# GCN_circulars

GRB_name: GRB131117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15499
SUBJECT: GRB 131117A, Swift-BAT refined analysis
DATE:    13/11/17 20:11:55 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), M. J. Page (UCL-MSSL) 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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131117A (trigger #577968)
(Page, et al., GCN Circ. 15490).  The BAT ground-calculated position is
RA, Dec = 332.354, -31.761 deg which is
  RA(J2000)  =  22h 09m 25.0s
  Dec(J2000) = -31d 45' 38.8"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-weighted light curve shows a single peak structure starts at ~T-1 sec
and ends at ~T+12 sec. T90 (15-350 keV) is 11.00 +- 3.16 sec (estimated error
including systematics).

The time-averaged spectrum from T-1.00 to T+12.00 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index -0.40 +- 1.41,
and Epeak of 44.0 +- 7.4 keV (chi squared 45.16 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.5 +- 0.4 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+0.00 sec in the 15-150 keV band is
0.7 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.79 +- 0.18 (chi squared 58.98 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/577968/BA/


GRB_name: GRB131117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15500
SUBJECT: GRB 131117A, Swift-BAT refined analysis
DATE:    13/11/17 20:11:56 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), M. J. Page (UCL-MSSL) 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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131117A (trigger #577968)
(Page, et al., GCN Circ. 15490).  The BAT ground-calculated position is
RA, Dec = 332.354, -31.761 deg which is
  RA(J2000)  =  22h 09m 25.0s
  Dec(J2000) = -31d 45' 38.8"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-weighted light curve shows a single peak structure starts at ~T-1 sec
and ends at ~T+12 sec. T90 (15-350 keV) is 11.00 +- 3.16 sec (estimated error
including systematics).

The time-averaged spectrum from T-1.00 to T+12.00 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index -0.40 +- 1.41,
and Epeak of 44.0 +- 7.4 keV (chi squared 45.16 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.5 +- 0.4 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+0.00 sec in the 15-150 keV band is
0.7 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.79 +- 0.18 (chi squared 58.98 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/577968/BA/


GRB_name: GRB131030A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15501
SUBJECT: GRB 131030A, Optical Observations
DATE:    13/11/18 11:03:11 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

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

We observed the Swift GRB 131030A field ( (Troja et al., GCN#15402) using
1.3m DFOT telescope at Devasthal, operated by ARIES Nainital, India. The
observations were started at 16:25:47 UT on 2013-10-31. Two frames in
each R_c and I_c bands with an exposure time of 300s each were obtained
in good seeing conditions.

In our individual frames, we clearly detect the optical counterpart of
GRB 131030A (GNC circular 15403, 15405, 14506, 15410). The
preliminary photometry of co-added R_c (300sec x 2) and
I_c (300sec x 2) frames yields following.

.................................................................
Time (MID-UT)  Exp (sec)  Filter   Magnitude
.................................................................
2013-10-31, 16:46:39 600    R_c 20.13 +/- 0.04
2013-10-31, 16:33:09 600     I_c 19.49 +/- 0.06
..................................................................

The photometry was performed in comparison to nearby USNO- B1
stars. This message may be cited.


GRB_name: GRB131108A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15502
SUBJECT: GRB 131108A: VLA Observations
DATE:    13/11/19 04:01:15 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

A. Corsi (GWU), S. B. Cenko (NASA/GSFC), and D. A. Perley (Caltech) report
on behalf of a larger collaboration:

We imaged the position of the Fermi-LAT GRB 131108A (Racusin et al., GCN
15464) with the Very Large Array in the 18.7-24.9 GHz frequency range,
starting at about 2.6 days after the burst. A provisional reduction shows
a source consistent with the location of the X-ray (Stroh and Kennea,
GCN 15468) and optical (e.g., Xu et al., GCN 15471) afterglow. At this
time, we estimate a preliminary flux of about 200 uJy at 19 GHz.

Further observations are planned.

We thank the VLA staff for their support.


GRB_name: GRB131118A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15503
SUBJECT: GRB 131118A: Fermi GBM detection
DATE:    13/11/19 18:35:12 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

Andrew C. Collazzi (NASA/ORAU) reports on behalf of the Fermi GBM Team:

"At 22:58:57.47 UT on 18 November 2013, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 131118A (trigger 406508340 / 131118.958). The
on-ground calculated location, using the Fermi GBM trigger data,
is RA = 349.7, Dec = -69.4 (J2000 degrees, equivalent to J2000 23h 18.8m,
-69 24' ), with a statistical uncertainty of 1.0 degrees (radius, 1-sigma
containment, statistical only; there is additionally a systematic error which
is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT
boresight is 150 degrees.

Due to the high zenith angle of this burst, there may be higher than normal
systematic errors on this location.  This burst was also observed by Swift-BAT
(ground analysis), Suzaku-WAM, and INTEGRAL/SPI-ACS.

The GBM light curve shows a multi-peaked event with a duration (T90)
of about 85 s (50-300 keV). The 1.024-s peak flux during this interval is
12.5 +/- 0.9 erg/s/cm^2 (10-1000 keV). The time-averaged spectrum
from T0-13.8 to T0+99.8 s is equally well fit to a Comptonized model
with Epeak = 370.5 +/- 10.6, alpha = -0.89 +/- 0.03 and a Band model with
Epeak = 366.8 +/- 12.5, alpha = -0.89 +/- 0.03, and beta = -3.4 +/- 0.6.
Both models yield a fluence (10-1000 keV) in this time interval 
of (9.2 +/- 0.1)E-05 erg/cm^2.

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


GRB_name: GRB131120A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15505
SUBJECT: GRB 131120A: Swift detection of a burst
DATE:    13/11/20 14:47:45 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Maselli (INAF-IASFPA), S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 14:37:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131120A (trigger=578227).  Swift could not slew to the burst
due to a Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 278.921, -11.997 which is 
   RA(J2000) = 18h 35m 41s
   Dec(J2000) = -11d 59' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for image triggers, the
immediately-available BAT lightcurve does not show strong
variation. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 15:39 UT on 2014 February 13. There will thus be no XRT
or UVOT data for this trigger before this time. 

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: GRB131118A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15506
SUBJECT: IPN Triangulation of GRB 131118A
DATE:    13/11/20 18:42:44 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

IPN Triangulation of GRB 131118A

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

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

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

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

V. Connaughton, M. S. 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:

The long-duration, intense GRB 131118A (Collazzi, GCN 15503) has been
observed by Fermi (GBM: trigger 406508340), INTEGRAL (SPI-ACS), Swift 
(BAT), Suzaku (WAM), MESSENGER (GRNS), Mars Odyssey (HEND), and 
Konus-Wind, so far, at about 82737 s UT (22:58:57). The burst was 
outside the coded field of view of the BAT.

We have triangulated it to a 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   349.863 (23h 19m 27s) -66.833 (-66d 49' 58")
  Corners:
   350.415 (23h 21m 40s) -66.930 (-66d 55' 47")
   349.800 (23h 19m 12s) -66.926 (-66d 55' 32")
   349.313 (23h 17m 15s) -66.733 (-66d 44' 00")
   349.924 (23h 19m 42s) -66.740 (-66d 44' 23")
  ---------------------------------------------
The error box area is 162 sq. arcmin, and its maximum
dimension is 29 arcmin (the minimum one is 12 arcmin). The Sun distance 
was 81.6 deg.

The center of the GBM ground position (Collazzi, GCN 15503) is 2.6 deg 
from the center of the box.

Some improvement in this triangulation is possible.


GRB_name: GRB131118A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15507
SUBJECT: Konus-Wind observation of GRB 131118A
DATE:    13/11/21 08:06:58 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 131118A
(Fermi GBM detection: Collazzi, GCN 15503;
IPN triangulation: Hurley at al., GCN 15506)
triggered Konus-Wind at T0=82738.919 s UT (22:58:58.919).

The burst light curve shows multiple partly overlapped pulses
from ~T0 to ~T0+140 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131118_T82738/
Note: the waiting mode LCs are corrupted for almost whole
duration of the burst.

As observed by Konus-Wind, the burst
had a fluence of (8.40  0.06)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+63.296 s,
of (5.1  0.5)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+139.520 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.88  0.05,
the high energy photon index beta = -2.83  0.25,
the peak energy Ep = 230  11 keV,
chi2 = 97.4/96 dof.

The spectrum near the maximum count rate
(measured from T0+57.600 s to T0+65.792 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.80  0.04,
the high energy photon index beta = -2.56  0.07,
the peak energy Ep = 286  8 keV,
chi2 = 110/97 dof.

All the quoted values are preliminary.

[GCN OPS NOTE(21nov13) The GRB name was corrected to 131118A.]


GRB_name: GRB131120A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15508
SUBJECT: GRB 131120A, Swift-BAT refined analysis
DATE:    13/11/22 01:12:54 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

A. Y. Lien (NASA/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), 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-250 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131120A (trigger #578227)
(Maselli, et al., GCN Circ. 15505).  The BAT ground-calculated position is
RA, Dec = 278.937, -12.026 deg which is 
  RA(J2000)  =  18h 35m 44.8s 
  Dec(J2000) = -12d 01' 34.8" 
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.

The mask-weighted light curve shows two weak peaks at T-20 sec and 
T+50 sec.  The emission starts at T-100 sec, and ends at T+80 sec.  
T90 (15-350 keV) is 131 +- 20 sec (estimated error including systematics).

The time-averaged spectrum from T-71.1 to T+64.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.94 +- 0.50.  The fluence in the 15-150 keV band is 5.7 +- 1.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+49.40 sec in the 15-150 keV band
is 0.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/578227/BA/

We note that the fluence ratio in a simple power-law fit between the
25-50 keV band and the 50-100 keV band is 1.92.  This fluence ratio is larger
than 1.32 which can be achieved in the Band function of alpha=-1.0, beta=-2.5,
and Epeak=30 keV.  Thus, preliminary analysis shows that Epeak of the burst
is very likely around or below 30 keV.  Therefore the burst can be classified
as an X-ray flash (e.g. Sakamoto et al. 2008, ApJ, 679, 570).


GRB_name: GRB131122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15509
SUBJECT: GRB 131122A (INTEGRAL trigger N6392): MASTER-NET  optical observation
DATE:    13/11/22 22:07:24 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)


There are two telescope from MASTER-NET was pointed to the  GRB131122A.

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB131122A 69 sec  after notice 
time and 76 sec after GRB time at 2013-11-22 21:26:33.898 UT in two 
polarizations. On our first (20s exposure) set we haven't found optical 
transient  within INTEGRAL trigger N 6392 error-box (ra=10 11 02 dec=+57 
38 22 r=0.054667). The polaroids have RA and DEC orientation on this 
observatory.
The 5-sigma upper limit has been about 16.4 mag

MASTER II  robotic telescope located in Blagoveschensk was pointed to the 
GRB131122A 76 sec  after notice time and 82 sec after GRB time at 
2013-11-22 21:26:39.328 UT in two polarizations. On our first (20s 
exposure) set we haven't found optical transient  within INTEGRAL trigger 
N 6392 error-box (ra=10 11 02 dec=+57 38 22 r=0.054667). The polaroids are 
oriented under corners 45 and 135 to the RA axis on this observatory.
The 5-sigma upper limit has been about 16.3 mag
The message may be cited.

The data reduction are continued.

The message may be cited.


GRB_name: GRB131122A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15510
SUBJECT: GRB 131122A: a long GRB detected with INTEGRAL
DATE:    13/11/22 22:39:22 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

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

a gamma ray burst lasting about 70 s  has been detected by IBAS in the IBIS/ISGRI data at 21:25:01 U.T. on November 22.
Its refined  coordinates (J2000)  are:

  R.A.: 152.5553 deg
  DEC.: 57.7398 deg

with an uncertainty of 1.6 arc min (90% c.l.).

The burst had a fluence of about 2x10^-6 erg/cmsq in the 20-200 keV energy band, and a peak flux of 0.4 ph/cmsq/s in the same energy band over 1 s.

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


GRB_name: GRB131122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15511
SUBJECT: GRB 131122A: Nanshan optical upper limit
DATE:    13/11/22 23:13:04 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), G.-J. Feng, X. Zhang, A. Esamdin, L. Ma (XAO) report:

We observed the IBIS/ISGRI field of GRB 131122A (Gotz et al., GCN
15510) using the 1m telescope located on Mt. Nanshan, Xinjiang, China.
We obtained 6x360s R-band frames at a mean time of 22:28:18 UT on
2013-11-22, i.e., 1.055 hr after the INTEGRAL trigger.

Visual inspect of the Intergral 1.6 arcmin error circle against DSS II
and SDSS shows that no new optical source is detected down to a
limiting magnitude of R=20.6 mag.


GRB_name: GRB131122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15512
SUBJECT: GRB 131122A: i-band observations from NOT
DATE:    13/11/23 02:08:00 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI),  D. Xu (DARK/NBI), S. Schulze (PUC, MCSS), N.R. Tanvir (U. Leicester),  O. Smirnova (NOT, U. Latvia), J. Kre (U. Oslo), E. Pakstiene (Vilnius U.), A.B. Aksnes, C. Eide, E.N. Traore, J. Joberg, L.K. Seljebotn, N. Von Huth, M. Lapadatu, R.W. Cale, M Heger (Horten videregende skole) report on behalf of a larger collaboration:

We observed the field of the INTEGRAL GRB 131122A (Gorbovskoy et al., GCN 15509) with the 2.5m Nordic Optical Telescope (NOT) equipped with ALFOSC. Observations began at 00:34 UT (3.13 hr after the burst), when the field was at an airmass of ~3, and consisted of 8x180s in i-band, covering the complete INTEGRAL error box. The seeing of the combined image is around 0.9".

We do not see any obvious new source down to the limit of the SDSS i-band image to which we have compared, although we note that our frame is somewhat deeper, showing faint sources not present in the SDSS. A more precise localisation and/or deeper comparison image will be needed in order to identify a possible optical counterpart to GRB 131122A.


GRB_name: GRB131122A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15513
SUBJECT: GRB 131122A: Swift-XRT observations
DATE:    13/11/23 09:31:05 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA) and V. D'Elia (ASDC) report on behalf of the
Swift-XRT team:

We have analysed 3.0 ks of XRT data for the INTEGRAL-detected burst GRB
131122A, from 13.7 ks to 21.1 ks after the INTEGRAL trigger. The data
are entirely in Photon Counting (PC) mode. An X-ray source is detected
within the INTEGRAL error circle. Using 1383 s of PC mode data and 1
UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 152.54219, +57.72770 which is equivalent to:

RA (J2000): 10h 10m 10.12s
Dec(J2000): +57d 43' 39.7"

with an uncertainty of 4.8 arcsec (radius, 90% confidence). This
position is 50 arcsec from the INTEGRAL position. We cannot determine
at the present time whether the source is fading.
 
