# GCN_circulars

GRB_name: GRB121011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13849
SUBJECT: Planned XMM-Newton and IRAM observation of GRB 121011A
DATE:    12/10/11 13:35:40 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@asdc.asi.it>

B. Gendre (ASDC/OaR/INAF), C. Feruglio (IRAM), G. Stratta (OaR) report 
on behalf of a larger collaboration:

The GRB 121011A will be observed by XMM-Newton from 2012 Oct. 11 18:33 
UT, until Oct 12 at 11:30 UT. This observation is coordinated with an 
IRAM observation at the Interferometer of the Plateau de Bure.

We encourage any follow-up at all wavelengths, and specially 
spectroscopic observations to derive a redshift for this event.

This message can be cited.


GRB_name: GRB121011A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13850
SUBJECT: GRB 121011A: Enhanced Swift-XRT position
DATE:    12/10/11 18:35:03 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 127 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 121011A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 260.21466, +41.11031 which is equivalent
to:

RA (J2000): 17h 20m 51.52s
Dec (J2000): +41d 06' 37.1"

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: GRB121011A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13852
SUBJECT: GRB 121011A, Swift-BAT refined analysis
DATE:    12/10/11 21:14:11 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC), T. Sakamoto (AGU), G. Sato (ISAS),
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 121011A (trigger #535764)
(Racusin, et al., GCN Circ. 13845).  The BAT ground-calculated position is
RA, Dec = 260.204, 41.123 deg, which is 
   RA(J2000)  =  17h 20m 49.0s 
   Dec(J2000) = +41d 07' 22.4" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 32%.
 
The mask-weighted light curve shows a single pulse starting at ~T-9 sec,
peaking at ~T+1 sec, and ending at ~T+110 or ~T+150 sec.
T90 (15-350 keV) is 75.6 +- 12.7 sec (estimated error including systematics).
 
The time-averaged spectrum from T-7.45 to T+80.10 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.10 +- 0.73, 
and Epeak of 101.5 +- 42.2 keV (chi squared 40.6 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.7 +- 0.7 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T-0.69 sec in the 15-150 keV band is
1.2 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.20 +- 0.14 (chi squared 49.2 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/535764/BA/


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13853
SUBJECT: GRB 121011A: TNG optical observations
DATE:    12/10/11 21:24:30 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK), P. D'Avanzo (INAF/OABr), A. Melandri (INAF/OABr), V. 
Nascimbeni (Univ. Padova), C. Padilla (INAF/TNG), report on behalf of 
the CIBO collaboration:

We observed the optical afterglow of GRB 121011A (Racusin et al., GCN 
13845) with the TNG equipped with DOLoRes.

The afterglow is well detected in a single 5-min exposure, with a mean 
time Oct 11.829 UT (8.63 hr after the GRB). Its magnitude is R = 21.74 
+- 0.06, assuming R = 17.84 for the USNO star at RA = 17:20:44.70, Dec = 
+41:04:52.7.

The afterglow has the following coordinates (calibrated against USNO-B1 
stars):

RA = 17:20:51.22
Dec = +41:06:37.4

with an estimated uncertainty of 0.4".


GRB_name: GRB121011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13854
SUBJECT: GRB 121011A: MASTER-Net bell light curve
DATE:    12/10/11 21:27:48 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, D.Denisenko, V.Krushinski (Ural), V. Lipunov, V.Kornilov, 
D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov,
A.Kuznetsov,  V.V.Chazov, A.Sankovich
Moscow Lomonosov State University, Sternberg Astronomical Institute,

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

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

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

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

I.Zalozhnich,  A. Popov, A. Bourdanov
Ural Federal University

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

Two MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Blagoveschensk and Tunka (Baykal lake) was pointed to the GRB 
121011A (Racusin et al., GCNC 13848) 51 sec after Trigger time at
2012-10-11 11:16:21.301 UT and 106 sec after Trigger time at
2012-10-11 11:17:14 UT in four polarizations (Yurkov et al., GCNC 13845).

Unfortunately the weather conditions were not very good at Tunka site.

We detected OT (Racusin et al., GCNC 13848; Kuroda et al. GCNC 13845;
Xin et al., GCNC 13847).

The preliminary results of the photometry calibrated to 0.8*R+0.2*B from 
USNO-B1.0:

     UTC    Tmean-Tgrb Exp,s.    mag s/n   magerr  filter  Site  Coadd

  11:16:21.0 56 10 >16.9 N/A N/A P/ Amur No
  11:16:21.0 56 10 >16.9 N/A N/A P\ Amur No
  11:16:21.0 96 80 >18.2 N/A N/A P/ Amur   Yes
  11:16:21.0 96 80 >18.2 N/A N/A P\ Amur   Yes
  11;18;29.0 200 40 >18.2 N/A N/A P/ Amur No
  11;18;29.0 200 40 >18.2 N/A N/A P\ Amur No
  11:19:20.429 255 50 17,38 5.9 0.18 P/ Amur No
  11:19:20.461 255 50 17,17 5.8 0.19 P\ Amur No
  11:20:21.37 321 60 16,89 8.9 0.12 P/ Amur No
  11:20:21.396 321 60 16,9 8.1 0.13 P\ Amur No
  11:21:32.001 397 70 16,77 11.1 0.10 P/ Amur No
  11:21:32.02 397 70 16,81 11.5 0.09 P\ Amur No
  11:22:52.945 487 90 16,59 14.7 0.07 P/ Amur No
  11:22:52.998 487 90 16,49 15.8 0.07 P\ Amur No
  11:24:33.654 599 110 16,42 18.7 0.06 P/ Amur No
  11:24:33.678 599 110 16,57 16.6 0.07 P\ Amur No
  11:26:34.121 729 130 16,55 17.6 0.06 P/ Amur No
  11:26:34.144 729 130 16,5 18.4 0.06 P\ Amur No
  11:28:54.944 885 160 16,69 18.1 0.06 P/ Amur No
  11:28:54.947 885 160 16,7 15.5 0.07 P\ Amur No
  11:31:45.672 1065 180 16,73 15.3 0.07 P/ Amur No
  11:31:45.706 1065 180 16,72 14.2 0.08 P\ Amur No
  11:35:11.589 1271 180 17,05 13.5 0.08 P/ Amur No
  11:35:11.606 1271 180 17,03 11.1 0.10 P\ Amur No
  11:38:37.563 1477 180 17,23 10.4 0.10 P/ Amur No
  11:38:37.586 1477 180 17,25 10.3 0.11 P\ Amur No
  11:42:12.62 1693 180 17,36 9.2 0.12 P/ Amur No
  11:42:12.636 1693 180 17,48 7.7 0.14 P\ Amur No
  11:45:38.297 1898 180 17,44 8.2 0.13 P/ Amur No
  11:45:38.319 1898 180 17,44 7.2 0.15 P\ Amur No
  11:49:03.877 2104 180 17,67 5.7 0.19 P/ Amur No
  11:49:03.906 2104 180 17,73 5.0 0.22 P\ Amur No
  11:52:29.982 2309 180 17,91 4.7 0.23 P/ Amur No
  11:52:30.004 2309 180 17,82 5.4 0.20 P\ Amur No
  11:55:55.714 2515 180 18,08 4.7 0.23 P/ Amur No
  11:55:55.710 2515 180 18,04 3.4 0.32 P\ Amur No



The mean (F/ - F\)/(F/ + F\) 100 < 2% during detection time.


The light curve between 200 sec and 6600 sec is very simmetrical in
log(F) - log (t) coordinates (like to bell) with parabolic low :

    m - m_max  = - A (log t/t_max)^2     (1)


A = 4.2 +/- 0.1



where t is time from GRB trigger in sec, t_max = 633+-11s, m_max = 
16.60+/-0.02 . We 
stress that this formulae does not depend on redshift.

The phenomenological formula discribed by Kocevski, D., Ryde, F., & Liang, E. 
(2003, ApJ, 596, 389) may be discussed in this situation but after z 
determination.

The preliminary light curve is available here:
http://master.sai.msu.ru/static/GRB/GRB121011_lc.gif

The preliminary approximation (formula(1)) is available here:
http://master.sai.msu.ru/static/GRB/GRB121011_lc_aproximation.png
This message can be cited.


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13855
SUBJECT: GRB 121011A: optical observations
DATE:    12/10/11 22:32:41 GMT
FROM:    Alexei Pozanenko at IKI  <alex@grb.rssi.ru>

A. Volnova (SAO MSI, IKI), A. Matkin (UAFO, ISON), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 121011A (Racusin et al., GCN 13845) with VT-50 (0.5-m) telescope of UAFO/ISON-Ussuriysk observatory starting on Oct. 11 (UT) 11:21:29, i.e. 6 minutes after burst trigger. We took several unfiltered images of 30 s exposures ending observations on (UT) 12:17:00. In initial frames we clearly detect afterglow (Racusin et al., GCN 13845). Preliminary photometry of some early images is based on USNO-B1.0 stars (R2):

T_start T0+, Filter, exposure, OT 
(UT) mid (d) (s) 

11:21:29 0.00433 none 30 16.70 +/- 0.08
11:27:04 0.00821 none 30 16.64 +/- 0.07
11:33:14 0.01249 none 30 16.80 +/- 0.10
11:38:12 0.01594 none 30 17.30 +/- 0.10


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13856
SUBJECT: GRB 121011A: NOT optical observations
DATE:    12/10/11 22:54:21 GMT
FROM:    Dong Xu at Weizmann Inst  <dong.dark@gmail.com>

J. P. U. Fynbo (DARK), D. Xu (WIS), D. Malesani (DARK), A.
Sodor(Konkoly Observatory of Hungary, Royal Observatory of Belgium) ,
P. Jakobsson (U. Iceland) report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 121011A (Racusin et al.,
GCN13845) using the 2.5m Nordic Optical Telescope (NOT) equipped with
ALFOSC.

The afterglow is clearly detected in each of the two 300s exposures,
with a mean time Oct. 11.830 UT (i.e., 8.666 hr after the BAT
trigger). We found its magnitude R=21.76+/-0.10, calibrated with the
USNO B1 star # 1310-0279773 (R1 = 17.84; same as calibration in
Malesani et al., GCN #13853).

We also carried out 2x20 min spectroscopic observations after the
above photometry. There is a faint trace in the 2D spectrum but the
S/N in the 1D spectrum is low. Preliminary analysis of the 1D spectrum
shows very weak sign of z~0.58.


GRB_name: GRB121011A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13857
SUBJECT: GRB 121011A: Swift-XRT refined Analysis
DATE:    12/10/11 23:36:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (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), A. Maselli  (INAF-IASFPA), J.A. Kennea (PSU), M.C. Stroh (PSU)
and J.L. Racusin report on behalf of the Swift-XRT team:

We have analysed 7.1 ks of XRT data for GRB 121011A (Racusin  et al.
GCN Circ. 13845), from 103 s to 16.8 ks after the  BAT trigger. The
data comprise 28 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 13850).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.50 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.71 (+0.35, -0.10). The
best-fitting absorption column is  consistent with the Galactic value
of 2.3 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.0 x 10^-11 (4.2 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+4.9, -0) x 10^20 cm^-2
Galactic foreground: 2.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.71 (+0.35, -0.10)

If the light curve continues to decay with a power-law decay index of
1.50, the count rate at T+24 hours will be 5.9 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.3 x
10^-14 (2.5 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00535764.

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


GRB_name: GRB121011A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13859
SUBJECT: GRB 121011A: Fermi-LAT detection of a burst
DATE:    12/10/12 02:13:58 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

M. Ohno (Hiroshima U.), G. Vianello (Stanford), J. L. Racusin (NASA/GSFC) and E. Sonbas (Adiyaman Univ.), report on behalf of the Fermi-LAT team:

The Fermi Large Area Telescope (LAT) detected emission from GRB 121011A, also detected by Swift (Racusin et al. GCN 13845) and GBM (trigger 371646928/121011469) at approximately 11:15:25 UT on October 11, 2012.

The burst location was inside the LAT field of view at an angle of ~56 degrees to the LAT boresight, and had a zenith angle of 86 degrees. No significant excess is seen using standard analysis procedures.

Using the non-standard LAT Low Energy (LLE) data selection, over 100 counts above background were detected within a 20 s interval coinciding with the time of the GBM emission, with a significance of 4 sigma. This data selection has insufficient spatial resolution to provide a reliable LAT localization. This detection is due to low energy gamma-rays (below 100 MeV). Indeed, no events were observed above 100 MeV using the standard analysis classes.

A GBM circular on GRB 121011A is forthcoming.

The Fermi LAT point of contact for this burst is Eda Sonbas (edasonbas AT gmail.com).

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


GRB_name: GRB121011A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13860
SUBJECT: GRB 121011A: Fermi GBM observation
DATE:    12/10/12 03:04:27 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH), David Byrne (UCD) and Charles Meegan (USRA)
report on behalf of the Fermi GBM Team:

"At 11:15:25.70 UT on 11 October 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121011A (trigger 371646928 / 121011469),
which was also detected by the Swift/BAT (Racusin et al. 2012, GCN 13845)
and Fermi/LAT (M. Ohno et al. 2012, GCN 13859).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is ~56 degrees.
This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve shows a single peak with long tail
with a duration (T90) of about 66 s (10-1000 keV).
The time-averaged spectrum from T0+0.0 s to T0+67.6 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.09 +/- 0.07 and
the cutoff energy, parameterized as Epeak, is 1160 +/- 410 keV.

The event fluence (10-1000 keV) in this time interval is
(1.00 +/- 0.05)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7.23 s in the 10-1000 keV band is 2.2 +/- 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: GRB121011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13861
SUBJECT: GRB 121011A: misprint  in GCNC 13854
DATE:    12/10/12 05:26:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V. Lipunov
Moscow Lomonosov State University, Sternberg Astronomical Institute,


The correct   formula (1) (Yurkov et al.,GCNC 13854) is:

"The light curve between 200 sec and 6600 sec is very simmetrical in
log(F) - log (t) coordinates (like to bell) with parabolic low :

    m - m_max  = A (log t/t_max)^2     (1)


A = 4.2 +/- 0.1

where t is time from GRB trigger in sec, t_max = 633+-11s, m_max =
16.60+/-0.02 . We
stress that this formulae does not depend on redshift."

This message can be cited.


GRB_name: GRB121011A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13862
SUBJECT: GRB 121011A: NOT redshift retraction
DATE:    12/10/12 09:20:33 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

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

We performed a careful analysis of the spectrum secured at the NOT 
(Fynbo et al., GCN 13856) of the afterglow of GRB 121011A (Racusin et 
al., GCN 13845). We confirm that a faint continuum is visible in our 
data, but we cannot detect any clear feature with confidence. The 
redshift z = 0.58 suggested in GCN 13856 is therefore not correct.

A sharp break is detected at the blue end of our spectrum around 4100 
AA, but its interpretation is not straightforward. If due to Ly alpha at 
z = 2.3, than we would expect surviving flux blueward of the break. If 
due to the Lyman limit at z = 3.4, than we would expect to see the Lyman 
forest redward of the break, which we do not. We thus believe this break 
to be an artifact of the data, but encourage other observers to attempt 
spectroscopy with large area telescopes, also given the detection of the 
GRB by Fermi/LAT (Ohno et al., GCN 13859).


GRB_name: GRB121011B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13863
SUBJECT: IPN Triangulation of short hard GRB 121011B
DATE:    12/10/12 15:14:53 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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 on behalf of the IPN,

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

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on
behalf of the AGILE MCAL team, report:

The short GRB 121011B has been observed so far by Konus-Wind,
INTEGRAL(SPI-ACS), Suzaku(WAM) and AGILE (MCAL) at about 81143 s UT
(22:32:23).

We have triangulated the burst to a preliminary, 3 sigma error box whose
coordinates are:
    ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
     182.809 (12h 11m 14s) +44.113 (+44d 06' 47")
    Corners:
     179.176 (11h 56m 42s) +41.963 (+41d 57' 48")
     178.172 (11h 52m 41s) +41.937 (+41d 56' 14")
     187.165 (12h 28m 40s) +46.167 (+46d 10' 01")
     188.461 (12h 33m 51s) +46.130 (+46d 07' 48")
    ---------------------------------------------
The error box area is 3.43 sq. deg, and its maximum
dimension is 8.49 deg (the minimum one is 0.75 deg).

This box can be improved.

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


GRB_name: GRB121011A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13864
SUBJECT: GRB 121011A: Swift/UVOT Detection
DATE:    12/10/12 19:58:04 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) 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 121011A 109 s after
the BAT trigger (Racusin et al., GCN Circ. 13845).  A source consistent with the
XRT position (Evans et al. GCN Circ. 13850) is detected in the initial UVOT
exposures.

The preliminary UVOT position is:
    RA  (J2000) =  17:20:51.23 = 260.21346 (deg.)
    Dec (J2000) = +41:06:37.1  = +41.11030 (deg.)
with an estimated uncertainty of 0.52 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              109          258          147         18.96 +/- 0.06
v                 4093         5729          393         19.81 +/- 0.21
b                 3476         3676          197         19.51 +/- 0.18
u                 4708         4908          197         19.67 +/- 0.18
w1                4503        15916         1183        >20.9
m2                4298         5933          393        >22.6
w2                3888         5524          393        >21.0

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


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13865
SUBJECT: GRB 121011A: optical observations
DATE:    12/10/13 04:55:08 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Vijay Kumar Bhatt, Archana Soam and S.B. Pandey (ARIES,
Nainital, India, on behalf of larger Indian GRB collaboration).


Follow-up observations of GRB 121011A (Racusin et al., GCN13845) were done
using 1.04m telescope at Nainital in good sky conditions starting at
13:17:03 (UT) on 11-10-2012. Several frames in B, V, R_c and I_c pass-bands
were obtained with exposure time of 300 sec each.

The optical afterglow candidate (Racusin et al., GCNC 13845) is clearly
detected in our frames. The preliminary photometry for the first R_c and
I_c frames were 19.59 +- 0.02 mag and 19.14 +- 0.05 mag respectively,
calibrated against nearby USNO stars. Further observations are continued.

This massage may be cited.


GRB_name: GRB121014A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13867
SUBJECT: GRB 121014A: Swift detection of a burst
DATE:    12/10/14 20:19:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Y. Lien (NASA/GSFC/ORAU), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and E. Sonbas (NASA/GSFC/Adiyaman Univ.)
report on behalf of the Swift Team:

At 20:11:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121014A (trigger=535960).  Swift did not slew because 
of sun constraint.  The BAT on-board calculated location is 
RA, Dec 166.631, -29.109, which is 
   RA(J2000)  =  11h 06m 31s
   Dec(J2000) = -29d 06' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows an initial 1-2 sec spike
at T0, and then smaller and longer peaks at ~T+20 sec and ~T+50 sec. 
structure with a duration of about 60 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 05:22 UT on 2012 October 30. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13868
SUBJECT: GRB 121011A: WSRT radio observation
DATE:    12/10/14 20:51:12 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

A.J. van der Horst (University of Amsterdam) reports on behalf
of a large collaboration:

"We observed the position of the GRB 121011A afterglow at 4.9 GHz
with the Westerbork Synthesis Radio Telescope at October 14 10.01
to 18.14 UT, i.e. 2.95 - 3.29 days after the burst (GCN 13845).
We do not detect a radio source at the position of the optical
counterpart (GCN 13853). The three-sigma rms noise in the map around
that position is 75 microJy per beam. The formal flux measurement for
a point source at the position of the optical counterpart is 44 +/- 25 
microJy.

We would like to thank the WSRT staff for scheduling and obtaining these
observations."


GRB_name: GRB121014A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13869
SUBJECT: GRB 121014A: Swift-BAT refined analysis
DATE:    12/10/15 10:52:56 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),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+222 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 121014A (trigger #535960)
(Lien, et al., GCN Circ. 13867).  The BAT ground-calculated position is
RA, Dec = 166.645, -29.105 deg, which is 
   RA(J2000)  =  11h 06m 34.7s 
   Dec(J2000) = -29d 06' 18.3" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 72%.
 
The mask-weighted light curve shows 3 main peaks starting at ~T-0.2 sec,
peaking at ~T+0.4, ~T+19, & ~T+50 sec, resp., and ending at ~T+90 sec.
T90 (15-350 keV) is 80.0 +- 22.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-12.21 to T+67.79 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.91 +- 0.17.  The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+59.29 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/535960/BA/


GRB_name: GRB121011B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13870
SUBJECT: Konus-Wind observation of GRB 121011B
DATE:    12/10/15 11:10:07 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-duration hard-spectrum GRB 121011B
(IPN localization: Golenetskii at al., GCN 13863)
triggered Konus-Wind at T0=81140.083s UT (22:32:20.083)

The light curve shows a single pulse with a duration of ~0.35 s.
The emission is seen up to ~7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB121011_T81140/

As observed by Konus-Wind the burst
had a fluence of (2.8  0.3)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.112 s,
of (2.3  0.4)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured T0 to T0+0.192 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.45  0.37,
the high energy photon index beta = -1.9  0.4,
the peak energy Ep = 670  340 keV,
chi2 = 16.3/17 dof.

All the quoted results are preliminary.


GRB_name: GRB121011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13871
SUBJECT: PdB IRAM observation of GRB 121011A
DATE:    12/10/15 15:59:29 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@asdc.asi.it>

B. Gendre (INAF-OAR/ASDC), C. Feruglio (IRAM), G. Stratta (INAF-OAR), A. 
Antonelli (INAF-OAR/ASDC), J.L. Atteia (IRAP/OMP), S. Basa (LAM/OAMP), 
M. Bor (Artemis/CNRS), S. Cutini (INAF-OAR/ASDC), V. D'Elia 
(INAF-OAR/ASDC), A. Klotz (IRAP/OMP), L. Piro (INAF-IAPS),  repport:

we observed the position of GRB 121011A (Racusin et al., GCN 13845) with 
the Interferometer of the Plateau de Bure on 2012-10-11, starting at 
15:30 UT for 1.46 hours, at frequency 130 GHz. The observing conditions 
were good, with a stable atmosphere (phase rms below 35 degrees), 
Tsys~200 and water vapor about 6 mm.

No afterglow has been detected, with an upper limit of 214 micro Jy.

Given the radio non detection (van der Horst, GCN 13868) and the 
faintness of this object as seen in X-ray (Burrows et al., GCN 13857), 
no further observations are planned.

We thank the technical staff of IRAM for fast support of the trigger.

This message can be cited.

Based on observations carried out with the IRAM Plateau de Bure 
Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) 
and IGN (Spain).


GRB_name: GRB121012A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13872
SUBJECT: GRB 121012A: Fermi GBM detection
DATE:    12/10/15 18:46:05 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 17:22:16.39 UT on 12 october 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121012A (trigger 371755339 / 121012724).

The on-ground calculated location, using the GBM trigger
data, is RA = 33.4, DEC = +14.6 (J2000 degrees,
equivalent to 02 h 14 m, 14 d 24 '), with an uncertainty
of 6.8 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 75 degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 0.45 s (50-300 keV).

The time-averaged spectrum from T0-0.128 s to T0+0.320 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.47 +/- 0.11 and
the cutoff energy, parameterized as Epeak, is 540 +/- 70 keV
(Castor statistics 708.86 for 729 d.o.f.).
The event fluence (10-1000 keV) in this time interval is
(1.15 +/- 0.07)E-06 erg/cm^2.

The 64-msec peak photon flux measured starting from T0+0.064 s
in the 10-1000 keV band is 12.4 +/- 1.1 ph/s/cm^2.

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


GRB_name: GRB121011A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13873
SUBJECT: GRB 121011A Suzaku WAM observation of the prompt emission
DATE:    12/10/16 08:58:49 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

K. Takaki, Y. Hanabata, T. Kawano, R. Nakamura, Y. Tanaka, M. Ohno,
Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.),
H. Ueno, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, M. Asahina,
S. Kobayashi, A. Sakamoto, Y. Ishida, S. Sugimoto (Saitama U.),
M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki)
Y. E. Nakagawa (Waseda U.), K. Yamaoka, M. Kokubun, T. Takahashi
(ISAS/JAXA),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The long GRB 121011A (Swift/BAT trigger #535764; Racusin et al., GCN 13845;
Fermi-LAT detection: Ohno et al., GCN 13777) was detected by
the Suzaku Wide-band  All-sky Monitor (WAM) which covers an energy range
of 50 keV - 5 MeV at 11:15:30.264 UT (=T0).


The observed light curve shows a single peak structure starting
at T0-10 s, ending at T0+30 s with the total duration (T90) is about 31
seconds. The fluence of main pulse in 100 - 1000 keV was
  4.70 (-0.15, +0.10) x 10^-6 erg/cm^2
The 1-s peak flux measured at T0-1.0 s was
0.41 (-0.31, +0.29) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-10 s
to T0+30 s is well fitted by by a single power-law with a photon index
of 1.61 (-0.14, +0.18) (chi^2/d.o.f = 20.4/25).


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: GRB121011B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13874
SUBJECT: GRB 121011B: Suzaku WAM observation of the prompt emission
DATE:    12/10/16 09:02:56 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

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

The short, IPN localized GRB 121011B (Golenetskii et al., GCN 13863)

triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 22:32:22.753 UT (=T0).
The observed light curve shows  a single peak structure starting at
T0 s, ending at T0+0.5 s,  with a duration (T90) of about 0.28 seconds.
The fluence in 100 - 1000 keV was 1.21 (-0.07, +0.15) x 10^-6 erg/cm^2
The 1-s peak flux measured from T0-0.5s  was 2.10 (-0.26, +0.15)
photons/cm^2/s in the same  energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+0.5s is well fitted by a power-law with exponential cutoff model:
   dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
   alpha       0.45 (-0.59, +0.50), and
   Epeak       810 (-139, 229) keV (chi^2/d.o.f. = 31.1/24).

We also shows the results with the same spectrum fitted by a GRB Band
model,
the low-energy photon index alpha: -0.39 (-0.53, +0.68),
the high-energy photon index beta: <-2.33
and the peak energy Epeak: 778 (-163, +237) keV
(chi^2/d.o.f = 30.3/23).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
The light curves for this burst are available at:

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


GRB_name: GRB121017A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13875
SUBJECT: GRB 121017A: Swift detection of a burst
DATE:    12/10/17 19:55:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Grupe (PSU), B. N. Barlow (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
E. A. Helder (PSU), S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 19:23:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121017A (trigger=536172).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 288.816, -1.595 which is 
   RA(J2000)  =  19h 15m 16s
   Dec(J2000) = -01d 35' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows at least two peaks 
with a duration of about 10 sec (possibly longer).  The peak count rate 
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 19:25:03.3 UT, 95.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 288.8302, -1.6042 which
is equivalent to:
   RA(J2000)  = 19h 15m 19.25s
   Dec(J2000) = -01d 36' 15.1"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 60 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.22 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 3
(+2.89/-2.40) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 1141 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. There is no new source down to a limit of
about 19th mag. The 8'x8' region for the list of sources generated on-board covers
100% of the XRT error circle. Because of the density of catalogued stars,
further analysis is required to report an upper limit for any afterglow in the
region. No correction has been made for the expected extinction corresponding
to E(B-V) of 0.44. 

XRT and UVOT detections were delayed due to entry into the SAA shortly
after the initial trigger. 

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: GRB121017A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13876
SUBJECT: GRB 121017A: BOOTES-2/TELMA observations
DATE:    12/10/17 20:34:07 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

GRB 121017A: BOOTES-2/TELMA observations

M. Jelnek, A. J. Castro-Tirado, J. Gorosabel (IAA-CSIC Granada), S. Guziy
(Nikolaev Univ.), O. Rabaza (Univ. de Granada),
on behalf of a larger collaboration, report:

Following the detection of GRB 121017A by Swift (Grupe et al. GCN Circ.
13875) the 0.6m TELMA robotic telescope (+ COLORES) in Mlaga (Spain)
started to take images (unfiltered) about 3 min postburst (19:26:10 UT),
following the initial BAT position. There is no optical counterpart within
the Swift/X-ray error box down to R = 18.5 for a 153s combined exposure (5
min post burst). Further exposures in i-band (22:05 UT, 1200s on the
aggregate) set a limit of 19.5 (35 min post burst). We note the
considerable extinction (A_v = 1.4) towards this direction 6 deg below the
Galactic Plane. Observations are ongoing.

[GCN OPS NOTE(17oct12): Per author's request, OR was added to the author list.]


GRB_name: GRB121017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13877
SUBJECT: GRB 121017A optical observations
DATE:    12/10/17 21:48:00 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. A. Volnova (SAI MSU, IKI RAS), A. S. Moskvitin (SAO RAS) on behalf
of larger collaboration, reports

We observed the field of GRB 121017A (Grupe et al., GCN Circ. 13875)
with the 1-m Zeiss-1000 telescope of SAO RAS
in Rc band. The weather conditions were good, airmass = 5 - 6, seeing
= 2.6". Observations were started since 9.5 minutes
after the BAT trigger, middle time t-t0 = 0.01407 days.

We do not detect any object in the XRT error circle down to a limiting
magnitude 18.8 as well as Jelnek et al. (GCN Circ. 13876).


GRB_name: GRB121017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13878
SUBJECT: GRB 121017A: 1.23m CAHA R-band observations
DATE:    12/10/18 00:31:03 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC, Granada), S. Mottola (DLR, Berlin), report on
behalf of a larger collaboration:

"We imaged the field of the Swift GRB 121017A (Grupe et al., GCN Circ.
13875) with the 1.23m Calar Alto telescope. The observations were carried
out in the R-band on Oct. 17.85440--17.86153 UT (1.11--1.29 hours post
burst) with a total exposure time of 2x300s. No optical source brighter
than R~20 was found within the XRT error circle."


GRB_name: GRB121017A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13879
SUBJECT: GRB 121017A: Enhanced Swift-XRT position
DATE:    12/10/18 00:37:34 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 388 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 121017A, 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 = 288.83026, -1.60418 which is equivalent
to:

RA (J2000): 19h 15m 19.26s
Dec (J2000): -01d 36' 15.0"

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: GRB121017A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13880
SUBJECT: GRB 121017A: Swift-BAT refined analysis
DATE:    12/10/18 02:26:15 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
D. Grupe (PSU), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC)
(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 121017A (trigger #536172)
(Grupe, et al., GCN Circ. 13875).  The BAT ground-calculated position is
RA, Dec = 288.820, -1.602 deg, which is 
   RA(J2000)  =  19h 15m 16.8s 
   Dec(J2000) = -01d 36' 07.3" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
 
The mask-weighted light curve a single peak starting at ~T-3 sec, peaking 
at ~T+1 sec, and ending at ~T+5 sec.  T90 (15-350 keV) is 4.2 +- 0.5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-2.72 to T+2.53 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.74 +- 0.17.  The fluence in the 15-150 keV band is 6.6 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.31 sec in the 15-150 keV band
is 3.3 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/536172/BA/


GRB_name: GRB121017A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13881
SUBJECT: GRB 121017A: GROND Observations
DATE:    12/10/18 02:37:07 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (MPE/Universe Cluster), M. Nardini (Milano-Bicocca), and J.
Greiner (MPE) report on behalf of the GROND team:

We observed the field of GRB 121017A (Swift trigger 536172, Grupe et al.,
GCN # 13875) 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 on October 17, 2012, at 23:50 UT, 4.45 hr after the
GRB trigger. They were performed at an average seeing of 1" (in r') and at
an average airmass of 1.3.

We do not detect any sources in the enhanced XRT error circle (Goad et
al., GCN # 13879), in agreement with earlier reports of optical
observations (Jelnek et al., GCN # 13876, Volnova et al., GCN # 13877,
Gorosabel & Mottola, GCN # 13878). There is a star at the eastern edge of
the error circle but this affects only a small part of it.

Based on 284 s of total exposures in g'r'i'z' (mean time 0.18978 days
after the trigger) and 480 s in JHK (mean time 0.19003 days after the
trigger) we estimate preliminary AB magnitudes (upper limits are 3 sigma)
of

g' > 23.2,

r' > 23.2,

i' > 22.4,

z' > 22.2,

J  > 19.8,

H  > 19.4 and

K  > 19.3.

Given magnitudes are calibrated against GROND zeropoints in the optical as
well as 2MASS field stars in the NIR and are not corrected for the high
Galactic foreground reddening of E_(B-V) = 0.44 mag (Schlegel et al.
1998).


