground: 3.1 x 10^20 cm^-2
Excess significance: 6.6 sigma
Photon index:      2.05 (+0.13, -0.07)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00509543.

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


GRB_name: GRB111211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12675
SUBJECT: GRB 111211A: NOT afterglow confirmation
DATE:    11/12/13 07:40:21 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler and D. Malesani (both DARK/NBI) report on behalf of a larger collaboration:

We observed the field of the AGILE GRB 111211A (Lazzarotto et al., GCN 12666) with the NOT telescope equipped with StanCam. A single R-band image with an integration time of 600 s was obtained on 2011-12-13 at 03:34 UT, which is roughly 29.3 hours after the trigger. 

We clearly detect the optical afterglow candidate (Kann et al., GCN 12668) at

RA = 10:12:21.68
Dec = +11:12:29.3

with an uncertainty of approximately 0.3 arcsec in each coordinate.

Calibrating our R-band image against the r- and i-band magnitudes of the SDSS catalog via the transformation of Lupton et al. (2006), we measure a preliminary magnitude of R = 19.5 +/- 0.1 (Vega system). This implies a significant fading with respect to the earlier measurements of Kann et al. (GCN 12668), and hence confirms this source to be the afterglow of GRB 111211A.

We are grateful to the NOT staff and observer, Ilya Ilyin for obtaining these observations.


GRB_name: GRB111211A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12676
SUBJECT: Konus-Wind observation of GRB 111211A
DATE:    11/12/13 12:48:30 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long GRB 111211A localized by SuperAGILE (Lazzarotto et al., GCN 
12666) was detected by Konus-Wind in the waiting mode.

The burst light curve shows two pulses with a total duration of ~25 s.

As observed by Konus-Wind, the burst had a fluence of (9.2 +/- 
0.8)x10^-6 erg/cm2 (in the 20 - 1200 keV energy range).

Fitting the K-W 3-channel time-integrated spectrum (from T0-18.141 s to 
T0+8.355 s) by a simple power-law model yields a power law index of 
2.77(-0.16, +0.18) (chi2=2.0/1 dof).

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

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB111211A/


GRB_name: GRB111211A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12677
SUBJECT: GRB 111211A: VLT/X-shooter redshift
DATE:    11/12/13 14:22:36 GMT
FROM:    Silvia Piranomonte at OAR  <piranomonte@mporzio.astro.it>

S.D. Vergani (OAB/INAF), S. Piranomonte (OAR/INAF), O.E.Hartoog (UvA,  
Netherland), V. D'Elia (ASDC/INAF), G. Cupani (OAT/INAF), A. de Ugarte  
Postigo (IAA-CSIC, DARK/NBI), T. Kruehler, J.P.U. Fynbo, Bo  
Milvang-Jensen, D. Malesani (DARK/NBI), P. Vreeswijk (U. Iceland), N.  
R. Tanvir (U. Leicester) and L. Kaper (UvA, Netherland) report on  
behalf of the X-shooter GTO GRB afterglow collaboration:


The afterglow of the AGILE GRB 111211A (Lazzarotto et al., GCN 12666,
Kann et al. 12668 and Kruehler et al. GCN 12675) was
observed with the X-shooter spectrograph mounted on the ESO-VLT.
Observations started around 7 UT on 13 December
2011 (1.3 days after the GRB). A series of four spectra of 600 s each
were secured, covering the approximate wavelength range 3000-25000 AA.

Preliminary reduction of the ultraviolet, visual and near-infrared
parts of the spectra show a smooth continuum with some weak
absorption features that we can identify with resonance absorption  
lines of FeII, MgII and CaII at a redshift of z=0.478, which very  
likely correspond to the redshift of GRB 111211A.
Weak emission lines ([O III] doublet and Halpha)  are also observed at  
the same redshift.
We thank D.A. Kann for providing us the GROND finding chart and we
are grateful for the excellent support from the Paranal Observatory
staff, in particular Willem-Jan de Wit (Shift coordinator), Dimitri
Gadotti (Night Astronomer), Marcelo Lopez (Telescope and
Instrument Operator) and Gabriel Brammer (Day Astronomer).