We note the presence of two DSS galaxies northbound the XRT source,
close to the XRT error circle.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020328.

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


GRB_name: GRB131122A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15514
SUBJECT: GRB 131122A: Upper limit from NOT imaging
DATE:    13/11/23 10:49:11 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (IAA-CSIC/UPV-EHU),
D. Xu (DARK/NBI), S. Schulze (PUC, MCSS), N.R. Tanvir (U. Leicester), 
O. Smirnova (NOT, U. Latvia), J. Kre (U. Oslo), E. Pakstiene (Vilnius U.),
A.B. Aksnes, C. Eide, E.N. Traore, J. Joberg, L.K. Seljebotn, N. Von Huth,
M. Lapadatu, R.W. Cale, M Heger (Horten videregende skole) report on 
behalf of a larger collaboration:

Further analysis of our i-band imaging from the 2.5 m NOT (Gorosabel et al., 
GCN 15512) of GRB 131122A (Gotz et al., GCN 15510), with mean epoch 
00:49 UT (3.40 hr after the burst), shows no new source within the Swift-XRT 
error box (Maselli et al., GCN 15513) down to a 3-sigma magnitude limit of 
i=23.5 (AB).


GRB_name: GRB131122A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15515
SUBJECT: GRB 131122A: Swift/UVOT Upper Limits
DATE:    13/11/23 15:59:12 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and A. Maselli (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 131122A
13578 s after the INTEGRAL trigger (Gotz et al., GCN Circ. 15510).
No optical counterpart consistent with the potential XRT afterglow position
(Maselli et al., GCN Circ. 15513) is detected in the initial UVOT exposures.

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

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

white            14302        20578          855         >21.3
v                20830        21061          227         >19.0
u                13578        20136         1375         >21.0

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: GRB131127A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15516
SUBJECT: GRB 131127A: Swift detection of a burst
DATE:    13/11/27 10:33:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. B. Markwardt (NASA/GSFC), S. D. Barthelmy (GSFC),
S. B. Cenko (GSFC), V. D'Elia (ASDC), D. Malesani (DARK/NBI),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and P. Romano (INAF-IASFPA) report on behalf of
the Swift Team:

At 10:11:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131127A (trigger=579571).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 332.751, +36.590 which is 
   RA(J2000)  =  22h 11m 00s
   Dec(J2000) = +36d 35' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several overlapping
peaks with a duration of about 50 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at 0 sec after the trigger. 

The XRT began observing the field at 10:13:09.3 UT, 93.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
332.7293, 36.6098 which is equivalent to:
   RA(J2000)  = 22h 10m 55.03s
   Dec(J2000) = +36d 36' 35.2"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 94 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 1.15
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.33e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 102 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
Data from the list of sources generated on-board are not available at this
time. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.14. 

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


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15517
SUBJECT: GRB 131127A: MASTER-NET  optical observations
DATE:    13/11/27 10:38:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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, 
D.Denisenko, A.Sankovich
Sternberg Astronomical Institute, Moscow State University

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, 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 Tunka was pointed to the  GRB131127A 503 sec after GRB time and 
40 sec after notice time at 2013-11-27 10:19:58 UT in two polarizations. 
On our first (100s  exposure) set we haven't  found optical transient 
within SWIFT error-box (ra=22 11 00 dec=+36 35 24 r=0.050000).
The 5-sigma upper limit has been about 17.5 mag
The message may be cited.


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15518
SUBJECT: GRB 131127A: Nanshan optical upper limit
DATE:    13/11/27 12:33:21 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), J.-Z. Liu, G.-J. Feng, H.-B. Niu, C.-H. Bai, A.
Esamdin, L. Ma (XAO) report:

We observed the field of GRB 131127A (Markwardt et al., GCN 15516)
using 1m telescope located on Mt. Nanshan, Xinjiang, China.
Observations started at 11:45:12 UT on 2013-11-27 (i.e., 1.56 hr after
the BAT trigger) and a series of R-band frames were obtained.

Within the SPER XRT error circle (http://www.swift.ac.uk/sper/) of
this burst, no crediable optical source is detected down to a limiting
magnitude of R=20.5 mag, calibrated with nearby USNO B1 field.


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15519
SUBJECT: GRB 131127A: Mondy optical upper limit
DATE:    13/11/27 13:18:01 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

E. Klunko (ISTP), A.Volnova (IKI),  M. Eselevich (ISTP), A. Pozanenko(IKI)
report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 131127A (Markwardt et al., GCN
15516)  with AZT-33IK telescope of Sayan observatory (Mondy) starting Nov.,
27 (UT) 10:40:06. We obtained  several images in R-filter with exposure of
30 and 60 seconds. Within the XRT circle  (Markwardt et al., GCN 15516)  we
did not detect any optical object.

The details of the photometry are the following:

UT start,      t-T0           Filter    Exp.             OT     UL
                 (mid, days)              (s)                        (3 sigma)
10:40:06     0.02839       R        7*30+21*60    n/d    21.3

The photometry is based on 3 USNO-B1.0 stars:

USNO-B id     RA              Dec             R2
1265-0518495 22:11:06.80 +36:35:45.6 16.06
1265-0518432 22:10:59.37 +36:35:56.7 16.45
1266-0522367 22:10:48.55 +36:36:43.7 15.45


GRB_name: GRB131127A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15520
SUBJECT: GRB 131127A: Enhanced Swift-XRT position
DATE:    13/11/27 20:23:42 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 3638 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 131127A, 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 = 332.73008, +36.60929 which is equivalent
to:

RA (J2000): 22h 10m 55.22s
Dec (J2000): +36d 36' 33.5"

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

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

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


GRB_name: GRB131127A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15521
SUBJECT: GRB 131127A, Swift-BAT refined analysis
DATE:    13/11/27 20:49:44 GMT
FROM:    Craig Markwardt at NASA/GSFC  <craigm@milkyway.gsfc.nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
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-240 to T+960 sec from the recent telemetry 
downlink, we report further analysis of BAT GRB 131127A (trigger 
#579571) (Markwardt, et al., GCN Circ. 15516).  The BAT 
ground-calculated position is
RA, Dec = 332.714, 36.596 deg which is
    RA(J2000)  =  22h 10m 51.3s
    Dec(J2000) = +36d 35' 46.9"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 39%.

The mask-weighted light curve has multiple peaks.  The first set of 
about 3 peaks occurs before the initial trigger between T-60 and T-38 
sec.  The main set of about 7-8 peaks occurs between T-5 and T+40 sec. 
The peak emission occurs at about T+0 sec.  T90 (15-350 keV) is 92.1 +- 
10.2 sec (estimated error including systematics).

The time-averaged spectrum from T-59.4 to T+37.5 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 2.34 +- 0.16.  The fluence in the 15-150 keV band is 1.9 +- 
0.2 x 10^-6 erg/cm2.  The 1-sec peak photon flux measured from T-0.54 
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/579571/BA/


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15522
SUBJECT: GRB 131127A. 1.5m OSN optical limit
DATE:    13/11/27 22:24:50 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. Sota, J. Gorosabel and A. J. Castro-Tirado (IAA-CSIC Granada) on behalf
of a larger collaboration, report:

"Following the detection of GRB 131127A by Swift (Markwardt et al. GCNC
15516), we have conducted I-band observations with the 1.5m OSN telescope at
Observatorio de Sierra Nevada (Granada, Spain), starting on 27 Nov 18:26
UT,(i.e. 8.2-hr post burst). A stack of 17 x 300s images shows nothing at
the enhanced Swift/XRT position (Evans et al. GCNC 15520) down to I = 21".


GRB_name: GRB131127A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15523
SUBJECT: GRB 131127A: Swift-XRT refined Analysis
DATE:    13/11/27 22:33:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.5 ks of XRT data for GRB 131127A (Markwardt et al.
GCN Circ. 15516),  from 84 s to 24.3 ks after the  BAT trigger. The
data comprise 62 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by Evans
et al. (GCN. Circ 15520).

The late-time light curve (from T0+4.5 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.55 (+0.26, -0.22).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.8 (+0.4, -0.3). The
best-fitting absorption column is  3.9 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.22 (+/-0.15) and a
best-fitting absorption column of 2.5 (+0.5, -0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (6.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.5 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 5.1 sigma
Photon index:      2.22 (+/-0.15)

If the light curve continues to decay with a power-law decay index of
1.55, the count rate at T+24 hours will be 2.3 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.0 x
10^-14 (1.4 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/00579571.

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


GRB_name: GRB131127A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15525
SUBJECT: GRB 131127A: RATIR Optical and NIR Observations, High-z Candidate
DATE:    13/11/28 08:41:53 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
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 131127A (Markwardt, et al., GCN 15516) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional
on Sierra San Pedro Mrtir from 2013/11 28.11 to 2013/11 28.26 UTC (16.42
to 19.94 hours after the BAT trigger), obtaining a total of 2.49 hours
exposure in the r and i bands and 1.04 hours exposure in the Z, Y, J, and H
bands.

We do not detect any sources within the Enhanced Swift-XRT error circle
(Evans et al., GCN 15520), in comparison with 2MASS, we obtain the
following upper limits (3-sigma):

  r > 24.19
  i > 23.53
  Z > 22.78
  Y > 22.16
  J > 22.04
  H > 21.48

However, we do detect a red source just outside (3.3" away from the center)
of the XRT position, at a position RA, DEC = 332.731227 , 36.609171 (J2000,
+/- 0.5").  We measure:

  r = 24.21 +/- 0.35
  i = 22.48 +/- 0.11
  Z = 21.85 +/- 0.16
  Y = 21.22 +/- 0.15
  J = 21.03 +/- 0.14
  H = 20.88 +/- 0.20

The faint flux in r band relative to the redder bands could be due to IGM
attenuation at high redshift, z ~ 5.  We cannot confirm fading of this
source.  Further observations of this source are encouraged.

The magnitudes above are in the AB system and are not corrected for
Galactic extinction, E[B-V]~0.1, in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15526
SUBJECT: GRB 131127A: AROMA-N Optical Observation
DATE:    13/11/28 11:36:56 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. Kawamura, T. Sakamoto, I. Takahashi, S. Sugai, A. Yoshida (AGU)

We observed the field of GRB 131127A detected by Swift (trigger #579571; 
Markwardt et al., GCN Circ. 15516) with the 12-inch AGU Robotic Optical 
Monitor for Astrophysical object - Narrow (AROMA-N) located at the Sagamihara 
campus of Aoyama Gakuin University.  

60 images of 60 sec exposures were taken in the R filter starting from 
November 27 10:42:18 (UT) about 30 minutes after the trigger and 
stopped on November 27 11:48:15 (UT).  We do not detect the optical 
afterglow both in the individual images and the stacked image, which 
combined 57 good quality images, inside the enhanced XRT position 
(Evans, et al., GCN #15520).  The estimated five sigma upper limit of 
the combined image (total exposure of 3420 sec) is ~16.6 mag using 
the USNO-B1 catalog.

[GCN OPS NOTE(29nov13): Per author's request, the "November 11" date
was changed to "November 27" in two places.]


GRB_name: GRB131127A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15527
SUBJECT: GRB 131127A: Swift/UVOT Upper Limits
DATE:    13/11/28 11:56:24 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and C. B. Markwardt (NASA/GSFC) report on 
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 131127A 
102 s after the BAT trigger (Markwardt et al., GCN Circ. 15516).
No optical afterglow consistent with the XRT position (Evans et al. GCN 
Circ. 15520) nor the RATIR position (Butler et al. GCN Circ. 15525) 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           102          252          147         >21.4
u_FC               315          565          246         >20.6
white              102         6711          746         >22.3
v                  645         7024          373         >20.3
b                  571         6506          452         >21.2
u                  315         6300          678         >21.1
w1                 694         6095          432         >20.6
m2                 669         5890          269         >20.1
w2                 621         6916          471         >20.9

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


GRB_name: GRB131127B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15528
SUBJECT: GRB 131127B: Fermi GBM detection
DATE:    13/11/28 12:53:49 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 14:12:18.36 UT on 27 November 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131127B (trigger 407254341 / 131127592).
The on-ground calculated location, using the GBM trigger
data, is RA = 306.1, DEC = -0.8 (J2000 degrees,
equivalent to 20h 24m, -00d 48'), with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 88 degrees.

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

Three candidates for an optical afterglow were found by iPTF 
(Singer et al, GCN 15524) using the GBM on-ground location.

The GBM light curve is multi-peaked with a duration (T90) 
of about 18 s (50-300 keV).
The time-averaged spectrum from T0-0.003 s to T0+20.480 s is
best fit by a Band function with Epeak = 181.7 (+7.9/-7.2) keV,
alpha = -1.05 +/- 0.02 , and beta = -2.24 (+0.05/-0.06)

The event fluence (10-1000 keV) in this time interval 
is (3.85 +/- 0.03)E-05  erg/cm^2. The 1.024-sec peak photon 
flux measured starting from T0+5.824 s in the 10-1000 keV band
is 37.6 +/- 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: GRB131127B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15529
SUBJECT: IPN Triangulation of GRB 131127B
DATE:    13/11/28 13:02:01 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

V. Connaughton, M. S. 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, and

K. Hurley on behalf of the IPN team, report:

The long-duration, intense GRB 131127B (von Kienlin, GCN 15528) has been 
observed by Fermi (GBM: trigger 407254341),  INTEGRAL (SPI-ACS), and 
Konus-Wind, so far, at about 51138 s UT (14:12:18).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   304.839 (20h 19m 21s)  -2.830 ( -2d 49' 46")
  Corners:
   304.599 (20h 18m 24s)  -0.050 ( +0d 03' 01")
   305.856 (20h 23m 26s)  -5.612 ( -5d 36' 45")
   305.066 (20h 20m 16s)  -5.608 ( -5d 36' 28")
   303.808 (20h 15m 14s)  -0.033 ( +0d 02' 00")
  ---------------------------------------------
The error box area is 4.38 sq. deg, and its maximum
dimension is 5.9 deg (the minimum one is 0.77 deg).
The Sun distance was 62 deg.

This box can be improved.

All optical afterglow candidates reported by iPTF (Singer, GCN 15524) 
are far outside of the box.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB131127_T51139/IPN/


GRB_name: GRB131127B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15530
SUBJECT: Konus-Wind observation of GRB 131127B
DATE:    13/11/28 13:06:06 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The bright, long-duration GRB 131127B
(Fermi GBM detection: von Kienlin, GCN 15528;
IPN triangulation: Golenetskii at al., GCN 15529)
triggered Konus-Wind at T0=51139.678 s UT (14:12:19.678).