GRB_name: GRB121017A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13882
SUBJECT: GRB 121017A: Swift-XRT refined Analysis
DATE:    12/10/18 07:55:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.0 ks of XRT data for GRB 121017A (Grupe  et al. GCN
Circ. 13875), from 1.1 ks to 30.0 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 13879).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.93 (+/-0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.10 (+0.28, -0.27). The
best-fitting absorption column is  6.0 (+1.7, -1.4) 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 4.6 x 10^-11 (9.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.0 (+1.7, -1.4) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: 4.4 sigma
Photon index:      2.10 (+0.28, -0.27)

If the light curve continues to decay with a power-law decay index of
0.93, the count rate at T+24 hours will be 9.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.4 x
10^-13 (8.7 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00536172.

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


GRB_name: GRB121017A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13883
SUBJECT: GRB 121017A: Swift/UVOT Upper Limits
DATE:    12/10/18 11:31:14 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (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 121017A 
1142 s after the BAT trigger (Grupe et al., GCN Circ. 13875).
No optical afterglow consistent with the XRT position (Goad et al. GCN 
Circ. 13879) 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          1142         1291          147         >21.1
white             1142         1442          167         >21.2
v                 1298         1492           39         >18.5
b                 1397         1417           19         >19.1
u                 1373         1392           19         >18.6
w1                1347         1367           19         >18.1
w2                1448         1468           19         >18.1

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.44 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13884
SUBJECT: GRB 121011A: early optical light curve
DATE:    12/10/18 23:12:12 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU, IKI), A. Matkin (UAFO, ISON), I. Molotov (KIAM), A. 
Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:

We report the light curve of the optical afterglow of the Swift GRB 121011A 
(Racusin et al., GCN 13845). The afterglow was observed with VT-50 (0.5-m) 
telescope of UAFO/ISON-Ussuriysk observatory starting on Oct. 11 (UT) 
11:21:29 (Volnova et al., GCN 13855). The light curve obtained from series 
of 30 s unfiltered imaging can be found at

http://grb.rssi.ru/GRB121011A/GRB121011A_lc.png

The photometry is based on several nearby USNO-B1.0 stars (R2). 


GRB_name: GRB121024A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13886
SUBJECT: GRB 121024A: Swift detection of a burst with an optical counterpart
DATE:    12/10/24 03:12:57 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

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

At 02:56:12 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121024A (trigger=536580).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 70.467, -12.269 which is 
   RA(J2000)  =  04h 41m 52s
   Dec(J2000) = -12d 16' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a few overlapping peaks
with a duration of about 15 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 02:57:45.5 UT, 93.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 70.4715, -12.2904 which is equivalent to:
   RA(J2000)  = +04h 41m 53.16s
   Dec(J2000) = -12d 17' 25.4"
with an uncertainty of 5.5 arcseconds (radius, 90% containment). This
location is 78 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 1.10e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
158 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 04:41:53.28 =  70.47201
  DEC(J2000) = -12:17:26.8  = -12.29079
with a 90%-confidence error radius of about 0.78 arc sec. This position is 2.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.38 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.10. 

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: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13887
SUBJECT: GRB 121024A: TAROT Calern observatory optical detection of a bright counterpart
DATE:    12/10/24 03:20:53 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 121024A detected by SWIFT
(trigger 536580) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 45.0s after the GRB trigger
(13.9s after the notice). The elevation of the field decreased from
32 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).

We detect a new fading source in the error box given by SWIFT
We detected the candidate couterpart mentioned by Pagani et al. (GCNC 13886)
at the following position (+/- 2 arcsec):

RA(J2000) = 04h 41m 53.41s
DEC(J2000) -12d 17' 26.9"

OT was R~13.3 betwenn 45.0s and 60s after GRB.
Then the flux decreases.

Observations are continuing.

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=209.4933 lat=-34.2488
and the galactic extinction in R band is about 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.

[GCN OPS NOTE(24oct12): Per author's request, the circular citation
was added and the uncertainty was increased from 1 to 2 arcsec.]


GRB_name: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13888
SUBJECT: GRB 121024A: BOOTES-1B optical detection
DATE:    12/10/24 05:03:53 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek, Alberto J. Castro-Tirado and Javier Gorosabel
(IAA-CSIC Granada) on behalf of a larger collaboration
report:

"The 0.3m  BOOTES-1B robotic telescope located in Huelva
(Spain), observed the optical afterglow of GRB 121024A
(Pagani et al., GCNC 13886; Klotz et al., GCNC 13887). 
The observations started 40 minutes after the GRB trigger. 
The sum of 20 minutes of unfiltered images with a mean
integration time 54 minutes after the GRB shows the OT 
with magnitude roughly 18.2+-0.5."


GRB_name: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13889
SUBJECT: Skynet PROMPT/Dolomiti observations of GRB121024A
DATE:    12/10/24 05:47:22 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

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

Skynet observed the field of GRB121024A (GCN 13886, Swift trigger #536580) 
with the PROMPT telescopes located at CTIO in Chile and the 16" Dolomites 
Astronomical Observatory telescope (DAO) in Italy beginning ~1 minute after 
the burst trigger.  We detect the fading optical source reported by Klotz 
et al. (GCN #13887) in all observed filters (g',r',i',z' and BRI.)

Further observations are ongoing.


GRB_name: GRB121024A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13890
SUBJECT: GRB 121024A: VLT/X-shooter redshift
DATE:    12/10/24 07:10:59 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), J. P. U. Fynbo (DARK/NBI), A. Melandri (INAF-OAB), 
A. J. Levan (U. Warwick), D. Xu (WIS), V. D'Elia (ASDC) report on behalf of 
the X-shooter GTO collaboration:

We observed the afterglow of GRB 121024A (Pagani et al. GCN 13886) with the
X-shooter spectrograph at the VLT. Observations began at 04:45 UT, approximately
1.8 hours after the initial detection of the burst. The afterglow is well detected in
the acquisition image, and in the resulting spectrum we see a strong, broad 
damped-Lya absorption feature at ~4000A, combined with numerous narrow metal 
lines of CIV, SiII, SiIV, FeII, SII and AlII, as well as fine-structure lines associated 
with SiII*. These point to a common redshift of z=2.298 for GRB 121024A.

We thank Maja Vuckovic, Giovanni Carraro, Marcelo Lopez and Felipe Gaete
for their assistance in obtaining these observations, and Gianni Marconi
and Gerry Gilmore for kindly allowing the ToO to be performed during their
visitor mode run.


GRB_name: GRB121024A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13891
SUBJECT: GRB 121024A: GROND Detection of the Optical/NIR Afterglow
DATE:    12/10/24 11:31:10 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

F. Knust, P. Schady and J. Greiner (all MPE Garching) report on behalf  
of the GROND team

We observed the field of GRB 121024A (Pagani et al., GCN 13886)  
simultaneously in g'r'i'z' with GROND (Greiner et al. 2008, PASP, 120,  
405) mounted on the 2.2 m MPG/ESO telescope at La Silla Observatory  
(Chile).

Due to clouds, observations only started at 05:53 UT no 24th October,  
3 hours after the GRB trigger, and continued until the end of the  
night, 3.8 hours later. They were performed at an average seeing of  
1.4" and at an average airmass of 1.1.

We find a single point source within the 0.8 arcsec Swift/UVOT error  
circle reported by Pagani et al. (GCN 13886) at

RA (J2000) = 04:41:53.30
Dec (J2000) = -12:17:26.5

with an uncertainty of 0.4" in each coordinate.

Based on the first 142 sec integration in g'r'i'z' and 240 sec  
integration in JHK taken at a mid-time of 05:58 UT and 05:54 UT in the  
optical and NIR respectively, we estimate preliminary magnitudes (all  
in AB system) of

g' = 21.0 +/- 0.2 mag
r' = 20.1 +/- 0.2 mag
i' = 19.8 +/- 0.2 mag
z' = 19.5 +/- 0.2 mag
J = 18.7 +/- 0.1 mag
H = 18.4 +/- 0.1 mag
K = 17.9 +/- 0.1 mag

Given magnitudes are calibrated against GROND zeropoints in the  
optical, and 2MASS field stars in the NIR, and are not corrected for  
the expected Galactic foreground extinction corresponding to a  
reddening of E(B-V) = 0.1 mag in the direction of the burst (Schlegel  
et al. 1998).


GRB_name: GRB121024A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13892
SUBJECT: GRB 121024A: Swift-XRT refined Analysis
DATE:    12/10/24 19:24:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

K.L. Page (U. Leicester), A. Maselli  (INAF-IASFPA), V. Mangano
(INAF-IASFPA), A. Melandri (INAF-OAB), M.C. Stroh (PSU), D.N. Burrows
(PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester) and C. Pagani
report on behalf of the Swift-XRT team:

We have analysed 7.0 ks of XRT data for GRB 121024A (Pagani  et al. GCN
Circ. 13886), from 82 s to 23.5 ks after the  BAT trigger. The data
comprise 242 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 refined XRT position is RA, Dec = 70.47078, -12.29099 which
is equivalent to:

RA (J2000): 04 41 52.99
Dec(J2000): -12 17 27.6

with an uncertainty of 3.5 arcsec (radius, 90% confidence).

The late-time light curve (from T0+3.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.89 (+/-0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.15 (+/-0.08). The
best-fitting absorption column is  8.0 (+2.1, -2.0) x 10^21 cm^-2, at a
redshift of 2.298, in addition to the Galactic value of 5.4 x 10^20
cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index
of 1.96 (+/-0.13) and a best-fitting absorption column of 7.1 (+4.0,
-3.6) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.7 x 10^-11 (4.7
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 5.4 x 10^20 cm^-2
Intrinsic column:    7.1 (+4.0, -3.6) x 10^21 cm^-2 at z=2.298
Photon index:      1.96 (+/-0.13)

If the light curve continues to decay with a power-law decay index of
0.89, the count rate at T+24 hours will be 0.016 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.8 x
10^-13 (7.3 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00536580.

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


GRB_name: GRB121024A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13893
SUBJECT: GRB 121024A: PAIRITEL NIR Detection
DATE:    12/10/24 19:52:45 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

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

We observed the field of GRB 121024A (Pagani et al., GCN 13886) with
the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began
at 2012-Oct-24 07h31m47s UT, ~4.6 hours after the Swift Trigger.  In
mosaics (effective exposure time of 0.46 hours) taken simultaneously
in the J, H, and K filters, we detect a source at the optical
afterglow location (Pagani et al., GCN 13886; Klotz et al., GCN 13887;
Jelinek et al., GCN 13888; LaCluyze et al., GCN 13889; Knust et al.
GCN 13891).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(hr) filt  mag    m_err
6.06       0.46     J     >18.4  3sig
6.06       0.46     H     17.1   0.2
6.06       0.46     Ks    >16.2  3sig

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: GRB121024A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13894
SUBJECT: GRB 121024A: Enhanced Swift-XRT position
DATE:    12/10/25 00:58:32 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 7610 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 121024A, 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 = 70.47208, -12.29052 which is equivalent
to:

RA (J2000): 04h 41m 53.30s
Dec (J2000): -12d 17' 25.9"

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: GRB121025A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13895
SUBJECT: GRB 121025A: MAXI/GSC detection
DATE:    12/10/25 10:50:20 GMT
FROM:    Mikio Morii at Tokyo Inst Tech  <morii@hp.phys.titech.ac.jp>

M. Asada, H. Negoro (Nihon U.), M. Serino (RIKEN), M. Morii  (Tokyo Tech), 
Nakahira (JAXA), K. Yamaoka (Waseda U.), S. Ueno, H. Tomida, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, T. Yamamoto, J. Sugimoto, M. Matsuoka (RIKEN), 
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii  (Tokyo Tech),
A. Yoshida (AGU), H. Tsunemi, M. Kimura (Osaka U.), 
M. Nakajima (Nihon U.), 
Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.)
M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.)
report on behalf of the MAXI team:

At 2012-10-25T07:46:30 UT, the MAXI/GSC nova alert system triggered
on a bright uncatalogued X-ray transient source.
The transient emission lasted at least 20 seconds
within the 44 second long triangular transit response of
MAXI/GSC. We identify this event as GRB 121025A.

Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (248.75 deg, +27.73 deg) = (16 35 00, +27 44 05)(J2000)

with a 90% C.L. statistical error of 0.27 deg and an additional systematic uncertainty
of 0.1 deg (90% containment radius). The 4-10 keV flux was  129 (+26/-22) mCrab.

Within the scan transit, the variability of the source was marginally detected with a chance 
probability of 0.084 for 4 - 10 keV band.

There was no significant excess flux in the previous transit at 06:13 UT and 
in the next transit at 09:18 UT with an upper limit of 20 mCrab for each.

Follow-up observations are encouraged.


GRB_name: GRB121024A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13896
SUBJECT: GRB 121024A: MITSuME Okayama Optical upper limits
DATE:    12/10/25 10:54:18 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 121024A (Pagani et al., GCNC 13886)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2012-10-24 13:51:59 UT (~10.9 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 13894) in all the three bands.
We also could not detect the previously reported afterglow
(Klotz et al., GCNC 13887).

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
------------------------------------------------------
0.55338    16:13:04    7740.0   >20.1  >20.0  >19.3
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121024A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13897
SUBJECT: GRB 121024A: MITSuME Ishigakijima upper limits
DATE:    12/10/25 12:20:18 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 121024A (Pagani et al., GCNC 13886)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical Observatory.

The observation started on 2012-10-24 14:30:52 UT (~11.6 h after the burst)
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 13894) in all the three bands.
We also could not detect the previously reported afterglow
(Klotz et al., GCNC 13887).

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
------------------------------------------------------
0.52401    15:30:47    6060.0   >21.7  >21.4  >20.6
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13898
SUBJECT: GRB 121024A: GMG optical observation
DATE:    12/10/25 13:49:44 GMT
FROM:    Xiao-hong Zhao at Yunnan Obs  <zhaoxiaohong78@gmail.com>

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

We observed the field of GRB 121024A (Pagani et al., GCN 13886) with 2.4m Gao-Mei-Gu (GMG) telescope. Observations
started at 16:30:00 UT on 2012-10-24 (i.e., 13.6 hrs after the burst) and 2x900s R-band images were obtained. The optical afterglow of this burst was clearly detected. The results are as follows:

mid time from trigger (hr)    Mag.    Err.    Exposure time (second)
  13.69                       20.88   0.1      900
  13.81                       20.81   0.1      900  
   
We thank the GMG staff, especially Fang Wang, De-Qing Wang and Jian-Duo He for
performing these observations.


GRB_name: GRB121024A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13899
SUBJECT: GRB 121024A: Swift-BAT refined analysis
DATE:    12/10/25 14:39:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), T. Sakamoto (AGU), 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), C. Pagani (U Leicester),
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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121024A (trigger #536580)
(Pagani, et al., GCN Circ. 13886).  The BAT ground-calculated position is
RA, Dec = 70.481, -12.255 deg, which is 
   RA(J2000)  =  04h 41m 55.5s 
   Dec(J2000) = -12d 15' 19.1" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.
 
The mask-weighted light curve shows two overlapping peaks starting
at ~T-9 sec, peaking at ~T-7 and ~T+2 sec, and ending at ~T+6 sec
with a long low tail out to ~T+70 sec (and possibly out to ~T+130 sec).
T90 (15-350 keV) is 69 +- 32 sec (estimated error including systematics).
 
The time-averaged spectrum from T-8.27 to T+75.73 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.41 +- 0.22.  The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.73 sec in the 15-150 keV band
is 1.3 +- 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/536580/BA/


GRB_name: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13900
SUBJECT: GRB 121024A:  CARMA 3mm Detection
DATE:    12/10/25 16:43:05 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

B. Zauderer, T. Laskar and E. Berger (Harvard) report on behalf of the
CARMA Key Project "A Millimeter View of the Transient Universe":

"We observed the position of GRB 121024A (Pagani et al; GCN 13886) with
the Combined Array for Research in Millimeter Astronomy beginning 2012
Oct 25.5 (dt=1.4 d after the burst).  At a mean frequency of ~85 GHz, we 
detect a radio counterpart with a preliminary flux of ~1 mJy within the 
enhanced Swft/XRT error circle (Osborne et al; GCN 13894) and consistent 
with the optical afterglow (e.g. Knust et al.; GCN 13891).
We thank the CARMA observers and staff for their support.  Followup 
observations are planned."


GRB_name: GRB121024A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13901
SUBJECT: GRB 121024A: Swift/UVOT Observations
DATE:    12/10/25 20:02:12 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

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

     The Swift/UVOT began settled observations of the field of GRB
121024A starting 158 s after the BAT trigger (Pagani et al., 2012,
GCNC 13886).  We continued to detect the optical afterglow until
approximately 10 ks after the BAT trigger.  Preliminary UVOT
photometry, and 3-sigma upper limits, for the afterglow is presented
below.

-----------------------------------------------------
Filter       TSTART   TSTOP   Exp Time       Mag  Err
-----------------------------------------------------
    u (fc)     158      408        246     18.43 0.10
-----------------------------------------------------
    v          464      483         19    >18.1
    b          413      433         19     18.44 0.25
    u          538      557         19    >18.5
 uvw1          513      533         19    >18.1
 uvm2          488      508         19    >17.6
 uvw2          439      459         19    >18.1
-----------------------------------------------------

    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} = 0.09 mag (Schlafly et al. 2011, ApJS, 737, 103).  The
photometry is in the UVOT photometric system (Breeveld et al. 2011,
AIP Conf. Proc. 1358, 373).


GRB_name: GRB121024A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13903
SUBJECT: GRB 121024A: EVLA Detection
DATE:    12/10/26 03:54:19 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer, and E. Berger (Harvard) report:

"We observed the position of GRB 121024A (Pagani et al; GCN 13886) with the
EVLA beginning on 2012 Oct 25.3 UT (1.2 days after the burst). At a mean
frequency of 22 GHz, we detect a radio counterpart with a preliminary flux
density of ~ 0.1 mJy consistent with the enhanced Swft/XRT position
(Osborne et al; GCN 13894), the optical position (e.g. Knust et al.; GCN
13891) and the CARMA 3 mm position (Zauderer et al; GCN 13900). Follow-up
observations are planned."


GRB_name: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13904
SUBJECT: GRB 121024A: optical observations
DATE:    12/10/26 08:18:43 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey and Brajesh Kuamr (ARIES Nainital India,
on behalf of larger Indian GRB collaboration).

We observed the GRB 121024A field (Pagani et al., GCN 13886) using
1.04m telescope at ARIES Nainital, starting ~16.9 hours after the
burst (19:49:49 UT, 2012-10-24). Several frames in R_c and I_c
pass-bands were acquired in high air-mass conditions.

In our co-added image (6x300 sec) of R_c band, the optical afterglow
candidate (Knust et al., GCN 13891) is clearly detected. The preliminary
photometry of the co-added frame (calibrated against nearby USNO stars)
estimates the magnitude of the optical afterglow to be 21.1 +- 0.1 mag.  
This massage may be cited.


GRB_name: GRB121027A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13906
SUBJECT: GRB 121027A: Swift detection of a burst
DATE:    12/10/27 07:55:18 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U Leicester), C. Gronwall (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 07:32:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121027A (trigger=536831).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 63.610, -58.801 which is
    RA(J2000) = 04h 14m 26s
    Dec(J2000) = -58d 48' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 80 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~3 sec after the trigger.

The XRT began observing the field at 07:33:37.0 UT, 67.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
63.5977, -58.8298 which is equivalent to:
    RA(J2000)  = 04h 14m 23.44s
    Dec(J2000) = -58d 49' 47.2"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 106 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.50
x 10^20 cm^-2 (Kalberla et al. 2005).

The initial flux in the 2.5 s image was 6.10e-09 erg cm^-2 s^-1 (0.2-10
keV).

UVOT took a finding chart exposure of 250 seconds with the U filter starting
288 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
0.02.

Due to the maintenance work at Goddard this weekend (GCN 13905) there
may be a delay in receiving the full dataset, and thus refined
analyses may not be available until late Sunday/early Monday.

Burst Advocate for this burst is P. A. Evans (pae9 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: GRB121027A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13907
SUBJECT: GRB 121027A: Swift detection of a burst
DATE:    12/10/27 07:58:39 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P. A. Evans (U Leicester), C. Gronwall (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 07:32:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121027A (trigger=536831).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 63.610, -58.801 which is 
   RA(J2000) = 04h 14m 26s
   Dec(J2000) = -58d 48' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 80 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 07:33:37.0 UT, 67.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 63.59612, -58.82887 which
is equivalent to:
   RA(J2000)  = 04h 14m 23.07s
   Dec(J2000) = -58d 49' 43.9"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 103 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 1.50
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 6.10e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
288 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
0.02. 

Due to the maintenance work at Goddard this weekend (GCN 13905) there
may be a delay in receiving the full dataset, and thus refined
analyses may not be available until late Sunday/early Monday. 

Burst Advocate for this burst is P. A. Evans (pae9 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: GRB121027A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13908
SUBJECT: GRB 121027A: MAXI/GSC detection 40 minutes after the Swift Trigger
DATE:    12/10/27 09:51:02 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

M. Serino (RIKEN), S. Nakahira (JAXA), N. Negoro, M. Asada (Nihon U.), 
K. Yamaoka (ISAS), S. Ueno, H. Tomida, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, T. Yamamoto, J. Sugimoto, M. Matsuoka (RIKEN), 
N. Kawai,  M. Morii,  R. Usui, K. Ishikawa, T. Yoshii  (Tokyo Tech),
A. Yoshida (AGU), H. Tsunemi, M. Kimura (Osaka U.), 
M. Nakajima (Nihon U.), 
Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.)
M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.)
report on behalf of the MAXI team:

At 2012-10-27T08:12:53UT, the MAXI/GSC nova alert system triggered on a
bright uncatalogued X-ray transient source.
The transient emission lasted at least 38 seconds within the 41 second
long triangular transit response of MAXI/GSC. 

Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (63.75 deg, -58.68 deg) = (04:15:00, -58:40:59)(J2000)

with a 90% C.L. statistical error of 0.43 deg and an additional systematic
uncertainty of 0.1 deg (90% containment radius). 
The 4-10 keV flux was ~150 mCrab.

The position is consistent with GRB 121027A (GCN 13906, 13907), 
so we identify the source is GRB 121027A observed 40 minutes after 
the Swift Trigger.

There was no significant excess flux in the previous transit at 06:40 UT
(92 min before the trigger time) with an upper limit of 20 mCrab.


GRB_name: GRB121025A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13909
SUBJECT: GRB 121025A: Swift-XRT observation
DATE:    12/10/27 10:34:49 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, R.L.C. Starling and P.A. Evans (U. Leicester) report on behalf
of the Swift-XRT team:

Swift performed a Target of Opportunity observation of the MAXI-detected
GRB 121025A (Asada et al., GCN Circ. 13895), starting 26.1 ks after the
trigger. A series of four tiled pointings was performed, in order to cover
the MAXI error circle. Within these fields, one > 3 sigma uncatalogued
source was detected, at RA, Dec = 248.38182, 27.67189, which is equivalent
to:

RA(J2000)  = 16h 33m 31.64s
Dec(J2000) = 27d 40' 18.8"

with an uncertainty of 3.8 arcsec (radius, 90% containment). This source
has a mean count rate of 0.022 +/- 0.004 count s^-1. A spectrum formed
from the 1.8 ks of data can be fitted with an absorbed power-law with a
photon spectral index of 2.36 (+0.57,-0.56). The best-fitting absorption
column is consistent with the Galactic value of 3.8 x 10^20 cm^-2
(Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (4.5 x
10^-11) erg cm^-2 count^-1.

It is not possible to determine whether this source is fading at this
time and, therefore, whether it is the X-ray afterglow.

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


GRB_name: GRB121027A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13910
SUBJECT: GRB 121027A: Swift-BAT refined analysis
DATE:    12/10/27 14:44:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
P. A. Evans (U Leicester), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121027A (trigger #536831)
(Evans, et al., GCN Circ. 13906 (not 13907)).  The BAT ground-calculated position is
RA, Dec = 63.598, -58.839 deg, which is 
   RA(J2000)  =  04h 14m 23.5s 
   Dec(J2000) = -58d 50' 21.3" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 80%.
 
The mask-weighted light curve shows a FRED with two small peaks on the tail,
starting at ~T-9 sec, peaking at ~T+3 sec, with a long tail out to
~T+105 sec (or possibly to ~T+165 sec).  T90 (15-350 keV) is 62.6 +- 4.8 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-9.34 to T+65.33 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.82 +- 0.09.  The fluence in the 15-150 keV band is 2.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.00 sec in the 15-150 keV band
is 1.3 +- 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/536831/BA/


GRB_name: GRB121027A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13911
SUBJECT: GRB 121027A: nIR afterglow candidate with AAT
DATE:    12/10/27 20:11:13 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling (U. Leicester), A.J. Levan (U. Warwick), K. Wiersema (U. Leicester), A.R. Lopez-Sanchez (AAO/Macquarie
+University), N.R. Tanvir (U. Leicester), T. Young (ANU), L. Spitler (Macquarie University/AAO) and S. Lee (AAO) report:

We triggered near-infrared observations with IRIS2 on the Anglo-Australian Telescope for GRB 121027A, beginning ~3.5 hours
+after the Swift BAT trigger (Evans et al. GCN Circ. 13907).

The field was observed for 2x10 minutes in each of J, H and K bands. In a preliminary analysis of the K band data (beginning
+13:49 UT) we clearly detect a source within the enhanced XRT error circle (www.swift.ac.uk/sper/536831) at position:

RA   04 14 23.44
Dec -58 49 47.4 (J2000)

with approximate magnitude K(AB)=21.10 +/- 0.13.

The source is not discernable from the J and H band images. These, however, do not go as deep owing to variable weather
+conditions; the limiting magnitude in H(AB) is 21.3 (3-sigma, beginning 13:22 UT).


These data were obtained under programme AAT/12B/30.

[GCN OPS NOTE(28oct12): Per author's request, ALG was changed to ARL-S in the author list.]


GRB_name: GRB121011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13912
SUBJECT: GRB 121011A: optical observations
DATE:    12/10/27 23:02:08 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (SAI MSU, IKI), Moskvitin (SAO RAS), V. Rumyantsev (CrAO),
A. Pozanenko (IKI)


We observed the field of the Swift GRB 121011A (Racusin et al., GCN
13845) with ZTSh telescope of CrAO on Oct. 15 between (UT) 17:36 and
18:54 under good weather condition with mean seeing of about 1.5
arcsec. We took 70 frames with exposure of 60 seconds in filter R.  In
a stacked image we do not detect any source within enhanced XRT error
circle (Evans et al., GCN 13850).

We also observed the field of this GRB with Zeiss-1000 telescope of
SAO RAS on Oct. 17 between (UT) 17:45 and 18:38 under good weather
conditions with mean seeing of about 2.4 arcsec. We took 12 frames
with exposure of 200 seconds. On a stacked image we do not detect any
source either. The photometry based on a USNO-B1 star #1310-0279773
(R1 = 17.84; same
as calibration in Fynbo et al., GCN Circ. 13856; Malesani et al., GCN
13853) is following:

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

4.292      R       70x60        n/d   23.5                ZTSh
6.294      R       12x200      n/d   22.3                Zeiss-1000


GRB_name: GRB121028A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13913
SUBJECT: GRB 121028A: Swift detection of a burst
DATE:    12/10/28 05:31:03 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

R. L. C. Starling (U Leicester), C. Gronwall (PSU),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report
on behalf of the Swift Team:

At 05:04:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121028A (trigger=536897).  Swift slewed immediately to the burst.   
The BAT on-board calculated location is
RA, Dec 271.923, -2.285 which is
  RA(J2000) = 18h 07m 42s
  Dec(J2000) = -02d 17' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 30 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger.

The XRT began observing the field at 05:06:41.7 UT, 129.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 271.8995, -2.2936 which
is equivalent to:
   RA(J2000)  = 18h 07m 35.89s
   Dec(J2000) = -02d 17' 36.8"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 90 arcseconds from the BAT onboard position, within the BAT  
error circle. This position may be improved as more data are received;   
the latest position is available at http://www.swift.ac.uk/sper.

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.48 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4.4
(+4.35/-3.23) x 10^21 cm^-2 (90% confidence).

UVOT took a finding chart exposure of 150  seconds with the White filter starting
134 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 extinction.

Due to the maintenance work at Goddard this weekend (GCN 13905) there
may be a delay in receiving the full dataset, and thus refined
analyses may not be available until late Sunday/early Monday.

Burst Advocate for this burst is R. L. C. Starling (rlcs1 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: GRB121028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13914
SUBJECT: GRB 121028A: Faulkes Telescope North observations
DATE:    12/10/28 08:12:16 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Gomboc (U. Ljubljana),
on behalf of a large collaboration report:

The 2-m Faulkes Telescope North automatically began observing
GRB 121028A (Starling et al. GCN Circ. 13913) on October 28 2012,
05:07:12 UT corresponding to 161 seconds post burst trigger
with BVRi' filters. Within the XRT error circle we don't see
any uncatalogued object down to the following limits:

Mid time from       Exposure        Filter       Limit
GRB (sec)           (s)
-------------------------------------------------------
198                3x10              R            > 19
535                 10               i'           > 18
-------------------------------------------------------

Magnitudes are calibrated against nearby USNOB1 stars.


GRB_name: GRB121028A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13915
SUBJECT: GRB 121028A: MITSuME Okayama Optical upper limits
DATE:    12/10/28 13:05:18 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 121028A (Starling et al., GCNC 13913)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2012-10-28 09:15:55 UT (~4.2 h after the burst).
We did not find any new point source within the XRT circle
(Starling et al., GCNC 13913) 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
------------------------------------------------------
0.21623    10:15:53    6360.0   >19.7  >19.4  >18.7
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121027A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13916
SUBJECT: GRB 121027A: Enhanced Swift-XRT position
DATE:    12/10/29 00:49:15 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 661 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 121027A, 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 = 63.59738, -58.82962 which is equivalent
to:

RA (J2000): 04h 14m 23.37s
Dec (J2000): -58d 49' 46.6"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB121028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13917
SUBJECT: GRB 121028A: Swift-BAT refined analysis
DATE:    12/10/29 00:53:25 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),
A. M. Parsons (GSFC), G. Sato (ISAS), M. Stamatikos (OSU),
R. L. C. Starling (U Leicester), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 121028A (trigger #536897)
(Starling, et al., GCN Circ. 13913).  The BAT ground-calculated position is
RA, Dec = 271.903, -2.298 deg, which is 
   RA(J2000)  =  18h 07m 36.7s 
   Dec(J2000) = -02d 17' 52.1" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.
 
The mask-weighted light curve shows a single pulse starting at ~T-0.9 sec, 
peaking at ~T+2 sec, and ending ~T+4 sec.  T90 (15-350 keV) is 3.8 +- 0.7 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.8 to T+3.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.79 +- 0.17.  The fluence in the 15-150 keV band is 3.7 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.01 sec in the 15-150 keV band
is 1.9 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/536897/BA/


GRB_name: GRB121028A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13918
SUBJECT: GRB 121028A: Enhanced Swift-XRT position
DATE:    12/10/29 07:15:58 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 2614 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 121028A, 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 = 271.89948, -2.29358 which is equivalent
to:

RA (J2000): 18h 07m 35.87s
Dec (J2000): -02d 17' 36.9"

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: GRB121028A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13919
SUBJECT: GRB 121028A: Swift-XRT refined Analysis
DATE:    12/10/29 07:39:59 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and R. L. C. Starling (U Leicester) report on
behalf of the Swift-XRT team:

We have analysed 9.4 ks of XRT data for GRB 121028A (Starling  et al.
GCN Circ. 13913), from 139 s to 48.8 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN. Circ 13918).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.87 (+/-0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.63 (+0.26, -0.25). The
best-fitting absorption column is  4.8 (+1.7, -1.4) x 10^21 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 5.6 x 10^-11 (7.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.8 (+1.7, -1.4) x 10^21 cm^-2
Galactic foreground: 2.5 x 10^21 cm^-2
Excess significance: 2.6 sigma
Photon index:      1.63 (+0.26, -0.25)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00536897.