----------------------------------------------------------------
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GRB_name: GRB111211A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12678
SUBJECT: GRB 111211A: Swift/UVOT Detection
DATE:    11/12/13 17:06:55 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

We have analyzed 4.5 ks of UVOT data for the SuperAGILE-detected burst GRB
111211A (Lazzarotto et al., GCN Circ 12666), taken 63.5 to 76.6 ks after the
trigger.  Data were taken entirely in the white filter.  We confirm the
uncatalogued source reported by Kann et al. (GCN Circ. 12668), Zhang (GCN
Circ. 12673) and Kruehler et al. (GCN Circ. 12675).  However, we can not
confirm any statistically significant fading at this time.  The UVOT position is
RA, Dec = 153.09037, +11.20801 which is equivalent to:

RA (J2000): 10h 12m 21.69s
Dec(J2000): +11d 12' 28.9"

with an uncertainty of 0.5 arcsec (radius, 90% confidence). Preliminary
photometry using the UVOT photometric system (Breeveld et al. 2011, AIP
Conf. Proc. 1358, 373) shows:

Filter         T_start(ks)   T_stop(ks)      Exp(s)         Mag
white             63.5         76.6          4550          19.51+-0.03

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: GRB111212A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12679
SUBJECT: GRB 111212A: GROND observations
DATE:    11/12/14 09:11:29 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, A. Rossi (TLS Tautenburg), V. Sudilovsky, P. Schady and J.
Greiner, (MPE Garching) report on behalf of the GROND team:

We observed the field of the Swift GRB 111212A (Swift trigger 509543;
Campana et al., GCN #12667) simultaneously in g'r'i'z'JHK with GROND
(Greiner et al. 2008, PASP, 120, 405) mounted at the 2.2 m ESO/MPG
telescope at La Silla Observatory (Chile). Observations started on
December 13, 2011, at 00:35 UT, in twilight, and are centered 0.658 days
after the GRB trigger. They were taken at an average seeing of 1".2 and at
an airmass of 2. Integration times were 1734 sec in the optical and 2640
sec in the NIR. These observations were obtained under challenging
conditions, with thick cirrus preventing guiding.

A second epoch was obtained on December 14, 2011, starting at 00:57 UT and
centered at 1.667 days after the GRB. It was taken at an average seeing of
1".2 and at an airmass of 2. Integration times were 2420 sec in the
optical and 2160 sec in the NIR. Conditions were much better, with clear,
moonless skies.

At the position of the X-ray afterglow (Osborne et al., GCN #12670), we do
not detect any significant sources in any bands. We derive the following
limits (3 sigma, AB magnitude system):

0.658 days after the trigger:

g' > 24.1
r' > 24.2
i' > 23.4
z' > 22.8
J > 20.5
H > 20.0
K > 18.1

1.667 days after the trigger:

g' > 24.8
r' > 24.8
i' > 23.8
z' > 23.4
J > 21.6
H > 21.0
K > 19.3

Magnitudes were calibrated against GROND zero points in g'r'i'z' and 2MASS
field stars in JHK.


GRB_name: GRB111201A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12680
SUBJECT: GRB 111201A, the review of the sky area in plate archive
DATE:    11/12/14 12:28:00 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 111201A (J.A.Kennea (PSU) and T.Sakamoto, GCN Circ.12609) 
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 
19870527/224011 GUA040C000022B 18.2 15.85 1200-06937537
19890205/015711 GUA040C001420 18.0 15.85 1200-06937537
19890504/200715 GUA040C001461A 16.0 15.85 1200-06937537
19900223/003254 GUA040C001582 16.0 16.55 1200-06937256
19930425/205928 GUA040C002202 22.5 15.35 1200-06936881
19930430/205716 GUA040C002205A 18.8 15.85 1200-06937537
Plates-the plate's identifier in GUA040C archive
        of DWA (D/F=400/2000, M=103"/mm) of the Ukrainian NAS 
        Main Astro obs in Kyiv (Marsden's number - 83)[1].
Exp.   - Duration of the maximum exposure (minutes). 
LimMag - Limited V mag, derived in the 18 minutes area around 
       the location given in GCN Circ.12609: 
       RA(J2000): 12h 41m 54.48s, Dec(J2000): +32d 59' 16.5"
Star USNOA2 - Comparison star.
  The preview images of 6 areas together with  
the 17x19 min.of arc area from SkyMap can be found in  
http://gua.db.ukr-vo.org/img/grb/111201A/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: GRB111215A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12681
SUBJECT: GRB 111215A: Swift detection of a burst
DATE:    11/12/15 14:18:28 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA), 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 14:04:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111215A (trigger=509717).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 349.548, +32.475 which is 
   RA(J2000) = 23h 18m 12s
   Dec(J2000) = +32d 28' 32"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for an image trigger, the BAT light 
curve shows nothing of note. 