The burst light curve shows multiple overlapped pulses
from ~T0-0.5 s to ~T0+20 s.
The emission is seen up to ~12 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131127_T51139/

As observed by Konus-Wind, the burst
had a fluence of (4.1  0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.160 s,
of (1.15  0.08)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+21.760 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.20  0.11,
the high energy photon index beta = -2.51  0.19,
the peak energy Ep = 165  17 keV,
chi2 = 140/97 dof.

The spectrum near the maximum count rate
(measured from T0 to T0+5.376 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.92  0.14,
the high energy photon index beta = -2.43  0.19,
the peak energy Ep = 218  27 keV,
chi2 = 128/97 dof.

All the quoted values are preliminary.


GRB_name: GRB131127B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15531
SUBJECT: GRB 131127B: Nanshan optical observations
DATE:    13/11/28 13:25:05 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), H.-B. Niu, J.-Z. Liu, G.-J. Feng, C.-H. Bai, A.
Esamdin, L. Ma (XAO) report:

We observed the fields of the three afterglow candidates of GRB
131127B (von Kienlin, GCN 15528; Singer & Kasliwal, GCN 15524;
Golenetskii et al., GCN 15530), using the 1m telescope located on Mt.
Nanshan, Xinjiang, China. Observations started at 11:37:34 UT on
2013-11-28, (i.e., 21.42 hr after the Fermi trigger) and a series of
R-band frames were obtained.

The three optical afterglow candidates are clearly detected in their
stacked images.

For the one dubbed iPTF13ecv, we measure its magnitude
m(R)=18.66+/-0.14, calibrated with two nearby SDSS stars and using the
Lupton (2005) transformation. This magnitude is basically consistent
with the value reported in Singer & Kasliwal (GCN 15524), indicating
that its significant fading is ruled out.

For the other two dubbed iPTF13ect and iPTF13ecu, given that they are
very close to the cores of the galaxies and not well resolved in our
images, we are not able to put good constraints on their magnitudes at
the moment.


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15532
SUBJECT: GRB 131127A: Bassano Bresciano Observatory optical upper limit
DATE:    13/11/28 15:00:35 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the field of GRB 131127A detected 
by SWIFT(trigger 00579571) with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy (www.osservatoriobassano.org).

The observations started 9h 2m. after the 
GRB trigger,with our schmidt telescope 
D=320/400 mm F/D=3.1.

Weather conditions were good.

We co-added a series of 5 exposures of 120 sec each.

We did not found any optical counterpart 
in the error box of the XRTcandidate
(Markwardt et al., GCN 15516).

Start      End       R.lim
542min     554min    18.5

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

The message may be cited.


GRB_name: GRB131128A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15533
SUBJECT: GRB 131128A: Swift detection of a burst
DATE:    13/11/28 15:22:39 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), W. H. Baumgartner (GSFC/UMBC),
M. G. Bernardini (INAF-OAB), S. B. Cenko (GSFC),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), S. T. Holland (STScI),
A. Y. Lien (NASA/GSFC/ORAU), D. Malesani (DARK/NBI),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester) and E. Troja (NASA/GSFC/UMCP) report
on behalf of the Swift Team:

At 15:06:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131128A (trigger=579683).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 355.323, +31.279 which is
   RA(J2000) = 23h 41m 18s
   Dec(J2000) = +31d 16' 45"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve showed a single FRED peak
structure with a duration of about 3 sec with a possible precursor
around T-8.  The peak count rate was ~3000 counts/sec (15-350 keV),
at ~0 sec after the trigger.

The XRT began observing the field at 15:07:51.3 UT, 86.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 355.3084,
31.3057 which is equivalent to:
   RA(J2000)  = 23h 41m 14.02s
   Dec(J2000) = +31d 18' 20.7"
with an uncertainty of 2.2 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 5.16
x 10^20 cm^-2 (Kalberla et al. 2005).

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 90 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.07.

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: GRB131127B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15534
SUBJECT: GRB 131127B: MASTER-Net  optical observations 
DATE:    13/11/28 15:22:44 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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, D.Denisenko, 
Sternberg Astronomical Institute, Moscow State University

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, 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 Tunka was pointed to the  GRB131127.59 73 sec after GRB time at 
2013-11-27 14:13:31.093 UT.

Fortunately, the central part (42%) of the IPN error box (Golenetskii et 
al., GCN 15529) was covered by first MASTER image (10s exposure). 
Unfortunatelly, observations was done at the very high zenit distance (~85 
degrees).

We haven't  found optical transient.
The 5-sigma upper limit has been about 14.1 mag
We have 4 images (the one of the tube was under horizont):

Id (image)     Coord              Pro.type     time    Exp.time  Limit

587443  20h 19m 27.4s -02d 51m 25s   Alert       14:13:31    10      14.1
587444  20h 19m 27.3s -02d 51m 31s   Alert       14:14:29    30      15.0
587446  20h 19m 27.0s -02d 51m 41s   Alert       14:15:52    40      14.8
587448 20h 19m 27.1s -02d 51m 42s   Alert   14:17:38    60      15.0

The fist image (FOW = 2x2 degrees) with IPN error box is available at 
http://master.sai.msu.ru/static/GRB/grb131127_IPN.jpeg .
The reduction is continued.
The message may be cited.


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15535
SUBJECT: GRB 131128A: Nanshan afterglow candidate
DATE:    13/11/28 15:49:12 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), H.-B. Niu, J.-Z. Liu, G.-J. Feng, C.-H. Bai, A.
Esamdin, L. Ma (XAO) report:

We observed the fields of GRB 131128A (Sonbas et al., GCN 15533),
using the 1m telescope located on Mt. Nanshan, Xinjiang, China.
Observations started 880s after the Swift trigger and a series of
R-band frames were obtained.

An optical source is clearly detected at coordinates:

R.A. (J2000) = 23:41:13.75
Dec.(J2000) = +31:18:23.14

Error Radius: ~1 arcsec

which is consistent with the SPER XRT position of this burst
(http://www.swift.ac.uk/sper/), thus it's likely the afterglow of the
GRB.

Note that there is a very bright star (r=14.76 mag from SDSS) just a
few arcsec away from this optical transient. Observations are ongoing.


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15536
SUBJECT: GRB 131128A: MASTER-Net  optical observations
DATE:    13/11/28 16:59:35 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,
Sternberg Astronomical Institute, Moscow State University

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


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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, 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  GRB131128.63 12 sec  after 
notice time and 315 sec after GRB time at 2013-11-28 15:11:39.707 UT. On 
our first (60s exposure) set we haven't found optical transient  within 
XRT SWIFT error-box.

There is bright star near XRT position USNO-A2.0 1200-19996598 R_mag ~ 12.
The 5-sigma upper limit has been about 17.1 mag.
We do not see OT at the Nanshan afterglow candidate position (Xu et al., 
GCN15535). 
The message may be cited.


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15537
SUBJECT: GRB 131128A: Nanshan afterglow confirmation
DATE:    13/11/28 17:21:23 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), H.-B. Niu, J.-Z. Liu, G.-J. Feng, C.-H. Bai, A.
Esamdin, L. Ma (XAO) report:

Continued observations of GRB 131128A, 120s each for the beginning and
240s each for the subsequent all in R-band, at the Nanshan observatory
show that the afterglow candidate in Xu et al (GCN 15535) has decayed
by more than 1 magnitude at 1.95 hr after the Swift trigger,
calibrated with the same nearby SDSS stars. The initial magnitude is
R~19 mag in GCN 15535. We thus conclude that this object is the
optical afterglow of GRB 131128A.


GRB_name: GRB131128A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15538
SUBJECT: GRB 131128A: Enhanced Swift-XRT position
DATE:    13/11/28 20:20:50 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 1158 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 131128A, 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 = 355.30781, +31.30635 which is equivalent
to:

RA (J2000): 23h 41m 13.88s
Dec (J2000): +31d 18' 22.9"

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: GRB131128A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15539
SUBJECT: GRB 131128A: Swift-BAT refined analysis
DATE:    13/11/28 20:51:42 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
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-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 131128A (trigger #579683)
(Sonbas, et al., GCN Circ. 15533).  The BAT ground-calculated position is
RA, Dec = 355.305, 31.293 deg which is 
   RA(J2000)  =  23h 41m 13.3s 
   Dec(J2000) = +31d 17' 34.1" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.
 
The mask-weighted light curve shows a single symetric peak starting 
at ~T-2 sec, peaking at ~T+0.2 src, and ending at ~T+2.5 sec.
T90 (15-350 keV) is 3.00 +- 1.41 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.90 to T+2.10 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.81 +- 0.17.  The fluence in the 15-150 keV band is 3.2 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.10 sec in the 15-150 keV band
is 2.7 +- 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/579683/BA/


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15540
SUBJECT: GRB 131128A: T100 observations
DATE:    13/11/28 22:43:36 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), T. Guver (Sabanci Univ.), E. Gogus (Sabanci
Univ.),
O. Erece (Akdeniz Univ), M. Kocak (TUG), M. Kaplan (Akdeniz Univ.) report
on behalf of a larger collaboration

    We observed the field of Swift GRB 131128A (Sonbas et al., GCN#15533)
with the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National
Observatory, Turkey), starting November, 28, 17:16:02 UT (~ 2.2 hours after
the trigger). 300 s $\times$ 5  exposures were obtained in the R filter
under moderate weather conditions.

We do not detect an optical  afterglow within the reported XRT error circle
down to  a limiting magnitude of 21.2 in the  R band. Our image is
calibrated  using USNO B1.0  star USNO-B1 1213-0590145 at  RA :355.25992,
DEC : +31.301542 (J2000).

We are grateful to TUBITAK National Observatory for prompt scheduling the
observations and technical support.


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15541
SUBJECT: GRB 131128A: Kanata/HOWPol optical observation
DATE:    13/11/29 03:01:30 GMT
FROM:    Koji Kawabata at HASC,Hiroshima U  <kawabtkj@hiroshima-u.ac.jp>

K. S. Kawabata, R. Itoh, N. Ebisuda, I. Ueno (Hiroshima Univ.) 
report on behalf of Kanata team:

We performed a series of optical imaging (polarimetric mode) for 
the optical afterglow of GRB 131128A (Sonbas et al., GCN 15533; 
Xu et al., GCN 15535; Gorbovskoy et al, GCN 15536; Goad et al., 
GCN 15538; Sonbas et al., GCN 15540) using HOWPol attached to 
the 1.5-m Kanata telescope at Higashi-Hiroshima Observatory, Japan. 

Our first 30 sec exposure began at t=360 sec since Swift/BAT trigger
and we detected the afterglow located at 9" west and 4" north of the 
bright star, USNO-B 2766-00858-1 (R2 = 11.63 mag). The magnitude of 
the afterglow is preliminarily estimated to be about R=17.5, although 
it might be still contaminated by the neaby bright star. The afterglow
quickly decayed and became fainter than ~18 mag at t=620 sec.


GRB_name: GRB131128A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15542
SUBJECT: GRB 131128A: Swift-XRT refined Analysis
DATE:    13/11/29 07:22:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester), A. Melandri
(INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), P. D'Avanzo (INAF-OAB), D.N.
Burrows (PSU), J.A. Kennea (PSU), V. Mangano (PSU), J.P. Osborne (U.
Leicester) and E. Sonbas report on behalf of the Swift-XRT team:

We have analysed 7.6 ks of XRT data for GRB 131128A (Sonbas  et al. GCN
Circ. 15533),  from 72 s to 40.8 ks after the  BAT trigger. The data
comprise 7 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Goad et al. (GCN. Circ 15538).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.9 (+/-0.4). At T+423 s  the decay
flattens to an alpha of 0.38 (+0.08, -0.14) before breaking again at
T+16.0 ks to a final decay with index alpha=1.7 (+0.7, -0.6).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.53 (+0.18, -0.12). The
best-fitting absorption column is  5.8 (+4.6, -0.7) 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 4.6 x 10^-11 (5.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.8 (+4.6, -0.7) x 10^20 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.53 (+0.18, -0.12)

If the light curve continues to decay with a power-law decay index of
1.7, the count rate at T+24 hours will be 3.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (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/00579683.

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


GRB_name: GRB131127B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15543
SUBJECT: GRB 131127B: Bassano Bresciano Observatory optical observations
DATE:    13/11/29 09:49:11 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the fields of GRB 131127B 
(von Kienlin, GCN 15528; Singer & Kasliwal, 
GCN 15524; Golenetskii et al., GCN 15530) with the robotic    
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy (www.osservatoriobassano.org).

The observations started 27h 55m. after the    
Fermi-GBM trigger (Fermi407254341) , with our 
schmidt telescope D=320/400 mm F/D=3.1.

Weather conditions were good.     

We co-added 3 series of 5 unfiltered exposures 
of 120 sec each.      

We detected the candidate couterpart of iPTFecv 
(Singer et al, GCN 15524) at the following 
position (+/- 1 arcsec):

RA (J2000) =  20h 31m 47.79s 
DEC(J2000) = +00d 59m 22.8s

The results of our photometry are:

    Date UT          Exp    R-mag     
    Middle           (s)   (rough)

2013 11 28.75862     600    18.84 +/- 0.2
2013 11 28.76579     600    18.85 +/- 0.2
2013 11 28.77297     600    19.08 +/- 0.3


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

The images are available at:
http://www.osservatoriobassano.org/GRB.asp

The message may be cited.


GRB_name: GRB131128A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15544
SUBJECT: GRB 131128A: AROMA-N Optical Observation
DATE:    13/11/29 11:17:17 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. Kawamura, T. Sakamoto, I. Takahashi, S. Sugai, A. Yoshida (AGU)

We observed the field of GRB 131128A detected by Swift (trigger #579683; 
Sonbas et al., GCN Circ. 15533) with the 12-inch AGU Robotic Optical 
Monitor for Astrophysical object - Narrow (AROMA-N) located at the Sagamihara 
campus of Aoyama Gakuin University.  

60 images of 10 sec exposures were taken in the R filter starting from 
November 28 15:12:47 (UT) about 383 sec after the trigger 
(77 sec after the BAT position notice) and stopped on November 28 15:30:30 (UT).  
We do not detect the optical afterglow both in the individual images and 
the stacked image inside the enhanced XRT position (Evans, et al., GCN #15538).  
The estimated five sigma upper limit of the combined image (total exposure of  600 sec) 
is ~16.2 mag using the USNO-B1 catalog.  


GRB_name: GRB131128A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15545
SUBJECT: GRB 131128A: Swift/UVOT Detection
DATE:    13/11/29 11:54:03 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL) 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 131128A
91 s after the BAT trigger (Sonbas et al., GCN Circ. 15533).
A source consistent with the optical position (Xu et al., GCN Circ. 15535) 
and the enhanced Swift-XRT position (Goad et al., GCN Circ 15538) is 
detected in the first UVOT white exposure only. A USNO-B1 catalogued star 
heavily contaminates the position of the optical candidate afterglow 
making the measurement very complicated.