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


GRB_name: GRB121027A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13920
SUBJECT: GRB 121027A: Brightening IR counterpart
DATE:    12/10/29 08:36:06 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), R.Starling, N.R. Tanvir, K. Wiersema (U.
Leicester), A. R. Lopez-Sanchez (AAO/Macquarie University), T. Young
(ANU), K. Glazebrook (Swinburne), L. Spitler (Macquarie University/AAO),
and S. Lee (AAO) report:

"We observed the candidate afterglow of GRB 121027A (Evans et al.
GCN 13906; Starling et al. GCN 13916) with the Anglo Australian
Telescope for a second epoch on the night of 28 October 2012. The
second epoch was obtained ~32 hours after the burst, and 26 hours
after the first epoch reported in Starling et al. (GCN 13916). We
clearly detect the afterglow candidate, and find that it has
brightened by approximately 1 magnitude in the K-band between the
two epochs. This confirms it as the infrared afterglow of GRB
121027A. We note that rising behaviour in the IR over this time
period is extremely unusual, and given the extremely bright, and
long lived X-ray afterglow (e.g. Serino et al. GCN 13908) could be
indicative of an event similar in nature to Swift J1644+57."


GRB_name: GRB121027A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13921
SUBJECT: GRB 121027A: Swift-XRT refined Analysis
DATE:    12/10/29 09:29:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans, K.L. Page and J.P. Osborne (U Leicester) report on behalf
of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 121027A (Evans  et al. GCN
Circ. 13906), from 57 s to 76.2 ks after the  BAT trigger. The data
comprise 2.0 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 13916).

This burst is unusual in showing multiple strong rebrightenings at high
flux in X-rays, a rebrightening has also reported in the IR (Levan et
al GCN 13920). This behaviour is reminiscent of the tidal disruption
event Swift J1644.

The light curve initially follows a power-law decay with an index of
alpha~1.8. This is interrupted by a flare beginning at T+220 s and
lasting ~300 s, after which the decay appears much steeper: alpha~6.6.
However at T+800 s the count rate jumps sharply, increasing by more
than 2 orders of magnitude in under 300 s; by T+1.1 ks the count rate
is ~30 ct/sec, corresponding to an observed flux of ~1e-9 erg/cm^2/s.
At this point the GRB left Swift's observing window, however during the
next observation (T+5.3 ks to T+6ks) the count rate remained high,
increasing from ~20 ct/s at the start of the observation to ~60 ct/s at
the end. The MAXI observation (GCN 13908) occurred between these
observations, and the flux reported by MAXI is consistent with the
Swift flux of ~1-2 e-9 erg cm^2/s. Over the next 4 exposures (T+11 ks
to T+30 ks), the count-rate declines with an index of ~3.8 to a level
of ~0.08 ct/s, it then remains at that level until T+76 ks, where our
current observations end. The hardness ratio follows the count-rate
during the rebrightenings (i.e. the emission is harder when brighter),
which is typical of flaring activity.

A spectrum formed from the first observation in WT mode data can be
fitted with an absorbed power-law with a photon spectral index of 2.55
(+/-0.06). The best-fitting absorption column is  2.80 (+0.16, -0.15) 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 1.94
(+0.29, -0.27) and a best-fitting absorption column of 1.1 (+0.7, -0.6)
x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.8 x 10^-11 (4.8 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      1.94 (+0.29, -0.27)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00536831.

Multi-wavelength follow-up is strongly recommended.

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


GRB_name: GRB121027A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13922
SUBJECT: GRB 121027A: MASTER early prompt optical limit
DATE:    12/10/29 11:09:57 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

H. Levato and C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

C. Mallamaci, C. Lopez and F. Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

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

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

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

V. Krushinski, I. Zalozhnich,  A. Popov, A. Bourdanov
Ural Federal University


MASTER-ICATE robotic Very Wide Field Cameras (FOV=2x384 square degrees,
D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located in
Argentina (Observatorio Astronomico Felix Aguilar,
http://93.180.27.230:8080/) were pointed to the GRB 121027A by Swift 
trigger (Evans et al., GCNC 13906)   85 s after GRB time at 
2012-10-27 07:33:54 UT.
We haven't found  optical transient  within Swift XRT 
error-box  on our first (1 s exposure) set and on coadd image
with complete exposure
of 11 seconds during gamma-burst activity (Barthelmy et al., GCN 13910).

The 5-sigma upper limit on unfiltered (with respect to Tyho V mag) single 
image has  been about 11.0 mag and 11.7 mag on coadded image.

The automatic photometry is:

Date         time     Exp.time Limit
                        Coadd

2012-10-27 07:33:54     11      11.7
2012-10-27 07:35:05     41      12.2
2012-10-27 07:37:25     7       11.2
2012-10-27 07:38:16     80      11.7
2012-10-27 07:44:18     17      11.2
2012-10-27 07:45:18     75      12.2
2012-10-27 07:50:38     11      11.6
2012-10-27 07:51:03     26      12.1
2012-10-27 07:51:56     30      12.2


Our cameras are continuously imaging the sky with 1 sec exposures without 
time gap.

This message can be cited.


GRB_name: GRB121028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13924
SUBJECT: GRB 121028A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    12/10/29 16:05:04 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made observations of Swift
trigger 536897 (Starling, et al., GCN 13913).  The burst location was within
the field of our wide-field monitor located in Maui, HI, which began a 10 s
integration of the location at 05:04:32.5 UT, 0.6 s after the Swift trigger
time and during the gamma-ray emitting interval including the time of peak
emission detected by the BAT (Sakamoto, et al., GCN 13917).  We detect no
new object at the location of the refined Swift XRT location (Evans, et al.,
GCN 13918).  Our 3-sigma limiting magnitude is 10.0 based on a comparison of
our unfiltered image to the Tycho-2 V-band catalog.


GRB_name: GRB121029A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13925
SUBJECT: GRB 121029A: Fermi GBM detection
DATE:    12/10/29 16:32:14 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin reports on behalf of the Fermi GBM Team:

"At 08:24:19.93 UT on 29 October 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121029A (trigger 373191862 / 121029350).

The on-ground calculated location, using the GBM trigger
data, is RA = 226.8, DEC = -28.2 (J2000 degrees,
equivalent to 15h 07m, -28d 12'), with an uncertainty
of 1.7 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 57 degrees.

The burst triggered an ARR (Automatic Repointing Request), 
causing Fermi to slew so the LAT would point to the source.  

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

The GBM light curve shows a double-peaked burst 
with a duration (T90) of about 16 s (50-300 keV).
The time-averaged spectrum from T0-0.128 s to T0+15.104 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.63 +/- 0.07  and
the cutoff energy, parameterized as Epeak, is 188 +/- 10 keV.

The event fluence (10-1000 keV) in this time interval is
(7.82 +/- 0.06)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+11.84 s in the 10-1000 keV band
is 13.3 +/- 0.3  ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak= 176 +/- 13 keV, 
alpha = -0.57 +/- 0.09  and beta = -2.82 +/- 0.42.

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


GRB_name: GRB121027A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13926
SUBJECT: GRB 121027A: GROND Confirmation of Rebrightening 
DATE:    12/10/29 19:48:09 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

V. Sudilovsky (MPE Garching), D. A. Kann (MPE Garching/Universe Cluster),
T. Krhler (DARK, Copenhagen), and J. Greiner (MPE Garching) report on
behalf of the GROND team:

Following two days of bad weather delay, we observed the field of GRB
121027A (Evans et al., GCN 13906) simultaneously in g'r'i'z'JHK with GROND
(Greiner et al. 2008, PASP, 120, 405) mounted on the 2.2 m MPG/ESO
telescope at La Silla Observatory (Chile).

Observations began at 08:10 on October 29th (mid-time ~2.05 days
post-trigger). They were performed at an average seeing of 1.6" (r'-band)
and at an average airmass of 1.2.

We detect the NIR afterglow reported by Starling et al. (GCN 13911) and
Levan et al. (GCN 13920) in all seven bands.

Based on a 460 sec integration in g'r'i'z' and 1200 sec integration in
JHK, we measure preliminary magnitudes (all in AB system) of

g' = 22.1 +/- 0.2 mag
r' = 21.6 +/- 0.1 mag
i' = 21.3 +/- 0.1 mag
z' = 20.9 +/- 0.1 mag
J  = 20.4 +/- 0.1 mag
H  = 19.7 +/- 0.1 mag
K  = 19.0 +/- 0.1 mag

We note an increase of brightness by ~ 1 magnitude relative to the
observations reported by Levan et al. (GCN 13920) at 32 hours after the
GRB.

Our detection in all bands constrains the redshift of this burst to z < 3.5.

Given magnitudes are calibrated against GROND zeropoints in the optical,
and 2MASS field stars in the NIR, and are not corrected for the expected
Galactic foreground extinction corresponding to a reddening of E(B-V) =
0.02 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB121028A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13927
SUBJECT: GRB 121028A: near-IR observations at Calar Alto
DATE:    12/10/29 20:15:14 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

M. Jelinek, A. J. Castro-Tirado (IAA-CSIC Granada), P. Ferrero (IAC Tenerife),
S. Guziy (Univ. of Nikolaev) and G. Bergond (CAHA Almera), on behalf of a larger
collaboration, report:

"Following the detection of GRB 121028A by Swift (Starling et al. GCNC
13913), we triggered the 3.5m CAHA telescope (+ Omega 2000) at the
German-Spanish Calar Alto Observatory. Observations (900s each) were taken
in the YJHK-bands, starting at 18:05 UT (i.e. 13 hr post burst). At the
position of the X-ray afterglow (Evans et al. GCNC 13918), we do not
detect a near-IR countepart in any band, particularly down to H = 20.5."

This message can be quoted.

[GCN OPS NOTE(30oct12):  Per author's request, PF was added to the author list.]


GRB_name: GRB121024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13928
SUBJECT: GRB 121024A: SMARTS optical/IR afterglow observations
DATE:    12/10/29 21:00:20 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU), reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained
optical/IR imaging of the error region of GRB 121024A (GCN 13886,
Pagani et al.)  over several epochs (with mid-exposure times of
2012-10-24 03:51 UT, 06:10 UT, 08:12 UT and 2012-10-25 06:53 UT).
For each epoch, several dithered images were obtained with
total summed exposure times of 15 min in V and I and 12 min in
J and K.  For the final epoch, total exposure times were
36 min in I and 30 min in J.

The fading afterglow of GRB 121024A (e.g. GCN 13887, Klotz et al.; GCN
13888, Jelinek et al.; GCN 13891, Knust et al.) was detected with the
following magnitudes (or 3-sigma limits):

mid-exposure
time
(hours)         I mag            J mag            K mag
0.90722       18.0 +/- 0.1   16.7 +/- 0.1   15.2 +/- 0.2
3.23611       19.4 +/- 0.1   17.9 +/- 0.1   16.3 +/- 0.2
5.27333       19.8 +/- 0.1   > 18.0           > 16.4
27.95278      > 21.9          > 19.3           ...

(Optical photometry is calibrated against USNO-B1.0 stars
and IR photometry is calibrated against 2MASS stars in the field.)


GRB_name: GRB121027A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13929
SUBJECT: GRB 121027A - Gemini South spectroscopy
DATE:    12/10/29 23:01:55 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir, K. Wiersema (U. Leicester), A. J. Levan (U. Warwick),
R. L. C. Starling (U. Leicester), S. Margheim, T. Hayward (Gemini) report:

We observed the counterpart of GRB 121027A (Starling et al.
GCN 13911; Levan et al. GCN 13920; Sudilovsky et al. GCN13926 ) 
with the GMOS-S spectrograph at Gemini-South, beginning at 
Oct 29 2012 05:42 UT.  The spectrum covers a wavelength range of
roughly 5200A to 7900A, and was obtained in rather
poor conditions.  Our provisional reduction shows a generally featureless
trace, with only one significant absorption feature, at about 7770A.
If we identify this feature with the MgII doublet at 2796/2803A
(the poor S/N and low resolution make it unclear whether or not the
observed line is a doublet), it would imply a redshift of z=1.77.
Whilst this is perhaps the most likely identification, further observations
are encouraged to test this possibility.


GRB_name: GRB121027A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13930
SUBJECT: GRB 121027A: X-shooter redshift confirmation
DATE:    12/10/30 09:05:32 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (DARK), N. R. Tanvir (U. Leicester), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI),
D. Malesani (DARK), J. Fynbo (DARK), A. Melandri (INAF-OAB), A. J. Levan (U. Warwick), 
K. Wiersema (U. Leicester), S. Schulze (PUC and MCSS), P. Goldoni (APC,CEA/Irfu), 
H. Flores (Obs. Paris) and L. Kaper (U. Amsterdam) report on behalf of a larger collaboration:

We observed the optical/NIR counterpart  (Starling et al. GCN 13911, 
Levan et al. GCN 13920, Sudilovsky et al. GCN 13926) of GRB 121027A 
(Evans et al. GCN 13906) with the VLT/X-shooter spectrograph, 
beginning at Oct 30 2012 04:52 UT, which is 2.89 days after the GRB.

We identify emission lines of [OIII]4959 and [OIII]5007, and several absorption
lines of CIV, AlII, AlIII, MgI, MgII and FeII at a common redshift of z=1.773.  This 
confirms the provisional redshift given in Tanvir et al. (GCN 13929) for this GRB.

We note that the afterglow remains remarkably bright at 2.9 days post burst.
From the photometry of the acquisition image, we measure R = 21.15 +- 0.05 
assuming R = 15.96 for the USNO star 0311-0027010 at RA = 04:14:21.83, 
Dec = -58:50:28.8.

We thank the VLT staff, in particular Linda Schmidtobreick and 
Myriam Rodrigues, for their assistance in obtaining these data, 
and acknowledge J. Elliott for private information about the transient brightness.


GRB_name: GRB121024A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13931
SUBJECT: GRB 121024A: LOAO RIzY Observation
DATE:    12/10/30 11:36:05 GMT
FROM:    Minsung Jang at Seoul National U  <rigel103@snu.ac.kr>

M. Jang, M. Im (SNU), and Y. Urata (NCU), on behalf of a larger collaboration

We observed GRB 121024A in RIzY-bands starting at UT 10:52:00, 2012-10-24,
~ 9 hrs after the BAT trigger (Baumgartner et al, GCN 10484),
using the 1.0m telescope at Mt.Lemmon in Arizona, U.S.

We do not detect the GRB afterglow in all bands within the error circle
of the enhanced XRT position (Evans et al.,GCN 13892).
We estimate the 3-sigma limiting magnitude of the afterglow to be
R ~ 20.0 at the midpoint time (~T0+9.3 hrs)
by calibrating it against seven USNO-B1 stars with R2 magnitudes
without the galactic extinction correction.

We thank the LOAO operator, J. Yoon, for performing the observation.


GRB_name: GRB121027A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13932
SUBJECT: GRB 121027A: Swift/UVOT Possible Detection
DATE:    12/10/30 17:59:26 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and P. A. Evans (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121027A
77 s after the BAT trigger (Evans et al., GCN Circ. 13906).
A source consistent with the XRT position (Beardmore et al. GCN Circ. 13916)
and the nIR position (Starling et al. GCN Circ. 13911)
is weakly detected in the initial UVOT exposures.

The preliminary detection 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               77         1192          353         21.55 +/- 0.25
v                  619         1239           75        >19.5
b                  544         1167           58        >19.7
u                  289         1143          285        >20.6
w1                 668         1118           58        >19.8

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: GRB121031A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13934
SUBJECT: GRB 121031A: Swift detection of a burst
DATE:    12/10/31 23:17:04 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), S. T. Holland (STScI), J. A. Kennea (PSU),
F. E. Marshall (NASA/GSFC) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 22:50:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121031A (trigger=537195).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 170.771, -3.511 which is 
   RA(J2000)  =  11h 23m 05s
   Dec(J2000) = -03d 30' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a large peak
with several smaller peaks riding on top with a total duration
of about 50 sec.  The peak count rate was ~4000 counts/sec (15-350 keV),
at ~4 sec after the trigger. 

The XRT began observing the field at 22:51:32.6 UT, 61.9 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 170.7694, -3.5153 which is equivalent to:
   RA(J2000)  = +11h 23m 4.66s
   Dec(J2000) = -03d 30' 55.1"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 17 arcseconds from the BAT onboard position, within the BAT
error circle. Despite the onboard localisation, no X-ray source was
detected in 732 s of promptly-downlinked data, suggesting that the
initial centroid may equally have been a cosmic ray. This position
should therefore be treated with caution. 

The initial flux in the 2.5 s image was 5.90e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White 
filter starting 70 seconds after the BAT trigger. No aspect solution
is available for the 2.7'x2.7' sub-image; results from the list of 
sources  generated on-board are not available at this time. The 
expected extinction corresponding to E(B-V) of 0.05. 

We note that the XRT position is 1.4 arcminutes from the galaxy 
2MASX J11225935-0331287, at redshift 0.1126, which has a nominal 
radius of 0.3 arcminutes according to NED. 

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: GRB121031A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13935
SUBJECT: GRB 121031A: Prompt enhanced Swift-XRT position
DATE:    12/10/31 23:39:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Using  promptly downlinked XRT event data for GRB 121031A, we find an
enhanced XRT position of the afterglow: RA, Dec: 170.7705, -3.5172
which is equivalent to:
   RA (J2000)  = 11 23 04.91
   Dec (J2000) = -03 31 01.9
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/537195.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB121031A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13936
SUBJECT: GRB 121031A: Swift-BAT refined analysis
DATE:    12/11/01 12:43:18 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

GRB 121031A: Swift-BAT refined analysis
 
S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
V. D'Elia (ASDC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 121031A (trigger #537195)
(D'Elia, et al., GCN Circ. 13934).  The BAT ground-calculated position is
RA, Dec = 170.772, -3.513 deg, which is 
   RA(J2000)  =  11h 23m 05.2s 
   Dec(J2000) = -03d 30' 47.7" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a FRED-like peak with a couple smaller peaks
superposed.  It starts at ~T-10 sec, peaks at ~T+4 sec, and ends at ~T+100 sec.
T90 (15-350 keV) is 62.5 +- 25.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.64 to T+98.31 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.59 +- 0.07.  The fluence in the 15-150 keV band is 3.1 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+4.10 sec in the 15-150 keV band
is 2.2 +- 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/537195/BA/


GRB_name: GRB121027A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13937
SUBJECT: GRB 121027A: sub-mm upper limit
DATE:    12/11/01 15:32:19 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

J. Greiner (MPE Garching), A. Belloche, T. Csengeri, F. Wyrowski 
(all MPIfR Bonn), F. Schuller, F. Montenegro (both APEX, ESO), 
V. Sudilovsky, J. Elliott (both MPE Garching), 
D. A. Kann (MPE Garching/Universe Cluster),
A. de Ugarte Postigo (IAA-CSIC Granada/DARK Copenhagen), 
T. Kruehler (DARK Copenhagen) report:

We observed the afterglow of the peculiar GRB 121027A (Starling et al. 2012, 
GCN 13911; Levan et al. 2012, GCN 13920; Evans et al. 2012, GCN 13921) with 
LABOCA/APEX at 870 micron. The observations in photometry mode started on 
Oct. 31, 7:57 UT, 4.02 days after the Swift trigger (Evans et al. 2012, 
GCN 13906, Barthelmy  et al. 2012, GCN 13910). They were performed under 
good weather conditions (pwv ~ 1 mm), and lasted for 1 hr.

No source is detected, down to a 3 sigma upper limit of 21 mJy/beam.


GRB_name: GRB121102A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13938
SUBJECT: GRB 121102A: Swift detection of a burst
DATE:    12/11/02 02:46:30 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 02:27:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121102A (trigger=537266).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 270.903, -16.966 which is 
   RA(J2000)  = 18h 03m 37s
   Dec(J2000) = -16d 57' 56"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single FRED-like peak
with a duration of about 25 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 02:27:50.4 UT, 47.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
270.9009, -16.9578 which is equivalent to:
   RA(J2000)  = 18h 03m 36.22s
   Dec(J2000) = -16d 57' 28.2"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 30 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (5.33 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 3.1
(+3.61/-1.55) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 3.45e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 57 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. Because of the density of catalogued stars,  further
analysis is required to report an upper limit for any afterglow in the
 region. No correction has been made for the large, but uncertain
extinction  expected. 

This event has all appearances of a GRB: hard BAT spectrum,
bright XRT initial detection and fading.  Still, we note that 
the galactic coordinates are l=12 deg, b=2.5 deg, consistent 
with a galactic origin.  We believe it is a GRB, but can not 
rule out a new galactic transient. 

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: GRB121102A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13939
SUBJECT: GRB 121102A : a long GRB detected by INTEGRAL
DATE:    12/11/02 03:47:34 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 20 s has been detected by IBAS in the 
IBIS/ISGRI data at 02:27:00 UT of November 2

The refined coordinates are

  RA  = 270.9034  deg 
BDEC = -16.9509  deg

with an uncertainty of 2 arcmin (90% c.l.).

A preliminary analysis gives a burst peak flux of about 1 counts/cm2/s 
(20-200 keV, 1-s integration time) and a fluence in the same energy range 
of about 1e-6 erg/cm2.

A plot of the light curve will posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB121029A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13940
SUBJECT: GRB 121029A Suzaku WAM observation of the prompt emission
DATE:    12/11/02 07:16:47 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

W. Iwakiri, M. Tashiro, Y. Terada,  T. Yasuda, M. Asahina,
S. Kobayashi, A. Sakamoto, Y. Ishida, S. Sugimoto,  H. Ueno(Saitama U.),
M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki),
Y. E. Nakagawa (Waseda U.),
Y. Hanabata, T. Kawano, K. Takaki, R. Nakamura, Y.Tanaka, M. Ohno,
Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), K. Yamaoka,
M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The long GRB 121029A ( Fermi-GBM detection : von Kienlin et al., GCN 13925)
was detected by the the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
 energy range of 50 keV - 5 MeV at 08:24:18 UT (=T0).

The observed light curve shows multi-peaked structure starting at T0-2
s, ending
 at T0+20 s with a duration
 (T90) of about 15 seconds. The fluence in 100 - 1000 keV was 6.05
(-0.33, +0.29) x 10^-6 erg/cm^2.
 The 1-s peak flux measured from T0+14 s was 4.63 (-0.42, +0.44)
photons/cm^2/s in the same
 energy range.

Preliminary result shows that the time-averaged spectrum from T0-2 s to
T0+20 s is well fitted by a single power-law with a photon index
of 2.76 (-0.21, +0.23) (chi^2/d.o.f = 6.9/14).

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

The light curves with 1-sec time resolution for this burst will be appeared at:

 http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB121025A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13941
SUBJECT: GRB 121025A: Confirmation of the X-ray afterglow
DATE:    12/11/02 08:41:47 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

Swift performed a follow-up observation of the possible X-ray afterglow of
MAXI-detected GRB 121025A (Asada et al., GCN Circ. 13895) announced in GCN
Circ. 13909 (Page, Starling & Evans). This second observation took place
on 2012-10-31, 5.8 days after the burst. The source has now faded by at
least an order of magnitude, with an upper limit on the count rate of
0.002 count s^-1 (corresponding to an observed flux of 8.1 x 10^-14 erg
cm^-2 s^-1). This source is therefore confirmed as the X-ray afterglow of
GRB 121025A.

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


GRB_name: GRB121102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13942
SUBJECT: GRB 121102A: Swift-BAT refined analysis
DATE:    12/11/02 12:13:27 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),
V. D'Elia (ASDC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121102A (trigger #537266)
(D'Elia, et al., GCN Circ. 13938).  The BAT ground-calculated position is
RA, Dec = 270.896, -16.951 deg, which is 
   RA(J2000)  =  18h 03m 35.1s 
   Dec(J2000) = -16d 57' 03.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a FED peak starting at ~T-0.2 sec,
peaking at ~T+6 sec, and ending at ~T+95 sec.  T90 (15-350 keV) is
24.7 +- 3.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.30 to T+35.25 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.88 +- 0.07.  The fluence in the 15-150 keV band is 1.9 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+5.68 sec in the 15-150 keV band
is 2.3 +- 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/537266/BA/


GRB_name: GRB121102A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13943
SUBJECT: GRB 121102A: Swift-XRT refined Analysis
DATE:    12/11/02 14:46:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

C. Pagani (U. Leicester), V. Mangano (INAF-IASFPA), A. Melandri
(INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), J.A.
Kennea (PSU), M.C. Stroh (PSU), A.P. Beardmore (U. Leicester), P.A.
Evans (U. Leicester) and V. D'Elia report on behalf of the Swift-XRT
team:

We have analysed 9.0 ks of XRT data for GRB 121102A (D'Elia  et al. GCN
Circ. 13938), from 53 s to 18.8 ks after the  BAT trigger. The data
comprise 203 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 = 270.9009,
-16.9576 which is equivalent to:

RA (J2000): 18 03 36.22
Dec(J2000): -16 57 27.5

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.33 (+0.22, -0.24). At T+111 s  the decay
flattens to an alpha of 1.59 (+0.18, -0.11) before breaking again at
T+696 s to a final decay with index alpha=1.04 (+0.08, -0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.95 (+/-0.13). The
best-fitting absorption column is  8.9 (+/-1.0) x 10^21 cm^-2, in
excess of the Galactic value of 5.3 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.74 (+0.23, -0.22)
and a best-fitting absorption column of 7.7 (+1.9, -1.6) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.9 x 10^-11 (9.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.7 (+1.9, -1.6) x 10^21 cm^-2
Galactic foreground: 5.3 x 10^21 cm^-2
Excess significance: 2.4 sigma
Photon index:      1.74 (+0.23, -0.22)

If the light curve continues to decay with a power-law decay index of
1.04, the count rate at T+24 hours will be 2.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.7 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00537266.

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


GRB_name: GRB121031A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13944
SUBJECT: GRB 121031A: Enhanced Swift-XRT position
DATE:    12/11/02 15:25:05 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 4059 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 121031A, 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 = 170.77019, -3.51704 which is equivalent
to:

RA (J2000): 11h 23m 4.85s
Dec (J2000): -03d 31' 01.3"

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: GRB121102A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13945
SUBJECT: GRB 121102A: Enhanced Swift-XRT position
DATE:    12/11/02 15:36:39 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 6668 s of XRT Photon Counting mode data and 8 UVOT
images for GRB 121102A, 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 = 270.90101, -16.95788 which is equivalent
to:

RA (J2000): 18h 03m 36.24s
Dec (J2000): -16d 57' 28.4"

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: GRB121031A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13946
SUBJECT: GRB 121031A: Swift-XRT refined Analysis
DATE:    12/11/02 16:48:38 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC) reports on behalf of the Swift-XRT team:

We have analysed 9.2 ks of XRT data for GRB 121031A (D'Elia  et al. GCN
Circ. 13934), from 68 s to 22.6 ks after the  BAT trigger. The data
comprise 276 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN. Circ 13935, 13944).

The late-time light curve (from T0+4.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.86 (+/-0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.03 (+/-0.08). The
best-fitting absorption column is  4.6 (+0.4, -0.3) x 10^21 cm^-2, in
excess of the Galactic value of 4.0 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.33 (+/-0.10) and a
best-fitting absorption column of 5.2 (+/-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 (9.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.2 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 4.0 x 10^20 cm^-2
Excess significance: 18.5 sigma
Photon index:      2.33 (+/-0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00537195.

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


GRB_name: GRB121031A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13947
SUBJECT: GRB 121031A: Swift/UVOT Upper Limits
DATE:    12/11/02 18:26:47 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. 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 121031A
70 s after the BAT trigger (D'Elia et al., GCN Circ. 13934).
No optical afterglow consistent with the enhanced XRT position
(Goad et al., GCN Circ. 13944) 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            70          220          147         >19.9
white             5366         7002          393         >20.5
v                 5776        11730          787         >19.4
b                 5161        18152          492         >20.0
u                16939        17239          295         >19.5
w1                4751        16932         1279         >20.5
m2                4545        22572         1870         >21.1
w2                5572        11120         1082         >20.8

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: GRB121102A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13948
SUBJECT: GRB 121102A: Swift/UVOT Upper Limits
DATE:    12/11/02 18:48:01 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. 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 121102A
58 s after the BAT trigger (D'Elia et al., GCN Circ. 13938).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 13945) 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            58          207          147         >20.1
u_FC               270          519          246         >19.6
white               58        24618         2113         >21.4
v                 4994        17253         1278         >20.0
b                 5814        23858         2022         >21.4
u                  270        22945         1524         >20.9
w1                5404        18848         1066         >20.8
m2                5200        18158         1279         >21.1
w2                4789        13077         1073         >21.2

The magnitudes in the table are not corrected for the high Galactic extinction
due to the reddening of E(B-V) = 1.48 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121031A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13949
SUBJECT: GRB 121031A, Early peak observed with Swift-BAT
DATE:    12/11/03 02:06:03 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

GRB 121031A, Early peak observed with Swift-BAT
  
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/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):


With an additional data set from T-240 to T-61 sec, we report further
analysis of BAT GRB 121031 (trigger #537195) (D'Elia, et al., GCN Circ.
13934).  In an earlier circular (Barthelmy, et al., GCN Circ. 13936) we
described the second of two equal-sized peaks from this burst.  BAT
triggered on that second peak.  The earlier peak occurred during a pre-
planned slew maneuver, and its time interval was not covered by the data
available at the time the circular was produced.

The entire burst had two large peaks at T-190 and T0 that were about the
same in flux, duration, and shape.  Each was a FRED about 60 seconds long as
seen in BAT.  There was a small peak at T-50 sec of about 5 seconds duration.
For the entire burst, T90 (15-350 keV) was 226 +- 19 sec (estimated error
including systematics).
  
The time-averaged spectrum from T-209.0 to T+98.3 sec is best fit by a
simple power-law model.  The power law index of the time-averaged spectrum
is 1.50 +- 0.05.  The fluence in the 15-150 keV band is
7.8 +- 0.2 x 10^-06 erg/cm2.  The 1-sec peak photon flux measured from
T-190.72 sec in the 15-150 keV band is 2.4 +- 0.2 ph/cm2/sec.  All the
quoted errors are at the 90% confidence level.


GRB_name: GRB121028A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13950
SUBJECT: GRB 121028A: Swift/UVOT Upper Limits
DATE:    12/11/05 16:58:22 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and R. L. C. Starling (U Leicester) report on
behalf of the Swift/UVOT team.

The Swift/UVOT began settled observations of the field of
GRB 121028A 133s after the BAT trigger (Starling et al.,
GCN Circ. 13913).  Data summed from the first and second orbits
do not reveal a source at the enhanced position of the X-ray
afterglow (Evans et al., GCN Circ. 13918).

The 3-sigma upper limits for the finding chart (fc) and
summed exposures are reported below:

FILTER     T_start(s)  T_stop    Exposure     Mag/3UL
========================================================
white (fc)   133        283        147        >19.96
white        877       7754        540        >21.07
v           6528       6727        196        >18.94
b           2713       2758         44        >19.10
u            345        595        245        >19.43
u           7143       7343        196        >19.68
uvw1        6938       7138        196        >19.61
uvw2        7761       7961        196        >19.90
=======================================================

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 1.41 (Schlegel et al., 
1998, ApJS, 500, 525). The photometry is on the UVOT photometric
system described in Breeveld et al. 2011 (AIP Conf. Proc. 1358, 373) 


GRB_name: GRB121031A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13951
SUBJECT: GRB 121031A: Fermi GBM detection
DATE:    12/11/07 03:29:06 GMT
FROM:    Adam Goldstein at Fermi-GBM/UAH  <adam.m.goldstein@msfc.nasa.gov>

A. Goldstein (UAH) and C.A. Meegan (USRA) report on behalf of the Fermi GBM Team:

"At 22:47:15.27 UT on 31 October 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121031A (trigger 373416438 / 121031949).
which was also detected by the Swift/BAT (V. D'Elia et al. 2012, GCN 13934).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 85 degrees.
This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of two main pulses separated by a
long quiescent period with a total burst duration (T90) of about 
242 s (50-300 keV) with a possible soft tail out to about T0+500 s. 
The time-averaged spectrum from T0=-47 s to T0+297 s is adequately fit 
by a power law function with an exponential high-energy cutoff.  The 
power law index is -0.87 +/- 0.07 and the cutoff energy, parameterized a
as Epeak, is 142.3 +/- 10.8 keV

The event fluence (10-1000 keV) in this time interval is 
(1.99 +/- 0.09)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.6 s in the 8-1000 keV band is 7.4 +/- 0.7 ph/s/cm^2.

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


GRB_name: GRB121108A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13952
SUBJECT: GRB 121108A: Swift detection of a burst
DATE:    12/11/08 17:59:49 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (MSU), V. D'Elia (ASDC), H. A. Krimm (CRESST/GSFC/USRA),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU)
and E. Sonbas (NASA/GSFC/Adiyaman Univ.) report on behalf of the Swift
Team:

At 17:47:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121108A (trigger=537921).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 83.186, +54.491 which is 
   RA(J2000) = 05h 32m 45s
   Dec(J2000) = +54d 29' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
peak structure for about 60 seconds, followed by an additional
peak at T+120 s.  The peak count rate was ~1500 counts/sec 
(15-350 keV), at ~28 sec after the trigger. 