The XRT began observing the field at 14:11:06.0 UT, 417.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 349.5578, 32.4938 which is equivalent to:
   RA(J2000)  = +23h 18m 13.87s
   Dec(J2000) = +32d 29' 37.7"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 73 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 1.51e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 426 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.06. 

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


GRB_name: GRB111215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12682
SUBJECT: GRB 111215A : Xinglong TNT upper limit  
DATE:    11/12/15 15:38:37 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 111215A ( Oates  et al., GCN 12681)
with Xinglong TNT telescope at 14:20:23  (UT), about 16.25 min  after 
the burst.  30 R-band images  were obtained. The exposure time is 60 sec 
for each frame.

No new source was detected in the combined R band image within 
the errorbox of XRT position. The upper limit was estimated 
to be about 18.0  mag derived from USNO B1.0 R2 mag,
at the mean time of 32.75 min after the burst. 

This message may be cited.

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


GRB_name: GRB111215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12683
SUBJECT: GRB 111215A: GMG optical upper limit
DATE:    11/12/15 17:07:53 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

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

We observed the field of GRB 111215A (Oates et al., GCN 12681) at the
2.4m Gao-Mei-Gu (GMG) telescope equipped with YFOSC. Observations
started at 14:26:44 UT (i.e., 22.6 mins after the burst) and a series
of R-band images (totally 1700s exposure) were obtained in a seeing of
~2.8".

No optical source was detected within the XRT error circle (ref., GCN
12681) to a 3sigma limit of R~22.8 mag, calibrated with nearby USNO B1
stars.

The image trigger mode of this burst and the above R-band upper limit
might indicate high-redshift. NIR follow-ups are encouraged.

We thank the GMG staff, especially Y.-X. Xin, D.-Q. Wang, and Y.-D.  
Lang for performing the observations.

[GCN OPS NOTE(15dec11): Par author's request, the last sentence was added.]


GRB_name: GRB111209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12684
SUBJECT: GRB 111209A: RAPTOR Limits Before and During the Gamma-ray Emitting Interval
DATE:    11/12/15 17:32:20 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 wide-field optical monitors were observing the location of
GRB 111209A (Hoversten et al., GCN 12632) during the gamma-ray emitting
interval as seen by the Swift BAT (Palmer et al., GCN 12640).  Our
system acquired 10 s exposures at 20 s intervals during the entire
emission period.  We have analyzed the the 77 images taken between
T-150 and T+1400 and we do not detect the counterpart to a typical
3-sigma limiting magnitude of 10.3.  Our unfiltered images were
calibrated to the Tycho-2 V-band.


GRB_name: GRB111215A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12685
SUBJECT: GRB 111215A: MITSuME Akeno Optical upper limits
DATE:    11/12/15 17:39:51 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 GRB 111215A (S. R. Oates et al, GCN12681) 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 387 sec after the BAT trigger
from 2011-12-15 14:10:35 UT.  And we did not find any new point source
within the XRT error circle (S. R. Oates et al, GCN12681) 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
----------------------------------------------------------------------------------------
    387         14:33:55        2700          > 19.3      > 19.4      > 19.0
----------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB111215A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12686
SUBJECT: GRB 111215A, Optical Observations
DATE:    11/12/15 17:48:48 GMT
FROM:    Rupak Roy at ARIES  <rupakroy1980@gmail.com>

 S. B. Pandey, Rupak Roy, Brajesh Kumar and R. K. S. Yadav (ARIES,
NainiTal, India, on behalf of larger Indian GRB collaboration).