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 (FC)          91          241           147        19.11 +/- 0.11
white      583         1181          206      >21.44
u (FC)              303         552           245        >20.2
u                   303         1130          285      >20.3
v                   632         1231          78         >19.0
b                   558         1155          58         >19.8
w1                  683         1275          53         >18.9
m2                  657         1255          78         >19.0
w2                  608         1206          78         >19.4

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


GRB_name: GRB131125A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15546
SUBJECT: IPN Triangulation of GRB 131125A (short/hard)
DATE:    13/11/29 13:08:03 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, 
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, and

K. Hurley on behalf of the IPN team, report:

The short-duration, hard spectrum GRB 131125A has been observed by Fermi 
(GBM: trigger 407089974), INTEGRAL (SPI-ACS), and Konus-Wind, so far, at 
about 59571 s UT (16:32:51).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   114.675 (07h 38m 42s) +48.414 (+48d 24' 49")
  Corners:
   114.485 (07h 37m 56s) +45.684 (+45d 41' 01")
   115.166 (07h 40m 40s) +45.939 (+45d 56' 21")
   114.817 (07h 39m 16s) +51.137 (+51d 08' 15")
   114.077 (07h 36m 18s) +50.873 (+50d 52' 22")
  ---------------------------------------------
The error box area is 2.5  sq. deg, and its maximum
dimension is 5.5 deg (the minimum one is 29 arcmin).
The Sun distance was 130 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB131125_T59571/IPN/

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


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15547
SUBJECT: GRB 131128A: GROND observations of the afterglow
DATE:    13/11/29 14:41:34 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Schmidl, S. Klose, A. Nicuesa Guelbenzu (TLS Tautenburg), and J. 
Greiner (MPE Garching) report:

We observed the field of GRB 131128A (Swift trigger 579683; Sonbas et al., 
GCN 15533) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla 
Observatory (Chile).

Observations started at 00:27 UT on November 29, about 9.5 hrs after the 
GRB trigger and were performed under moderate seeing conditions (1.6") and 
moderate airmass (2.3). For the optical afterglow discovered by Xu et al. 
(GCN 15535, 15537) we measure

RA, DEC (J2000) = 23:41:13.795, +31:18:22.32 (+/- 0.2"),

and

r'(AB) = 22.6 +/- 0.1,

calibrated against SDSS field stars (mean time 01:12 UT). Photometry in 
the other GROND bands is affected by a bright star very close to the 
afterglow. It might be improved once second-epoch data are obtained.


GRB_name: GRB131127A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15548
SUBJECT: GRB 131127A: CQUEAN riz Observation
DATE:    13/11/29 14:43:29 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Changsu Choi (CEOU/SNU), Hyein Lee, Huynh Ahn N. Le,
and Soojong Pak (Kyunghee Univ.)

We observed the field of GRB 131127A (Markwardt et al. GCN 15516),
using CQEUAN (Park et al. 2012) on the 2.1-m Otto-Struve telescope 
at the McDonald Observatory in Texas, US. The observation started 
at 2013-11-29 01:31:43 UT, or about 1.63 days after the BAT alert. 
A series of images were taken in r, i, and z-band for about 45 min.

We identify the red source reported in Butler et al. (GCN 15525), but
no significant fading of the source was found with z = 21.90 +- 0.15 AB mag,
consistent with Z = 21.85 +- 0.16 mag from Butler et al. (GCN 15525).
This suggests that the red source may not be the GRB afterglow,
or the light curve is changing very slowly.


GRB_name: GRB131125A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15549
SUBJECT: Konus-Wind observation of GRB 131125A
DATE:    13/11/29 15:52:50 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, 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 131125A
(IPN Triangulation: Golenetskii et al. GCN 15546)
triggered Konus-Wind at T0=59572.927 s UT (16:32:52.927).

The burst duration is ~0.5 s.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131125_T59572/

As observed by Konus-Wind, the burst
had a fluence of (1.3  0.2)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.064,
of (5.7  1.2)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The 3-channel time-integrated spectrum
(measured from T0-0.448 to T0+0.064 s)
can be modeled, in the 22 keV - 1.3 MeV range,
by the cutoff power law with the following model parameters:
the photon index alpha = 0.00  0.13,
and the peak energy Ep = 638  62 keV.

The 3-channel spectrum at the maximum count rate
(measured from T0-0.064 s to T0)
can be modeled, in the 22 keV - 1.3 MeV range,
by the cutoff power law with the following model parameters:
the photon index alpha = +0.2  0.3,
and the peak energy Ep = 665  113 keV.

All the quoted results are preliminary.


GRB_name: GRB131126A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15550
SUBJECT: IPN Triangulation of GRB 131126A (short/hard)
DATE:    13/11/29 16:58:21 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

K. Hurley on behalf of the IPN team, report:

The short-duration, hard spectrum, bright GRB 131126A has been observed 
by Fermi (GBM: trigger 407130853) and Konus-Wind, so far, at about 14050 
s UT (03:54:10).

We have triangulated it to a Konus-GBM annulus centered at 
RA(2000)=219.687 deg (14h 38m 45s)  Dec(2000)=-12.489 deg (-12d 29' 
20"), whose radius is 65.710 Â± 0.084 deg (3 sigma).

Combined with the GBM 1-sigma statistical+systematic error contour, this 
constrains the arrival direction to that portion of the annulus between 
RA, Dec = 206.1, +52.1 and 222.6, +53.2 degrees.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB131126_T14048/IPN/

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


GRB_name: GRB131126A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15551
SUBJECT: Konus-Wind observation of GRB 131126A
DATE:    13/11/29 17:01:35 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, 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, bright GRB 131126A
(IPN Triangulation: Golenetskii et al., GCN 15550)
triggered Konus-Wind at T0=14048.270 s UT (03:54:08.270).

The burst light curve shows a pulse with a duration of ~140 ms.
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/GRB131126_T14048/

As observed by Konus-Wind, the burst
had a fluence of (2.1  0.2)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.016,
of (2.4  0.2)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum
(measured from T0 to T0+0.128 s)
is best fit, in the 20 keV - 15 MeV range,
by a cutoff power law with the following model parameters:
the photon index alpha = -0.43  0.14
and the peak energy Ep = 633  85 keV,
chi2 = 46.2/65 d.o.f.

The spectrum near the maximum count rate
(measured from T0 to T0+0.064 s)
is best fit, in the 20 keV - 15 MeV range,
by a cutoff power law with the following model parameters:
the photon index alpha = -0.20  0.20
and the peak energy Ep = 680  100 keV,
chi2 = 40.6/60 d.o.f.


All the quoted results are preliminary.


GRB_name: GRB131125A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15552
SUBJECT: GRB 131125A: iPTF upper limits on the afterglow of a short GRB
DATE:    13/11/29 17:47:17 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories), and
S. B. Cenko (NASA/GSFC) report on behalf of the intermediate Palomar
Transient Factory (iPTF) collaboration:

The short-hard GRB 131125A triggered Fermi GBM (Fermi trigger 407089974)
at 2013-11-25 16:32:47 and was localized by IPN using Fermi, INTEGRAL,
and Konus-Wind (Golenetskii et al., GCN 15546).

Starting 2013-11-26 04:16 UT, we imaged about 95 deg^2 surrounding the
Fermi GBM localization, covering most of the intersection between the
GBM 1-sigma statistical+systematic error contour and the IPN Fermi-INTEGRAL
3-sigma annulus, also including the entire intersection with the Fermi-Wind
annulus. Using standard iPTF vetting procedures including Palomar 60-inch
follow-up, we find no afterglow candidates to an average limiting magnitude
of R~20.4 at 11.8 hours after the burst.

See http://www.its.caltech.edu/~lsinger/iptf/Fermi407089974.pdf for a
diagram of the PTF fields observed in relation to the Fermi and IPN
localizations.


GRB_name: GRB131125A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15553
SUBJECT: GRB 131125A: MASTER-Net very early optical observations
DATE:    13/11/29 18:47:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, 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  GRB131125A 10 s after notice 
time and 24 sec after GRB time at 2013-11-25 16:33:25 UT.
But IPN  error box (GCN 15546) was outside of FOV of our MASTER-II 
telescope and very wide field camera (usually we follow up all Fermi 
alerts).

After first coordinates specification we cover IPN error box using very 
wide field cameras. The first images covered  error-box was obtained 49 
sec after GRB time at 2013-11-25 16:33:40 UT.
The 5-sigma upper limit has been about 12 mag on single 5 seconds exposure 
images and 13.5 on coadd of first 14 consecutive images
The 5-sigma upper limit has been about 14.1 mag
We find several optical marginal candidates to OT.

Name        R.A.           Dec.      m
MASTER_1  114.775649     46.120371   13.6
MASTER_2  114.597740     48.927898   13.7
MASTER_3  114.835195     47.047021   13.0

One sigma coordinate error is +- 7 arcsec.

The first image available here:
http://master.sai.msu.ru/static/GRB/GRB131125_first.jpeg

The coadd images here:
http://master.sai.msu.ru/static/GRB/GRB131125_coadd.jpeg

The message may be cited.


GRB_name: GRB131128A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15554
SUBJECT: GRB 131128A; Fermi GBM observation
DATE:    13/11/29 20:02:16 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 131128A: Fermi GBM observation

Hoi-Fung Yu (MPE) reports on behalf of the Fermi GBM Team:

"At 15:06:25.28 UT on 28 November 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131128A (trigger 407343988 / 131128629), which
was also detected by the Swift/BAT (Sonbas et al., GCN 15533). This burst,
tentatively classified as a particle event by the FSW onboard, is in fact
a gamma-ray burst. The GBM on-ground location is consistent with the 
Swift/XRT position.

The angle from the Fermi LAT boresight is 71 degrees.

The GBM light curve consists of a single pulse with a duration (T90) of 
~2.0 s (50-300 keV). The time-averaged spectrum from T0-1.024 s 
to T0+2.560 s is adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.9 +/- 0.3 and the cutoff 
energy, parameterized as Epeak, is 61.0 +/- 9.0 keV.

The event fluence (10-1000 keV) in this time interval is
(4.4 +/- 0.5)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.83 s in the 10-1000 keV band is 3.8 +/- 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: GRB131127A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15555
SUBJECT: GRB 131127A: RATIR Rejection of High-z Candidate
DATE:    13/11/29 20:57:31 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
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We again observed the field of GRB 131127A (Markwardt, et al., GCN 15516)
with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio Astronmico
Nacional on Sierra San Pedro Mrtir from 2013/11 29.09 to 2013/11 29.17 UTC
(40.06 to 41.98 hours after the BAT trigger), obtaining a total of 1.42
hours exposure in the r and i bands and 0.60 hours exposure in the Z, Y, J,
and H bands.

For the red source 3.3" away from the center of the XRT positions (Butler
et al., GCN 15525), in comparison with 2MASS, we obtain:

r > 23.78
i = 22.68 +/- 0.16 (0.20 +/- 0.19)
Z = 22.02 +/- 0.26 (0.17 +/- 0.31)
Y = 21.31 +/- 0.24 (0.09 +/- 0.28)
J = 21.26 +/- 0.29 (0.23 +/- 0.32)
H = 20.55 +/- 0.24 (-0.33 +/- 0.31)

The change in magnitude relative to the observations on the previous night
are given in the parentheses.  There is slight (~<1-sigma) evidence for a
fade in most bands, but the shallowness ~t^(-0.2) of the fade is not
expected for a GRB afterglow.  We conclude, as did Im et al. (GCN 15548),
that this source is not the afterglow of GRB 131127A.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB131128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15556
SUBJECT: GRB 131128A: Bassano Bresciano Observatory optical upper limit
DATE:    13/12/01 15:34:26 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the field of GRB 131128A detected 
by SWIFT(trigger 579683) with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy (member of ISSP:Italian 
Supernovae Search Project)

The observations started 1h 28m after the                 
GRB trigger at the end of the twilight
with our schmidt telescope 
D=320/400 mm F/D=3.1.

Weather conditions were good.

We co-added 6 series of 10 exposures of 120 sec each.

We did not found any optical counterpart 
in the error box of the XRTcandidate
(E.Sonbas et al. GCNC 15533).

Start      End       Vlim
88min     279min     19.3                                   

The afterglow probably results absorbed in the light of 
the near star USNO-B 2766-00858-1 (R2 = 11.63 mag)   
due to the focal lenght very short (1000mm) of our 
Schmidt telescope.

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

The images are available at:
http://www.osservatoriobassano.org/GRB.asp

The message may be cited.


GRB_name: GRB131122A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15557
SUBJECT: GRB 131122A: Swift-XRT Further Observation
DATE:    13/12/01 18:49:09 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA) reports on behalf of the Swift-XRT team:

Swift-XRT performed a second observation of the INTEGRAL-detected burst 
GRB 131122A (Gotz et al., GCN Circ. 15510) starting on 2013 November 29, 
from 596 to 690 ks after the INTEGRAL trigger, for a total exposure of 
4.9 ks. The source reported in occasion of the first XRT observation by 
Maselli & D'Elia (GCN Circ. 15513) is now detected at a count rate of 
(1.59+/-0.69)e-3 ct/s. This value is considerably lower than 
(1.06+/-0.21)e-2 ct/s corresponding to the first observation: therefore, 
we point at this source as the afterglow of GRB 131122A.

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


GRB_name: GRB131127B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15558
SUBJECT: GRB 131127B: Bassano Bresciano Observatory optical observations of  iPTF13ecv
DATE:    13/12/01 21:25:56 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged again the field of iPTF13ecv optical afterglow
candidate of GRB 131127B (Leo Singer: GCN 15524) with
the robotic telescope of (IAU station 565) Bassano
Bresciano Observatory, Italy (member of ISSP:Italian
Supernovae Search Project).

We have observed that the brightness of this object
is not decreased during 5 days after the discovery.

Follow the results of our photometry +/- 0.2 mag:

    Date UT          Exp    R-mag
    Middle           (s)   (rough)

2013 11 28.76209     600    18.77
2013 11 28.76914     600    18.69
2013 11 28.76926     600    18.58
2013 11 28.77644     600    18.89
2013 11 29.75051     600    18.47
2013 12 01.72377     600    18.85
2013 12 01.73159     600    18.85
2013 12 01.74629     600    18.93


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

The images are available at:
http://www.osservatoriobassano.org/GRB.asp

The message may be cited.