The XRT began observing the field at 17:48:33.2 UT, 54.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 83.19368, 54.47191
which is equivalent to:
   RA(J2000)  = 05h 32m 46.48s
   Dec(J2000) = +54d 28' 18.9"
with an uncertainty of 4.3 arcseconds (radius, 90% containment). This
location is 70 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.87
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.96e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 63 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
0.37. 

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


GRB_name: GRB121108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13953
SUBJECT: GRB 121108A: TAROT Calern observatory optical observations
DATE:    12/11/08 18:12:31 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 121108A detected by SWIFT
(trigger 537921) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 33.8s after the GRB trigger
(19.2s after the notice). The elevation of the field increased from
20 degrees above horizon and weather conditions
were good for the first images and became cloudy.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT with a limiting magnitude of:
t0+33.8s to t0+93.8s : R > 15.8

The second image is 90.0s exposure in tracking mode:
t0+417.6s to t0+507.6s : R > 16.5

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

N.B. Galactic coordinates are lon=156.8411 lat=+11.3702
and the galactic extinction in R band is about 1.0 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB121108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13954
SUBJECT: GRB 121108A: MASTER early prompt optical limit
DATE:    12/11/08 19:33:45 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB121108A (Ukwatta et. al. 
GCN13952)  36 sec after notice  time and 54 sec after GRB time at 
2012-11-08 17:48:33.174 UT in two  polarizations. On our first (10s 
exposure) set we haven't found optical transient  within SWIFT  error-box.
The 5-sigma upper limit has been about 15.8 mag
The message may be cited.


GRB_name: GRB121108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13955
SUBJECT: GRB 121108A: Weihai observatory optical observations
DATE:    12/11/08 20:02:23 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), J.-M. Ai, C. Cao, S.-M. Hu (SDU) report:

We observed the field of GRB 121108A (Ukwatta et al., GCN 13952) using
the 1m telescope located at Weihai, Shandong Province, China.
Observations started at 18:10 UT on 2012-11-08 (i.e., 22 mins after
the BAT trigger) and 4x600s exposures in the R filter were obtained.
No optical source was found within the enhanced XRT error circle down
to a limit of R~20.5 mag (3sigma), calibrated with the USNO B1
catalog.


GRB_name: GRB121108A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13956
SUBJECT: GRB 121108A: MITSuME Ishigakijima upper limits
DATE:    12/11/09 01:38:02 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 121108A (Ukwatta et al., GCNC 13952)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2012-11-08 18:29:39 UT (~42 min after the
burst). We did not find any new point source within the XRT circle
(Ukwatta et al., GCNC 13952) 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
------------------------------------------------------
0.06526    19:21:37    5820.0   >22.6  >22.0  >20.0
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13957
SUBJECT: GRB 121108A: Optical observations
DATE:    12/11/09 04:37:07 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

Brajesh Kumar, Sumit Jaiswal and S.B. Pandey (ARIES, Nainital, India, on
behalf 
of larger Indian GRB collaboration).

Swift GRB 121108A (Ukwatta et al., GCN 13952) was observed with the 1.3m
Devasthal Fast Optical Telescope at Nainital. Three images in R_c pass-band
(300s each) were obtained starting at 2012-11-08 19:56:19 (UT).

In the co-added R_c frame (300s x 3), we did not detect any optical source
within the XRT error-box down to a limiting magnitude of ~21 mag.

This massage may be cited.


GRB_name: GRB121108A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13958
SUBJECT: GRB 121108A : Lulin/TRIPOL2 Optical Limits
DATE:    12/11/09 06:41:31 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

C.D. Lee, Y. Urata (NCU), K.Y. Huang (ASIAA)
on behalf of EAFON:

"We imaged the field of GRB 121108A (Ukwatta et al. GCN 13952) with
the Triple Range Imager and POLarimeter 2 (TRIPOL2) attached to the
Lulin 1m telescope. The simultaneous three color observations were
started on 2012-11-08 20:12:18.2 UT (~2.41 hrs after the burst).
There is no new sources in the error region of the X-ray afterglow
reported by Ukwatta et al. (GCN 13952) with three sigma limits of
g~20.6, r~20.5 and i~20.2 mag (at 2.92 hrs after the burst)."


GRB_name: GRB121108A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13959
SUBJECT: GRB 121108A: Enhanced Swift-XRT position
DATE:    12/11/09 07:29:21 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 1705 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 121108A, 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 = 83.19408, +54.47352 which is equivalent
to:

RA (J2000): 05h 32m 46.58s
Dec (J2000): +54d 28' 24.7"

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

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

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


GRB_name: GRB121108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13960
SUBJECT: GRB 121108A: Xinglong TNT upper limit
DATE:    12/11/09 12:22:18 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB121108A ( Ukwatta  et al., GCN 13952 ) 
with Xinglong TNT telescope at  17:49:47 (UT), about 128s after 
the burst.  A series of white and R-band images were obtained. 
No any optical counterpart was found in the X-ray errorbox 
(Beardmore et al., GCN 13959).  The 3 sigma upper limit is about 19.9 
mag in R-band calibrated by USNO B1.0 R2 mag,  at the mean 
time of 58 min after the burst. 

This message may be cited.


GRB_name: GRB121108A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13961
SUBJECT: GRB 121108A, Swift-BAT refined analysis
DATE:    12/11/09 14:24:40 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

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 (AGU), 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 121108A (trigger #537921) (Ukwatta, et al., GCN Circ. 13952).
The BAT ground-calculated position is RA, Dec = 83.216, 54.520 deg
which is
   RA(J2000)  =  05h 32m 51.9s
   Dec(J2000) = +54d 31' 11.2"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.

BAT light curve shows two multi-peak episodes. First one starts
at the trigger time and lasts for about 50 seconds and the
second weak episode starts around T+130 seconds and lasts for about
40 seconds. T90 (15-350 keV) is 89 +- 48 sec (estimated error
including systematics).

The time-averaged spectrum from T-0.15 to T+137.98 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 2.28 +- 0.20.  The fluence in the 15-150 keV band is
9.6 +- 1.2 x 10^-07 erg/cm2. The 1-sec peak photon flux measured
from T+43.18 sec in the 15-150 keV band is 1.6 +- 0.2 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/537921/BA/


GRB_name: GRB121108A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13962
SUBJECT: GRB 121108A: Swift/UVOT Upper Limits
DATE:    12/11/09 18:03:29 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and T. N. Ukwatta (MSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121108A
64 s after the BAT trigger (Ukwatta et al., GCN Circ. 13952).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 13959)
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            64          213          147         >20.9
u_FC               276          526          246         >20.5
white               64         1721          412         >21.3
v                  605         1771          136         >19.6
b                  531         1697          117         >19.9
u                  276         1672          362         >20.6
w1                 655         1814          129         >19.6
m2                1429         1623           39         >19.6
w2                 581         1747          136         >19.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.37 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121108A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13963
SUBJECT: GRB 121108A: Swift-XRT refined Analysis
DATE:    12/11/10 17:14:07 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB) and T. N. Ukwatta (MSU) report on behalf of the
Swift-XRT team:

We have analysed 24 ks of XRT data for GRB 121108A (Ukwatta  et al. GCN
Circ. 13952), from 47 s to 82.6 ks after the  BAT trigger. The data
comprise 129 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 Beardmore
et al. (GCN. Circ 13959).

The light curve (from T0+0.8 ks) can be modelled with a power-law decay
with a decay index of alpha=1.0 (+/-0.1). Flare activity is detected
from T0+100 and T0+200 s after the burst event.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.60 (+/-0.09). The
best-fitting absorption column is  3.6 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.9 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.70 (+0.20, -0.18)
and a best-fitting absorption column of 2.3 (+0.7, -0.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.6 x 10^-11 (6.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+0.7, -0.4) x 10^21 cm^-2
Galactic foreground: 1.9 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.70 (+0.20, -0.18)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00537921.

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


GRB_name: GRB121117A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13967
SUBJECT: GRB 121117A: Swift detection of a burst
DATE:    12/11/17 09:07:42 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. R. Cummings (NASA/UMBC), A. P. Beardmore (U Leicester),
V. D'Elia (ASDC), C. Gronwall (PSU), C. Guidorzi (U Ferrara),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 08:50:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121117A (trigger=538696).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 31.635, +7.379 which is 
   RA(J2000) = 02h 06m 32s
   Dec(J2000) = +07d 22' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 08:51:49.2 UT, 52.2 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT prompt data are not available at this time.  We are waiting for
the full dataset to search for an UVOT counterpart. 

This burst occurred as the Swift spacecraft was approaching the
South Atlantic Anomaly and the source was approaching the
Earth Limb observing constraint.  As a result, only a brief exposure 
under high background conditions is available for the
narrow-field instruments during the first orbit. 

Burst Advocate for this burst is J. R. Cummings (jayc 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: GRB121117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13968
SUBJECT: GRB 121117A: BOOTES-3 early optical upper limit
DATE:    12/11/17 10:42:15 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C. Tello (IAA-CSIC), J. Gorosabel (IAA-CSIC), A.J. Castro-Tirado
(IAA-CSIC),  W. Allen (Vintage Lane Obs.), Ph. Yock and Kuan-Yu Lin
(Auckland Univ.), P. Kubanek (IP AS CR & IAA-CSIC), report on behalf of a
larger collaboration:

"We observed the field of GRB 121117A (Cummings et al., GCNC 13967) ,
detected by Swift/BAT, with the 0.6m Yock-Allen robotic telescope
(BOOTES-3) located in Blenheim, New Zealand. Unfiltered images were
obtained starting 09:04:07UT (13m after the burst, limited by clouds). An
exposure of 30 seconds resulted in a limiting magnitude of 16.0 when
calibrated with the R1Mag value of USNO-B1.0 catalogue stars. Due to
clouds, combining images did not provide a deeper limiting magnitude"


This message may be cited.


GRB_name: GRB121117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13969
SUBJECT: GRB 121117A: ROTSE-III Optical Limits
DATE:    12/11/17 13:05:41 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (U Mich), report on behalf of the ROTSE collaboration: 

 

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 121117A
(Swift trigger 538696; Cummings et al., GCN 13967), producing images
beginning 9.1 s after the GCN notice time. An automated response took the
first image at 08:51:21.1 UT, 24.1 s after the burst, under fair 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). 

 

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle. Individual images have limiting magnitudes
ranging from 14.9-16.4; we set the following specific limits. 

 

start UT       end UT      t_exp(s)   mlim   Coadd?

---------------------------------------------------

08:50:57.0   08:55:57.0         5     15.0     N 

08:51:32.0   08:51:37.0         5     15.0     N 

08:51:43.0   08:51:48.0         5     15.4     N 

08:51:55.0   08:52:00.0         5     15.2     N 

08:52:07.0   08:52:12.0         5     15.2     N 

08:50:57.0   08:53:04.0        50     16.8     Y 

08:53:18.0   08:57:59.0       200     17.2     Y

 


GRB_name: GRB121117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13970
SUBJECT: GRB 121117A, Swift-BAT refined analysis
DATE:    12/11/17 21:31:41 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
  
Using the data set from T-61 to T+191 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121117A (trigger #538696)
(Cummings, et al., GCN Circ. 13967).  The BAT ground-calculated position is
RA, Dec = 31.617, 7.432 deg which is
    RA(J2000)  =  02h 06m 28.1s
    Dec(J2000) = +07d 25' 55.6"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
  
The mask-weighted light curve shows a single FRED peak.  Swift was close to
the SAA and BAT entered SAA mode about 250 seconds after the trigger.  T90
(15-350 keV) is 30 +- 5 sec (estimated error including systematics).
  
The time-averaged spectrum from T+0.0 to T+158.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.16 +- 0.18.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+7.06 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/538696/BA/


GRB_name: GRB121117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13971
SUBJECT: GRB 121117A: MASTER  prompt optical limit 
DATE:    12/11/18 07:56:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB121117A 47 sec after 
GRB time at 2012-11-17 08:51:43.208 UT. On our first (10s exposure) set we 
haven't found optical transient  within SWIFT error-box (Cummings et 
al., GCN Circ.  13967).

The 5-sigma upper limit has been about 13.7 mag

This is the prompt limit because our observations was done during 
Gamma-ray activity (Cummings et al., GCN Circ.  13970).

The message may be cited.


GRB_name: GRB121117A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13972
SUBJECT: GRB 121117A: Swift-XRT refined Analysis
DATE:    12/11/18 08:37:46 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A.P. Beardmore (U. Leicester) and J. R. Cummings (NASA/UMBC) report on
behalf of the Swift-XRT team:

We have analysed 13 ks of XRT data for GRB 121117A (Cummings  et al.
GCN Circ. 13967), from 41 s to 62.7 ks after the  BAT trigger. The data
comprise 204 s in Windowed Timing (WT) mode (the first 5 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. Using 3463 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 = 31.61064, +7.41954
which is equivalent to:

RA (J2000): 02h 06m 26.55s
Dec(J2000): +07d 25' 10.4"

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.27 (+/-0.04).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.55 (+0.22, -0.19). The
best-fitting absorption column is  8.4 (+7.2, -3.2) x 10^20 cm^-2,
consistent with the Galactic value of 5.2 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 4.2 x 10^-11 (4.7 x
10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      8.4 (+7.2, -3.2) x 10^20 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.55 (+0.22, -0.19)

If the light curve continues to decay with a power-law decay index of
1.27, the count rate at T+24 hours will be 9.9 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.2 x
10^-14 (4.7 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00538696.

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


GRB_name: GRB121117A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13973
SUBJECT: GRB 121117A: Swift/UVOT Observations
DATE:    12/11/18 12:41:31 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 121117A
s after the BAT trigger (Cummings et al., GCN Circ. 13967).
We find an optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 13972) in the initial UVOT white exposure.
The refined UVOT position is (RA,DEC) = 31.61063, 7.41956 (J2000), 
which is equivalent to:

RA (J2000)  =  02:06:26.56
Dec (J2000) =  +07:25:10.5

with an estimated uncertainty of 0.6 arcsec (radius, 90% confidence).

Preliminary magnitudes and 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 (FC)        57            205          146         19.17 +/- 0.10
white             4606        10267         1150         >21.9
v                 3580        11882         1077         >20.3
b                 4400         6037          393         >20.6
u                 4195         5831          393         >20.3
w1                3990         5627          393         >20.3
m2                3785         5421          393         >20.2
w2                4811        11174         1082         >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).


GRB_name: GRB121118A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13975
SUBJECT: IPN Triangulation of GRB 121118A
DATE:    12/11/19 17:34:19 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

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

The long GRB 121118A with a single short bright peak has been observed 
by Konus-Wind, Fermi(GBM: trigger 374939337), INTEGRAL(SPI-ACS), 
Suzaku(WAM), and MESSENGER(GRNS), so far, at about 49734 s UT (13:48:54).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
    ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
     299.379 (19h 57m 31s) +65.654 (+65d 39' 16")
    Corners:
     296.557 (19h 46m 14s) +67.903 (+67d 54' 12")
     297.432 (19h 49m 44s) +66.848 (+66d 50' 53")
     301.756 (20h 07m 01s) +63.386 (+63d 23' 11")
     301.156 (20h 04m 37s) +64.447 (+64d 26' 48")
    ---------------------------------------------
The error box area is 0.91 sq. deg, and its maximum dimension is 5.0 deg 
(the minimum one is 1.1 deg).

This box can be improved.

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


GRB_name: GRB121117A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13976
SUBJECT: GRB 121117A: GROND confirmation of the UVOT afterglow candidate
DATE:    12/11/19 22:35:54 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Klose (both TLS Tautenburg), M. Nardini 
(Universita degli studi di Milano-Bicocca), and J.Greiner (MPE Garching) 
report on behalf of the GROND team:

We observed the field of GRB 121117A (Swift trigger 538696, Cummings et 
al., GCN #13967) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla 
Observatory (Chile).

First-epoch observations started on November 18, 2012, at 00:16 UT, about 
15.5 hrs after the GRB trigger. Second-epoch observations were performed 
the following night. On the first-epoch images we find a faint source 
within the r=1.7 arcsec XRT error circle (Beardmore et al., GCN 13972) at 
coordinates RA(J2000) = 02:06:26.58, Dec. = 07:25:10.2 (+/- 0".3). Within 
the astrometric error this is consistent with the object seen by UVOT in 
the white band during the first 200 seconds after the GRB trigger (Oates 
et al., GCN 13973). For this source we measure the following preliminary 
AB magnitudes:

g' > 24.0,
r' = 23.6 +/- 0.2,
i' = 23.0 +/- 0.2,
z' > 23.1,
J > 21.3,
H > 20.8,
K > 19.5,

calibrated against SDSS and 2MASS field stars. On the second-epoch images 
the object had faded to r'=24.5 +/- 0.2 and i'>24.3, implying that this 
was the GRB afterglow.


GRB_name: GRB121118B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13977
SUBJECT: IPN Triangulation of GRB 121118B (long/intense)
DATE:    12/11/20 19:42:38 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

J. Goldsten, on behalf of the MESSENGER GRNS 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,

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

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

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on
behalf of the AGILE MCAL team,

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

The long-duration, intense GRB 121118B was observed by Konus-Wind,
INTEGRAL (SPI-ACS), MESSENGER (GRNS), Mars Odyssey (HEND), Swift (BAT), 
AGILE (MCAL), and Suzaku (WAM), at about 80826 s UT (22:27:06). The 
burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    171.704 (11h 26m 49s)  -3.059 ( -3d 03' 31")
   Corners:
    172.128 (11h 28m 31s)  -2.327 ( -2d 19' 38")
    170.954 (11h 23m 49s)  -4.797 ( -4d 47' 48")
    171.309 (11h 25m 14s)  -3.726 ( -3d 43' 33")
    172.662 (11h 30m 39s)  -0.850 ( +0d 51' 00")
   ---------------------------------------------
The error box area is 0.4 sq. deg, and its maximum dimension is 4.3 deg
(the minimum one is 1.1 deg, the minimum annulus width is 8.5 arcmin).

This box can be improved.

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


GRB_name: GRB121117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13978
SUBJECT: GRB 121117A: optical upper limit
DATE:    12/11/21 07:21:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU, IKI), D.Varda (ISON), E.Sinyakov (ISON), I. Molotov 
(KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of GRB 121117A (Cummings et al., GCN 13967) with 
ORI-25 telescope of ISON-Blagoveshensk observatory starting on Nov.17 
(UT) 09:05:39. We took several unfiltered exposures within 2 hours after 
the start. We do not detect the OT (Oates et al., GCN 13973) in the XRT 
error circle (Beardmore et al. GCN 13972) in any stacked images. A 
photometry is based on nearby USNO-B1.0 stars (R2):


T_start   T0+,    Filter, exposure, UL (3 sigma)
(UT)      mid (d)         (s)

09:05:39  0.03105 none    80 x 40   18.3
10:05:44  0.07483 none    88 x 40   18.4
09:05:39  0.05397 none   168 x 40   18.9


GRB_name: GRB121118B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13979
SUBJECT: Konus-Wind observation of GRB 121118B 
DATE:    12/11/21 10:33:10 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-duration intense GRB 121118B
(IPN detection and localization: Hurley et al., GCN 13977)
triggered Konus-Wind at T0=80847.239s UT (22:27:27.239)

The light curve shows multiple pulses with increasing amplitude
in the time interval starting at ~60s before KW trigger and ending at ~T0+40s.
The emission is seen up to 9 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB121118_T80847/

As observed by Konus-Wind the burst
had a fluence of (8.5  0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+13.696 s,
of (1.0  0.6)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the triggered part
of the burst (measured T0 to T0+32.512 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.30  0.05,
the high energy photon index beta = -3.05  0.70,
the peak energy Ep = 520  64 keV,
chi2 = 78.4/82 dof.

The spectrum at the maximum count rate (measured T0+8.448 to T0+16.128 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff (CPL) model, for which:
the photon index alpha = -1.18  0.04
and the peak energy Ep = 599  52 keV,
chi2 = 91.4/83 dof.
Fitting this spectrum with the Band function yields the same
alpha and Ep with only an upper limit for beta <-3.0 (90% conf.)

All the quoted results are preliminary.


GRB_name: GRB121117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13980
SUBJECT: GRB 121117A: Optical observations
DATE:    12/11/21 11:24:44 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

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

GRB 121117A (Cummings et al., GCN 13967) field was observed with the 1.3m
Devasthal Fast Optical Telescope at Nainital. Three images in R_c pass-band
(300 sec each) starting at 2012-11-17 14:35:26 (UT) were acquired. In the
co-added R_c frame (300sec x 3), we did not detect the optical source
(Oates et al., GCN 13973) down to a limiting magnitude of ~20.5 mag
(in comparison to nearby USNO- B1 stars).

This massage may be cited.


GRB_name: GRB121108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13981
SUBJECT: GRB 121108A: optical upper limit
DATE:    12/11/21 17:12:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of  the Swift GRB 121108A (Ukwatta et al., GCN 
13952) with  AZT-11 telescope of CrAO observatory  starting on  Nov. 08 
(UT) 18:07:04. We took  several images in R-filter of 180 s exposure. 
Within enhanced XRT afterglow position (Beardmore et al., GCN 13959) we 
do not detect any new object.   A photometry of co-added frame is based 
  on the USNO-B1.0 (R2)  nearby  stars is following:

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

0.02395     R        10x180      n/d         18.9


GRB_name: GRB121123A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13982
SUBJECT: GRB 121123A: Swift detection of a burst with optical counterpart
DATE:    12/11/23 10:17:59 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. A. Helder (PSU), S. D. Barthelmy (GSFC), V. D'Elia (ASDC),
P. A. Evans (U Leicester), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 10:02:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121123A (trigger=539358).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 307.362, -11.860 which is 
   RA(J2000)  =  20h 29m 27s
   Dec(J2000) = -11d 51' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
structure with a duration of about 25 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 10:04:44.3 UT, 123.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 307.3179, -11.8590 which is equivalent to:
   RA(J2000)  = +20h 29m 16.30s
   Dec(J2000) = -11d 51' 32.4"
with an uncertainty of 5.4 arcseconds (radius, 90% containment). This
location is 155 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 1.30e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 131 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 20:29:16.31 = 307.31794
  DEC(J2000) = -11:51:35.4  = -11.85983
with a 90%-confidence error radius of about 0.67 arc sec. This position is 3.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.34 with a 1-sigma error of about  0.17. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.05. 

Burst Advocate for this burst is E. A. Helder (helder AT 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: GRB121123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13983
SUBJECT: GRB 121123A: GMG optical observation
DATE:    12/11/23 12:32:40 GMT
FROM:    Xiao-hong Zhao at Yunnan Obs  <zhaoxiaohong78@gmail.com>

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

We observed the field of GRB 121123A (Helder et al., GCN 13982) with 2.4m Gao-Mei-Gu (GMG) telescope. Observations
started at ~1.5 hrs after the burst. The optical afterglow of this burst was detected. The preliminary magnitude was R~19.2. 
observation is on going.
   
We thank the GMG staff, especially Hong-Yan Gao, and De-Qing Wang for doing these observations.


GRB_name: GRB121123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13984
SUBJECT: GRB 121123A: MASTER-NET  optical limit
DATE:    12/11/23 12:37:39 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

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

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB121123A 100 sec after 
GRB time at 2012-11-23 10:04:21.926 UT.
  On our first (20s exposure) set we haven't found optical transient 
within SWIFT error-box (Helder et. al., GCN13982).
  The 5-sigma upper limit has been about 16.5 mag
  The field was observed at large (more than 70 deg.) zenith distance.
  The message may be cited.


GRB_name: GRB121123A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13985
SUBJECT: GRB 121123A: Fermi GBM observation
DATE:    12/11/23 19:16:43 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

S. Foley (UCD)
reports on behalf of the Fermi GBM Team:

"At 10:06:00.59 UT on 23 November 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located the second emission episode of GRB 121123A
(trigger 375357963 / 121123421) which was also detected by the
Swift/BAT (Helder et al. 2012, GCN 13982,
http://gcn.gsfc.nasa.gov/notices_s/sw00539358000msbx.gif).
The emission detected by GBM is contemporaneous with the UVOT
observation of an afterglow candidate for GRB 121123A reported by
Helder et al.
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 85 degrees.

The GBM light curve consists of a single peak with a long tail
with a duration (T90) of about 102 s (50-300 keV).
The time-averaged spectrum from T0+3.1 s to T0+106.5 s is
well fit by a Band function with Epeak = 85 (+/-3) keV,
alpha = -0.25 (+/-0.09), and beta = -3.0 (+0.2/-0.3).

The event fluence (10-1000 keV) in this time interval is
(2.20 +/- 0.08)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+32.6 s in the 10-1000 keV band
is 4.00 +/- 0.25 ph/s/cm^2.


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


GRB_name: GRB121123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13986
SUBJECT: GRB 121123A: NOT optical observations
DATE:    12/11/23 21:31:18 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu, T. Kruehler, D. Malesani (DARK/NBI), G. Leloudas (OKC Stockholm
and DARK/NBI) I. Ilyin (AIP), J. Clasen (NOT), P. Jakobsson (U.
Iceland), J. P. U. Fynbo (DARK/NBI) report on behalf of a larger
collaboration:

We observed the field of GRB 121123A (Helder et al., GCN 13982) using
the 2.5m Nordic Optical Telescope (NOT) equipped with StanCam.
Observations started at 20:03:43 UT on 2012-11-23 (i.e., 9.972 hr
after the BAT trigger) and 5x300s R-band frames were obtained with
mid-time of 10.218 hr post-trigger.

The afterglow is clearly detected in the stacked image at coordinates

R.A.(J2000)= 20:29:16.289
Dec.(J2000)=-11:51:35.87

with R=19.65+/-0.03 mag, calibrated with the #0781-0714632 star
(R1=R2=17.17 mag with a scatter of 0.3 mag) in the USNO B1 catalog.

We note that our measurement is only modestly fainter than the one
reported by Zhao et al. (GCN 13983) at 1.5 hr after the BAT trigger,
indicating a shallow decay or an irregular light curve.


GRB_name: GRB121123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13987
SUBJECT: GRB 121123A: BOOTES-4 and IAC80 optical observations
DATE:    12/11/23 22:40:22 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

S. Guziy (Mykolaiv Nat. Univ.), R. Sanchez-Ramirez (IAA-CSIC), L.
Monteagudo Narvion (IAC), O. Lara, M. Jelinek (IAA-CSIC), P. Kubanek (IP
AS CR), Y. Fan, X. Zhao, J. Bai, C. Wang, Y. Xin (Yunnan National
Astronomical Observatory), Chenzhou Cui (Beijing National Astronomical
Observatory), R. Cunniffe, A.J. Castro-Tirado, J.C. Tello and J. Gorosabel
(IAA-CSIC), on behalf of a larger collaboration, report:

We have observed the GRB 121123A optical afterglow (GCN 13982, Helder et
al.) with the 0.6m BOOTES-4/MET robotic telescope at the Lijiang
Astronomical Observatory (China) and with the 0.82m IAC80 telescope
(Tenerife, Spain). The afterglow is detected as follows:

   Tel.  Date Nov  To-Tgrb Texp  Filter  Mag(Vega)
         UT-start   (hr)    (s)
 --------------------------------------------------------
  BOOTES-4 23.5196  2.43  5x120    r   18.87 +/- 0.15
  BOOTES-4 23.5711  3.66  5x120    r   19.01 +/- 0.15
  IAC80    23.7853  8.80  4x300    I   18.90 +/- 0.12

Our measurements confirm the shallow decay reported by Xu et al. (GCN 13986).


GRB_name: GRB121123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13988
SUBJECT: GRB 121123A: optical observations
DATE:    12/11/24 01:50:55 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAO MSI, IKI), A. Stepura (UAFO), A. Matkin (UAFO),  D. 
Erofeev (UAFO), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf 
of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 121123A (Helder et al., GCN 
13982) with VT-50 (0.5-m) telescope and GAS-250 of UAFO/ISON-Ussuriysk 
observatory starting on Nov. 23 (UT) 10:10:15, i.e. 6 minutes after 
burst trigger. We took several unfiltered images of 30 s. We do not 
detect detect afterglow (Helder et al., GCN 13982; Zhao et al., GCN 
13983) in a stacked images. Preliminary photometry of a stacked image 
obtained with VT-50 is based on USNO-B1.0 stars (R2):

T_start  T0+,    Filter, exposure, UL (3 sigma)
(UT) mid (d)     (s)

10:10:15 0.02793 none    90x30     18.1


GRB_name: GRB121123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13989
SUBJECT: GRB 121123A: Swift-XRT refined Analysis
DATE:    12/11/24 02:17:12 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), 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 E.A. Helder report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 121123A (Helder  et al. GCN
Circ. 13982), from 129 s to 23.8 ks after the  BAT trigger. The data
comprise 669 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
307.3183, -11.85898 which is equivalent to:

RA (J2000): 20 29 16.39
Dec(J2000): -11 51 32.3

with an uncertainty of 3.5 arcsec (radius, 90% confidence).

The late-time light curve (from T0+4.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.50 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.448 (+0.023, -0.022). The
best-fitting absorption column is  8.9 (+/-0.6) x 10^20 cm^-2, in
excess of the Galactic value of 4.0 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.97 (+/-0.11) and a
best-fitting absorption column of 5.8 (+2.3, -1.8) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (4.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.8 (+2.3, -1.8) x 10^20 cm^-2
Galactic foreground: 4.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.97 (+/-0.11)

If the light curve continues to decay with a power-law decay index of
0.50, the count rate at T+24 hours will be 0.051 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-12 (2.1 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00539358.

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


GRB_name: GRB121123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13990
SUBJECT: GRB 121123A: Swift-BAT refined analysis
DATE:    12/11/24 02:20:12 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), E. A. Helder (PSU),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), 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 121123A (trigger #539358)
(Helder, et al., GCN Circ. 13982).  The BAT ground-calculated position is
RA, Dec = 307.334, -11.873 deg, which is 
   RA(J2000)  =  20h 29m 20.2s 
   Dec(J2000) = -11d 52' 24.3" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.
 
The mask-weighted light curve shows the burst starting off at a weak level
at ~T-90 sec, with the triggering peak at ~T+10 sec, then a level period
until ~T+200 sec with the onset of a large FRED peak extending out
to ~T+700 sec.  T90 (15-350 keV) is 317 +- 14 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-6.34 to T+419.00 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.96 +- 0.20, 
and Epeak of 65.0 +- 5.1 keV (chi squared 45.4 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.5 +- 0.1 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+232.56 sec in the 15-150 keV band is
2.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.78 +- 0.04 (chi squared 101.58 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/539358/BA/


GRB_name: GRB121123A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13991
SUBJECT: GRB 121123A: Enhanced Swift-XRT position
DATE:    12/11/24 02:23:43 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 12254 s of XRT Photon Counting mode data and 15 UVOT
images for GRB 121123A, 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 = 307.31813, -11.86023 which is equivalent
to:

RA (J2000): 20h 29m 16.35s
Dec (J2000): -11d 51' 36.8"

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: GRB121123A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13992
SUBJECT: GRB 121123A: GROND observations
DATE:    12/11/24 03:38:49 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of GRB 121123A (Swift trigger 539358; Helder et al.,
GCN 13982; Fermi trigger 375357963 / 121123421; Foley et al., GCN 13985)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPG/ESO telescope at La Silla Observatory
(Chile).

Observations started at 00:20 UT on Nov 24, about 15 hours after the GRB
trigger. They were performed at an average seeing of 1.3" and at an
average airmass of 1.9. The optical afterglow (Helder et al., GCN 13982;
Zhao et al., GCN 13983; Xu et al., GCN 13986; Guziy et al., GCN 13987) is
clearly detected in all bands. Based on 1500 s of total exposures in
g'r'i'z' and 1200 s in JHK, we measure the following preliminary AB
magnitudes at a midtime of 15.25 hrs after the burst:

g' = 20.8 +/- 0.1,
r' = 20.3 +/- 0.1,
i' = 19.9 +/- 0.1,
z' = 19.8 +/- 0.1,
J  = 19.2 +/- 0.1,
H  = 18.9 +/- 0.1,
K  = 18.6 +/- 0.2,

calibrated against GROND zeropoints and 2MASS stars. The SED can be fit
with a power law with a slope of beta = 1.2 +/ -0.1 and a g-band affected
by a dropout with a redshift of z = 2.7 +/- 0.3, taking into acount a
Galactic reddening along the line of sight of E_(B-V)= 0.05 mag (Schlegel
et al.1998). We note that the data can also be fit with a modest host
extinction and no dropout-affected g-band. At present we cannot solve this
ambiguity.