GRB 111215A field, localized by Swift (Oates et al., GCN 12681), was
observed with 1.04m telescope at ARIES NainiTal starting 14:22:30 UT (~18
minutes after the burst) in R_c pass-band with an exposure time of 300 sec
each.

Photometry of the co-added R_c frame (300 sec x 6) in comparison to nearby
USNO stars did not detect any new source within the XRT error-box down to a
limiting magnitude of ~ 21.5 mag.

This message may be cited.


GRB_name: GRB111215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12687
SUBJECT: GRB 111215A: MASTER-Net optical prompt and follow up observations
DATE:    11/12/15 17:53:12 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
  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

  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

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

3 Robotic telescopes MASTER II was pointing to the GRB111215A (Oates et
al., GCN CIRCULAR NUMBER:  12681). Two very wide field cameras
was observed Swift error box before, during and after GRB trigger time.

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka(Siberia) was pointed to the  GRB111215A 26 sec s after
notice time and 381 sec after GRB time at 2011-12-15 14:10:29.44 UT in two  
polarizarions.  On our first (80s exposure) set we haven't found optical
transient  within SWIFT error-box (ra=23 18 12 dec=+32 28 47 r=0.050000).
  The 5-sigma upper limit has been about 18.8 mag

  MASTER II  robotic telescope
located in MASTER-Amur was pointed to the  GRB111215A 214 sec s after
notice time and 567 sec after GRB time at 2011-12-15 14:13:35.289 UT in
two diagonal  polarizarions. On our first (110s exposure) set we haven't
found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 17.5 mag

MASTER II  robotic telescope
located near Kislovodsk was pointed to the  GRB111215A 7655 sec s after
notice time and 8007 sec after GRB time at 2011-12-15 16:17:35.91 UT
(time delay is so long  due to weather conditions). On
our first (180s exposure) set we haven't found optical transient  within
SWIFT error-box.
The 5-sigma upper limit has been about 18.1 mag

Two   MASTER Very Wide Field Cameras 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  12.0 m at the edge of FOW.

We do not detect OT.
The video from MASTER VWF cameras is available at
http://master.sai.msu.ru/static/GRB111215/grb111215.html

The reduction is continuated.

  The message may be cited.


GRB_name: GRB111215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12688
SUBJECT: GRB 111215A: OSN I-band observations
DATE:    11/12/15 21:05:16 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

F. Aceituno (OSN,IAA-CSIC), A.J. Castro-Tirado, A. de Ugarte Postigo, J.C. Tello, J. Gorosabel (IAA-CSIC), report on behalf of a larger collaboration:

"We have observed the field of GRB 111215A (Oates et al., GCN 12681) with the 1.5m telescope at Observatorio de Sierra Nevada (OSN), Granada, Spain. The data were acquired in the I-band on Dec 15.7537 -- Dec. 15.8168 UT (starting ~4 hour post burst), with a total exposure time of 18x300s. A preliminary analysis reveals no object brighter than I=21.7 in the XRT error circle. The calibration was carried out using the USNO B1.0 catalogue."


GRB_name: GRB111215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12689
SUBJECT: GRB 111215A: Swift-BAT refined analysis
DATE:    11/12/15 23:04:57 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), S. R. Oates (UCL-MSSL), 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 111215A (trigger #509717)   
(Oates, et al., GCN Circ. 12681).  The BAT ground-calculated position is
RA, Dec = 349.582, 32.440 deg, which is
   RA(J2000)  =  23h 18m 19.6s
   Dec(J2000) = +32d 26' 24.2"
with an uncertainty of 4.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.
   
The mask-weighted light curve shows the emission starting at ~T-110 sec,
although we note that the burst location came into the BAT FoV around
T-200 sec, so we can not make any statement about possible earlier emission.
There are a few overlapping peaks at ~T+20 sec, ~T+170 sec, and T+300 sec,
the the lightcurve slowly decreases back to baseline around T+1500 sec.
T90 (15-350 keV) is 796 +- 250 sec (estimated error including systematics).
   