GRB_name: GRB131202A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15559
SUBJECT: GRB 131202A: Swift detection of a burst
DATE:    13/12/02 15:29:01 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Kocevski (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), M. G. Bernardini (INAF-OAB),
D. N. Burrows (PSU), S. B. Cenko (GSFC), P. D'Avanzo (INAF-OAB),
V. D'Elia (ASDC), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
D. Malesani (DARK/NBI), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. H. Siegel (PSU) and R. L. C. Starling (U Leicester) report on
behalf of the Swift Team:

At 15:12:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131202A (trigger=579982).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 344.056, -21.658 which is 
   RA(J2000) = 22h 56m 13s
   Dec(J2000) = -21d 39' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 30 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 15:14:02.9 UT, 113.7 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 344.0540,
-21.6627 which is equivalent to:
   RA(J2000)  = 22h 56m 12.96s
   Dec(J2000) = -21d 39' 45.6"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 18 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 (2.29 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.3
(+3.70/-2.92) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 116 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03. 

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


GRB_name: GRB131202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15561
SUBJECT: GRB 131202A : XMM-Newton planned observation
DATE:    13/12/02 18:16:44 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@gmail.com>

G. Stratta (OAR/INAF), B. Gendre (ARTEMIS), S. Dall'Osso (IAAT), 
Giovanni De Cesare (IAPS) report :

We have activated a ToO observation of GRB 131202A with XMM-Newton, 
starting at 2013-12-03 00:23:14 UTC for about 8 hours and 20 minutes. 
All ground based follow-up (especially in optical and radio) are encouraged.


This message can be cited.


GRB_name: GRB131202A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15562
SUBJECT: GRB 131202A:  Tautenburg observations
DATE:    13/12/02 19:53:49 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Klose, B. Stecklum, and S. Schmidl (TLS Tautenburg)
report:

We observed the field of GRB 131202A (Kocevski et al., GCN 15559) with the
Tautenburg 1.34-m Schmidt telescope under very high airmass (> 3).
Observations in R, I and GunnZ started at 16:23 UT, around 70 min after
the GRB trigger.

Inside the 2.3 arcsec XRT error circle (Kocevski et al.) we do not find
any new object in any band. We estimate a preliminary magnitude of R > 20.


GRB_name: GRB131202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15563
SUBJECT: GRB 131202A: Bassano Bresciano Observatory optical upper limit
DATE:    13/12/02 19:54:50 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the field of GRB 131202A 
with the robotic telescope of (IAU 
station 565) Bassano Bresciano 
Observatory, Italy (member of ISSP:
Italian Supernovae Search Project).

The observations started 88m. after the    
GRB trigger,at the end of the twilight,
with our schmidt telescope 
D=320/400 mm F/D=3.1.

Weather conditions were good.     

We co-added 3 series of 20 unfiltered exposures 
of 120 sec each.      

We did not found any optical counterpart 
in the error box of the XRTcandidate
(D. Kocevski et al, GCN 15559).

Start      End       Vlim
88min     235min     19.5  


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

The images are available at:
http://www.osservatoriobassano.org/GRB.asp

The message may be cited.


GRB_name: GRB131202A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15564
SUBJECT: GRB 131202A: Enhanced Swift-XRT position
DATE:    13/12/03 00:53:16 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 1178 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 131202A, 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 = 344.05424, -21.66247 which is equivalent
to:

RA (J2000): 22h 56m 13.02s
Dec (J2000): -21d 39' 44.9"

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

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

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


GRB_name: GRB131202A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15565
SUBJECT: GRB 131202A: Fermi GBM Detection
DATE:    13/12/03 03:34:07 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

Andrew C. Collazzi (NASA/ORAU) reports on behalf of the Fermi GBM
Team:

"At 15:12:10.85 UT on 2 December 2013, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 131202A (trigger 407689933 / 
131202633), which was also detected by the Swift/BAT and Swift/XRT
(Kocevski et al., GCN 15559). The GBM on-ground location is
consistent with the Swift/XRT position.

The angle from the Fermi LAT boresight is 86 degrees.

The GBM light curve consists of a single pulse with a duration (T90)
of 26 s (50-300 keV). We find the 1.024-s peak flux (10 - 1000 keV),
measured starting from T0-2.560, to be 1.5 +/- 0.2 ph/(s cm^2).
The time-averaged spectrum from T0-8.2 s to T0+11.3 s is best fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.10 +/- 0.25 and the cutoff energy,
parameterized as Epeak, is 288.4 +/- 172.0 keV.

The event fluence (10-1000 keV) in this time interval is
(1.6 +/- 0.4)E-06 erg/cm^2.

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


GRB_name: GRB131202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15566
SUBJECT: GRB 131202A: RATIR Optical and NIR Observations
DATE:    13/12/03 04:32:41 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (ORAU/GSFC), 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),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-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 131202A (Kocevski, et al., GCN 15559) 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 2013/12 3.08 to 2013/12 3.15 UTC (10.81
to 12.32 hours after the BAT trigger), obtaining a total of 1.04 hours
exposure in the r and i bands and 0.44 hours exposure in the Z,
Y, J, and H bands.

For a source within the Swift-XRT error circle, in comparison with 
2MASS, we
obtain the following upper limits (3-sigma):

  r > 22.99
   i > 22.56
   Z > 21.50
   Y > 20.68
   J > 20.43
   H > 20.05

These magnitudes are in the AB system and 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: GRB131202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15567
SUBJECT: GRB 131202A: Swift-XRT refined Analysis
DATE:    13/12/03 05:29:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B.P. Gompertz (U. Leicester), B. Sbarufatti (INAF-OAB/PSU), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), J.A. Kennea (PSU), V. Mangano (PSU), M.C.
Stroh (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and
D. Kocevski report on behalf of the Swift-XRT team:

We have analysed 7.1 ks of XRT data for GRB 131202A (Kocevski  et al.
GCN Circ. 15559),  from 99 s to 33.8 ks after the  BAT trigger. The
data comprise 267 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by
Osborne et al. (GCN. Circ 15564).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=2.00 (+0.23, -0.24).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+0.4, -0.3). The
best-fitting absorption column is  1.3 (+1.0, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 2.3 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+1.0, -0.8) x 10^21 cm^-2
Galactic foreground: 2.3 x 10^20 cm^-2
Excess significance: 2.2 sigma
Photon index:      2.1 (+0.4, -0.3)

If the light curve continues to decay with a power-law decay index of
2.00, the count rate at T+24 hours will be 6.2 x 10^-6 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x
10^-16 (3.0 x 10^-16) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00579982.

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


GRB_name: GRB131202A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15568
SUBJECT: GRB 131202A: Swift/UVOT Upper Limits
DATE:    13/12/03 12:56:44 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 131202A
117 s after the BAT trigger (Kocevski et al., GCN Circ. 15559).
No optical afterglow consistent with the XRT position
(Osborne et al., GCN Circ. 15564) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag
white_FC        117          267            147         >20.6
white           117      1344           363         >21.2
v               608      1231           78          >18.6
b               534      1330           78          >19.6
u_FC            277      527            246         >19.9
u               277      1305           304         >20.1
w1              657      1280           78          >19.0
m2              632      1256           78          >18.9
w2              583      1207           78          >19.3

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: GRB131202A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15569
SUBJECT: GRB 131202A, Swift-BAT refined analysis
DATE:    13/12/03 15:12:51 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), N. Gehrels (GSFC),D. Kocevski (NASA/GSFC/ORAU),
H. A. Krimm (GSFC/USRA),A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC),
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+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131202A (trigger #579982)
(Kocevski, et al., GCN Circ. 15559).  The BAT ground-calculated position is
RA, Dec = 344.005, -21.650 deg which is
    RA(J2000)  =  22h 56m 01.3s
    Dec(J2000) = -21d 38' 58.9"
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 63%.  The mask-weighted light curve shows a pair of
overlapping peaks covering the period from T-10 to T+40 seconds.
T90 (15-350 keV) is 30.4 +- 10.9 sec (estimated error including systematics).

The time-averaged spectrum from T-1.62 to T+37.98 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.58 +- 0.26.  The fluence in the 15-150 keV band is 6.1 +- 1.0 x 10^-7erg/cm2.
The 1-sec peak photon flux measured from T+1.64 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/579982/BA/


GRB_name: GRB131127A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15570
SUBJECT: GRB 131127A: optically dark burst
DATE:    13/12/03 16:26:09 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A.Volnova (IKI), E. Klunko (ISTP), M. Eselevich (ISTP), A.
Pozanenko(IKI) report on behalf of larger GRB follow-up collaboration:

We report about revised photometry of the GRB 131127A (Markwardt et
al., GCN 15516) published earlier (Klunko et al., GCN 15519).
Using combined image of full data set of the observations on Nov. 27
we do not detect any optical counterpart in the enhanced XRT error
circle (Evans et al., GCN 15520). The details of the photometry are
the following:

UT start       t-T0           Filter    Exp.   OT   UL
                 (mid, days)             (s)             (3 sigma)
10:40:06     0.04680      R         4650   n/d   22.5

The photometry is based on the same 3 USNO-B1.0 stars listed in the GCN 15519.

The deep upper limit obtained at ~67 min (mid time) after burst
trigger together with Swift/XRT observations
(www.swift.ac.uk/xrt_curves/00579571/flux.qdp) suggests the upper
limit of optical-to-X-ray spectral slope beta_OX = -0.02 and classify
the GRB 131127A as a dark burst according to Jakobsson (Jakobsson et
al., 2004, ApJ, 614, L21).


GRB_name: GRB090530A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15571
SUBJECT: GRB 090530: X-shooter redshift
DATE:    13/12/03 18:31:28 GMT
FROM:    Paolo Goldoni at U.Paris/APC  <goldoni@apc.univ-paris7.fr>

 P. Goldoni (APC/Irfu - CEA), A. de Ugarte Postigo (IAA - CSIC and DARK/NBI) and J.P.U. Fynbo (DARK/NBI) report on behalf of the X-shooter GRB collaboration :


 We reduced with the most recent pipeline the observations of the optical afterglow of GRB 090530 (Cannizzo et al., GCN 9438) made using the ESO VLT equipped with the X-shooter spectrograph. The observations were performed during commissioning with the instrument not fully calibrated. The observations started on 2009-05-30 at 23:56 UT (i.e., 20.63 hr after the burst). A total exposure of 1x900 s + 4x1200 s was obtained, covering the spectral range from ~3000 to ~24000 Ang. 
The afterglow is detected in the UVB and VIS arms with a faint continuum. Superposed on the continuum we detected spectral features consistent with MgII, MgI, SiII, FeII and AlIII at a redshift ~1.266 fully consistent with the photometric redshift 1.28 (+0.16, -0.15) (Kruehler et al. 2011, A&A 526, 153).


GRB_name: GRB131126A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15572
SUBJECT: GRB 131126A: iPTF upper limits on the afterglow of a short GRB
DATE:    13/12/03 19:24:27 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories), and
S. B. Cenko (NASA/GSFC) report on behalf of the intermediate Palomar
Transient Factory (iPTF) collaboration:

The short-hard GRB 131126A triggered Fermi GBM (Fermi trigger
407130853) at 2013-11-26 03:54:10 and was localized by IPN using
Fermi and Konus-Wind (Golenetskii et al., GCN 15550; Golenetskii
et al., GCN 15551).

Starting 2013-11-26 10:50:40, we imaged about 60 deg^2 surrounding
the trigger's localization using the Palomar 48-inch Oschin telescope
(P48), covering most of the GBM 1-sigma statistical+systematic error
region and most of its intersection with the IPN Fermi-Konus 3-sigma
annulus. Sifting through candidate variable sources using standard
iPTF vetting procedures, we find no afterglow candidates to an
average limiting magnitude of R~19.5 at 7 hours after the burst.

See http://www.its.caltech.edu/~lsinger/iptf/Fermi407130853.pdf for
a diagram of the PTF fields observed in relation to the Fermi and
IPN localizations.


GRB_name: GRB131126A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15573
SUBJECT: GRB 131126A: Fermi GBM observation
DATE:    13/12/04 03:48:52 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa and C. Meegan (UAH) report on behalf of the Fermi GBM Team:

"At 03:54:10.43 UT on 26 November 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131126A (trigger 407130853 / 131126163)
which was also detected by Konus/Wind (Golenetskii et al 2013, GCN 15551)
leading to an IPN Konus/GBM annulus (Golenetskii et al 2013, GCN 15550).
The angle from the Fermi LAT boresight is 108 degrees.

iPTF also performed a tiled observation of the localization error box and
established an upper limit on the GRB afterglow (Singer et al 2013, GCN 15572).

The GBM light curve consists of a single pulse with a duration (T90)
of about 0.3 s (50-300 keV).

The time-averaged spectrum from T0-0.064 s to T0+0.256 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.06 +/- 0.13 and
the cutoff energy, parameterized as Epeak, is 600 +/- 62 keV
(Castor statistics 397.51 for 364 d.o.f.).
A Band function fits the spectrum equally well (Castor statistics 391.35
for 363 d.o.f.) with Epeak= 489 +/- 74 keV, alpha = 0.13 +/- 0.20
and beta = -2.29 +/- 0.26.

The event fluence (10-1000 keV) in this time interval is
(2.0 +/- 0.1)E-06 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+0.000 s in the 10-1000 keV band
is 36 +/- 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: GRB131127B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15575
SUBJECT: GRB 131127B: archival confirmation of iPTF13ecv as a CV
DATE:    13/12/04 15:06:54 GMT
FROM:    Denis Denisenko at SAI MSU  <d.v.denisenko@gmail.com>

D. Denisenko (Sternberg Astronomical Institute at Moscow State
University) reports:

The position of the optical transient iPTF13ecv (Singer et al., GCN
15524) in the Fermi field of GRB 131127B (von Kienlin, GCN 15528) was
observed in the past with the NEAT project (Teegarden et al., ApJ Vol.
589, pp. L51-L53, 2003). A total of 87 images were obtained on 33
different nights from 1998 July 19 to 2005 Sep. 08. Images can be
downloaded from the SkyMorph website at
http://skyview.gsfc.nasa.gov/skymorph/obs.html The object at the
position of iPTF13ecv was detected in outburst on four last nights,
namely on 2005 Aug. 21, Sep. 01, 07 and 08. It was below the detection
limit (typically 19.5-20.0m) on the other nights.

The following photometry was obtained from the unfiltered NEAT images
using SDSS J203153.05+005858.4 as a reference star with r=16.40:

20050821.372  17.0
20050901.371  18.1
20050908.271  19.3

The coordinates of the object measured from the combination of three
2005-08-21 images are (J2000): 20 31 47.76 +00 59 23.8, consistent
to 0.4" with the position reported by Singer et al. and to 1" with
those by Quadri et al. (GCN 15543).