GRB_name: GRB121125A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13993
SUBJECT: GRB 121125A: Swift detection of a burst with optical counterpart
DATE:    12/11/25 08:43:43 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. N. Barlow (PSU), S. D. Barthelmy (GSFC), D. Grupe (PSU),
E. A. Helder (PSU) and C. J. Mountford (U Leicester) report on behalf
of the Swift Team:

At 08:32:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121125A (trigger=539563).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 228.520, +55.322 which is 
   RA(J2000) = 15h 14m 05s
   Dec(J2000) = +55d 19' 18"
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 70 sec.  The peak count rate
was ~4600 counts/sec (15-350 keV), at ~34 sec after the trigger. 

The XRT began observing the field at 08:33:34.1 UT, 66.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 228.52496, 55.31330 which
is equivalent to:
   RA(J2000)  = 15h 14m 05.99s
   Dec(J2000) = +55d 18' 47.9"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 32 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.27 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.7
(+2.20/-1.89) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.27e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 75 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 15:14:06.54 = 228.52724
  DEC(J2000) = +55:18:48.0  =  55.31332
with a 90%-confidence error radius of about 0.74 arc sec. This position is 1.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.19 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is B. N. Barlow (bnb2 AT 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: GRB121125A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13994
SUBJECT: GRB 121125A: MASTER-NET  optical observations
DATE:    12/11/25 09:52:04 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

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

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


  MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB121125.36 44 sec after 
GRB time at 2012-11-25 08:33:11.383 UT. On our first (10s exposure) set we 
haven't found optica
l transient  within SWIFT error-box (Barlow et al., GCN Circ 13993).
Unfortunately notice alert have come immodiatly after sunset when 
telescope prepearing
calibration images.

  So  5-sigma upper limit of the first images has been about 13.8 mag that 
is not very good.
We see OT (Barlow et al., GCN Circ 13993) on UVOT position on the next 
images with 14.5 mag limit (UT_start = 2012-11-25 08:34:34, 127 
s after trigger time, exp_time = 30s).

  We note that there is 16.5 mag star 9 arcsec from UVOT OT coordinates.
The observations is continuated.

  The message may be cited.


GRB_name: GRB121125A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13995
SUBJECT: GRB 121125A: LOAO Observation
DATE:    12/11/25 16:47:57 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

M. Im (CEOU/SNU) and Y. Urata (NCU) on behalf of EAFON.

  We observed the field of GRB 121125A 
(Barlow et al., GCN 13993) in B and R filters using 
the 1-m telescope at Mt. Lemmon observatory in Arizona, US.

  The observation started at 2012-11-25 12:24:27 UT, 
or about 3.87 hours after the BAT alert, and continued for
about 30 min. We identify an object in stacked images of 
both B and R at

  RA=15:14:06.586, Dec=55:18:47.95 with rms error of 0.6".

  This is consistent with the UVOT coordinate of
the afterglow candidate reported in Barlow et al.
  The object has R-band magnitude of R = 19.29 +- 0.14 mag,
calibrated against R2 magnitude (16.13 mag) of a USNO-B1 star 
at RA=15:14:07.14, Dec=+55:18:40.30. Combined with the result
from Yurkov et al. (GCN 13994) and Barlow et al., our result
reveals a fading behavior of the object, thus we identify 
the object to be the afterglow of GRB 121125A.

  We thank the LOAO operator, Jae-Hyuk Yoon for performing 
the observation.


GRB_name: GRB121125A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13996
SUBJECT: GRB 121125A: Swift-BAT refined analysis
DATE:    12/11/25 20:28:47 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), B. N. Barlow (PSU), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121125A (trigger #539563)
(Barlow, et al., GCN Circ. 12993).  The BAT ground-calculated position is
RA, Dec = 228.519, 55.318 deg, which is 
   RA(J2000)  =  15h 14m 04.6s 
   Dec(J2000) = +55d 19' 03.5" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 80%.
 
The mask-weighted light curve shows two clusters of overlapping peaks
that start at ~T-7 sec, peaks at ~T+37 sec, and ends at ~T+100 sec.
T90 (15-350 keV) is 52.2 +- 4.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.31 to T+77.64 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.52 +- 0.06.  The fluence in the 15-150 keV band is 4.7 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+36.56 sec in the 15-150 keV band
is 2.9 +- 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/539563/BA/


GRB_name: GRB121125A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13997
SUBJECT: GRB 121125A: Fermi GBM Observation
DATE:    12/11/25 21:08:30 GMT
FROM:    Sinead McGlynn at Excellence Cluster/TUM  <smcglynn@tum.de>

Sinead McGlynn (MPE/TUM)
reports on behalf of the Fermi GBM Team:

"At 08:32:29.63 UT on 25 Nov 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121125A (trigger 375525152/121125356), which was also detected by the Swift/BAT
(Barthelmy et al. 2012, GCN 13996). The GBM on-ground location is consistent with the Swift/UVOT afterglow candidate position (Barlow et al. 2012, GCN 13993).

The on-ground calculated location, using the GBM trigger
data, is RA = 229.30, DEC = +54.14 (J2000 degrees,
equivalent to 15h 17m 12s, 54d 08' 24"), with an uncertainty
of 2.22 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 37 degrees.

The GBM light curve shows/consists of several pulses
with a duration (T90) of about 50 s (50-300 keV).
The time-averaged spectrum from T0-11.3 s to T0+49.1 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.38 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 196 +/- 26 keV.

The event fluence (10-1000 keV) in this time interval is
(9.5 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+32 s in the 10-1000 keV band
is 4.2 +/- 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: GRB121125A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13998
SUBJECT: GRB 121125A: Enhanced Swift-XRT position
DATE:    12/11/25 22:06:30 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 4397 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 121125A, 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 = 228.52806, +55.31335 which is equivalent
to:

RA (J2000): 15h 14m 6.73s
Dec (J2000): +55d 18' 48.1"

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: GRB121125A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  13999
SUBJECT: GRB 121125A: Swift-XRT refined Analysis
DATE:    12/11/25 23:43:03 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 B.N. Barlow report on behalf of the Swift-XRT team:

We have analysed 9.6 ks of XRT data for GRB 121125A (Barlow  et al. GCN
Circ. 13993), from 73 s to 23.5 ks after the  BAT trigger. The data
comprise 196 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN. Circ 13998).

The late-time light curve (from T0+4.0 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.28 (+/-0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.02 (+0.10, -0.09). The
best-fitting absorption column is  1.49 (+0.23, -0.22) x 10^21 cm^-2,
in excess of the Galactic value of 1.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.14 (+0.13, -0.12)
and a best-fitting absorption column of 1.02 (+0.28, -0.26) x 10^21
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.02 (+0.28, -0.26) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^20 cm^-2
Excess significance: 5.6 sigma
Photon index:      2.14 (+0.13, -0.12)

If the light curve continues to decay with a power-law decay index of
1.28, the count rate at T+24 hours will be 0.013 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.2 x
10^-13 (5.7 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00539563.

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


GRB_name: GRB121118B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14000
SUBJECT: GRB 121118B: Suzaku WAM observation of the prompt emission
DATE:    12/11/26 03:04:30 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

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


The long, IPN localized GRB 121118B: (Hurley et al., GCN 13977)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 22:27:6.662 UT (=T0).

The observed light curve shows a multi-peaked structure starting at
T0-30 s, ending at T0+70 s, with a duration (T90) of about 50
seconds. The fluence in 100 - 1000 keV was 4.52(-1.27 +0.85) x 10^-5
erg/cm^2. The 1-s peak flux measured from T0-0.5s was 8.48(-0.64 +0.56)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-30s to
T0+70s is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 1.39(-0.67 +0.50), and
Epeak 450(-224 +121) keV (chi^2/d.o.f. = 28.5/22).

All the quoted errors are at statistical 90% confidence level.
Due to the brightness of this burst, a 3% systematic error was added
for low energy channels.

The light curves for this burst will be available at:

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


GRB_name: GRB121122A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14001
SUBJECT: IPN Triangulation of GRB 121122A (long/intense)
DATE:    12/11/26 20:19:40 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

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

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

A long-duration, intense GRB 121122A with strong spectral evolution was 
observed by Konus-Wind, Fermi (GBM: trigger 375311695), INTEGRAL 
(SPI-ACS), MESSENGER (GRNS), Swift (BAT), and Suzaku (WAM), at about 
76493 s UT (21:14:53). The burst was outside the coded field of view of 
the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
     35.262 (02h 21m 03s) +45.139 (+45d 08' 21")
   Corners:
     50.638 (03h 22m 33s) +46.661 (+46d 39' 39")
     46.318 (03h 05m 16s) +47.134 (+47d 08' 01")
     25.058 (01h 40m 14s) +40.194 (+40d 11' 39")
     27.431 (01h 49m 44s) +41.325 (+41d 19' 31")
   ---------------------------------------------
The error box area is 6.9 sq. deg, and its maximum dimension is 19.6 deg 
(the minimum one is 2.1 deg, the minimum annulus width is 0.2 deg).

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB121122_T76497/IPN/

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


GRB_name: GRB121125A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14002
SUBJECT: GRB 121125A: Swift/UVOT Detection
DATE:    12/11/26 22:17:56 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and B. N. Barlow (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121125A
75 s after the BAT trigger (Barlow et al., GCN Circ. 13993).
A source consistent with the XRT position
(Goad et al., GCN Circ. 13998) is detected in the initial UVOT exposures.

The refined UVOT position is:
    RA  (J2000) =  15:14:06.58 = 228.52740 (deg.)
    Dec (J2000) = +55:18:48.0  =  55.31332 (deg.)
with an estimated uncertainty of 0.50 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               75          225          147         16.35 +/- 0.03
v                 4693         4892          197         19.11 +/- 0.19
b                 4076         4276          197         19.31 +/- 0.13
u                  288          423          134         16.21 +/- 0.04
w1                5103         5302          197         20.06 +/- 0.32
m2                4897        11750         1082        >21.9
w2                4488         6123          393        >21.6

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: GRB121123A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14003
SUBJECT: GRB 121123A: Swift/UVOT Observations
DATE:    12/11/26 22:25:09 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and
E. A. Helder (PSU)
report on behalf of the Swift/UVOT team:

     The Swift/UVOT began settled observations of the field of GRB
121123A starting 131 s after the BAT trigger (Helder et al., 2012,
GCNC 13982).  The refined UVOT position is

     RA (J2000)  20:29:16.30  =  307.31792 (deg)
    Dec (J2000) -11:51:35.6   =  -11.85989 (deg)

with an estimated uncertainty of 0.44 arcsec (radius, 90% confidence,
statistical + systematic).  We observe a slow decay of the optical
afterglow, consistent with that reported by Xu et al., (2012, GCNC
13986).  The afterglow is weakly detected in white at approximately 40
ks after the BAT trigger.  However, the UVOT photometry is affected by
a bright (B ~ 14 mag) star (USNO B1.0 0781-0714667) located
approximately 22 arcsec north of the afterglow, so the late-time
behavior of the optical afterglow's light curve requires further
analysis.  Preliminary UVOT photometry, and 3-sigma upper limits, for
the afterglow are presented below.

------------------------------------------------------
Filter      TSTART     TSTOP    Exposure     Mag   Err
------------------------------------------------------
white (fc)     131       281         147   19.43  0.15
u (fc)         289       539         246   19.35  0.23
white (fc)     869      1019         147   19.13  0.12
------------------------------------------------------
v              619      1070          58   18.29  0.33
b              546      1169          58   19.12  0.29
u              695      1145          39   18.58  0.32
uvw1           669    18,011        2137  >21.5
uvm2           645    17,104        1376  >21.3
uvw2           595    22,980        1376  >21.5
white          570       590          19  >19.7
------------------------------------------------------

    The detection in the UVOT u band, combined with the non-detection
in the UVOT uvw1 band, is consistent with GRB 121123A having a
redshift of approximately 1.5 < z < 3.4.

    The quoted magnitudes and upper limits have not been corrected for
the Galactic extinction along the line of sight to this burst of
E_{B-V} = 0.05 mag (Schlafly et al. 2011, ApJS, 737, 103).  The
photometry is in the UVOT photometric system (Breeveld et al. 2011,
AIP Conf. Proc. 1358, 373).


GRB_name: GRB121117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14004
SUBJECT: GRB 121117A: Terskol obseravtions
DATE:    12/11/27 08:45:18 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

I. V. Sokolov, A. V. Sergeev, M. V. Andreev (TB INASAN, Russia),
V. B. Petkov (BNO INR RAS, Russia),
A. S. Moskvitin, V. N. Komarova (SAO RAS, Russia), on behalf of larger GRB
collaboration report:

GRB 121117A (Cummings et al., GCN 13967) field was observed with the 2-m
telescope
at the Mt. Peak Terskol since 6 hours after the trigger (2012-11-17,
14:50:02 -- 15:05:20 UT).
We obtained 3 x 300 sec. images in R and did not detect any source
(reported in Oates et al.,
GCN 13973 and in Nicuesa Guelbenzuet al., GCN 13976) down to a limiting
magnitude of ~21.1 mag
as well as the Indian team observing at the same time (Kumar et al.,  GCN
13980).
Calibrations were done by the same nearby USNO-B1 stars as in Volnova et
al., GCN 13978.
The magnitude was not corrected for the Galactic extinction E(B-V) = 0.06.


GRB_name: GRB121122A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14005
SUBJECT: Konus-Wind observation of GRB 121122A
DATE:    12/11/27 12:04:59 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-duration intense GRB 121122A
(IPN detection and localization: Hurley et al., GCN 14001)
triggered Konus-Wind at T0=76497.048s UT (21:14:57.048)

The burst light curve is formed by three overlapped FRED-like pulses;
a total duration of the burst is ~12 s.
A behavior of hardness ratios between the instrument's light curves
in different energy bands suggests a strong hard-to-soft spectral evolution.
The emission is seen up to 7 MeV.

As observed by Konus-Wind, the burst
had a fluence of (4.1  0.1)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.728 s,
of (1.0  0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst (measured T0 to T0+15.616 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.53  0.05,
the high energy photon index beta = -3.3  0.2,
the peak energy Ep = 183  4 keV,
chi2 = 106/91 dof.

The spectrum at the maximum count rate (measured T0 to T0+1.792 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = +0.58  0.12,
the high energy photon index beta = -3.0  0.2,
the peak energy Ep = 308  13 keV,
chi2 = 69.4/60 dof.

The time-resolved spectral analysis reveals
a steady decrease of Ep from ~700 keV to ~100 keV
during the first 8 seconds of the burst,
which can be described by a power law with
the temporal decay index of ~0.6 .

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB121122_T76497/

All the quoted results are preliminary.


GRB_name: GRB121123A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14006
SUBJECT: GRB 121123A: Suzaku WAM observation of the prompt emission
DATE:    12/11/27 15:03:15 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

T.Yasuda, M. Tashiro, Y. Terada, W. Iwakiri, K. Takahara,
M. Asahina, S. Kobayashi, A. Sakamoto, Y. Ishida,
H. Ueno, S. Sugimoto (Saitama U.),
M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, Y. E. Nakagawa (Waseda U.),
Y. Hanabata, T. Kawano, K. Takaki, R. Nakamura, Y.Tanaka, M. Ohno,
Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), M. Kokubun, T.
Takahashi (ISAS/JAXA),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The long GRB 121123A (Helder et al., GCN 13982; Zhao et al., GCN 13983;
Yurkov et al., GCN 13984; Foley, GCN 13985; Xu et al., GCN 13986;
Guziy et al., GCN 13987; Volnova et al., GCN 13988; Melandri et al.,
GCN 13989; Barthelmy et al., GCN 13990; Evans et al., GCN 13991;
Schmidl et al., GCN 13992) was detected by the the Suzaku Wide-band 
All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV
at 10:06:00 UT (=T0).

The observed light curve shows a single peak followed by a long weak
tail seen up to T0+74 s with a duration (T90) of about 73 seconds.
The fluence in 100 - 1000 keV was 7.72 (+0.44/-7.11) x 10-6 erg/cm^2.
The 1-s peak flux measured from T0+33 s was
0.74 (+0.54/-0.34) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0+1 s to
T0+74 s is well fitted by a single power-law with a photon index
of 3.29 (+0.64/-0.50) (chi2/d.o.f = 4.7/11).

The light curves with 1-sec time resolution for this burst will be
appeared at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB121128A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14007
SUBJECT: GRB 121128A: Swift detection of a burst with an optical counterpart
DATE:    12/11/28 05:18:00 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester),
M. H. Siegel (PSU) and M. Stamatikos (OSU/NASA/GSFC) report on behalf
of the Swift Team:

At 05:05:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121128A (trigger=539866).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 300.583, +54.321 which is 
   RA(J2000) = 20h 02m 20s
   Dec(J2000) = +54d 19' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 40 sec.  The peak count rate
was ~20,000 counts/sec (15-350 keV), at ~20 sec after the trigger. 

The XRT began observing the field at 05:06:54.3 UT, 77.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 300.60067, 54.30060 which
is equivalent to:
   RA(J2000)  = 20h 02m 24.16s
   Dec(J2000) = +54d 18' 02.2"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 82 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 2.08
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.58e-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. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 20:02:24.01 = 300.60004
  DEC(J2000) = +54:17:59.2  =  54.29977
with a 90%-confidence error radius of about 0.61 arc sec. This position is 5.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.11 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.31. 

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: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14008
SUBJECT: GRB 121128A: FTN optical afterglow confirmation
DATE:    12/11/28 07:11:25 GMT
FROM:    Jure Japelj at U. of Ljubljana,Slovenia  <jure.japelj@fmf.uni-lj.si>

J. Japelj (U. Ljubljana), N.R. Tanvir (U. Leicester), C. Guidorzi
(U. Ferrara) report on behalf of a large collaboration report:

The 2-m Faulkes Telescope North automatically began observing
GRB 121128A (Oates et al. GCN Circ. 14007) on November 28 2012,
05:07:51 UT corresponding to 134 seconds post burst trigger. We confirm
the presence of a fading source at the optical afterglow candidate position
reported by Oates et al. GCN Circ. 14007. In the first 10 s exposure,
we measure a preliminary R magnitude of 14.5 +- 0.1, calibrated against
nearby USNO-B1 stars.

The candidate was discovered automatically by the LT-TRAP pipeline.


GRB_name: GRB121128A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14009
SUBJECT: GRB 121128A - Gemini North redshift
DATE:    12/11/28 07:46:48 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), T.  Matulonis (Gemini)
report on behalf of a larger collaboration:

We observed the counterpart of GRB 121128A (Oates et al. GCN 14007;
Japelj et al. GCN 14008) with the GMOS-N spectrograph at Gemini-North,
beginning at Nov 28 2012 06:06 UT, approximately 1hr post-burst.
The afterglow is well detected and our provisional reduction shows a
series of absorption lines of AlII, FeII, CIV, SiII, SiIV with a common 
redshift of z=2.20.


GRB_name: GRB121128A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14010
SUBJECT: Konus-Wind observation of GRB 121128A
DATE:    12/11/28 12:12:07 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-duration soft GRB 121128A
(Swift-BAT trigger #539866: Oates et al., GCN 14007)
triggered Konus-Wind at T0=18353.307s UT (05:05:53.307)

The burst light curve shows a multi-peaked structure with
a total duration of ~30 s.
The emission is seen up to 6 MeV.

As observed by Konus-Wind, the burst
had a fluence of (7.0  0.6)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+5.568 s,
of (2.05  0.15)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst (measured T0 to T0+16.640 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.94  0.14,
the high energy photon index beta = -3.36  0.48,
the peak energy Ep = 76  4 keV,
chi2 = 82.6/87 dof.

The spectrum at the maximum count rate (measured T0 to T0+8.848 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = +0.87  0.13,
the high energy photon index beta = -3.32  0.46,
the peak energy Ep = 87  4 keV,
chi2 = 69.4/60 dof.

Assuming the Gemini North redshift of z=2.20 (Tanvir et al., GCN 14009)
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 (8.2  0.7)x10^52 erg,
the isotropic peak luminosity L_iso_max is (7.7  0.6)x10^52 erg/s,
and Ep_rest is (243  13) keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB121128_T18353/

All the quoted results are preliminary.


GRB_name: GRB121128A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14011
SUBJECT: GRB 121128A, Swift-BAT refined analysis
DATE:    12/11/28 14:32:00 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@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), S. R. Oates (UCL-MSSL),
T. Sakamoto (AGU), 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-119 to T+195 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121128A (trigger #539866)
(Oates, et al., GCN Circ. 14007).  The BAT ground-calculated position is
RA, Dec = 300.589, 54.301 deg which is
    RA(J2000)  =  20h 02m 21.3s
    Dec(J2000) = +54d 18' 02.6"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.  The mask-weighted light curve shows a complex,
multi-peaked structure.  The burst began with a faint precursor at ~T-4 sec.
The main emission started at ~T+10 sec, peaked at T+22 sec and continued
until just after T+40 sec, with weak emission extending out to ~T+70 sec.
T90 (15-350 keV) is 23.3 +- 1.6 sec (estimated error including systematics).

The time-averaged spectrum from T-0.00 to T+41.69 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.32 +- 0.18,
and Epeak of 64.5 +- 6.8 keV (chi squared 33.43 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 6.9 +- 0.4 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+21.68 sec in the 15-150 keV band is
12.9 +- 0.4 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.86 +- 0.04 (chi squared 62.32 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/539866/BA/


GRB_name: GRB121128A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14012
SUBJECT: GRB 121128A: Fermi GBM observation
DATE:    12/11/28 14:42:17 GMT
FROM:    Sinead McGlynn at Excellence Cluster/TUM  <smcglynn@tum.de>

Sinead McGlynn (TUM/MPE)
reports on behalf of the Fermi GBM Team:

"At 05:05:50.96 UT on 28 Nov 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121128A (trigger 375771953/121128212)
which was also detected by the Swift/BAT and UVOT
(Oates et al. 2012, GCN 14007).
The GBM on-ground location is consistent with the Swift UVOT position.

The angle from the Fermi LAT boresight is 83 degrees.

The GBM light curve shows two bright pulses
with a duration (T90) of about 17s (50-300 keV).
The time-averaged spectrum from T0-5.1 s to T0+27.6 s is
best fit by a Band function with Epeak = 62.2 +/- 4.6 keV,
alpha = -0.80 +/- 0.12, and beta = -2.41 +/- 0.10.

The event fluence (10-1000 keV) in this time interval is
(1.04 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7.9 s in the 10-1000 keV band
is 17.9 +/- 0.5 ph/s/cm^2.

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


GRB_name: GRB121128A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14013
SUBJECT: GRB 121128A: RAPTOR Detection During Gamma-Ray Emitting Interval
DATE:    12/11/28 16:42:41 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made follow-up observations
of Swift trigger 539866 (Oates, et al., GCN 14007).  Our narrow-field
RAPTOR-S telescope located in Los Alamos, NM, began imaging at 05:06:12.6 UT,
35.4 s after the Swift BAT trigger and during the period that the BAT was
still detecting gamma-ray emission (Palmer, et al., GCN 14011).  Starting
during the gamma-ray emitting interval we detect a brightening counterpart
that ultimately peaks at T+75s with a R-band equivalent magnitude of
approximately 13.9 before beginning to fade.  Our unfiltered images are
calibrated to the USNO-B1 R-band.


GRB_name: GRB121122A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14014
SUBJECT: GRB 121122A: Fermi GBM observation
DATE:    12/11/28 17:15:05 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

George Younes (USRA/NASA/MSFC)
reports on behalf of the Fermi GBM Team:

"At 21:14:52.55 UT on 22 Nov 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located the intense GRB 121122A (trigger 375311695/121122885,
IPN detection and localization: Hurley et al., GCN 14001).

The angle from the Fermi LAT boresight is 159 degrees.

The GBM light curve consists of two overlapping peaks with FRED-like pulses
with a duration (T90) of about 8.2 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+17.4 s is
well fit by a Band function with Epeak = 178 +/- 4 keV,
alpha = -0.68 +/- 0.06 , and beta = -3.1 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(5.46 +/- 0.07)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.7 s in the 10-1000 keV band
is 56 +/- 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: GRB121128A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14015
SUBJECT: GRB 121128A: Enhanced Swift-XRT position
DATE:    12/11/28 20:06:28 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 2286 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 121128A, 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 = 300.60001, +54.29971 which is equivalent
to:

RA (J2000): 20h 02m 24.00s
Dec (J2000): +54d 17' 58.9"

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: GRB121128A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14016
SUBJECT: GRB 121128A: Swift-XRT refined Analysis
DATE:    12/11/28 21:18:04 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
S.R. Oates report on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 121128A (Oates  et al. GCN
Circ. 14007), from 66 s to 41.5 ks after the  BAT trigger. The data
comprise 108 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 14015).

The late-time light curve (from T0+6.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.67 (+0.16, -0.15).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.43 (+/-0.11). The
best-fitting absorption column is  1.2 (+/-0.4) x 10^22 cm^-2, at a
redshift of 2.2, in addition to the Galactic value of 2.1 x 10^21 cm^-2
(Kalberla et al. 2005). The PC mode spectrum has a photon index of 1.99
(+0.10, -0.09) and a best-fitting absorption column of 1.1 (+0.5, -0.4)
x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.1 x 10^-11 (6.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.1 x 10^21 cm^-2
Intrinsic column:    1.1 (+0.5, -0.4) x 10^22 cm^-2 at z=2.2
Photon index:      1.99 (+0.10, -0.09)

If the light curve continues to decay with a power-law decay index of
1.59, the count rate at T+24 hours will be 3.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.3 x
10^-13 (2.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00539866.

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


GRB_name: GRB121128A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14017
SUBJECT: GRB 121128A: Swift/UVOT Detection
DATE:    12/11/28 22:58:50 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 121128A
85 s after the BAT trigger (Oates et al., GCN Circ. 14007). A source consistent 
with the XRT position (Osborne et al., GCN Circ. 14015) is detected in the initial 
white, v, b and u exposures only. The non-detection in the UV filters is consistent 
with the redshift of z=2.2 reported by Gemini North (Tanvir et al., GCN Circ. 14009)

The preliminary UVOT position is:
 RA  (J2000) =  20:02:24.00 = 300.60000 (deg.)
 Dec (J2000) = +54:17:59.1  =  54.29974 (deg.)
with an estimated uncertainty of 0.50 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               85          235          147         16.19 +/- 0.03
v                  629          649           19         17.00 +/- 0.23
b                  554          573           20         17.51 +/- 0.17
u                  298          547          246         17.33 +/- 0.06
w1                 679         2173          175        >19.6
m2                 654         2496          214        >19.6
w2                 605         2447          214        >20.0

The magnitudes in the table are not corrected for the significant Galactic extinction
due to the reddening of E(B-V) = 0.31 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14018
SUBJECT: GRB 121128A: WSRT radio observation
DATE:    12/11/28 23:16:59 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

A.J. van der Horst (University of Amsterdam) reports on behalf
of a large collaboration:

"We observed the position of the GRB 121128A afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at November 28 11.34 to
21.06 UT, i.e. 6.2 - 16.0 hours after the burst (GCN 14007).
We do not detect a radio source at the position of the optical
counterpart (GCN 14007). The three-sigma rms noise in the map around
that position is 69 microJy per beam. The formal flux measurement for
a point source at the position of the optical counterpart is 59 +/- 23 
microJy.

We would like to thank the WSRT staff for quickly scheduling and
obtaining these observations."


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14019
SUBJECT: GRB 121128A: optical observation in Mondy observatory
DATE:    12/11/29 17:50:57 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A.Volnova (SAI MSU), E. Klunko (ISTP), A. Pozanenko (IKI) on behalf of
larger GRB follow up collaboration report:
We observed the field of the Swift GRB 121128A (Oates et al., GCN 14007)
with AZT-33IK telescope of Sayan observatory (Mondy). We took several
images in R-filter of 60 s exposure on Nov. 28, between (UT) 10:27:30 -
13:43:09 under favorable weather conditions. We detected optical afterglow
(Oates et al., GCN 14007; Japelj et al., GCN 14008) in stacked images. A
photometry of some stacked image in the beginning of our observations and
final stacked image is based on nearby USNO-B1.0 stars:
t_start, T0+ (mid), filter, exp., OT, err
(UT)     d                           s

10:46:51 0.24047 R     10x60 19.95 +/- 0.06
13:00:21 0.34123 R     49x40 20.58 +/- 0.07

The photometry is still preliminary.


GRB_name: GRB121125A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14020
SUBJECT: GRB 121125A: optical upper limit
DATE:    12/11/29 17:52:31 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (SAI MSU, IKI), D. Varda (ISON), E. Sinyakov (ISON), I. Molotov
(KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up
collaboration:

We observed the field of GRB 121125A (Barlow et al., GCN 13993) with ORI-25
telescope of ISON-Blagoveshensk observatory starting on Nov.25 (UT)
09:05:39. We took several unfiltered images. We do not detect the OT
(Barlow et al., GCN 13993; Yurkov et al., GCN 13994; Im et al., GCN 13995)
in any combined images. A photometry of stacked image is based on nearby
USNO-B1.0 stars (R2):

T_start T0+, Filter, exposure, UL (3 sigma)
(UT) mid (d) (s)

08:58:19 0.03078 none 52 x 40 15.6


GRB_name: GRB121127A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14021
SUBJECT: IPN Triangulation of GRB 121127A (short/hard)
DATE:    12/11/29 22:05:59 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 on behalf of the Mars Odyssey and MESSENGER GRB teams,

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

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

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

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

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

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

A short-duration, hard spectrum GRB 121127A was observed by Konus-Wind, 
Fermi (GBM: trigger 375746163), INTEGRAL (SPI-ACS), MESSENGER (GRNS), 
Swift (BAT), Mars Odyssey (HEND), and Suzaku (WAM) at about 78960 s UT 
(21:56:00).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   176.438 (11h 45m 45s) -52.414 (-52d 24' 52")
  Corners:
   176.369 (11h 45m 29s) -52.649 (-52d 38' 58")
   176.255 (11h 45m 01s) -52.512 (-52d 30' 44")
   176.507 (11h 46m 02s) -52.179 (-52d 10' 45")
   176.620 (11h 46m 29s) -52.316 (-52d 18' 59")
  ---------------------------------------------
The error box area is 158 sq. arcmin, and its maximum
dimension is 29 arcmin (the minimum one is 9 arcmin; the minimum annulus 
width is 3.6 arcmin).

This box can be improved.

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


GRB_name: GRB121127A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14022
SUBJECT: Konus-Wind observation of GRB 121127A
DATE:    12/11/30 07:37:36 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-duration hard-spectrum GRB 121127A
(IPN localization: Golenetskii at al., GCN 14021)
triggered Konus-Wind at T0=78957.290s UT (21:55:57.290)

The light curve shows a single pulse with a duration of ~0.25 s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB121127_T78957/

As observed by Konus-Wind the burst
had a fluence of (3.8  0.8)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.016 s,
of (2.6  0.6)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured T0 to T0+0.192 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = 0.0  0.3,
the high energy photon index beta = -2.0  0.3,
the peak energy Ep = 600  170 keV,
chi2 = 11/19 dof.

All the quoted results are preliminary.