The time-averaged spectrum from T-116.4 to T+960.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.70 +- 0.18.  The fluence in the 15-150 keV band is 4.5 +- 0.5 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+216.35 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 duration of this burst is very long, and we note that this location is
well off the Galactic Plane (lon=101,lat=-26).  We can not rule out
a non-GRB source for this event.
   
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/509717/BA/


GRB_name: GRB111215A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12690
SUBJECT: GRB 111215A: Enhanced Swift-XRT position
DATE:    11/12/16 00:26:54 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 2785 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 111215A, 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 = 349.55538, +32.49401 which is equivalent
to:

RA (J2000): 23h 18m 13.29s
Dec (J2000): +32d 29' 38.4"

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: GRB111215A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12691
SUBJECT: Possible detection of pre-trigger X-ray emission from GRB 111215A by MAXI/GSC
DATE:    11/12/16 09:38:44 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

N. Kawai, M. Morii (Tokyo Tech), H. Negoro (Nihon U.),  M. Serino (RIKEN),
K. Sugimori, R. Usui, T. Toizumi, Y. Aoki, S. Song (Tokyo Tech),
S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, S. Nakahira, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN), 
A. Yoshida, K. Yamaoka (AGU),
H. Tsunemi, M. Kimura, H. Kitayama (Osaka U.), 
M. Nakajima, F. Suwa, 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 observed the position of GRB 111215A
(swift trigger=509717, Oates et al. GCN #12681)
at 13:12 and 14:44 on December 5, 2011 (UT), 
52 min before and 40 min after the trigger time.

The source was marginally detected as follows: 

Time    2-4 keV          4-10 keV
13:12   4 +-  7 mCrab  52 +- 19 mCrab
14:44  16 +- 10 mCrab  41 +- 19 mCrab

(uncertainties are 1-sigma statistical errors) 

If this detections are true it implies that the emission of GRB 111215A lasted
for more than 1.5 hours. Together with the long trigger timescale (320 s)
by Swift BAT, unusual for a GRB, we suggest that it may be a
non-GRB X-ray transient, such as an X-ray binary, AGN, or extragalactic TDE.

Multiwavelength follow-up observations are strongly encouraged.


GRB_name: GRB111215A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12692
SUBJECT: GRB 111215A: Swift-XRT refined Analysis
DATE:    11/12/16 11:18:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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), J.A. Kennea (PSU), M.C. Stroh (PSU),
D.N. Burrows (PSU) and S.R. Oates report on behalf of the Swift-XRT
team:

We have analysed 7.1 ks of XRT data for GRB 111215A (Oates  et al. GCN
Circ. 12681), from 407 s to 59.3 ks after the  BAT trigger. The data
comprise 2.2 ks in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 12690).

The late-time light curve (from T0+5.9 ks) can be modelled with an
initial power-law decay with an index of alpha=2.13 (+0.13, -0.12),
followed by a break at T+14.6 ks to an alpha of 1.21 (+0.15, -0.16).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.847 (+/-0.027). The
best-fitting absorption column is  4.10 (+/-0.12) x 10^21 cm^-2, in
excess of the Galactic value of 5.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.14 (+/-0.12) and a
best-fitting absorption column of 3.2 (+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 3.9 x 10^-11 (6.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 5.6 x 10^20 cm^-2
Excess significance: 10.2 sigma
Photon index:      2.14 (+/-0.12)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00509717.

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


GRB_name: GRB111215A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  12693
SUBJECT: GRB 111215A: Swift/UVOT Upper Limits
DATE:    11/12/16 11:29:50 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 111215A
426 s after the BAT trigger (Oates et al., GCN Circ. 12681).
No optical afterglow consistent with the XRT position
(Beardmore et al., GCN Circ. 12690) 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           426          576          147         >21.7
white              426        19036          645         >22.0
v                  732        13257          608         >20.1
b                  657        18972         1198         >21.6
u                  632         6983          313         >20.7
w1                 608        22616          593         >20.6
m2                 583         6572          313         >20.7
w2                 708        12928         1260         >21.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.06 in the direction of the burst
(Schlegel et al. 1998).