Comparison of NEAT images of the variable object in outburst (2005
Aug. 21, Sep. 01 and 08) and at quiescence is uploaded to
http://master.sai.msu.ru/static/OT/iPTF13ecv-NEAT-2005.jpg (5'x5' FOV
centered at the variable). Reference star is marked on the bottom left
(2005-09-01) panel as 16.4r.

No object is detected at this position on the combination of 26 good
quality NEAT images to the limit ~22.5m. No previous outbursts were
found on 15 DSS plates. Combination of DSS plates and SDSS color image
suggests that the object is fainter than 23m at quiescence. 2005
outburst amplitude about 6 mag and duration of at least about 20 days
are typical for superoutbursts of SU UMa-type dwarf novae.

Thus, the cataclysmic variable nature of iPTF13ecv already determined
spectroscopically by Keck telescopes (Singer et al., GCN 15574) is
independently confirmed by the archival light curve, once again
showing the powerful capabilities of data mining methods.

This message can be cited.


GRB_name: GRB131202A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15576
SUBJECT: GRB 131202A: theoretical estimation of the redshift
DATE:    13/12/04 15:14:58 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, C.L. Bianco, M. Enderli, M. Kovacevic, M. Muccino, A.V. Penacchioni, G.B. Pisani, J.A. Rueda, Y. Wang report:

The X-ray observations of GRB 131202A (1) point to the possibility that it fulfills the IGC paradigm (2,3). A preliminary overlapping of its X-ray (0.3-10 keV in rest-frame) luminosity within the one of GRB 090618, namely an IGC prototype (4), gives an estimate of the redshift of z~10 (see Fig. 1 http://www.icranet.org/images/GCN/GRB131202A_Fig1.pdf). Continuous monitoring and complementary observations in all possible wavelengths are encouraged.

The extension of the validity of the IGC paradigm to very large cosmological distances has already been clearly demonstrated by the case of GRB 090423 (5) at z=8.2 (6,7,8,9,10,11): its X-ray (0.3-10 keV in rest-frame) luminosity again overlaps perfectly well with the one of GRB 090618 (see Fig. 2 http://www.icranet.org/images/GCN/GRB131202A_Fig2.pdf).


References:

(1) Kocevski et al., GCN 15559
(2) Rueda & R. Ruffini, ApJLett, 758, L7 (2012)â€¨
(3) Pisani et al., A&A, 552, L5 (2013)â€¨
(4) Izzo et al., A&A, 548, L5 (2012)
(5) Krimm et al., GCN 9198
(6) Cucchiara et al., GCN 9213
(7) Olivares et al., GCN 9215
(8) Thoene et al., GCN 9216
(9) Perley et al., GCN 9217
(10) Tanvir et al., GCN 9219
(11) Fernandez-Soto et al., GCN 9222


GRB_name: GRB131127B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15577
SUBJECT: GRB 131127B: Bassano Bresciano Observatory,archival confirmation of  iPTF13ecv
DATE:    13/12/04 16:29:52 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli

of the (IAU station 565) Bassano Bresciano 
Observatory, Italy (member of ISSP:Italian
Supernovae Search Project) report:

Follow the GCN 15575 (D. Denisenko - Sternberg Astronomical 
Institute at Moscow State University), we communicate 
that the optical transient iPTF13ecv (Singer et al., GCN
15524) is also present in the POSS1-BLUE plate 
on 1953-08-16. with magnitude = 20.1 +/- 0.2

Magnitude were estimated with the USNO-B1 cat. 

The image are available at:

http://archive.stsci.edu/cgi-bin/dss_search?v=poss1_blue&r=20+31+48&d=00+59+23&e=J2000&h=15.0&w=15.0&f=gif

The message may be cited.


GRB_name: GRB131205A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15578
SUBJECT: GRB 131205A: Swift detection of a burst
DATE:    13/12/05 09:40:23 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

T. N. Ukwatta (MSU), V. D'Elia (ASDC), C. B. Markwardt (NASA/GSFC),
A. Melandri (INAF-OAB), K. L. Page (U Leicester) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 09:18:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131205A (trigger=580267).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 131.609, -60.174 which is 
   RA(J2000) = 08h 46m 26s
   Dec(J2000) = -60d 10' 25"
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 60 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:20:07.5 UT, 88.7 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 131.6276, -60.1556
which is equivalent to:
   RA(J2000)  = 08h 46m 30.63s
   Dec(J2000) = -60d 09' 20.0"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 74 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 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 93 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
Data from the list of sources generated on-board are not available at this
time. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.26. 

We note that the spacecraft star tracker was out of lock during a 
portion of this GRB, but we believe the burst is real. The position
may be revised after further processing. 

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: GRB131205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15579
SUBJECT: GRB 131205A: Zadko observatory - Gingin optical observations
DATE:    13/12/05 14:28:19 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
D. Turpin (IRAP-CNRS-OMP), B. Gendre , M. Boer, K. Siellez, H. Dereli ,
O. Bardho (UNS-CNRS-OCA), A. Williams (PO-UWA), R. Martin (PO-UWA)
report:

We imaged the field of GRB 131205A detected by SWIFT
(trigger 580267) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 3.74h after the GRB trigger
which occured during Australian day time.
The elevation of the field increased from
19 degrees above horizon and weather conditions
were excellent.

We co-added a series of exposures but
we do not detect any OT with a limiting magnitude of:
t0+3.74h to t0+4.45h : Rlim = 20.2

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


GRB_name: GRB131205A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15580
SUBJECT: GRB 131205A: Enhanced Swift-XRT position
DATE:    13/12/05 15:16:19 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 2064 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 131205A, 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 = 131.62784, -60.15601 which is equivalent
to:

RA (J2000): 08h 46m 30.68s
Dec (J2000): -60d 09' 21.6"

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: GRB131205A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15581
SUBJECT: GRB 131205A: Swift/UVOT Upper Limits
DATE:    13/12/05 17:40:58 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and T. N. Ukwatta (MSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 131205A
94 s after the BAT trigger (Ukwatta et al., GCN Circ. 15578).
No optical afterglow consistent with the enhanced XRT position
(Beardmore et al. GCN Circ. 15580) is detected in the initial UVOT
exposures.  Because the spacecraft attitude was not stable during
the first finding chart exposure, we do not report on that exposure here.

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

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

u_FC               306          556          246 >20.8
white              586        12884         1171 >21.7
v                  636         6778          471 >20.5
b                  561        12313         1160 >21.5
u                  306        11400         1386 >22.0
w1                 685         7121          385 >20.4
m2                 660         6983          471 >20.4
w2                 611         6574          471 >20.6

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


GRB_name: GRB131205A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15583
SUBJECT: GRB 131205A: Swift-XRT refined Analysis
DATE:    13/12/05 21:40:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. Maselli  (INAF-IASFPA), V.
Mangano (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), C. Pagani (U. Leicester) and T.N.
Ukwatta report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 131205A (Ukwatta  et al. GCN
Circ. 15578),  from 226 s to 24.4 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 15580).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.10 (+0.09, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.4). The
best-fitting absorption column is  3.2 (+1.4, -1.2) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 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 3.9 x 10^-11 (6.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+1.4, -1.2) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 2.3 sigma
Photon index:      2.1 (+/-0.4)

If the light curve continues to decay with a power-law decay index of
1.10, 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 3.8 x
10^-14 (6.7 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/00580267.

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


GRB_name: GRB131205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15584
SUBJECT: GRB 131205A: Swift-BAT refined analysis
DATE:    13/12/05 22:11:19 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), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+771 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131205A (trigger #580267)
(Ukwatta, et al., GCN Circ. 15578).  The BAT ground-calculated position is
RA, Dec = 131.573, -60.181 deg which is 
   RA(J2000)  =  08h 46m 17.6s 
   Dec(J2000) = -60d 10' 51.5" 
with an uncertainty of 2.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 95%.
 
The mask-weighted light curves two peaks starting at ~T-5, peaking at ~T+1,
and ending at ~T+5 sec, and the second peak from ~T+18 to ~T+22 sec.
T90 (15-350 keV) is 37.5 +- 9.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-18.50 to T+20.41 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.57 +- 0.38.  The fluence in the 15-150 keV band is 2.9 +- 0.7 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+19.30 sec in the 15-150 keV band
is 0.6 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/580267/BA/


GRB_name: GRB131205A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15585
SUBJECT: GRB131205A : GROND Observations 
DATE:    13/12/06 17:35:52 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

S. Schmidl (TLS Tautenburg ), K. Varela and J. Greiner (both MPE Garching)
report on behalf of the GROND team:

We observed the field of the GRB 131205A (Ukwatta et al., GCN #15578)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPG telescope at La Silla Observatory (Chile).

Observations started at 05:07 UT on 06 December 2013, 19.5 hours after the
GRB. They were performed at an average seeing of 1.0" and at an average
airmass of 1.3.

Based on six co-added observations with individual exposure times of 1500s
in g'r'i'z' and 1200s in JHK, we do not detect any source inside the
enhanced XRT error circle (Beardmore et al., GCN #15580) down to
preliminary 3 sigma limiting magnitudes (all in the AB system) :

g' > 25.8 mag,
r' > 25.6 mag,
i' > 24.9 mag,
z' > 24.5 mag,
J > 22.1 mag,
H > 21.5 mag,
K > 20.8 mag.

Magnitudes are calibrated against GROND zeropoints (griz) and 2MASS stars
(JHK), and are not corrected for the Galactic foreground extinction
corresponding to a reddening of E_(B-V)=0.25 mag in the direction of the
burst (Schlegel et al. 1998).

We note the marginal detection of a source, located 1.9" from the center
of the XRT circle, at

RA : 08:46:30.86
DEC : -60:09:20.6,

with an uncertainty of 0.2 arcsec and magnitudes of

r = 24.8 +/- 0.2
i = 24.7 +/- 0.3
z = 24.3 +/- 0.3.

This is consistent with a power law and thus could be the afterglow of
GRB131205A, but no statement can be made about fading at this time.
Follow-up observations are required to determine the nature of this
source.


GRB_name: GRB131202A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15586
SUBJECT: GRB131202A : GROND observations
DATE:    13/12/06 20:16:10 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

K. Varela, J. Graham, J. Greiner and D.A. Kann (all MPE Garching) report
on behalf of the GROND team:

We observed the field of the GRB 131202A (Kocevski et al., GCN #15559)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPG telescope at La Silla Observatory (Chile).

Observations started at 01:01 UT on 03 December 2013, 9.5 hours after the
GRB. They were performed at an average seeing of 1.4" and at an average
airmass of 1.5.

Based on an observation with a total integration time of 6920 s in
g'r'i'z' and 5760s in JHK, we detect a source inside the enhanced XRT
circle (Osborne et al., GCN #15564) in the i' and z' bands, with
magnitudes

i' = 24.5 +/- 0.3 mag,
z' = 23.6 +/- 0.2 mag,

and 3 sigma limiting magnitudes (all in the AB system) :

g'> 25.5 mag,
r'> 25.3 mag,
J > 22.0 mag,
H > 21.4 mag,
K > 19.9 mag.

Magnitudes are calibrated against GROND zeropoints (griz) and 2MASS stars
(JHK), and are not corrected for the Galactic foreground extinction
corresponding to a reddening of E_(B-V) = 0.03 mag in the direction of the
burst (Schlegel et al. 1998).

Performing a joint fit with contemporary Swift X-ray data, we find that
the detections and upper limits can be explained with a low redshift and
high extinction (up to Av ~ 4.2 for z = 0 and SMC dust), with low
extinction and a redshift z ~ 5, or combinations in between. The
near-negligible NH column density at z = 0 ((1.3+1.0-0.8) x 10^21 cm^-2,
Gompertz et al., GCN #15567) and assuming a non-extreme dust-to-gas ratio
point to a higher probability for the z ~ 5 scenario.

We note that in any case, the significant detection in i' and the i'- z'
color conservatively imply z < 6, in contrast to the prediction by Ruffini
et al. (GCN #15576).


GRB_name: GRB131209A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15587
SUBJECT: GRB 131209A: Fermi-LAT detection of a burst
DATE:    13/12/10 02:06:01 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G.Vianello (Stanford), N.Omodei (Stanford), report on behalf of the
Fermi-LAT team:

At 13:07:56.97on December 9, 2013, Fermi LAT detected a faint high energy
signal from GRB131209A, which was also detected by Fermi-GBM (trigger
408287279/131209547).

The data from the Fermi LAT show a significant increase in the event rate
within 10 degree of the GBM location after the GBM trigger that is
spatially and temporally correlated with the GBM emission. Although the
detection is slightly above the 5 sigma level, there are only 4 photons
likely associated with this GRB in the first 200 s after the trigger. The
localization has therefore a large statistical error. The best LAT
on-ground location is found to be RA, DEC 136.5, -33.2 (J2000) with an
error radius of 0.9 deg (68% containment, statistical error only), this was
20 deg from the LAT boresight at the time of the trigger.

The Fermi LAT point of contact for this burst is Giacomo Vianello (
giacomov@stanford.edu).

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: GRB131209A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15588
SUBJECT: IPN Triangulation of GRB 131209A
DATE:    13/12/10 13:01:52 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, 
on behalf of the Fermi GBM team, report:

The long-duration GRB 131209A (Vianello et al., GCN Circ. 15587) has 
been observed by Fermi (GBM: trigger 408287279), Konus-Wind, INTEGRAL 
(SPI-ACS), Swift (BAT), and MESSENGER (GRNS), so far, at about 47277 s 
UT (13:07:57). The burst was outside the coded field of view of the BAT.

We have triangulated this GRB to a Konus-MESSENGER annulus centered at 
RA(2000)=64.917 deg (04h 19m 40s)  Dec(2000)=+21.195 deg (+21d 11' 41"), 
whose radius is 87.724 +/- 0.105 deg (3 sigma).

This annulus intersects the Fermi-LAT 1 sigma error circle (Vianello et 
al., GCN Circ. 15587) to form an error box whose area is about 16 times 
smaller than that of the LAT error circle (2.5 sq. deg.), and whose 
corners are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
   Corners:
    137.365 (09h 09m 28s) -32.668 (-32d 40' 06")
    137.509 (09h 10m 02s) -32.892 (-32d 53' 32")
    136.780 (09h 07m 07s) -34.069 (-34d 04' 09")
    136.475 (09h 05m 54s) -34.100 (-34d 05' 59")
  ---------------------------------------------
The error box area is 559 sq. arcmin, and its maximum dimension is
1.48 deg (the minimum one is 12.6 arcmin).

This box may be improved.