GRB_name: GRB121128A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14023
SUBJECT: GRB 121128A: MITSuME Akeno Optical upper limits
DATE:    12/11/30 09:17:45 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

T. Yoshii, R. Usui, Y.Aoki, S. Kurita, M. Hayashi,
Y. Saito, Y. Yatsu, and N. Kawai (Tokyo Tech)  report
on behalf of the MITSuME collaboration:

We observed GRB 121128A ( Oates et al., GCN Circular #14007) with the
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME
50 cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation was started on 2012-11-28 08:49:50 UT ( ~13453  sec
after the burst).
We detected the previously reported afterglow ( Oates et al., GCN
Circular #14007)
in Ic band.  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
-------------------------------------------------------------------------------------------
  14491      09:07:08        1800        > 19.4         > 19.1
17.92+/-0.14
-------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14024
SUBJECT: GRB 121128A: optical observation in Mondy observatory
DATE:    12/11/30 21:19:10 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We observed the field of the Swift GRB 121128A (Oates et al., GCN 14007)
with AZT-33IK telescope of Sayan observatory (Mondy). We took several
images in R-filter of 60 s exposure on Nov. 29, between (UT) 10:16:58-
13:33:38 under favorable weather conditions. We do not detect the optical
afterglow (Oates et al., GCN 14007; Japelj et al., GCN 14008) in stacked
images. A photometry of stacked image

t_start,      T0+ (mid), filter,  exp.,   UL (3 sigma)
(UT)          d                            s

10:16:58 1.28450      R       11200  22.1

is based on the same nearby USNO-B1.0 stars used in our previous
observation (Volnova et al., GCN 14019):

USNO-B1.0       RA(J2000)     Dec(J2000) R
1442-0304687 20:02:23.58 +54:16:58.9 16.67
1442-0304744 20:02:29.58 +54:16:57.0 18.66
1442-0304807 20:02:36.33 +54:17:58.9 18.20
1443-0305750 20:02:37.10 +54:18:34.6 17.72
1443-0305710 20:02:32.72 +54:18:46.9 17.25


GRB_name: GRB121201A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14025
SUBJECT: GRB 121201A: a GRB with an optical counterpart
DATE:    12/12/01 12:47:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. N. Yershov (UCL-MSSL), D. N. Burrows (PSU),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
S. R. Oates (UCL-MSSL), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 12:25:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121201A (trigger=540178).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 13.488, -42.952 which is 
   RA(J2000) = 00h 53m 57s
   Dec(J2000) = -42d 57' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve is incomplete at this time
due to a telemetry drop out, lacking most of the time period covered
by this image trigger.  Activity is visible starting at T-10s,
but this is coincident with a pre-planned slew. 

The XRT began observing the field at 12:27:37.1 UT, 115.1 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 13.4676,
-42.9432 which is equivalent to:
   RA(J2000)  = 00h 53m 52.22s
   Dec(J2000) = -42d 56' 35.6"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 62 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 (1.99 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 1.9
(+1.03/-0.96) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 119 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 00:53:52.17 =  13.46736
  DEC(J2000) = -42:56:34.4  = -42.94290
with a 90%-confidence error radius of about 0.66 arc sec. This position is 3.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.71 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is V. N. Yershov (vny 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: GRB121201A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14026
SUBJECT: GRB 121201A: BOOTES-4 optical observations
DATE:    12/12/01 15:07:39 GMT
FROM:    Sergey Guziy at IAA CSIC  <gss@iaa.es>

S. Guziy (Mykolaiv Nat. Univ.), R. Sanchez-Ramirez (IAA-CSIC), L.
Monteagudo Narvion (IAC), O. Lara, M. Jelinek (IAA-CSIC), P. Kubanek (IP
AS CR), Y. Fan, X. Zhao, J. Bai, C. Wang, Y. Xin (Yunnan National
Astronomical Observatory), Chenzhou Cui (Beijing National Astronomical
Observatory), R. Cunniffe, A.J. Castro-Tirado, J.C. Tello and J. Gorosabel
(IAA-CSIC), on behalf of a larger collaboration, report:

We have observed the GRB 121201A optical afterglow (GCN 14025, Yershov et
al.) with the 0.6m BOOTES-4/MET robotic telescope at the Lijiang
Astronomical Observatory (China). The afterglow is clear detected in XRT
and UVOT position.

[GCN OPS NOTE(31dec12): As pointed out by E.Helder and confirmed by the author,
the Subject-line was changed from "121123A" to "121201A".]


GRB_name: GRB121201A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14027
SUBJECT: GRB 121201A: Enhanced Swift-XRT position
DATE:    12/12/01 18:34:19 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 2580 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 121201A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 13.46759, -42.94306 which is equivalent
to:

RA (J2000): 00h 53m 52.22s
Dec (J2000): -42d 56' 35.0"

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: GRB121201A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14028
SUBJECT: GRB 121201A: Swift-BAT refined analysis
DATE:    12/12/01 18:45:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (AGU), 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), V. N. Yershov (UCL-MSSL)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121201A (trigger #540178)
(Yershov, et al., GCN Circ. 14025).  The BAT ground-calculated position is
RA, Dec = 13.473, -42.929 deg, which is 
   RA(J2000)  =  00h 53m 53.6s 
   Dec(J2000) = -42d 55' 45.9" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows 3 main peaks starting at ~T-23,
peaking at ~T-18, -8, & +4 sec, and ending at ~T+55 sec.  T90 (15-350 keV) is
85 +- 21 sec (estimated error including systematics).
 
The time-averaged spectrum from T-24.00 to T+71.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.90 +- 0.21.  The fluence in the 15-150 keV band is 7.8 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-9.00 sec in the 15-150 keV band
is 0.8 +- 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/540178/BA/


GRB_name: GRB121201A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14029
SUBJECT: GRB 121201A: Swift-XRT refined Analysis
DATE:    12/12/02 00:48:05 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), A. Maselli  (INAF-IASFPA) and 
report on behalf of the Swift-XRT team: report on behalf of the
Swift-XRT team:

We have analysed 8.7 ks of XRT data for GRB 121201A (Yershov et al. et
al. GCN Circ. 14025), from 101 s to 33.6 ks after the  BAT trigger. The
data comprise 24 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
Beardmore et al. (GCN. Circ 14027).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.24 (+0.06, -0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.62 (+0.15, -0.09). The
best-fitting absorption column is  2.15 (+3.39, -0.16) x 10^20 cm^-2,
consistent with the Galactic value of 2.0 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.3 x 10^-11 (4.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.15 (+3.39, -0.16) x 10^20 cm^-2
Galactic foreground: 2.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.62 (+0.15, -0.09)

If the light curve continues to decay with a power-law decay index of
1.24, the count rate at T+24 hours will be 1.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.8 x
10^-14 (6.0 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00540178.

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

[GCN OPS NOTE(19dec12): Per author's request, in the first sentence
the Yershov/14025 reference was filled in.]


GRB_name: GRB121201A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14030
SUBJECT: GRB 121201A: Swift/UVOT Detection
DATE:    12/12/02 00:48:41 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 121201A
120 s after the BAT trigger (Yershov et al., GCN Circ. 14025).
A source consistent with the XRT position is detected in the
initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  00:53:52.16 =  13.46732 (deg.)
    Dec (J2000) = -42:56:34.5  = -42.94292 (deg.)
with an estimated uncertainty of 0.62 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              120          270          147         20.3 +/- 0.2
white              558          578           20         19.9 +/- 0.4
white             5689         5888          200         21.3 +/- 0.4
v                  608         1080           59        >19.6
b                  534         1178           58         19.4 +/- 0.2
u                  278          528          125        >24.8
u                 6714         6914          200         20.6 +/- 0.5
w1                 830         6710          432        >21.3
m2                 632         6504          413        >21.1
w2                1036         6094          413        >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).

[GCN OPS NOTE(17feb13):  The "A" was added to the GRB name in the Subject-line
and in the body of the Circular.]


GRB_name: GRB121201A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14031
SUBJECT: GRB 121201A: GROND afterglow observations and photometric redshift
DATE:    12/12/02 04:20:52 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (DARK/NBI), S. Klose (TLS Tautenburg) and J. Greiner (MPE Garching) 
report on behalf of the GROND team:

We observed the field of the Swift GRB 121201A (Yershov et al., GCN 14025) 
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 December 02, 2012, 00:28 UT which is roughly
12.0 hr after the trigger. We clearly detect the afterglow of 
GRB 121201A (Yershov et al., GCN 14025) in the optical filters, 
but not in the NIR bands. Based on stacked images at
a mid-time of 01:05 UT with an effective integration time of 25 min
in g'r'i'z' and 20 min in JHKs, we estimate preliminary AB magnitudes and 
upper limits of:

g' = 24.2 +- 0.2 
r' = 23.0 +- 0.1
i' = 22.7 +- 0.1
z' = 22.5 +- 0.1
J > 21.5
H > 21.0
Ks > 19.9

These magnitudes and upper limits are calibrated against SDSS standards 
in the optical, and 2MASS field stars in the NIR bands. After correcting 
for the Galactic extinction corresponding to a reddening of E(B-V)=0.01
(Schlegel et al. 1998),  a fit to this SED returns a photometric redshift of 3.6 +0.2 -0.3.


GRB_name: GRB121202A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14032
SUBJECT: GRB 121202A: Swift detection of a burst
DATE:    12/12/02 04:29:22 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), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 04:20:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121202A (trigger=540255).  Swift did not slew because
of the Earth limb observing constraint. 
The BAT on-board calculated location is 
RA, Dec 256.815, +23.952, which is 
   RA(J2000)  =  17h 07m 16s
   Dec(J2000) = +23d 57' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows muliple peaks
with a total duration of about 40 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~13 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+44.1
minutes. There will be no XRT or UVOT data until this time. 

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: GRB121202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14033
SUBJECT: GRB 121202A: TAROT Calern observatory optical observations
DATE:    12/12/02 05:09:10 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 121202 detected by SWIFT
(trigger 540255) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 34.0s after the GRB trigger
(15.8s after the notice). However, the elevation of the field
increased from 1 degrees above horizon so it was possible
to detect stars on images only 275s after the trigger.

The first image does not show any optical counterpart:
t0+275s to t0+305s : R > 14.9

We co-added series of exposures:
t0+275s to t0+1419s : R > 16.2
t0+1633s to t0+2578s : R > 16.9

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

N.B. Galactic coordinates are lon= 45.1864 lat=+32.8357
and the galactic extinction in R band is about 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB121202A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14034
SUBJECT: GRB121202A: Swift/UVOT Observations
DATE:    12/12/02 05:19:54 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

Swift/UVOT began settled observations of the field of GRB 121202A
2828 s after the BAT trigger (Oates et al., GCN Circ 14032).  UVOT took a 
finding chart exposure of 150 seconds with the White filter. 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. 


GRB_name: GRB121201A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14035
SUBJECT: GRB 121201A: X-shooter redshift
DATE:    12/12/02 05:43:10 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

R. Sanchez-Ramirez (IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), 
T. Kruehler (DARK/NBI), B. Milvang-Jensen (DARK/NBI), J.P.U. Fynbo (DARK/NBI), 
N. Tanvir (U. Leicester), D. Malesani (DARK/NBI), S. Schulze (PUC & MCSS), 
L. Kaper (U. Amsterdam), H. Flores (Obs. Paris) report on behalf of the X-shooter 
GTO GRB collaboration,

We observed the afterglow of GRB121201A (Yeshov et al., GCN 14025, Kruehler 
et al. GCN 14031) using the X-shooter spectrograph on the VLT (Paranal Observatory, 
Chile). Observations consisted of 4x1200s exposures in the UVB and VIS arms and 
8x600s exposures in the NIR, and started on 2 December 1:17 UT (12.87 hr after the 
burst).

In a preliminary reduction we detect Ly-alpha in emission as well as several 
absorption features (SiIV, CIV, AlII, AlIII) at a common redshift of z=3.385, which we 
identify as the redshift of the GRB.

We acknowledge the excellent support of the VLT staff, in particular G. Carraro.


GRB_name: GRB121202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14036
SUBJECT: GRB 121202A: Swift-XRT observations
DATE:    12/12/02 06:10:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 121202A at 05:07:09.7 UT,
2824.7 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 256.79704,
23.94886 which is equivalent to:
   RA(J2000)  = 17h 07m 11.29s
   Dec(J2000) = +23d 56' 55.9"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 60 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 (3.91 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.9
(+2.19/-1.90) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB121202A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14037
SUBJECT: GRB 121202A: Swift-BAT refined analysis
DATE:    12/12/02 16:04:27 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), S. R. Oates (UCL-MSSL),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121202A (trigger #540255)
(Oates, et al., GCN Circ. 14032).  The BAT ground-calculated position is
RA, Dec = 256.790, 23.942 deg, which is 
   RA(J2000)  =  17h 07m 09.7s 
   Dec(J2000) = +23d 56' 32.5" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 70%.
 
The mask-weighted light curve shows a cluster of overlapping peaks
starting at ~T-10 sec and ending at ~T+25 sec.  T90 (15-350 keV)
is 20.1 +- 1.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.18 to T+20.84 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.59 +- 0.11.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.02 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/540255/BA/


GRB_name: GRB121202A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14038
SUBJECT: GRB 121202A: Enhanced Swift-XRT position
DATE:    12/12/02 16:36:10 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 4781 s of XRT Photon Counting mode data and 9 UVOT
images for GRB 121202A, 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 = 256.79689, +23.94818 which is equivalent
to:

RA (J2000): 17h 07m 11.25s
Dec (J2000): +23d 56' 53.4"

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: GRB121202A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14039
SUBJECT: GRB 121202A: Fermi GBM observation
DATE:    12/12/02 18:14:21 GMT
FROM:    David Tierney at UCD  <david.tierney@ucd.ie>

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

"At 04:20:09.17 UT on 02 December 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121202A (trigger 376114812 / 121202181)
which was also detected by the Swift/BAT (Oates et al. 2012, GCN 14032)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 62 degrees.

The GBM light curve consists of a single weak pulse
with a duration (T90) of 17.7 +/- 1.7 s (50-300 keV).
The time-averaged spectrum from T0-4.1 s to T0+17.4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.14 (+0.19/-0.17) and
the cutoff energy, parameterized as Epeak, is 135.4 (+23.6/-23.0) keV.

The event fluence (10-1000 keV) in this time interval is
(2.0 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-5.1 s in the 10-1000 keV band
is 2.0 +/- 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: GRB121202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14040
SUBJECT: GRB 121202A: Swift-XRT refined Analysis
DATE:    12/12/02 18:41:45 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and S. R. Oates (UCL-MSSL) report on behalf of
the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 121202A (Oates  et al. GCN
Circ. 14032), from 2.8 ks to 31.9 ks after the BAT trigger. The data
comprise 16 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 14038).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.66 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.08 (+/-0.15). The
best-fitting absorption column is  1.7 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 3.9 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.6 x 10^-11 (5.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 3.9 x 10^20 cm^-2
Excess significance: 5.5 sigma
Photon index:      2.08 (+/-0.15)

If the light curve continues to decay with a power-law decay index of
1.66, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.5 x
10^-14 (1.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00540255.

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


GRB_name: GRB121202A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14041
SUBJECT: GRB 121202A: Swift/UVOT Upper Limits
DATE:    12/12/02 19:50:51 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 121202A
2828 s after the BAT trigger (Oates et al., GCN Circ. 14032).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 14038)
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          2828         2978          147         >20.3
white             2828         5033          541         >21.0
v                 3808        16147         1205         >20.2
b                 3192        22680         1059         >20.9
u                 2987        28451         2637         >21.2
w1                4218        27811         2853         >21.4
m2                4012        26905         2713         >21.5
w2                3603        31934         1549         >21.2

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: GRB121122A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14042
SUBJECT: GRB 121122A: Suzaku WAM observation of the prompt emission
DATE:    12/12/03 01:23:19 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

T. Yasuda, M. Tashiro, Y. Terada, W. Iwakiri, K. Takahara,
M. Asahina, S. Kobayashi, A. Sakamoto, Y. Ishida,
H. Ueno, S. Sugimoto (Saitama U.),
M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. Hanabata, T. Kawano, K. Takaki, R. Nakamura, Y.Tanaka, M. Ohno,
Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), Y. E. Nakagawa
(Waseda U.),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:

The long, IPN localized GRB 121122A (Hurley et al., GCN 14001)
was detected by the the Suzaku Wide-band All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 21:14:53 UT (=T0).

The observed light curve shows double-peaked FRED-like structure
lasting from T0 to T0+7 s with a duration (T90) of about 7 seconds.
The fluence in 100 - 1000 keV was 1.98 (+0.11/-0.16) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0 was 12.7 (+10.1/-1.25) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+7 s is well fitted by a single power-law with a photon index
of 3.08 (+0.17/-0.15) (chi2/d.o.f = 9.6/14).

The light curves with 1-sec time resolution for this burst will be
appeared at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14043
SUBJECT: GRB 121128A: Optical Observations
DATE:    12/12/04 05:24:30 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S.B. Pandey and Brajesh Kumar (ARIES Nainital, India, on behalf of larger 
Indian GRB collaboration)

We observed GRB 121128A (Swift trigger 539866, Oates et al. 2012, GCN
Circ.14007) field with the 1.04m telescope at ARIES, Nainital starting at
2012-11-28 14:02:55 (UT). Several images in R_c and I_c pass-bands were 
obtained.

The optical afterglow  candidate ( Oates et al. 2012, GCN Circ.14007,
Japelj 
et al. 2012, GCN Circ. 14008) was clearly detected in our frames. The
preliminary photometry of the co-added R_c (300sec x 3) and I_c (300sec x
3) frames yield following magnitudes.

--------------------------------------------------------------------------
Time (MID-UT)                Exp (sec)           Filter      Magnitude
--------------------------------------------------------------------------
2012-11-28, 14:12:11           900                 R_c      20.35 +/- 0.05
2012-11-28, 14:55:40           900                 I_c      19.65 +/- 0.11
--------------------------------------------------------------------------

Nearby USNO stars have been used for calibration.

This massage may be cited.


GRB_name: GRB121127A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14044
SUBJECT: GRB 121127A: Suzaku WAM observation of the prompt emission
DATE:    12/12/06 08:05:47 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

Y.Ishida, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda,
K. Takahara,ã€€M. Asahina, S. Kobayashi, A. Sakamoto, H. Ueno,
S. Sugimoto (Saitamaã€€U.), M. Akiyama, N. Ohmori, E. Mochinaga,
M. Yamauchi (Univ. ofã€€Miyazaki), K. Yamaoka, M. Kokubun,
T. Takahashi (ISAS/JAXA), Y.ã€€Hanabata, T. Kawano, K. Takaki,
R. Nakamura, Y.Tanaka, M. Ohno, Y.ã€€Fukazawa (Hiroshima U.),
S. Sugita (Nagoya U.), Y. E. Nakagawa (Wasedaã€€U.),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. ofã€€Tokyo),
on behalf of the Suzaku WAM team, report:

The short, IPN localized GRB 121127A (Golenetskii et al., GCN 14021)
was detected by the the Suzaku Wide-band All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 21:56:01 UT (=T0).

The observed light curve shows a single peak starting at T0-1s, ending
at T0s with a duration (T90) of about 1 seconds.
The fluence in 100 - 1000 keV was 9.34(+0.73/-2.40) x 10^-7 erg/cm^2.
The 1-s peak flux measured from T0-1s was
1.78(+0.16/-0.47) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1s to
T0s is well fitted by a power-law with exponential cutoff model :
   dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
   alpha 0.55(+0.57/-0.80), and
   Epeak 759(+273/-166) keV (chi^2/d.o.f. = 32.6/29).
All the quoted errors are at statistical 90% confidence level, in
which the systematic uncertainties are not included.

The light curves with 1-sec time resolution for this burst will be
appeared at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB121209A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14045
SUBJECT: GRB 121209A: Swift detection of a burst
DATE:    12/12/09 22:09:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Maselli (INAF-IASFPA), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU)
and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team:

At 21:59:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121209A (trigger=540964).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 326.801, -8.244 which is 
   RA(J2000)  =  21h 47m 12s
   Dec(J2000) = -08d 14' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a total duration of about 60 sec.  The peak count rate
was ~3300 counts/sec (15-350 keV), at ~20 sec after the trigger. 

The XRT began observing the field at 22:00:43.3 UT, 92.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 326.78917, -8.23262 which is equivalent
to:
   RA(J2000)  = 21h 47m 09.40s
   Dec(J2000) = -08d 13' 57.4"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 58 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 (3.81 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.8
(+2.58/-2.19) x 10^21 cm^-2 (90% confidence). 

UVOT data is not yet available. 

Burst Advocate for this burst is A. Maselli (maselli 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: GRB121209A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14046
SUBJECT: GRB 121209A: UVOT Observation
DATE:    12/12/09 22:27:57 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and A. Maselli (INAF-IASFPA) report on behalf of the
Swift/UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 96 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. 


GRB_name: GRB121209A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14047
SUBJECT: GRB 121209A: PAIRITEL NIR Observations
DATE:    12/12/10 03:07:55 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 121209A (Maselli et al., GCN 14045) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2012-Dec-10 01h16m41s UT, ~3.2 hours after the Swift trigger.  In  mosaics
(effective exposure time of 1940 s) taken simultaneously in the J, H, and
Ks filters, we do not detect any source within the XRT error circle.

post burst
t_mid (hr) exp.(hr) filt  U. Limit (3 sig)
3.68      0.54     J     > 18.1
3.68      0.54     H     > 17.2
3.68      0.54     Ks    > 16.2


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


GRB_name: GRB121209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14048
SUBJECT: GRB 121209A: Gemini-South imaging
DATE:    12/12/10 03:50:12 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the location of GRB 121209A (Maselli et al., GCN14045) with
the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini-South 8-meter
telescope starting on 2012 Dec 10.028 UT (2.68 hr after the BAT trigger).
We obtained 60-sec in each of the r- and i-bands in 0.75" seeing. We do not
detect any optical source within the XRT position reported in GCN 14045,
nor within the latest reported position (
http://www.swift.ac.uk/xrt_unenh_positions/00540964/). Calibrated to stars
in the SDSS DR8 field, we place 3-sigma limits of r > 22.6 mag and i > 23.0
mag on the optical afterglow of GRB 121209A at 2.7 hr after the burst
(uncorrected for Galactic extinction in the direction of the burst).

We thank the Gemini staff for their assistance with these observations."


GRB_name: GRB121209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14049
SUBJECT: GRB 121209A: GROND optical afterglow candidate
DATE:    12/12/10 07:37:57 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (DARK/NBI), A. Nicuesa Guelbenzu (TLS Tautenburg) 
and J. Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of the Swift GRB 121209A (Maselli et al., GCN 14045)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120, 405)
mounted at the 2.2m MPG/ESO telescope at La Silla Observatory (Chile).

Observations started on December 10, 2012, 00:24 UT which is roughly 2.4 hr 
after the trigger. Within the UVOT-enhanced XRT position (see link in Maselli et al.,
GCN 14045), we detect a faint source in the stack of all g'r'i'z' data at:

RA (J2000) = 21:47:08.96
Dec (J2000) = -08:14:06.3

with an estimated uncertainty of 0.5" in each coordinate.

Forcing photometry on this position, we estimate preliminary AB magnitudes and 
upper limits in the individual filters of:

g' > 24.0 mag
r' = 23.9 +- 0.3 mag
i' = 23.6 +- 0.4 mag
z' = 23.2 +- 0.3 mag
J  > 21.5 mag
H  > 21.0 mag
Ks > 19.5 mag

These magnitudes and upper limits are based on images with a mid-time 
of 00:59 UT and an effective integration time of 26.4 min in griz and 
24.0 min in the JHKs filters. They are calibrated against SDSS and 2MASS field stars 
and have not been corrected for the expected Galactic foreground extinction 
corresponding to a reddening of  E(B-V) = 0.05 mag (Schlegel et al. 1998). 
No statement about variability can be made at this point.


GRB_name: GRB121209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14050
SUBJECT: GRB121209A: RATIR Optical and NIR Upper Limits
DATE:    12/12/10 08:06:34 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

GRB121209A: RATIR Optical and NIR Upper Limits

Nat Butler (ASU), Alan Watson (UNAM), Alexander Kutyrev (GSFC), and
Michael Richer (UNAM), on behalf of a larger collaboration, report:

We observed the location of GRB 121209A (Maselli et al., GCN14045)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at Sierra San
Pedro Martir on 2012 Dec 10.072 UT (3.72 hr after the BAT trigger).

In integrations spanning approximately one hour, in poor (3") seeing
conditions, no optical or NIR sources are detected within the XRT
error circle (GCN14045).  In comparison with SDSS DR8 and 2MASS, we
derive the following (3-sigma) upper limits in the AB magnitude
system:

 r' 21.7
 i' 22.1
 Z  20.5
 Y  20.0
 J  19.8
 H  19.5

These magnitudes are not corrected for Galactic extinction in the
direction of the GRB.


GRB_name: GRB121209A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14051
SUBJECT: GRB 121209A: Enhanced Swift-XRT position
DATE:    12/12/10 09:50:09 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 3204 s of XRT Photon Counting mode data and 9 UVOT
images for GRB 121209A, 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 = 326.78723, -8.23545 which is equivalent
to:

RA (J2000): 21h 47m 8.94s
Dec (J2000): -08d 14' 07.6"

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

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

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


GRB_name: GRB121209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14052
SUBJECT: GRB 121209A: Swift-BAT refined analysis
DATE:    12/12/10 12:40:00 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), A. Maselli (INAF-IASFPA),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121209A (trigger #540964)
(Maselli, et al., GCN Circ. 14045).  The BAT ground-calculated position is
RA, Dec = 326.800, -8.232 deg, which is 
   RA(J2000)  =  21h 47m 12.0s 
   Dec(J2000) = -08d 13' 55.8" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.
 
The mask-weighted light curve shows multiple peaks starting at ~T-5 sec,
max peak at ~T+28 sec, and ending at ~T+80 sec.  T90 (15-350 keV) is
42.7 +- 2.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.16 to T+44.28 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.43 +- 0.08.  The fluence in the 15-150 keV band is 2.9 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+27.91 sec in the 15-150 keV band
is 3.4 +- 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/540964/BA/


GRB_name: GRB121209A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14053
SUBJECT: GRB 121209A: Swift-XRT refined Analysis
DATE:    12/12/10 15:09:04 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), J.A. Kennea (PSU) and A. Maselli report on
behalf of the Swift-XRT team:

We have analysed 18 ks of XRT data for GRB 121209A (Maselli  et al. GCN
Circ. 14045),  from 95 s to 48.0 ks after the  BAT trigger. The data
comprise 28 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN. Circ 14051).

The late-time light curve (from T0+5.2 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.20 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.31 (+/-0.14). The
best-fitting absorption column is  5.3 (+/-0.6) x 10^21 cm^-2, in
excess of the Galactic value of 3.8 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (9.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.3 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 3.8 x 10^20 cm^-2
Excess significance: 13.4 sigma
Photon index:      2.31 (+/-0.14)

If the light curve continues to decay with a power-law decay index of
1.20, the count rate at T+24 hours will be 0.014 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.8 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00540964.

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


GRB_name: GRB121209A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14054
SUBJECT: GRB 121209A: EVLA Observations
DATE:    12/12/10 17:18:25 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

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

"We observed the position of GRB 121209A (Maselli et al; GCN 14045) with
the EVLA beginning on 2012 Dec 10.01 UT (131 minutes after the burst). No
significant radio emission is detected at the enhanced Swift-XRT position
(Goad et al; GCN 14051) or the optical position (Kruehler et al.; GCN
14049), to a three-sigma upper limit of 27.3 uJy at 5.8 GHz."


GRB_name: GRB121209A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14055
SUBJECT: GRB 121209A: CARMA 3mm Observations
DATE:    12/12/11 06:05:41 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

A. Zauderer, T. Laskar, W. Fong, and E. Berger (Harvard) report on 
behalf of the CARMA Key Project "A Millimeter View of the Transient 
Universe":

"We observed the position of GRB 121209A (Maselli et al.; GCN 14045) 
with the Combined Array for Research in Millimeter Astronomy beginning 
2012 Dec 10.93 (dt=1.0 d) at a mean frequency of ~85 GHz. We do not 
detect significant millimeter emission at the enhanced Swift/XRT error
circle (Goad et al.; GCN 14051) or at the position of the GROND optical
afterglow candidate (Kruehler et al.; GCN 14049) to a 3-sigma limit of
0.5 mJy.

We thank the CARMA observers and staff for their support."


GRB_name: GRB121209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14056
SUBJECT: GRB 121209A: Keck observations
DATE:    12/12/11 11:17:36 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), S. B. Cenko, A. N. Morgan (UC Berkeley), and T. 
Kruehler (DARK) report:

We observed the position of GRB 121209A with the Low Resolution Imaging 
Spectrograph (LRIS) on Keck I on the night of UT December 11.  We 
acquired two 900-second spectra of the GROND afterglow candidate 
(Kruehler et al., GCN 14049) at a mean UT of 05:15 (1.30 day after the 
burst) followed by single exposure each of U- and I-band imaging at a 
mean UT of 06:33 (1.36 day after the burst).  The observations were 
affected by clouds and poor seeing, especially the imaging epoch.

We detect a source at the position of the GROND object in the I-band 
imaging frame.  Performing photometry relative to SDSS stars, we measure 
a magnitude of

I = 23.2 +/- 0.2 mag  (I=23.6 AB)

Which is consistent with the magnitude at 2.4 hours after the burst 
reported by Kruehler et al.  The lack of fading over this time range 
suggests that the source is not a GRB afterglow.  However, it may be the 
event's host galaxy.   Given the bright X-ray afterglow concurrent with 
the lack of an optical/IR counterpart in PAIRITEL, Gemini GROND and 
RATIR observations (GCNs 14047, 14048, 14049, 14050), GRB 121209A is 
"dark" burst (beta_OX ~< 0, taking the GROND host magnitudes as upper 
limits).

Preliminary analysis of our 2D spectra shows no evidence of line 
emission across the spectral range (effectively continuous from the 
atmospheric cutoff to 10300 Angstroms), despite detection of a (weak) 
continuum trace down to approximately 10000 Angstroms.  If this is a 
star-forming galaxy, this absence of lines (in particular, from OII) 
would suggest a moderately high redshift (z>~1.7).  Deeper spectroscopy 
and in particular infrared observations would be needed to confirm this 
hypothesis.  If this is a distant galaxy, its apparent optical 
brightness indicates that it quite luminous.


GRB_name: GRB121211A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14057
SUBJECT: GRB 121211A: Swift detection of a burst with an optical counterpart
DATE:    12/12/11 14:00:52 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
M. M. Chester (PSU), V. D'Elia (ASDC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), S. T. Holland (STScI), J. A. Kennea (PSU),
A. Maselli (INAF-IASFPA), K. L. Page (U Leicester),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
E. Sonbas (NASA/GSFC/Adiyaman Univ.), R. L. C. Starling (U Leicester)
and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team:

At 13:47:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121211A (trigger=541200).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 195.544, +30.161 which is 
   RA(J2000)  =  13h 02m 11s
   Dec(J2000) = +30d 09' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a total duration of about 180 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 13:48:32.3 UT, 89.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 195.5332, 30.1489 which is equivalent to:
   RA(J2000)  = +13h 02m 7.97s
   Dec(J2000) = +30d 08' 56.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 55 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 96 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  = 13:02:08.01 = 195.53339
  DEC(J2000) = +30:08:54.9  =  30.14858
with a 90%-confidence error radius of about 1.10 arc sec. This position is 1.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.49. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.01. 

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: GRB121211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14058
SUBJECT: GRB 121211A - Faulkes Telescope North afterglow confirmation
DATE:    12/12/11 14:34:34 GMT
FROM:    Jure Japelj at U. of Ljubljana,Slovenia  <jure.japelj@fmf.uni-lj.si>

J. Japelj, D. KopaÄ (U. Ljubljana), C. Guidorzi (U. Ferrara), C. Mundell,
F. Virgili (Liverpool JMU) report on behalf of a large collaboration:

The 2-m Faulkes Telescope North automatically began observing
GRB 121211A (Mangano et al. GCN Circ. 14057) on Dec 11 2012,
13:50:46 UT corresponding to 224 seconds post burst trigger. We confirm
the presence of a fading source at the optical afterglow candidate position
reported by Mangano et al. GCN Circ. 14057. In the first 3x10 s exposure,
we measure a preliminary R magnitude of 17.9 +- 0.3, calibrated against
nearby USNO-B1 stars.


GRB_name: GRB121211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14059
SUBJECT: GRB 121211A: Keck/LRIS redshift
DATE:    12/12/11 18:38:05 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), J. X. Prochaska (UCO/Lick), and A. N. Morgan (UC 
Berkeley) report:

We slewed with the Keck I telescope (+LRIS) to the location of GRB 
121211A (Mangano et al., GCN 14057) immediately following the GCN 
notice.   The optical transient (Mangano et al.; Japelj et al., GCN 
14058) was identified on the guider camera and longslit exposures began 
at 14:01 UT, 14 minutes after the GRB trigger.  After a single short 
observation in low resolution we acquired 2x860s exposures on the blue 
and red side.  The spectral range extends from 3150-5630 and 5790-7440 
Angstroms.

We identify FeII (2344, 2374, 2382, 2586, 2600) and possible FeII* and 
MnII at a redshift of z=1.023, as well as a marginal detection of MgII 
(2796, 2804) at the same redshift using the short initial exposure, 
which covers the dichroic gap.   We suggest this as the redshift of GRB 
121211A.