The distance between the annulus center line and the center of Fermi-LAT 
location is 0.5 deg.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB131209_T47280/IPN/

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


GRB_name: GRB131209A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15589
SUBJECT: Konus-Wind observation of GRB 131209A
DATE:    13/12/10 13:08:14 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 131209A
(Fermi LAT detection: Vianello & Omodei, GCN 15587;
IPN triangulation: Hurley at al., GCN 15588)
triggered Konus-Wind at T0=47280.491 s UT (13:08:00.491).

The burst light curve shows a broad pulse from ~T0-3 s to ~T0+17 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131209_T47280/

As observed by Konus-Wind, the burst
had a fluence of (1.4  0.1)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+7.744 s,
of (3.2  0.3)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.49  0.19,
the high energy photon index beta = -2.68  0.46,
the peak energy Ep = 235  29 keV,
chi2 = 91.2/97 dof.

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.17  0.17,
the high energy photon index beta = -2.49  0.22,
the peak energy Ep = 246  18 keV,
chi2 = 87.2/97 dof.

All the quoted values are preliminary.


GRB_name: GRB131209A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15590
SUBJECT: GRB 131209A Tiled Swift observations
DATE:    13/12/10 15:35:35 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 131209A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00022

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177).

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


GRB_name: GRB131209A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15591
SUBJECT: GRB 131209A: Fermi GBM observation
DATE:    13/12/11 12:21:13 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 13:07:56.97 UT on 09 December 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131209A (trigger 408287279 / 131209547),
which was also detected by the Fermi/LAT(Vianello et al. 2013, GCN 15587),
Konus-Wind (Golenetskii et al. 2013, GCN 15589) and INTEGRAL SPI-ACS. 
The GBM on-ground location is consistent with the error box derived by
the intersection of the IPN annulus with the Fermi-LAT 1 sigma 
error circle (Hurley et al. 2013, GCN 15588).

The GBM light curve shows a structured pulse
with a duration (T90) of about 14 s (50-300 keV).
The time-averaged spectrum from T0-2.560 s to T0+19.968 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.46 (+0.04/-0.04)  and
the cutoff energy, parameterized as Epeak, is 287 (+12/-11)keV

The event fluence (10-1000 keV) in this time interval is
(1.44 +/- 0.03)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+11.328 s in the 10-1000 keV band
is 8.0 +/- 0.3  ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak= 267 (+17/-14)
keV, 
alpha = -0.41 (+0.06/-0.05)  and beta = -2.79 (+0.24/-0.61).

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


GRB_name: GRB131209A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15592
SUBJECT: GRB 131209A: Swift XRT and UVOT observations 
DATE:    13/12/11 16:28:07 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (PSU) and Alice Breeveld (MSSL) report on behalf of the 
Swift team:

We report on Swift observations of the field of the FERMI/LAT-
discovered GRB 131209A (Vianello et al., GCN circ. 15587) starting
26.5 hours after the FERMI/LAT trigger. Swift  performed three 
observations with and exposure tome of 3 ks each to cover most of 
the IPN error box reported by Hurley et al. (GCN circ. 15588). 
We found two X-ray sources with in the IPN error box, one 
of which coincides with a radio source, NVSS J090753-333724. The
second source at the position 
 
RA-2000:   09 07 19.2 
Dec-2000: -33 51 20.0

does not have an entry in the NED or Simbad. Its count rate in the
XRT is at a level of (4.7+/-1.9)e-3 counts/s which is equivalent to
a flux in the 0.3-10 keV band of (1.9+/-0.7)e-13 erg/s/cm2.
Swift started observing the tile that covered this source 33 hours
after the Fermi/LAT trigger (Vianello et al., GCN Circ. 15587). 

Only one of the XRT potential candidate 
sources (source 2) is in the field of view of the UVOT and there 
is no new source found at this position. Preliminary 3-sigma upper 
limits using the UVOT photometric system (Breeveld et al. 2011, 
AIP Conf. Proc. 1358, 373) for the initial summed exposures are:

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

white        33.16          33.37          754         >21.8
v            33.37          33.60          801         >20.1
u            32.94          34.78         1367         >21.1

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.36 in the direction 
of the burst (Schlegel et al. 1998).


GRB_name: GRB131205A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15595
SUBJECT: GRB 131205A: GROND confirmation of afterglow
DATE:    13/12/13 12:39:29 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

K. Varela, D.A. Kann and J. Greiner (all MPE Garching)
report on behalf of the GROND team:
  
We observed again the field of the GRB 131205A (Ukwatta et al., GCN #15578)
simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPG telescope at the La Silla Observatory (Chile).
  
Observations started at 05:22 UT on 11 December 2013. They were performed
at an average seeing of 0.7 arcsec and at an average airmass of 1.3.
  
Based on four co-added observations with individual exposure times of 2214s
in g'r'i'z' and 1800s in JHKs, we measure for the source at the border
of the X-ray error circle (Beardmore et al., GCN #15580), which was
proposed as potential counterpart (Schmidl et al. 2013, GCN #15585),
the following magnitudes:
  
r' = 26.5 +/- 0.4
i' = 25.3 +/- 0.4
  
Compared to our earlier measurements of r' = 24.8+/-0.2, i' = 24.7+/-0.3
this implies a fading of 1.7+/-0.5 in r', and 0.6+/-0.5 in i'. 
We conclude that the fading in r' is significant, and propose this
source as the optical counterpart of GRB 131205A.  The low amplitude
in the i'-band may be caused by the emergence of light from a red
host galaxy. Observations with bigger glasses are required to verify
this interpretation.
  
Note that the above r'i' magnitudes are calibrated against GROND zeropoints 
and are not corrected for the Galactic foreground extinction corresponding
to a reddening of E_(B-V)=0.25 mag in the direction of the burst (Schlegel
et al. 1998).


GRB_name: GRB131215A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15597
SUBJECT: GRB 131215A: MAXI/GSC detection
DATE:    13/12/15 12:10:27 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

K. Fukushima, H. Negoro (Nihon U.),
S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, M. Morii, M. Serino,  J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, T. Yoshii, Y. Tachibana (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, M. Sasaki (Osaka U.), 
M. Nakajima, H. Sakakibara, T. Onodera, K. Suzuki (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, M. Higa (Chuo U.), 
M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada (Miyazaki U.), 
K. Yamaoka (Nagoya U.) 
report on behalf of the MAXI team:

The MAXI/GSC Nova alert system triggered a bright uncatalogued X-ray transient source at
UT 2013-12-15T09:08:20.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (258.654 deg, 7.862 deg) = (17 14 36, +07 51 43) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.25 deg and 0.21 deg, respectively. 
The roll angle of the long axis from the north direction is 90.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 350 +- 55 mCrab (4-10keV, 1 sigma error).
Without the assumption about the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (258.538 deg, 7.338 deg) = (17 14 09, +07 20 16) (J2000)
(R.A., Dec) = (258.123 deg, 7.633 deg) = (17 12 29, +07 37 59) (J2000)
(R.A., Dec) = (258.913 deg, 8.557 deg) = (17 15 39, +08 33 24) (J2000)
(R.A., Dec) = (259.333 deg, 8.266 deg) = (17 17 19, +08 15 57) (J2000)

There was no significant excess flux in the previous transit at 07:35 UT
and in the next transit at 10:50 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB131216A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15598
SUBJECT: GRB 131216A: Fermi-LAT detection of a burst
DATE:    13/12/16 14:51:54 GMT
FROM:    Peter Veres at ELTE,Budapest  <veresp@gmail.com>

P. Veres (Penn State), D. Kocevski (NASA/Goddard), E. Bissaldi
(University & INFN Trieste), R. Desiante (University of Udine and INFN
Trieste), J. Racusin (NASA/Goddard), report on behalf of the Fermi-LAT
team:

The Fermi Large Area Telescope (LAT) detected emission from GRB
131216A, also detected by GBM (trigger 408851795/131216081) at T0 =
01:56:32.06 UT on December 16, 2013.

The GBM location was initially inside the LAT field of view at an
angle of 44 degrees to the LAT boresight and triggered an autonomous
repoint of the spacecraft. However, LAT did not collect data while in
the South Atlantic Anomaly (SAA) from T0+200 to T0+800 s. No
significant excess is seen using standard analysis procedures.

Using the LAT Low Energy (LLE) event selection, over 120 counts above
background were detected within a 0.3 s interval coinciding with the
time of the GBM emission. This data selection has insufficient spatial
resolution to provide a reliable LAT localization. Since an excess of
events were not seen using the standard analysis selection, this
detection is likely due to low energy gamma-rays (below 100 MeV).

The Fermi LAT point of contact for this burst is Peter Veres  (puv2@psu.edu).

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: GRB131216A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15599
SUBJECT: GRB 131216A: Fermi GBM observation
DATE:    13/12/17 01:59:46 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 01:56:32.06  UT on 16 December 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131216A (trigger 408851795 / 131216081).
It was also detected by the Fermi Large Area Telescope (Veres et al 2013,
GCN 15598).

The on-ground calculated location, using the GBM trigger data, is
RA = 91.6, DEC = -35.5 (J2000 degrees, equivalent to +06h 06m, -35d 30'),
with an uncertainty of 2.7 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 was
44 degrees at trigger time, then an autonomous repoint maneuver placed the
GRB near the center of the LAT field-of-view.

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

The GBM light curve consists of a single FRED pulse
with a duration (T90) of about 24 s (50-300 keV).
The time-averaged spectrum from T0-0.256 s to T0+11.264 s, when the flux is
highest, is best fit by a Band function with Epeak = 359 +/- 40 keV,
alpha = -0.64 +/- 0.07, and beta = -2.03 +/- 0.13
(Castor statistics 777.70 for 716 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(8.60 +/- 0.20)E-06  erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.512 s in the 10-1000 keV band
is 7.9 +/- 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: GRB131216A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15600
SUBJECT: IPN Triangulation of GRB 131216A
DATE:    13/12/18 18:06:25 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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, and

V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, 
on behalf of the Fermi GBM team, report:

The long-duration GRB 131216A (V. Pelassa GCN Circ. 15599; P. Veres et 
al. GCN Circ. 15598) was observed by Fermi (GBM: trigger 408851795), 
Konus-Wind, INTEGRAL (SPI-ACS), Swift (BAT), Suzaku (WAM), and MESSENGER 
(GRNS) at about 6992 s UT (01:56:32). 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:
      94.674 (06h 18m 42s) -41.627 (-41d 37' 35")
    Corners:
      88.596 (05h 54m 23s) -43.014 (-43d 00' 51")
      99.822 (06h 39m 17s) -40.204 (-40d 12' 16")
     100.505 (06h 42m 01s) -39.743 (-39d 44' 34")
      89.379 (05h 57m 31s) -42.669 (-42d 40' 08")
    ---------------------------------------------
The error box area is 1.8 sq. deg, and its maximum dimension is 9.5 deg 
(the minimum one is 0.2 deg).

The center of the GBM ground position (V. Pelassa GCN Circ. 15599) is 
6.58 deg from the center of the box.

This box may be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB131216_T06993/IPN/


GRB_name: GRB131218A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15601
SUBJECT: GRB 131218A: a long GRB detected with INTEGRAL
DATE:    13/12/18 22:15:53 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

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

a gamma ray burst lasting about 6 s has been detected by IBAS in the IBIS/ISGRI data at  21:05:32 U.T. on December 18.
Its refined  coordinates (J2000)  are:

  R.A.: 113.7807 deg
  DEC.: -64.7373 deg

with an uncertainty of 1.8 arc min (90% c.l.).

A preliminary estimation of the burst fluence is 5x10^-7 erg/cmsq in the 20-200 keV energy band.

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


GRB_name: GRB131218A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15602
SUBJECT: GRB 131218A: TAROT La Silla observatory optical observations
DATE:    13/12/19 21:21:34 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D. (IRAP-CNRS-OMP), Gendre B.,
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 131218A detected by INTEGRAL
(trigger 6409) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 3.41h after the GRB trigger
which occured during day. The elevation of the field
increased from 26 degrees above horizon and weather
conditions were good.

We co-added a series of exposures but we do not
detect any OT with a limiting magnitude of:

t0+3.41h to t0+4.98h : Rlim = 19.6

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

N.B. Galactic coordinates are lon=276.4490 lat=-19.8751
and the galactic extinction in R band is about 0.4 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB131218A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15603
SUBJECT: GRB 131218A: Zadko observatory - Gingin optical candidate
DATE:    13/12/19 21:45:22 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre, M. Boer, K. Siellez, H. Dereli , O. Bardho (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA), D. Turpin (IRAP-CNRS-OMP)
report:

We imaged the field of GRB 131218A detected by INTEGRAL
(trigger 6409) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations are R filtered, started 0.87 day after
the GRB trigger. The limiting magnitude of the co added
image is Rlim = 20.5.

In the error box provided by INTEGRAL notice we detect
only one faint candidate not present on the DSS atlas:

RA(J2000) = 07h 35m 10.50s
DEC(J2000) = -64d 43' 19.4"

OT was R~20.0 0.87 day after GRB.

We have no more images so we cannnot conclude if it
is a fading source or not. Additional images are
programmed to be recorded in the next nights.


GRB_name: GRB131218A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15605
SUBJECT: GRB 131218A: Swift XRT and UVOT observations
DATE:    13/12/20 15:32:27 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC) and F.E. Marshall (NASA/GSFC)
report on behalf of the Swift team:


We report on Swift observations of the field of the INTEGRAL discovered GRB131218A (Gotz et al. GCN Circ 15601), starting 17.5 hours after the trigger. Due to an observing constraint, only a very short exposure was carried out.

XRT began observing the field on 2013-12-19 at 14:32:15 UT, i.e.,  62803 s after the trigger, for a total of 99 s. No source is detected within the INTEGRAL error circle. The 3-sigma upper limit on the count rate is ~9E-02 cts/s.

The Swift/UVOT began settled observations of the field of GRB 131218A 62782 s after the trigger. No optical afterglow consistent with the optical position (Klotz et al., GCN Circ. 15603) is detected in the initial UVOT exposure.
The preliminary 3-sigma upper limit using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposure is:

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

v                62782        62900          116         >19.8

The magnitude in the table is not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.17 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB131218A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15606
SUBJECT: GRB 131218A: GROND Upper Limits
DATE:    13/12/22 01:25:42 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, M. Tanga (both MPE Garching), S. Klose, S. Schmidl (both TLS
Tautenburg) and J. Greiner (MPE Garching) report on behalf of the GROND
collaboration:

We observed the field of GRB 131218A (INTEGRAL-6409, Gotz et al., GCN
#15601) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG telescope at La Silla Observatory
(Chile).

A first series of observations (integration time 6750 sec in the optical,
5400 sec in the NIR, midtime 0.24 days after the trigger, seeing 1".0 and
airmass 1.5) yield the following image depths (AB magnitudes):

g' > 24.6,
r' > 24.9,
i' > 24.5,
z' > 24.4,
J > 22.4,
H > 21.8, and
K > 20.8.