GRB_name: GRB121211A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14060
SUBJECT: GRB 121211A: Enhanced Swift-XRT position
DATE:    12/12/11 21:08:53 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 2289 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 121211A, 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 = 195.53315, +30.14869 which is equivalent
to:

RA (J2000): 13h 02m 7.96s
Dec (J2000): +30d 08' 55.3"

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: GRB121211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14061
SUBJECT: GRB 121211A: Swift-XRT refined Analysis
DATE:    12/12/12 02:01:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), A. Maselli  (INAF-IASFPA), A.
Melandri (INAF-OAB), J.A. Kennea (PSU), M.C. Stroh (PSU) and V. Mangano
report on behalf of the Swift-XRT team:

We have analysed 12 ks of XRT data for GRB 121211A (Mangano  et al. GCN
Circ. 14057),  from 95 s to 29.5 ks after the  BAT trigger. The data
comprise 203 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN. Circ 14060).

The late-time light curve (from T0+3.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.77 (+/-0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.15 (+/-0.04). The
best-fitting absorption column is  2.85 (+/-0.13) x 10^21 cm^-2, in
excess of the Galactic value of 9.5 x 10^19 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.11 (+0.15, -0.14)
and a best-fitting absorption column of 1.4 (+0.4, -0.3) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.5 x 10^-11 (5.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.4 (+0.4, -0.3) x 10^21 cm^-2
Galactic foreground: 9.5 x 10^19 cm^-2
Excess significance: 6.4 sigma
Photon index:      2.11 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
0.76, the count rate at T+24 hours will be 0.025 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.9 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00541200.

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


GRB_name: GRB121211A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14062
SUBJECT: GRB 121211A: MITSuME Okayama Optical Observation
DATE:    12/12/12 02:38:27 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 121211A (Mangano et al., GCNC 14057)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2012-12-11 16:29:09 UT (~2.7 h after the burst).
We detected the previously reported afterglow (Japelj et al., GCNC 14058)
in all the three bands.

Photometric results and three sigma upper limit of the OT are listed below.
We used SDSS catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'   g'_err Rc    Rc_err Ic    Ic_err
-----------------------------------------------------------------------
0.15443    17:29:25    6360.0   >20.5         20.4  0.2    19.6  0.3
0.23818    19:30:01    6360.0    20.9  0.3    21.1  0.3    20.1  0.3
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121211A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14063
SUBJECT: GRB 121211A: Swift/UVOT Detection
DATE:    12/12/12 03:15:42 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester (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 121211A
97 s after the BAT trigger (Mangano et al., GCN Circ. 14057).  A source
consistent with the enhanced Swift-XRT position (Osborne et al. GCN  
Circ.
14060) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  13:02:07.99 = 195.53328 (deg.)
   Dec (J2000) = +30:08:54.6  =  30.14849 (deg.)
with an estimated uncertainty of 0.52 arc sec. (radius, 90% confidence).

The following table provides preliminary detections and 3-sigma upper
limits for the finding charts and summed exposures using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373).
The lack of a detection in uvw2 is consistent with the redshift of
1.023 reported by Perley et al. (GCN Circ. 14059).


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

white_FC            97          247          147         18.4 +/- 0.1
white             4103         5738          393         19.9 +/- 0.1
v                 4514         6148          393        >19.9
b                 3899         5533          393         20.4 +/- 0.2
u_FC               255          297           41         18.3 +/- 0.3
u                 5128         5328          197         19.6 +/- 0.2
w1               10576        11476          886         20.6 +/- 0.2
m2                4718        10569         1082         20.6 +/- 0.2
w2                4309         5943          393        >21.1

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: GRB121212A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14064
SUBJECT: GRB 121212A: Swift detection of a burst
DATE:    12/12/12 07:05:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Grupe (PSU), W. H. Baumgartner (GSFC/UMBC),
C. Guidorzi (U Ferrara), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. Stamatikos (OSU/NASA/GSFC) report on behalf
of the Swift Team:

At 06:56:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121212A (trigger=541371).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 177.841, +78.034 which is 
   RA(J2000) = 11h 51m 22s
   Dec(J2000) = +78d 02' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED-like
structure with a duration of about 20 sec.  The peak count rate
was ~2300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 06:57:21.7 UT, 68.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 177.78252, 78.03720 which is equivalent
to:
   RA(J2000)  = 11h 51m 07.80s
   Dec(J2000) = +78d 02' 13.9"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 45 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.67 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.2
(+2.54/-2.19) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 71 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.07. 

Burst Advocate for this burst is D. Grupe (dxg35 AT 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: GRB121212A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14065
SUBJECT: GRB 121212A: A long GRB detected by INTEGRAL
DATE:    12/12/12 09:54:06 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 10 s has been detected by IBAS in the 
IBIS/ISGRI data at 06:56:12 UT of December 12.
Its refined coordinates (J2000) are:

R.A.= 177.8217  deg
DEC.=  78.0257  deg

with an uncertainty of 2 arcmin (90% c.l.).

The burst has a peak flux of 0,4 counts/cm2/s (20-200 keV, 1-s integration 
time) and a fluence in the same energy range of about 8e-8 erg/cm2.

This burst has also been detected by Swift (Grupe et al. GCN Circ.14064).

Due to the significance of the detection below the high confidence 
threshold, only an Alert Packet of WEAK type was distributed by IBAS in 
real time (Packet n. 6720).

A plot of the light curve has been posted at 
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB121212A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14066
SUBJECT: GRB 121212A: Enhanced Swift-XRT position
DATE:    12/12/12 12:02:15 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 1934 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 121212A, 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 = 177.79152, +78.03739 which is equivalent
to:

RA (J2000): 11h 51m 9.96s
Dec (J2000): +78d 02' 14.6"

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: GRB121211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14067
SUBJECT: GRB 121211A: Swift-BAT refined analysis
DATE:    12/12/12 13:36:02 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 (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 121211A (trigger #541200)
(Mongano, et al., GCN Circ. 14057).  The BAT ground-calculated position is
RA, Dec = 195.575, 30.173 deg, which is 
   RA(J2000)  =  13h 02m 18.0s 
   Dec(J2000) = +30d 10' 24.4" 
with an uncertainty of 4.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 23%.
 
The mask-weighted light curve shows a peak starting at ~T-5 sec, peaking at
~T+2 sec, and returning to baseline at ~T+5 sec. Then a second set of peaks
starts at ~T+20 with the main emission from T+105 to ~T+200 sec.
T90 (15-350 keV) is 182 +- 39 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.48 to T+196.77 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.36 +- 0.26.  The fluence in the 15-150 keV band is 1.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.07 sec in the 15-150 keV band
is 1.0 +- 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/541200/BA/


GRB_name: GRB121212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14068
SUBJECT: GRB 121212A: Swift-BAT refined analysis
DATE:    12/12/12 13:47:49 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), D. Grupe (PSU),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 121212A (trigger #541371)
(Grupe, et al., GCN Circ. 14064).  The BAT ground-calculated position is
RA, Dec = 177.787, 78.052 deg, which is 
   RA(J2000)  =  11h 51m 08.8s 
   Dec(J2000) = +78d 03' 05.4" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a couple peaks starting at ~T-3 sec,
peaking at ~T+0 sec, and ending at ~T+16 sec.  T90 (15-350 keV) is
6.8 +- 1.3 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.02 to T+7.84 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.65 +- 0.40.  The fluence in the 15-150 keV band is 1.2 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.02 sec in the 15-150 keV band
is 0.7 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/541371/BA/


GRB_name: GRB121212A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14069
SUBJECT: GRB121212A: Swift/UVOT Detection
DATE:    12/12/12 17:14:59 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (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 121212A
72 s after the BAT trigger (Grupe et al., GCN Circ. 14064).  A source
consistent with the enhanced XRT position (Beardmore et al. GCN Circ.
14066) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  11:51:10.30 = 177.79292 (deg.)
   Dec (J2000) = +78:02:14.3  =  78.03730 (deg.)
with an estimated uncertainty of 0.62 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               72         7133          824         21.23 +/- 0.17
v                  615         6108          352        >20.3
b                  540        13527         1160        >20.9
u                  285         1138          285         20.25 +/- 0.25
w1                 664        11960         1238        >20.8
m2                 639         6313          216        >20.5
w2                 763         5904          255        >20.9

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: GRB121212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14070
SUBJECT: GRB 121212A: Keck observations
DATE:    12/12/12 17:24:46 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley and A. Horesh (Caltech) report:

We slewed to the position of GRB121212A (rupe et al., GCN 14064) with 
the Keck I telescope (+LRIS) and acquired a series of exposures with the 
slit guider beginning at 15:40 UT, 8.7 hours after the event.

We identified a source near the DSS limit consistent with the XRT 
position, at coordinates (J2000) of:

RA  = 11:51:10.43
Dec = +78:02:15.3
(+/- 1.5 arcsec)

This is consistent with the XRT and UVOT positions (Beardmore et al., 
GCN 14066; Kuin et al., GCN 14069).

The magnitude is approximately R~21 on the guider camera at this time.

A series of 600s spectroscopic exposures were then taken during 
brightening morning twilight.

A provisional reduction of the (low S/N) spectrum shows a significant 
flux across the spectral range, extending to at least 3500 Angstroms 
with no break or strong absorption lines, suggesting z ~< 2 and 
consistent with the detection in the UVOT u filter.  Analysis is ongoing.


GRB_name: GRB121212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14071
SUBJECT: GRB 121212A: optical observations in ISON-NM observatory
DATE:    12/12/12 18:12:28 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  A. Pozanenko (IKI), A. Volnova (SAI MSU, IKI), V. 
Savanevych (KNURE), A. Bryukhovetskiy (NSFCTC), I. Molotov (KIAM), report on 
behalf of  larger GRB  follow-up collaboration:

We observed the field of  the Swift GRB 121212A (Grupe et al., GCN   14064) 
with 0.45-m telescope of ISON-NM observatory  starting on  Dec. 12 (UT) 
06:58:31, i.e  138 s after burst trigger.  We took  several unfiltered 
images of 30 s exposures.  An automatic real-time pipeline did not detect 
any new object. However after stacking all images we marginally detected the 
source not visible in any filter of DSS2  in coordinates  11 51 10.40 +78 02 
15.3 with uncertainty of 0.3 arcsec in both coordinates. The source is 
consistent with enhanced XRT afterglow position    (Beardmore et al. GCN 
14066)  and optical transient (Kuin et al. GCN  14069;  Perley and Horesh 
GCN  14070) .   A  preliminary  photometry  of co-added frames is based  on 
the USNO-B1.0 (R2)  nearby  stars is following:

UT start,      Exposure,  OT,              UL (3 sigma)

06:58:31         30       n/d                 18.3
06:58:31       3x30       n/d                 18.7
06:58:31      10x30       n/d                 19.4
06:58:31      40x30       20.7 +/- 0.4        20.5


GRB_name: GRB121212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14072
SUBJECT: GRB 121212A: P60 Observations
DATE:    12/12/12 18:26:40 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 the Swift (Grupe et al., GCN 14064) and
Integral (Mereghetti et al., GCN 14065) GRB121212A with the robotic
Palomar 60 inch telescope.  Observations began at 08:06 UT on 12 December
2012 (~ 1.2 hours after the Swift trigger) and were obtained in the r',
i', and z' filters.

At the location of the UVOT (Kuin et al., GCN 14069) and Keck/LRIS (Perley
and Horesh, GCN 14070) afterglow, we identify a faint source in our r' and
i' images.  Using several nearby USNO-B1 point sources for reference, we
measure a magnitude of R = 20.45 +/- 0.19 at this time.


GRB_name: GRB121212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14073
SUBJECT: GRB 121212A: Swift-XRT refined Analysis
DATE:    12/12/12 19:06:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), O.M.
Littlejohns (U. Leicester), V. Mangano (INAF-IASFPA), A. Melandri
(INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), J.A. Kennea (PSU), M.C. Stroh
(PSU), D.N. Burrows (PSU) and D. Grupe report on behalf of the
Swift-XRT team:

We have analysed 9.1 ks of XRT data for GRB 121212A (Grupe  et al. GCN
Circ. 14064),  from 81 s to 19.3 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 14066).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.80 (+/-0.24).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.48 (+0.17, -0.16). The
best-fitting absorption column is  2.2 (+/-0.4) 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 3.1 x 10^-11 (6.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: 7.7 sigma
Photon index:      2.48 (+0.17, -0.16)

If the light curve continues to decay with a power-law decay index of
0.80, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.3 x
10^-13 (6.6 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00541371.

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


GRB_name: GRB121212A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14074
SUBJECT: GRB 121212A: PAIRITEL NIR Observations
DATE:    12/12/12 22:17:33 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 121212A (Grupe et al., GCN 14064) with
the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began
at 2012-Dec-12 09h50m10s UT, ~2.9 hours after the Swift trigger.  In
mosaics (effective exposure time of 1.96 h) taken simultaneously in
the J, H, and Ks filters, we do not detect any source at the afterglow
location (Kuin et al., GCN 14069; Perley and Horesh, GCN 14070; Elenin
et al., GCN 14071; Cenko, GCN 14072).

post burst
t_mid (hr) exp.(hr) filt  U. Limit (3 sig).
4.79      1.96     J     > 19.0
4.79      1.96     H     > 17.9
4.79      1.96     Ks    > 17.1


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: GRB121211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14075
SUBJECT: GRB 121211A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    12/12/13 01:05:47 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made observations of Swift
trigger 541200 (Mangano, et al., GCN 14057).  The burst location was within
the field of our wide-field monitor located in Maui, HI, which began a 10 s
integration of the location at 03:47:00.17 UT, 2.8 s before the Swift trigger
time and during the gamma-ray emitting interval.  During the period that the
BAT was detecting gamma-ray emission, from ~T-5 s to ~T+200 s (Barthelmy,
et al., GCN 14067), we have a total of twenty 10 s exposures with limiting
magnitudes of R~9.8.  We do not detect the optical counterpart in any of
our images.  Our 3-sigma limiting magnitudes are based on a comparison of
our unfiltered image to the Tycho-2 V-band catalog.


GRB_name: GRB121212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14076
SUBJECT: GRB 121212A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    12/12/13 01:06:51 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made observations of Swift
trigger 541371 (Grupe, et al., GCN 14064).  The burst location was within
the field of our wide-field monitor located near Los Alamos, NM USA, which
began a 10 s exposure of the location at 06:56:03.18 UT, 10.2 s before the
Swift trigger time and covering the initial few seconds of gamma-ray emission
as detected by the BAT (Barthelmy, et al., GCN 14068).  The next 10 s exposure
begins at 06:56:23.58 UT, 10.2 s after the Swift trigger time and overlapping
the end stages of the gamma-ray emission.  We do not detect the optical
counterpart detected by the UVOT (Kuin, et al., GCN 14069) and others.  Our
3-sigma limiting magnitudes are R~10.1 based on comparison of our unfiltered
images to the Tycho-2 V-band catalog.

Our narrow-field instruments began a series of 10 s exposures at 06:58:08.59
UT, 115 s after the Swift trigger.  These images also do not show the optical
counterpart to a limiting magnitude of R~16.4 based on comparison to the
USNO-B1 R-band.


GRB_name: GRB121211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14077
SUBJECT: GRB 121211A: RATIR Optical and NIR Observations
DATE:    12/12/13 04:12:26 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (UCSC), Eleonora Troja (GSFC), Enrico Ramirezâ€Ruiz (UCSC),
JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), and Harvey
Moseley (GSFC) report:

We observed the field of GRB 121211A (Mangano, et al., GCN 14057) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico
Nacional on Sierra San Pedro MÃ¡rtir from 2012 Dec 12.48 to 2012 Dec
12.58 UTC (21.8 to 24.1 hours after the BAT trigger), obtaining a
total of 1.8 hours exposures in the r' and i' bands and 0.67 hours of
exposure in the Z, Y, J, and H bands.

In comparison with SDSS DR8 and 2MASS, we derive the following
detections and upper limits (3-sigma) in the AB magnitude system:

 r' 22.9 +/- 0.2
 i' 23.2 +/- 0.2
 Z  22.1 +/- 0.4
 Y  >21.3
 J  >21.9
 H  >21.1

These magnitudes are not corrected for Galactic extinction in the
direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro MÃ¡rtir.


GRB_name: GRB121211A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14078
SUBJECT: GRB 121211A: Fermi GBM observation
DATE:    12/12/13 09:02:10 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

David Yu (MPE) reports on behalf of the Fermi GBM Team:

"At 13:47:03.59 UT on 11 December 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 121211A (trigger 376926426 / 121211574)
which was also detected by the Swift/BAT (Mangano et al. 2012, GCN 14057).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 74 degrees.

The GBM light curve consists of a double peaked pulse
with a duration (T90) of about 5.4 s (50-300 keV).
The time-averaged spectrum from T0-3.072 s to T0+1.536 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.30 +/- 0.34 and
the cutoff energy, parameterized as Epeak, is 95.96 +/- 12.60 keV.

The event fluence (10-1000 keV) in this time interval is
(4.825 +/- 0.507)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.768 s in the 10-1000 keV band
is 2.402 +/- 0.202 ph/s/cm^2.

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


GRB_name: GRB121212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14079
SUBJECT: GRB 121212A: Maidanak optical observations
DATE:    12/12/13 20:46:21 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Sergeev (Institute of Radio Astronomy of NASU), 
A. Volnova (SAI MSU), O. Burhonov (UBAI), I. Molotov (KIAM) report on 
behalf GRB follow-up collaboration:

We observed  the field of Swift  GRB 121212A  (Grupe et al., GCN 
14064) with AZT-22 telescope of Maidanak observatory starting on Dec. 12 
(UT) 20:51:02 under mean seeing (FWHM) of about 1 arcsec. Totally we 
obtained 6 images of 600 s exposure in R  filter. At the position of the 
OT of GRB 121212A (Kuin et al., GCN  14069;  Perley and Horesh, GCN 
14070; Elenin et al., GCN 14071) we marginally detected an extended 
object. If it will be confirmed the object might be a host galaxy of GRB 
121212A.

A preliminary photometry of the object:

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

0.60088     R       6x600       23.0 Â± 0.35

is based on USNO-B1.0 nearby stars:

USNO-B1.0 1680-0064718 11:51:09.04 +78:00:39.9 R2 = 16.34
USNO-B1.0 1680-0064713 11:51:05.10 +78:02:00.1 R2 = 19.35


GRB_name: GRB121211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14080
SUBJECT: GRB 121211A: Continued RATIR Optical and NIR Observations, Fading
DATE:    12/12/13 22:56:58 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico Ramirezâ€Ruiz (UCSC), JosÃ© A. de Diego (UNAM),
Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 121211A (Mangano, et al., GCN 14057) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir for a second time from 2012 Dec 13.46 to 2012 Dec
13.57 UTC (45.2 to 47.8 hours after the BAT trigger), obtaining a total of
1.8 hours exposures in the r' and i' bands, 1.2 hours exposure in the Z and
J bands, and 10 minutes exposure in the Y and H bands.

For a source spatially coincident with the UVOT position (Chester et al.,
GCN 14063), in comparison with SDSS DR8 and 2MASS, we derive the following
detections and upper limits (3-sigma) in the AB magnitude system:

 r' 23.8 +/- 0.3  (delta= -0.9 +/- 0.4)
 i' 24.0 +/- 0.4  (delta= -0.8 +/- 0.4)
 Z  >22.4
 Y  >21.8
 J  >21.3
 H  >20.6

The delta values give the fade in 24 hours relative to the values quoted in
GCN 14077.  These magnitudes are not corrected for Galactic extinction in
the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB121209A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14081
SUBJECT: GRB 121209A: Early CARMA Observations
DATE:    12/12/14 01:24:38 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley and A. Horesh (Caltech) report on behalf of a larger 
collaboration:

We observed the position of GRB 121209A (Maselli et al., GCN 14045) with 
the Combined Array for Research in Millimeter-Wave Astronomy (CARMA) at 
a frequency of 93 GHz (3mm) between 00:46 and 01:14 on 2012-12-10 (UT). 
The mean observation time was 3.01 hours after the GRB trigger.

No source is detected at the position of the X-ray afterglow (Goad et 
al., GCN 14051) or of the possible host galaxy (GCN 14049, Kruehler et 
al.).  The 3-sigma limit of the map is 1.8 mJy.


GRB_name: GRB121212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14082
SUBJECT: GRB121212A: NOT optical imaging
DATE:    12/12/14 06:48:13 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC, MCSS), D. Malesani (DARK/NBI), T. Pursimo, J.
Jessen-Hansen (NOT) and P. Jakobsson (U Iceland) report on behalf a larger
collaboration:

We observed the field of GRB 121212A, detected by Swift (Grupe et al., GCN
14064) and INTEGRAL (Mereghetti et al., GCN 14065), with ALFOSC mounted at
the NOT. Observations started at 03:07:39 UT on 14 December, i.e. 1.8412
days after the trigger. We obtained a series of four R-band images with an
individual exposure time of 300 s.

We detect an object inside the UVOT-refined XRT
(http://www.swift.ac.uk/xrt_positions/00541371/) at

RA (J2000): 11:51:10.22
Dec (J2000): +78:02:14.51

We measured an R-band brightness of 23.5 +/- 0.1 mag with respect to four
USNO B1.0 stars (R2 magnitude). We did not apply any correction for
foreground extinction. Our measurement is consistent with Pozanenko et al.
(GCN 14079) and confirms that the object first reported by Kuin et al.
(GCN 14069) is the optical afterglow of GRB 121212A.


GRB_name: GRB121212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14083
SUBJECT: GRB 121212A: PdBI mm observations
DATE:    12/12/14 08:43:04 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC Granada), M. Bremer and J.-M. Winters (IRAM
Grenoble), on behalf of a larger collaboration, report:

"We conducted mm observations towards GRB 121212A (Grupe et al. GCNC
14064, Mereghetti et al. GCNC 14065) starting at 10.5 hr post burst with
the PdBI at 90 GHz. At the position of the X-ray/optical afterglows
(Beardmore et al. GCNC 14066, Kuin et al. GCNC 14069), no emission is
detected down to 0.3 mJy (3 sigma limit)."

This message can be quoted.


GRB_name: GRB121209A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14084
SUBJECT: GRB 121209A: MAXI/GSC detection
DATE:    12/12/14 13:24:21 GMT
FROM:    Satoshi Nakahira at JAXA/MAXI  <nakahira.satoshi@jaxa.jp>

R. Sato(Kyoto U.), S. Nakahira (JAXA), M. Serino (RIKEN),
Y. Ogawa (Miyazaki U.), N. Kawai (Tokyo Tech),
H. Negoro, M. Asada (Nihon U.),
S. Ueno, H. Tomida, M. Ishikawa, K. Yamaoka, M. Kimura (JAXA),
T. Mihara, M. Sugizaki, K. Morihana, T. Yamamoto, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN),
M. Mori, R. Usui, K. Ishikawa (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Nakano (AGU), H. Tsunemi, M. Sasaki (Osaka U.),
M. Nakajima, (Nihon U.), Y. Ueda, K. Hiroi, M. Shidatsu, T. Kawamuro (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.)
M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.)
on behalf of the MAXI team

At 2012-12-09T21:59:11 UT, the MAXI/GSC detected an uncatalogued
X-ray transient source. Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec.) = (327.02deg, -7.69deg) = (21:48:05, -07:41:38)(J2000)

with a 90% C.L. statistical error of 0.4 deg and an additional systematic
uncertainty of 0.1 deg (90% containment radius).

The trigger time is consistent with that of GRB 121209A (Maselli et al, GCN #14045).
The Swift position lies 0.1 deg outside of the MAXI error circle.
However, assuming the position for GRB 121209A, the transit by MAXI
should have occurred from
2012/12/09T21:58:38 UT(=T0-32 s, where T0 is the Swift/BAT trigger time)
to T0+11 s, suggesting that GRB 121209A was detected near the end
of the MAXI transit, causing the small difference in the formal position.

The time interval of the significant MAXI detection was T0+0 s to T0+5 s
with 2-20 keV X-ray flux of 600+/-140 mCrab (2-20 keV).
The average spectrum is fitted by a power-law model with photon index of  0.97(-0.57/+0.62).
There was no significant excess flux at the previous transit at 17:21 UT and
at the next transit at 23:31 UT on Dec 9 with an upper limit of 20 mCrab for each.


GRB_name: GRB121212A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14085
SUBJECT: GRB 121212A: LOAO IzY Observation
DATE:    12/12/14 15:44:35 GMT
FROM:    Minsung Jang at Seoul National U  <rigel103@snu.ac.kr>

M. Jang, M. Im (SNU), and Y. Urata (NCU), on behalf of EAFON

We observed GRB 121212A in IzY-bands starting at UT 08:51:52, 2012-12-12, 
~ 2 hrs after the BAT trigger (Grupe et al, GCN 14064), 
using the 1.0m telescope at Mt.Lemmon in Arizona, U.S. 

We do not detect the GRB afterglow in all bands at the position 
of the Swift/UVOT detection (Kuin et al. 14069). 
We estimate the 3-sigma limiting magnitude (AB system) of the afterglow
for each band, 

I > 20.0 (T0+7900s) 
z > 18.3 (T0+9370s) 
Y > 17.7 (T0+8260s),

by calibrating it against USNO-B1 stars with I2 magnitudes 
and 2MASS point sources without the galactic extinction correction. 

We thank the LOAO operator, I. Baek, for performing the observation. 


GRB_name: GRB121209A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14086
SUBJECT: GRB 121209A: Swift/UVOT Upper Limits
DATE:    12/12/14 17:19:02 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) and A. Maselli (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121209A
96 s after the BAT trigger (Maselli et al., GCN Circ. 14045).
No optical afterglow consistent with the optical position (Kruehler
et al. GCN Circ. 14049) 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            96          246          147         >21.4
white               96        12808         1217         >21.7
v                 5857        35749         1967         >20.3
b                 5241        24926         1784         >21.1
u                  308        30697         1959         >21.6
w1                6267        29936         1968         >21.5
m2                6062        36468         2314         >22.3
w2                5652        34835         1968         >21.8

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: GRB121209A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14087
SUBJECT: Subject : GRB 121209A: LOAO Observation
DATE:    12/12/15 14:17:50 GMT
FROM:    Seong-Kook Lee at CEOU,SNU,Korea  <s.joshualee@gmail.com>

Seong-Kook Lee, Myungshin Im (SNU), and Y. Urata (NCU) report:

We observed the location of GRB 121209A with the ARC Camera mounted on the
1.0m
Telescope at Mt. Lemmon Optical Astronomy Observatory (LOAO) on 2012 Dec
10,
09:06 UT.
We obtained a series of 300 seconds exposure images in I-band and Z-band
under 4" seeing.

We do not detect any source in both bands.
Calibrated to SDSS stars, we derive 3-sigma detection limit (in AB system)
in each band,

I > 20.9
Z > 19.6

We thank KASI staff for their support.


GRB_name: GRB121123A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14088
SUBJECT: GRB 121123A: NIKA (New IRAM KID Arrays) millimetre observations at the 30-m Pico Veleta telescope
DATE:    12/12/16 09:29:40 GMT
FROM:    Alessandro Monfardini at CNRS,Grenoble  <alessandro.monfardini@grenoble.cnrs.fr>

A. Monfardini (I. NÃ©el, Grenoble), F.-X. DÃ©sert (IPAG, Grenoble),
N. Ponthieu (IPAG, Grenoble), R. Adams (LPSC, Grenoble), M. Calvo (I.
NÃ©el, Grenoble), J. Macias-Perez (LPSC, Grenoble), A. Catalano (LPSC,
Grenoble), S. Leclercq (IRAM, Grenoble), P. Mauskopf (Arizona State U. &
Cardiff U.), A. Benoit (I. NÃ©el, Grenoble), on behalf of the NIKA
collaboration, report: 

"During a technical run, we observed the
position of GRB 121123A (E. A. Helder et al., GCN 13982) with the NIKA
instrument being commissioned at the IRAM 30-m at Pico Veleta.
Observations were accomplished between 15h and 16h UT on 24th November
2012 (mean time 29.5 hours after the burst), under poor observing
conditions (tau225GHz ~ 0.35) and at relatively low elevation (35 deg).
In roughly 40 minutes effective time on source, we do not detect the
afterglow at the position given by D. Xu et al., GCN 13986. The
following 3-sigma upper limits were derived:

 U.L. 3 mJy at 150 GHz
(99.7% C.L.)
 U.L. 40 mJy at 240 GHz (99.7% C.L.), strongly limited by
unstable weather conditions

NIKA is a multi-hundred-pixels dual-band
continuum instrument operating simultaneously at central frequencies of
150 GHz (bandwidth 40 GHz) and 240 GHz (bandwidth 60 GHz). It is the
first instrument based on the intrinsically multiplexable KID (Kinetic
Inductance Detectors) technology installed permanently at a telescope.
For more information about the instrument and the future project NIKA-2,
see A. Monfardini et al., ApJS 194, Issue 2, id. 24 (2011). 

We thank
the IRAM Granada and Grenoble staff for their outstanding support
before, during and after the NIKA run." 


GRB_name: GRB121217A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14089
SUBJECT: GRB 121217A: Swift detection of a burst
DATE:    12/12/17 07:31:58 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), B. N. Barlow (PSU), D. N. Burrows (PSU),
M. M. Chester (PSU), V. D'Elia (ASDC), D. Grupe (PSU),
N. P. M. Kuin (UCL-MSSL), C. B. Markwardt (NASA/GSFC),
D. M. Palmer (LANL) and M. Stamatikos (OSU/NASA/GSFC) report on behalf
of the Swift Team:

At 07:17:47 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121217A (trigger=542441).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 153.724, -62.304 which is 
   RA(J2000) = 10h 14m 54s
   Dec(J2000) = -62d 18' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with some substructure, with a duration of about 60 sec.  The peak count rate
was ~3200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 07:18:51.8 UT, 64.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 153.70643, -62.35064 which
is equivalent to:
   RA(J2000)  = 10h 14m 49.54s
   Dec(J2000) = -62d 21' 02.3"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 170 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.72
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.93e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 72 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 0.00% of the
XRT error circle. Because of the density of catalogued stars,  further
analysis is required to report an upper limit for any afterglow in the
region. No correction has been made for the large, but uncertain
extinction  expected. 

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: GRB121217A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14090
SUBJECT: GRB 121217A: Enhanced Swift-XRT position
DATE:    12/12/17 13:01:45 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 2474 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 121217A, 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 = 153.70999, -62.35047 which is equivalent
to:

RA (J2000): 10h 14m 50.40s
Dec (J2000): -62d 21' 01.7"

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

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

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


GRB_name: GRB121217A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14091
SUBJECT: GRB 121217A: GROND Detection of the Afterglow
DATE:    12/12/17 13:32:56 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

J. Elliott (MPE Garching), S. Schmidl (TLS Tautenburg), and J.Greiner (MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 121217A (Swift trigger 542441; Siegel et al.,
GCN 14089) 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 on December 17, 2012, at 07:21 UT, 210 s after the
GRB trigger. They were performed at an average seeing of 1.6" and at an
average airmass of 1.2.

We found a fading point source at the border of the enhanced XRT error
circle given in Evans et al. (GCN 14090)

RA (J2000) = 10:14:50.407
DEC (J2000) = -62:21:03.53

with an uncertainty of 0.5" in each coordinate.

Based on a total exposure time of 456 s in g'r'i'z' and 480 s in JHK,
at a midtime of 1882 s after the burst, we estimate preliminary
AB magnitudes of

g' = 20.3 +/- 0.1,
r' = 19.3 +/- 0.1,
i' = 18.9 +/- 0.1,
z' = 18.6 +/- 0.1,
J  = 18.1 +/- 0.1,
H  = 17.7 +/- 0.1,
K  = 17.4 +/- 0.1.

In the r' band the source faded with a decay slope of 0.7 +/- 0.1
between 2000 s and  4200 s after the trigger. The SED can be fit
with a power-law with a slope of beta = 0.8 +/- 0.1.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the Galactic foreground extinction
corresponding to a reddening of E(B-V)= 0.38 mag in the direction of the
burst (Schlegel et al. 1998).

The extinction-corrected SED suggests a photo-z of 3.0 +/- 0.2. We
caution, however, that the high Galactic extinction along the line of
sight might affect this result.


GRB_name: GRB121217A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14092
SUBJECT: GRB 121217A: Swift/UVOT Detection
DATE:    12/12/17 18:14:46 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (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 121217A
73 s after the BAT trigger (Siegel et al., GCN Circ. 14089).
A source consistent with the GROND optical position (Elliott et al. GCN Circ. 14091)
is detected in the initial UVOT exposures. The preliminary UVOT position is: 

    RA (J2000) = 10:14:50.32 = 153.7097  (deg)
   Dec (J2000) = -62:21:03.3 = -62.35096 (deg)

with an estimated uncertainty of 0.6 arcsec (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               73          222          147         19.58 +/- 0.13
v                  616         5906          313         19.01 +/- 0.22
b                  541          560          19          18.76 +/- 0.36
u                  285         6522          540         20.09 +/- 0.34
w1                 666         6317          313        >19.96
m2                 641         6112          313        >19.85
w2                 591         7138          510        >20.37

The magnitudes in the table are not corrected for the significant Galactic extinction
due to the reddening of E(B-V) = 0.37 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121217A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14093
SUBJECT: GRB 121217A: Swift-XRT refined Analysis
DATE:    12/12/17 21:32:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.1 ks of XRT data for GRB 121217A (Siegel  et al. GCN
Circ. 14089),  from 70 s to 30.3 ks after the  BAT trigger. The data
comprise 655 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 14090).

The late-time light curve (from T0+5.5 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.63 (+/-0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.15 (+0.11, -0.08). The
best-fitting absorption column is  consistent with the Galactic value
of 3.7 x 10^21 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a
photon index of 1.92 (+0.11, -0.10) and a best-fitting absorption
column of 4.02 (+0.51, -0.30) 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 (7.3 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.02 (+0.51, -0.30) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.92 (+0.11, -0.10)

If the light curve continues to decay with a power-law decay index of
0.52, the count rate at T+24 hours will be 0.091 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.2 x
10^-12 (6.7 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00542441.

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


GRB_name: GRB121217A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14094
SUBJECT: GRB 121217A: Fermi GBM observation
DATE:    12/12/18 10:26:28 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Yu and David Gruber (both MPE)
report on behalf of the Fermi GBM Team:

"At 07:30:01.58 UT on 17 December 2012, the Fermi Gamma-Ray Burst Monitor
triggered and located a burst (trigger 377422204 / 121217313), whose
location is consistent with the Swift GRB 121217A (Siegel et al. GCN 14089)
which triggered BAT ~13 minutes prior to the GBM.
Upon closer examination, we found that GRB 121217A is also present in the 
GBM data. GBM did not trigger on this earlier emission period owing to the
triggering being disabled while Fermi was passing through a
region of high geomagnetic latitude.

The GBM light curve consists of two epochs of emission,
separated by an epoch of quiescence of about 700 s.
The duration of the first pulse is about 50 s while 
the second pulse is about 30 s long. The overall event T90 is 
about 780 s (50-300 keV).
The time-averaged spectrum of the first emission epoch,
from T0-749.6 s to T0-704.5 s, is well fit by a power law 
function with an exponential high-energy cutoff.  The power law index 
is -1.20 +/- 0.12 and the cutoff energy, parameterized as Epeak, 
is 264 +/- 75 keV. The time-averaged spectrum of the 
second emission epoch, from T0-8.2 s to T0+24.6 s, is well fit 
by the same model, having a power law index of -1.29 +/- 0.14 and an 
Epeak of 184 +/- 56 keV.

The event fluence (10-1000 keV) over the overall event is
(1.11 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.68 s in the 10-1000 keV band
is 3.47 +/- 0.29 ph/s/cm^2.

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


GRB_name: GRB121217A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14095
SUBJECT: GRB 121217A theoretical estimate of redshift and of supernova occurrence
DATE:    12/12/18 12:28:55 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, L. Izzo, G.B. Pisani, C.L. Bianco, on behalf of a larger collaboration, report:

GRB 121217A, following our theoretical considerations based on the Induced
Gravitational Collapse scenario for GRBs-SNe, allows also for a different
solution with a cosmological redshift of z=0.8 (+- 0.1). We base this
result on a preliminary analysis of the superposition of the late X-ray
afterglow emission, considering GRB 090618 as the prototype of the class.
We have considered the first 75 ks of the X-ray afterglow light curve of
GRB 121217A in this preliminary analysis.
More details on the model will appear soon on the arXiv.

We also predict a presence of a SN emerging after about 18 (+- 3) days
from the GRB trigger, e.g. in the first days of January 2013.
Assuming an interstellar extinction obtained from the Schlegel et al.
(1998) extinction map and a supernova emission similar to the 1998bw one,
we estimate an observed magnitude of +24.5 (+- 0.5) in the J filter. We
further notice that, given the galactic latitude less than 5 deg (-4.89
deg), the calculated extinction value can differ at least of 1 mag.

Follow-up photometric and possibly spectroscopical observations are
strongly requested.


GRB_name: GRB121217A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14096
SUBJECT: GRB 121217A: Swift-BAT refined analysis
DATE:    12/12/19 22:23:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), T. Sakamoto (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),
A. M. Parsons (GSFC), G. Sato (ISAS), M. H. Siegel (PSU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 121217A (trigger #542441)
(Siegel, et al., GCN Circ. 14089).  The BAT ground-calculated position is
RA, Dec = 153.708, -62.354 deg, which is 
   RA(J2000)  =  10h 14m 50.0s 
   Dec(J2000) = -62d 21' 15.5" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.
 
The mask-weighted light curve shows two well-separated periods of emission.
The first starts at ~T-110 sec with weak emission, then peaks at ~T+1 sec,
and returns to baseline at ~T+80 sec.  The second period of emission starts
at ~T+500 sec, with weak peaks at ~T+500 and ~T+610 sec and the main peak
at ~T+730 sec and returns to baseline out past T+960 sec (where the data ends).
There are enough differences in the profiles of these two periods of emission
to conclude they are not gravitationally lensed.
T90 (15-350 keV) is 778 +- 16 sec (estimated error including systematics).
 
The time-averaged spectrum from T-17.7 to T+783.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.53 +- 0.08.  The fluence in the 15-150 keV band is 6.2 +- 0.3 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+735.96 sec in the 15-150 keV band
is 1.8 +- 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/542441/BA/


GRB_name: GRB121217A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14097
SUBJECT: GRB 121217A: ATCA 44GHz upper limit
DATE:    12/12/21 23:17:02 GMT
FROM:    Paul Hancock at U of Sydney  <hancock@physics.usyd.edu.au>

P. Hancock, T. Murphy, B. Gaensler, M. Bell, D. Burlon (University of
Sydney/CAASTRO), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI)

We observed GRB121217A (GCN 14809) with the Australia Telescope
Compact Array at 44GHz for 90 minutes centered on 12:55UT Dec 21 2012
(T0+4.234days) in poor weather.

We detect no radio source at the optical location of the GRB (GCN
14091) and place a 3sigma upper limit of 0.6mJy on the flux of an
afterglow.

These observations were obtained as part of ATCA project C2689. We
thank the observatory staff for their support and scheduling the
observations. The Australia Telescope is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO.


GRB_name: GRB121225A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14100
SUBJECT: GRB 121225A: MAXI/GSC detection
DATE:    12/12/25 12:00:15 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

Y. Ogawa (Miyazaki U.), S. Nakahira (JAXA), M. Serino (RIKEN), 
S. Ueno, H. Tomida, M. Kimura, M. Ishikawa (JAXA), 
T. Mihara, M. Sugizaki, K. Morihana, T. Yamamoto, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), 
N. Kawai, M. Morii, R. Usui, K. Ishikawa (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Nakano (AGU), 
H. Tsunemi, M. Sasaki (Osaka U.), H. Negoro, M. Nakajima, M. Asada (Nihon U.), 
Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato, T. Kawamuro (Kyoto U.), 
Y. Tsuboi, M. Higa (Chuo U.), 
M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.), 
K. Yamaoka (ISAS) report on behalf of the MAXI team

At 2012-12-25T09:50:24 UT, the MAXI/GSC nova alert system triggered on a bright uncatalogued X-ray transient source.
The transient emission lasted at least 33 seconds
within the 55 second long triangular transit response of
MAXI/GSC. We identify this event as GRB 121225A.

Assuming that the source flux was constant over the transit,
we obtain the source position at

 (R.A., Dec) = (264.86 deg, -66.07 deg) = (17 39 27, -66 04 16)(J2000)

with a 90% C.L. statistical error of 0.2 deg and an additional systematic 
uncertainty of 0.2 deg (90% containment radius). The 4-10 keV flux was  500 +- 50 mCrab.

There was no significant excess flux in the previous transit at 08:17 UT 
and in the next transit at 11:23 UT$B!!(Bwith an upper limit of 20 mCrab for each.


GRB_name: GRB121225B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14101
SUBJECT: GRB 121225B: Fermi LAT Detection
DATE:    12/12/25 15:38:34 GMT
FROM:    Daniel Kocevski at SLAC  <dankocevski@gmail.com>

D. Kocevski (NASA/GSFC U.), J. L. Racusin (NASA/GSFC) and E. Sonbas (Adiyaman Univ.), report on behalf of the Fermi-LAT team:

The Fermi Large Area Telescope (LAT) detected emission from GRB 121225B (GBM  trigger 378122456/121225417) at approximately 10:00:54 UT on December 25th, 2012.

The burst location was at the edge of the the LAT field of view at an angle of ~65 degrees to the LAT boresight, and had a zenith angle of 92 degrees. No significant excess is seen using standard analysis procedures.  The burst exited the nominal LAT field of view roughly ~100 s after the GBM trigger and remained above an angle of 70 degrees to the LAT boresight for at least the next 5000 s.

Using the non-standard LAT Low Energy (LLE) data selection, over 100 counts above background were detected in a single FRED like pulse, peaking 20s after the GBM trigger and coinciding with the time of the GBM emission, with a significance of 10 sigma. This detection is due to low energy gamma-rays, below 75 MeV, and therefore has insufficient spatial resolution to provide a reliable LAT localization. Indeed, no events were observed above 75 MeV using the standard analysis classes.

A GBM circular on GRB 121225B is forthcoming.

The Fermi LAT point of contact for this burst is Daniel Kocevski (daniel.kocevski at nasa.gov).

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


GRB_name: GRB121225B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14102
SUBJECT: GRB 121225B: Fermi GBM observation
DATE:    12/12/25 18:11:28 GMT
FROM:    Michael S. Briggs at UAH and MSFC  <michael.briggs@nasa.gov>

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

"At 10:00:53.58 UT on 25 December 2012, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 121225B (trigger 378122456 /
121225417). This GRB was also detected by the Fermi LAT (GCN 14101,
Kocevski et al.)

The on-ground calculated location, using the GBM trigger data, is RA =
310.45, DEC = -34.83 (J2000 degrees, equivalent to 20 h 41 m, -34 d 49'),
with an uncertainty of 1.5 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 66 degrees.

The GBM light curve has a multi-pulse time history with with the main
emission complexes at 15 to 25 seconds and at 45 to 65 seconds.  The
duration (T90) is 58.5 +/- 0.8 s (50-300 keV).  The time-averaged
spectrum from T0-1.8 s to T0+73.0 s is best fit by a Band function
with Epeak = 277.6 (+13.1/-12.4) keV, alpha = -1.08 (+0.02/-0.02), and
beta = -2.14 (+0.05/-0.06).

The event fluence (10-1000 keV) in this time interval is (7.16 +/-
0.07)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from
T0+22.0 s in the 10-1000 keV band is 23.6 +/- 0.4 ph/s/cm^2.

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




 

 

 

 

 
 


GRB_name: GRB121225B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14103
SUBJECT: IPN Triangulation of GRB 121225B
DATE:    12/12/26 15:28:17 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

V. Connaughton, M. Briggs, C. Meegan, and V. Pelassa, on behalf of the
Fermi GBM 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 GRB 121225B has been observed by Fermi (GBM: trigger 
363381140, Tierney, GCN Circ. 14102; LAT: Kocevski et al., GCN Circ. 
14101), Konus-Wind, INTEGRAL (SPI-ACS), and MESSENGER (GRNS), so far, at 
about 36054 s UT (10:00:54).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   308.913 (20h 35m 39s) -34.355 (-34d 21' 18")
  Corners:
   308.749 (20h 35m 00s) -30.606 (-30d 36' 21")
   308.950 (20h 35m 48s) -30.654 (-30d 39' 14")
   308.778 (20h 35m 07s) -38.039 (-38d 02' 19")
   308.567 (20h 34m 16s) -37.991 (-37d 59' 27")
  ---------------------------------------------
The error box area is 1.3 sq. deg, and its maximum dimension is 7.4 deg 
(the minimum one is 0.2 deg, the minimum annulus width is 0.2 deg).

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB121225_T36066/IPN/


GRB_name: GRB121225B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14104
SUBJECT: Konus-Wind observation of GRB 121225B
DATE:    12/12/26 16:21:17 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 intense long-duration hard-spectrum GRB 121225B
(Fermi-LAT detection: Kocevski et al., GCN 14101;
Fermi-GBM detection: Tierney et al., GCN 14102;
IPN detection and localization: Hurley et al., GCN 14103)
triggered Konus-Wind at T0=36066.467s UT (10:01:06.467)

The burst light curve shows a hard multi-peaked structure
from ~T0-18s to ~T0+15s followed by a softer complex pulse
from ~T0+23s to ~T0+56s. The total duration of the burst is ~75s.
The emission is seen up to 15 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB121225_T36066/

As observed by Konus-Wind, the burst
had a fluence of (9.0  0.7)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.288 s,
of (9.9  0.9)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst (measured T0 to T0+55.296 s)
is best fit in the 20 keV - 17 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.00  0.08,
the high energy photon index beta = -2.3  0.1,
the peak energy Ep = 230  20 keV,
chi2 = 102.0/95 dof.

The spectrum at the maximum count rate (measured T0 to T0+6.144 s)
is best fit in the 20 keV - 17 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = +0.85  0.07,
the high energy photon index beta = -2.3  0.1,
the peak energy Ep = 410  40 keV,
chi2 = 89.7/93 dof.

All the quoted results are preliminary.


GRB_name: GRB121226A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14105
SUBJECT: GRB 121226A: Swift detection of a burst
DATE:    12/12/26 19:24:11 GMT
FROM:    Hans Krimm at NASA-GSFC  <krimm@milkyway.gsfc.nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA), J. R. Cummings (NASA/UMBC),
V. D'Elia (ASDC), S. T. Holland (STScI), K. L. Page (U Leicester),
T. Sakamoto (AGU), M. H. Siegel (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 19:09:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121226A (trigger=544027).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 168.658, -30.414 which is 
   RA(J2000) = 11h 14m 38s
   Dec(J2000) = -30d 24' 51"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with a duration of about 2 sec.  The peak count rate was ~2700 counts/sec
(15-350 keV), at ~0 sec after the trigger.  Although the duration of this
burst is moderately short, it has a fairly soft spectrum.  Therefore we must
wait for further data to determine whether to classify GRB 121226A as
a short or long burst. 

The XRT began observing the field at 19:11:24.4 UT, 100.6 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 168.6424, -30.4066
which is equivalent to:
   RA(J2000)  = 11h 14m 34.17s
   Dec(J2000) = -30d 24' 23.8"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 55 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 (6.11 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 6.4
(+3.77/-3.06) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 104 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 H. A. Krimm (krimm 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: GRB121226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14106
SUBJECT: GRB 121226A: BOOTES-4/MET optical observations
DATE:    12/12/26 22:35:11 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

S. Guziy (Mykolaiv Nat. Univ.), O. Lara-Gil, R. Cunniffe, J. Gorosabel, M.
Jelinek (IAA-CSIC), P. Kubanek (IP AS CR), Y. Fan, X. Zhao, J. Bai, C.
Wang, Y. Xin (Yunnan Nacional Astronomical Observatory), Ch. Cui (Beijing
National Astronomical Observatory) and A. J. Castro-Tirado (IAA-CSIC), on
behalf of a larger collaboration, report:

Following the detection of GRB 121226A by Swift (Krimm et al. GCNC
14105), the 0.6m BOOTES-4/MET robotic telescope at the Lijiang
Astronomical Observatory (China) responded automatically to the trigger
alert at 19:10:21 UT, 9 s after the GCN reception (i.e. 36 s after the
onset of the event). After initial 0.5 s exposures, the first 19
unfiltered images (5 s exposure time each) starting 6 m 24 s postburst,
show no optical afterglow at the refined XRT position down to 19th mag
limiting magnitude (for the combined image). Observations are ongoing.

[GCN OPS NOTE(26dec12): Per author's request, "Lara" was changed to "Lara-Gil".]


GRB_name: GRB121226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14107
SUBJECT: GRB 121226A: Zadko observatory - Gingin optical observations
DATE:    12/12/26 23:18:31 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (ASDC/INAF-OAR), M. Boer (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA) report:

We imaged the field of GRB 121226A detected by SWIFT
(trigger 544027) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 62.8s after the GRB trigger
(38.6s after the notice). The elevation of the field
increased from 64 degrees above horizon and weather
conditions were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT in the XRT error box with a
limiting magnitude of:
t0+62.8s to t0+122.8s : Rlim 17.5

The second image is 30.0s exposure in tracking mode:
t0+138s to t0+168s : Rlim 18.7

We co-added a series of exposures:
t0+138s to t0+335s : Rlim 19.4

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

This message may be cited.


GRB_name: GRB121226A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14108
SUBJECT: GRB 121226A: MITSuME Okayama Optical upper limits
DATE:    12/12/26 23:55:05 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 121226A (Krimm et al., GCNC 14105)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2012-12-26 19:11:59 UT (~2.3 min after the burst).
We did not find any new point source within the XRT circle
(Krimm et al., GCNC 14105) 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
------------------------------------------------------
0.04333    20:12:06    6360.0   >20.2  >20.2  >19.5
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB121226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14109
SUBJECT: GRB 121226A: Optical Observations
DATE:    12/12/27 07:29:30 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

V.K. Bhatt, S.B. Pandey and Brajesh Kumar ((ARIES Nainital, India, on
behalf 
of larger Indian GRB collaboration)

We observed GRB 121226A (Swift trigger 518731, Krimm et al. 2012, GCNC
14105) field with the 1.04m telescope at ARIES, Nainital starting at
2012-12-26 
21:09:09 (UT). Several frames in R_c and I_c pass-bands, with an exposure
time 
of 300 sec each, were obtained.

Within the XRT error-circle, we do not detect any optical source down to 
following limiting magnitudes.

Dec 26.9118 UT, 300sx4, I_c ~ 18.8 mag
Dec 26.9292 UT, 300sx6, R_c ~ 19.5 mag

The nearby USNO stars have been used for calibrate.

This massage may be cited.


GRB_name: GRB121226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14110
SUBJECT: GRB 121226A: NOT optical upper limit
DATE:    12/12/27 07:46:12 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), O. Smirnova, T. Purismo (NOT), J. P. U. Fynbo
(DARK/NBI), P. Jakobsson (U. Iceland) report on behalf of a larger
collaboration:

We observed the field of GRB 121226A (Krimm et al., GCN 14105) using
the 2.5m Nordic Optical Telescope (NOT) equipped with ALFOSC. We
obtained 3x600s R-band and 3x360s z-band images with their median time
of 06:14:49 UT on 2012-12-27 (i.e., 11.085 hr after the BAT trigger)
and 06:53:54 UT (i.e., 11.736 hr post-trigger), respectively.

No optical source was detected within the XRT error circle in both
R-and z-bands, down to a 3sigma limit of R~23.0 mag ,calibrated with
the USNO B1 catalogue.


GRB_name: GRB121226A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14111
SUBJECT: GRB 121226A, Swift-BAT refined analysis
DATE:    12/12/27 14:27:06 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
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+111 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121226A (trigger #544027)
(Krimm, et al., GCN Circ. 14105).  The BAT ground-calculated position is
RA, Dec = 168.620, -30.413 deg which is
    RA(J2000)  =  11h 14m 28.7s
    Dec(J2000) = -30d 24' 47.0"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.  The mask-weighted light curve shows a single peak
with duration approximately 1.5 seconds, with no sign of extended emission.
T90 (15-350 keV) is 1.00 +- 0.20 sec (estimated error including systematics).

The time-averaged spectrum from T-0.36 to T+0.80 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.51 +- 0.29.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.21 sec in the 15-150 keV band
is 1.6 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

When plotting GRB 121226A on the T90-hardness diagram (see web link below),
we see that it falls within the short-hard region of phase space, with T90 = 1.0 
sec and Hardness ratio (energy fluence ratio 50-100 keV/25-50 keV) = 1.4.
Therefore we now suggest that GRB 121226A should be classified as a short-hard 
burst.  We do not have a lag analysis available at this time.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/544027/BA/


GRB_name: GRB121226A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14112
SUBJECT: GRB 121226A: Swift-XRT refined Analysis
DATE:    12/12/27 18:24:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 121226A (Krimm  et al. GCN
Circ. 14105),  from 109 s to 35.4 ks after the BAT trigger. The data
are entirely 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 = 168.6423, -30.4064 which is equivalent to:

RA (J2000): 11 14 34.14
Dec(J2000): -30 24 23.1

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=0.98 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.4 (+/-0.4). The
best-fitting absorption column is  8.2 (+2.5, -2.1) x 10^21 cm^-2, in
excess of the Galactic value of 6.1 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 4.4 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.2 (+2.5, -2.1) x 10^21 cm^-2
Galactic foreground: 6.1 x 10^20 cm^-2
Excess significance: 6.0 sigma
Photon index:      2.4 (+/-0.4)

If the light curve continues to decay with a power-law decay index of
0.98, the count rate at T+24 hours will be 1.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.7 x
10^-14 (1.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00544027.

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


GRB_name: GRB121226A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14113
SUBJECT: GRB 121226A: Swift/UVOT Upper Limits
DATE:    12/12/27 21:17:57 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aab@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and H. A. Krimm (CRESST/GSFC/USRA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121226A 
104 s after the BAT trigger (Krimm et al., GCN Circ. 14105). No optical 
afterglow consistent with the XRT position (Littlejohns et al. GCN Circ. 
14112) 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           104          254          147         >20.6
u_FC               317          566          246         >19.6
white              104        18160         1317         >21.6
v                  646        10716         1121         >20.4
b                  572        17397         1317         >21.3
u                  317        16485         1544         >20.9
w1                 696        12390         1163         >20.7
m2                 671        11621         1298         >21.0
w2                 622         6620          351         >20.2

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.055 in the direction of 
the burst (Schlegel et al. 1998).


GRB_name: GRB121226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14114
SUBJECT: GRB 121226A: 10.4m GTC optical observations
DATE:    12/12/28 01:49:33 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

A.J. Castro-Tirado, M. Jelinek, R. Snchez-Ramrez, J.C. Tello (IAA-CSIC),
J.M. Gonzlez-Prez (GTC/IAC), S. Guziy (Mykolaiv Nat. Univ.), D.
Prez-Ramrez (Univ. de Jan), P. Ferrero (IAC), J.M. Castro Cern (ESAC),
A. Fernndez-Soto (IFCA-UNICAN) and J. Gorosabel (IAA-CSIC), report:

We have obtained deep riz images with the 10.4m GTC telescope at
Observatorio del Roque de los Muchachos for GRB 121226A (Krimm et al. GCNC
14105; Baumgartner et al. GCNC 14111) starting on Dec 27.230--27.261 UT
(i.e., 10.3--11.1 hr post burst). A faint object is detected at
RA(J2000)=11:14:34.14, DEC(J2000)=-30:24:22.9 (0.7" error in each
coordinate), consistent with the position of the X-ray afterglow
(Littlejohns et al. GCNC 14112). The object shows a magnitude around
r'~25. At this stage we cannot conclude whether this is the GRB 121226A
optical afterglow or the underlying host galaxy.


GRB_name: GRB121229A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14115
SUBJECT: GRB 121229A: Swift detection of a burst
DATE:    12/12/29 05:15:29 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), V. D'Elia (ASDC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), T. Sakamoto (AGU)
and M. H. Siegel (PSU) report on behalf of the Swift Team:

At 05:00:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 121229A (trigger=544347).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 190.100, -50.594 which is 
  RA(J2000) = 12h 40m 24s
  Dec(J2000) = -50d 35' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Since this is an image trigger, the BAT light 
curve does not show any particular structure.  The peak count rate 
was ~1000 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 05:02:47.8 UT, 145.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 190.09755, -50.59366 which
is equivalent to:
  RA(J2000)  = 12h 40m 23.41s
  Dec(J2000) = -50d 35' 37.2"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 5.7 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 1.35
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.21e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 155 seconds after the BAT trigger. 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
0.16. 

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


GRB_name: GRB121229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14116
SUBJECT: Skynet/PROMPT observations of GRB121229a
DATE:    12/12/29 06:28:57 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

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

Skynet began observing the field of GRB121229a beginning ~2 minutes after 
the burst using three of the PROMPT telescopes located at CTIO in Chile in 
B,R, and I.  No optical afterglow is detected in the early observations.

Calibrating to several nearby USNO B1.0 stars, and co-adding the early 
observations, the following 3-sigma limiting magnitudes are obtained, at a 
mean observing time of ~30 minutes post burst:

Filt Time 3-Sig Limit
B 29.7m >20.6
R 29.7m >20.7
I 33.1m >20.5


Further observations are ongoing.


GRB_name: GRB121229A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14117
SUBJECT: GRB 121229A: GROND detection of the afterglow
DATE:    12/12/29 06:59:20 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

K. Varela (MPE Garching), V. Sudilovsky (MPE Garching), S. Klose (TLS
Tautenburg), and J. Greiner (MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 121229A (Swift trigger 544347; Sonbas et al.,
GCN 14115) 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 on December 29, 2012, at 05:09 UT, 540 s after the
GRB trigger. They were performed at an average seeing of 1.0" and at an
average airmass of 1.8.

We find a point source at the border of the XRT error
circle at a position

RA (J2000) = 12:40:24.29
DEC (J2000) = -50:35:39.48

with an uncertainty of 0.5" in each coordinate.

Based on a total exposure time of 1500 s in g'r'i'z' and 1200 s in JHK,
at a midtime of 3840s after the burst, we estimate preliminary
AB magnitudes of

g' = 22.2 +/- 0.2,
r' = 21.5 +/- 0.1,
i' = 21.3 +/- 0.1,
z' = 21.1 +/- 0.1,
J  = 20.9 +/- 0.1,
H  = 20.2 +/- 0.1, and
K  > 19.7.

This source's spectral energy distribution is best fit with a power-law of
slope beta = 0.8 +/- 0.2.
We suggest that this source is the afterglow of GRB 121229A.

Given magnitudes are calibrated against GROND zeropoints in g'r'i'z' and
2MASS
field stars in JHK, and are not corrected for the Galactic foreground
extinction
corresponding to a reddening of E(B-V)= 0.16 mag in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB121229A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14118
SUBJECT: GRB 121229A: MAXI/GSC detection
DATE:    12/12/29 10:35:00 GMT
FROM:    Satoshi Nakahira at JAXA/MAXI  <nakahira.satoshi@jaxa.jp>

S. Nakahira (JAXA), Y. Ogawa, Y. Nishimura, T. Hanayama (Miyazaki U.),
Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato, T. Kawamuro (Kyoto U.),
N. Kawai, M. Morii, R. Usui, K. Ishikawa (Tokyo Tech),
K. Yamaoka (ISAS), S. Ueno, H. Tomida, M. Kimura, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, M. Serino, K. Morihana, T. Yamamoto,
J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN),
A. Yoshida, T. Sakamoto, Y. Nakano (AGU), H. Tsunemi, M. Sasaki (Osaka U.),
H. Negoro, M. Nakajima, M. Asada (Nihon U.), Y. Tsuboi, M. Higa (Chuo U.),
M. Yamauchi, K. Yoshidome (Miyazaki U.)$B!!(B
report on behalf of the MAXI team

At 2012-12-29T05:01:08 UT, the MAXI/GSC detected an uncatalogued X-ray
transient source. Assuming that the source flux was constant over the
transit, we obtain the source position at
(R.A., Dec.) = (189.70deg, -50.84deg) = (12:38:48.98, -50:50:36.0)(J2000)
with a 90% C.L. statistical error of 0.4 deg and an additional systematic
uncertainty of 0.1 deg (90% containment radius).

The position and time are consistent with those of GRB 121229A (Sonbas
et al, GCN #14115). The transit by MAXI occurred from 2012/12/29
05:00:47 (=T0+26 s, where T0 is the Swift/BAT trigger time) to T0+70s.
The averaged X-ray flux was 103 +/- 23 mCrab (2-20 keV).
The spectrum is fitted by a power-law model with a photon index of
1.85 (-0.58/+0.68). There was no significant excess flux at the previous
transit at 2012/12/28 18:12 UT and at the next transit at 2012/12/29
06:43 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB121229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14120
SUBJECT: GRB 121229A: VLT/X-shooter redshift
DATE:    12/12/29 14:38:02 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

J. P. U. Fynbo (DARK/NBI), N. R.  Tanvir (U. Leicester), V. D'Elia
(ASDC, INAF), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI),
D. Malesani (DARK), O. E. Hartoog (Uva, NL), D. Xu (DARK), H. Flores
(Obs. Paris), A. J. Levan (U. Warwick), B. Milvang-Jensen (DARK/NBI)

We observed the field of GRB 121229A (Sonbas et al., GCN 14115; Varela
et al., GCN 14117) with the ESO VLT equipped with the X-shooter
spectrograph. Observations started at 07:00 UT on 2012-12-29 (2 hr
after the BAT trigger), for a total exposure time of ~30 min in each
of the UVB, VIS, and NIR arms, covering the wavelength range
3000-21000A.

The spectrum exhibits two relatively broad troughs (centered at ~ 3800
and 4500 A) which we interpreted as Lyman-beta and -alpha features,
respectively, at z=2.707. We measured the HI column density,
logN(HI)~21.7, from the Lyman-alpha feature. At this redshift there
are tentative indications of other metal absorption features, although
they are weak and we have yet to establish their significance. The
lack of strong resonance metal lines, together with the low X-ray
absorption (Sonbas et al., GCN 14115), suggests a low metallicity. We
also report a tentative evidence for an intervening MgII absorber at
z=1.658

We acknowledge the excellent support of the ESO observing staff, in
particular Maja Vu?kovi?.


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GRB_name: GRB121229A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14121
SUBJECT: GRB 121229A: Enhanced Swift-XRT position
DATE:    12/12/29 14:44:25 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 2407 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 121229A, 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 = 190.10130, -50.59414 which is equivalent
to:

RA (J2000): 12h 40m 24.31s
Dec (J2000): -50d 35' 38.9"

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: GRB121229A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14122
SUBJECT: GRB 121229A: Swift/UVOT Upper Limits
DATE:    12/12/29 19:01:22 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and E. Sonbas (NASA/GSFC/Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 121229A
155 s after the BAT trigger (Sonbas et al., GCN Circ. 14115).
No optical afterglow consistent with the optical position
(Varela et al. GCN Circ. 14117)
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           155          305          147         >20.9
u_FC               314          563          246         >19.9
white              155         6156          363         >21.2
v                  644         6466          116         >18.9
b                  570         5952          216         >20.5
u                  314         5747          442         >20.1
w1                3947         4136          186         >20.0
m2                 670          690           19         >17.6
w2                 620         6362          216         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.16 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14123
SUBJECT: GRB 121229A, Swift-BAT refined analysis
DATE:    12/12/30 02:33:05 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA),S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC),J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC),C. B. Markwardt (GSFC),D. M. Palmer (LANL),
T. Sakamoto (AGU), E. Sonbas (NASA/GSFC/Adiyaman Univ.),
M. Stamatikos (OSU),J. Tueller (GSFC),T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 121229A (trigger #544347)
(Sonbas, et al., GCN Circ. 14115).  The BAT ground-calculated position is
RA, Dec = 190.095, -50.588 deg which is
    RA(J2000)  =  12h 40m 22.7s
    Dec(J2000) = -50d 35' 16.9"
with an uncertainty of 2.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 39%.  The mask-weighted light curve shows a broad
structure beginning at least at T-60 seconds and lasting until T+60 sec.
Since there is no data from before the start of the burst, T90 cannot be
accurately calculated at this time.  It is approximately 100 seconds.

The time-averaged spectrum from T+0.00 to T+64.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.43 +- 0.46.  The fluence in the 15-150 keV band is 4.6 +- 1.3 x 10^-7erg/cm2.
The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band
is 0.1 +- 0.0 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/544347/BA/