A second set of observations (integration time 3750 sec in the optical,
3000 sec in the NIR, midtime 2.31 days after the trigger, seeing 0".9 and
airmass 1.3) yield somewhat deeper limits in the optical, while they are
somewhat shallower in the NIR.

Image subtraction between these two epochs shows no evidence for variable
sources, both in the INTEGRAL error circle and around it, and therefore we
can only place upper limits on the presence of any afterglow.

Magnitudes are calibrated against GROND zeropoints (g'r'i'z') and 2MASS
stars (JHK), and are not corrected for the Galactic foreground extinction
corresponding to a reddening of E_(B-V)=0.17 mag in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB131224A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15607
SUBJECT: GRB 131224A: A short GRB detected by INTEGRAL
DATE:    13/12/24 18:17:19 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a short gamma ray burst lasting about 0.8 s has been detected by IBAS in the 
IBIS/ISGRI data at 16:54:37  UT of 24 December.

The refined coordinates (J2000) are:

R.A.= 296.8337  deg
DEC.= +31.6677  deg

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

The burst had a peak flux of about 1 counts/cm2/s (20-200 keV, 0.1-s 
integration time) and a fluence in the same energy range of about 3x10e-8 
erg/cmq.

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


GRB_name: GRB131224A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15608
SUBJECT: GRB 131224A: MASTER-Net early optical observations
DATE:    13/12/25 08:14:39 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  GRB131224A 33 sec after notice 
time and 39 sec after trigger time at 2013-12-24 16:55:24 UT in two 
polarizations.
Observations were made on high (z=75 deg) zenith distance and on the 
extremely stars rich  field (with galactic latitude  b=3 deg).
On our first (10s exposure) set we haven't found optical transient  within 
INTEGRAL error-box (S.Mereghetti et. al. GCN 15607).
The 5-sigma upper limit has been about 15.5 mag
The message may be cited.


GRB_name: GRB131225A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15609
SUBJECT: GRB 131225A: MAXI/GSC detection
DATE:    13/12/25 11:04:12 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

A. Kawagoe (Chuo U.), H. Negoro (Nihon U.), M. Morii (RIKEN), T. Sakamoto (AGU), 
S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, M. Serino,  J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, T. Yoshii, Y. Tachibana (Tokyo Tech), 
A. Yoshida, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, M. Sasaki (Osaka U.), 
M. Nakajima, H. Sakakibara, T. Onodera, K. Fukushima, K. Suzuki (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, M. Higa (Chuo U.), 
M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada (Miyazaki U.), 
K. Yamaoka (Nagoya U.) 
report on behalf of the MAXI team:

The MAXI/GSC Nova alert system triggered a bright uncatalogued X-ray transient source 
on 2013-12-25 at 09:54:50 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (95.150 deg, 5.413 deg) = (06 20 36, +05 24 46) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.28 deg and 0.19 deg, respectively. 
The roll angle of the long axis from the north direction is 43.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 273 +- 50 mCrab (4-10keV, 1 sigma error).
Without the assumption about the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (94.339 deg, 5.886 deg) = (06 17 21, +05 53 08) (J2000)
(R.A., Dec) = (94.737 deg, 6.296 deg) = (06 18 56, +06 17 45) (J2000)
(R.A., Dec) = (95.508 deg, 5.443 deg) = (06 22 01, +05 26 36) (J2000)
(R.A., Dec) = (95.114 deg, 5.029 deg) = (06 20 27, +05 01 44) (J2000)

There was no significant excess flux in the previous transit at 08:22 UT 
with an upper limit of 20 mCrab.
A possibility of a new X-ray transient, e.g., X-ray nova, can not be excluded
since the location is close to the Galactic plane (b = -4.5 deg). 
We also tentatively name this GRB 131225A as MAXI J0620+053.
The next transit by MAXI/GSC will be at 11:27 UT.


GRB_name: GRB131224A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15610
SUBJECT: GRB 131224A: Swift-XRT observation
DATE:    13/12/25 21:21:07 GMT
FROM:    Ben Gompertz at U.of Leicester  <bpg6@leicester.ac.uk>

B.P Gompertz, K.L. Page (U. Leicester) and M. De Pasquale (UCL-MSSL)
report on behalf of the Swift-XRT team:

We report on Swift-XRT observations of the field of the INTEGRAL
discovered GRB 131224A (Mereghetti et al. GCN Circ 15607), starting 10.8
ks after the trigger.

XRT began observing the field on 2013-12-24 at 19:53:56 UT (10.8 ks after
trigger), with an exposure time of of 3.96 ks. No source is detected
within the INTEGRAL error circle. The 3-sigma upper limit on the count
rate is 3.5E-03 cts/s, which is 1.4E-13 erg cm^-2  s^-1  using a typical
flux conversion of 4E-11 erg cm^-2  count^-1.

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


GRB_name: GRB131216A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15611
SUBJECT: GRB 131216A: Suzaku WAM observation of the prompt emission
DATE:    13/12/26 00:50:21 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

T. Nagayoshi, M. Tashiro, Y. Terada, S. Koyama, T. Yasuda, S. Takeda,
Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.), M. Yamauchi, N. Ohmori, M. 
Akiyama, R. Kinoshita (Univ. of Miyazaki), M. Ohno, K. Takaki,
T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa,
M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri(RIKEN),
Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report:

The GRB 131216A (Fermi LAT detection: Veres et al.,GCN Circ. 15598,
IPN localization:Hurley et al., GCN Circ. 15600) triggered the Suzaku
Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 01:56:32.11 UT (=T0).

The observed light curve shows a single FRED-like peak starting at
T0-1 s, ending at T0+8s, with a duration T90 of 5.69 seconds.
The fluence in 100 - 1000 keV was 7.46 (+0.99/-0.86) x10^-6 erg/cm^2.
The 1-s peak flux measured from T0+2s was
6.05 (+0.50/-0.73) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum fromT0-1s
to T0+8s is well fitted by a power-law with exponential cutoff model:

    dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
    alpha 1.42(+0.05/-0.73), and
    Epeak 400(+135/-142) keV (chi^2/d.o.f. = 15.5/13).

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

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


GRB_name: GRB131226A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15612
SUBJECT: GRB 131226A: Swift detection of a burst
DATE:    13/12/26 06:01:22 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

S. R. Oates (UCL-MSSL), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 05:47:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131226A (trigger=582123).  
The BAT on-board calculated location is 
RA, Dec 301.307, -64.962 which is 
   RA(J2000) = 20h 05m 14s
   Dec(J2000) = -64d 57' 43"
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 10 sec.  The peak count rate
was ~15000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 2014 January 27. There will thus be no XRT or
UVOT data for this trigger. 

Burst Advocate for this burst is S. R. Oates (samantha.oates AT 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: GRB131226A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15613
SUBJECT: GRB 131226A, Swift-BAT refined analysis
DATE:    13/12/26 13:30:30 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), S. R. Oates (UCL-MSSL),
D. M. Palmer (LANL), T. Sakamoto (AGU), J. Tueller (GSFC),
T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+481 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131226A (trigger #582123)
(Oates, et al., GCN Circ. 15612).  The BAT ground-calculated position is
RA, Dec = 301.309, -64.943 deg which is
    RA(J2000)  =  20h 05m 14.2s
    Dec(J2000) = -64d 56' 35.2"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.

The mask-weighted light curve shows a very complex structure with more than a 
dozen peaks covering the time period from T-0.5 sec to T+8.5 sec and peaking at 
T+1 sec.  This is followed by lower-level extended emission out to ~T+180 sec. 
T90 (15-350 keV) is 7.20 +- 0.16 sec (estimated error including systematics).

The time-averaged spectrum from T-0.26 to T+8.42 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.38 +- 0.04.  The fluence in the 15-150 keV band is 4.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.11 sec in the 15-150 keV band
is 10.4 +- 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/582123/BA/


GRB_name: GRB131225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15614
SUBJECT: GRB 131225A: MASTER-Net optical observations
DATE:    13/12/26 16:29:15 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, D.Denisenko, V. Lipunov, V.Kornilov, D.Kuvshinov, 
A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov,
V.V.Chazov, 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  GRB131225A 6 hours after trigger 
time at 2013-12-25 15:53:40 UT.
We cover full MAXI error box (A. Kawagoe et al GCN 15609) using MASTER II 
twin telescope in parallel mode with FOV 4 sq. degrees.
Observations were made in the extremely  rich field (with galactic 
latitude b=-4 deg).
The  5-sigma upper limit has been about 19.0 mag on our first (180s 
exposure) image. On coadd of first 19 images with total exposure 3420 sec 
and middle time 2013-12-25 16:30:25 UT the  5-sigma upper limit has been 
20.5 mag.

Inside MAXI field of view we have detected two objects not present in
USNO-B1.0 catalog with the following coordinates and unfiltered
magnitudes:

ID #1191735: 06 19 43.71 +04 47 37.6  (20.13m)
ID #1191736: 06 17 51.08 +04 57 19.8  (20.26m)

We have identified both objects with the red stars on the digitized
Palomar IR plates, as well as in WISE and UKIDSS catalogs.

WISE J061943.55+044738.8 (W1=14.33 W2=14.14)
UGPS J061943.55+044739.1 (J=15.42 H=14.88 K=14.47)

WISE J061751.09+045719.6 (W1=15.79 W2=15.46)
UGPS J061751.05+045719.7 (J=18.24 H=17.40 K=17.17)

Also, in error box we found 2 known minor planets (Groom and 2004 OZ). The 
total number of known asteroids in our FOV is 11. There is no new minor 
planet found in error box.

The combined optical image is available here
http://master.sai.msu.ru/static/GRB/GRB131225A_MAXI/GRB131225A.jpeg

The message may be cited.


GRB_name: GRB131224A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15615
SUBJECT: GRB 131224A: Swift/UVOT Upper Limits
DATE:    13/12/26 17:44:22 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 131224A 
10748 s after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 15607).
The field is very crowded and no optical afterglow consistent with the 
INTEGRAL position is detected in the initial UVOT exposures. Preliminary 
3-sigma upper limits using the UVOT photometric system (Breeveld et al. 
2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

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

u                10748        18662         3918         >21.1

The magnitudes in the table are not corrected for the strong Galactic 
extinction due to the reddening of E(B-V) = 0.96 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB131227A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15616
SUBJECT: GRB 131227A: Swift detection of a burst
DATE:    13/12/27 05:09:45 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

S. R. Oates (UCL-MSSL), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 04:44:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131227A (trigger=582184).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 67.386, +28.864 which is 
   RA(J2000) = 04h 29m 33s
   Dec(J2000) = +28d 51' 52"
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 20 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 04:45:48.0 UT, 57 seconds
after the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 67.3781,
28.8827 which is equivalent to:
   RA(J2000)  = 04h 29m 30.74s
   Dec(J2000) = +28d 52' 57.9"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). 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 (1.53 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.1
(+2.23/-1.94) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 6.01e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 66 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
1.02. 

Burst Advocate for this burst is S. R. Oates (samantha.oates AT 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: GRB131227A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15617
SUBJECT: GRB 131227A: OT candidate from KAIT Optical observations
DATE:    13/12/27 07:06:02 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to GRB 131227A (Oates et al., GCN 15616)
starting at 04:47:49 UT, 178 s after the burst. Observations were
performed with an automatic sequence in the V, I, and clear(roughly R)
filters, and the exposure time was 20 s per image.
Within the XRT error circle, we detected a new faint source at
coordinate of (J2000):

Ra =  04:29:30.83,   Dec= +28:52:58.81 (uncertainty about 1")

The object faded from mag ~18.6 to be below than 20.0 in our clear
band image about 10 minutes after (calibrated to USNO B1.0). We
suggest this is the OT of GRB 131227A. Further observations are
encouraged.


GRB_name: GRB131227A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15618
SUBJECT: GRB 131227A: Enhanced Swift-XRT position
DATE:    13/12/27 14:13:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 4481 s of XRT Photon Counting mode data and 6 UVOT
images, we find an astrometrically corrected X-ray position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 67.37825, 28.88310 which is equivalent to:

RA (J2000):  04 29 30.78
Dec (J2000): +28 52 59.2

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB131226A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15619
SUBJECT: Konus-Wind observation of GRB 131226A
DATE:    13/12/27 14:44:44 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long-duration GRB 131226A (Swift-BAT trigger 582123: Oates, et al., 
GCN 15612; Stamatikos, et al. GCN 15613) triggered Konus-Wind at 
T0=20858.013 s UT (05:47:38.013).

The burst light curve shows a multi-peaked structure with a total 
duration of ~7 s.

As observed by Konus-Wind, the burst
had a fluence of 1.01(-0.07,+0.08)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+2.704 s,
of (5.0 +/- 1.0)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+8.448 s)
is well fitted (in the 20 keV - 2 MeV range) by a power law with 
exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep), with
alpha = -0.90(-0.12,+0.13),  and
Ep = 264(-17,+20) keV (chi2 = 65.6/60 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.5.

All the quoted values are preliminary.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131226_T20858/


GRB_name: GRB131227A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15620
SUBJECT: GRB 131227A: Swift-BAT refined analysis
DATE:    13/12/27 15:00:28 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), S. R. Oates (UCL-MSSL), 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-240 to T+651 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 131227A (trigger #582184)
(Oates, et al., GCN Circ. 15616).  The BAT ground-calculated position is
RA, Dec = 67.369, 28.879 deg which is 
   RA(J2000)  =  04h 29m 28.5s 
   Dec(J2000) = +28d 52' 44.3" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-2 sec, peaking at ~T+2 sec, and ending at ~T+22 sec with a long low-level
tail out to ~T+100 sec.  T90 (15-350 keV) is 18.0 +- 1.6 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-1.19 to T+19.23 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.12.  The fluence in the 15-150 keV band is 8.4 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.61 sec in the 15-150 keV band
is 1.1 +- 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/582184/BA/


GRB_name: GRB131227A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15621
SUBJECT: GRB 131227A: Swift/UVOT Upper Limits
DATE:    13/12/27 15:55:33 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 131227A
66 s after the BAT trigger (Oates et al. GCN Circ. 15616).
No optical afterglow consistent with the enhanced XRT position
(Evans et al. GCN Circ. 15618) or the source detected by KAIT (Zheng
et al. GCN 15617) 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            66          216          147         >20.6
u_FC               278          528          246         >19.9
white               66        13019         1430         >21.9
v                  608         6785          471         >19.7
b                  534        12318         1160         >21.1
u                  278        11406         1366         >20.9
w1                5558         7195          393         >20.1
w2                4942         6580          393         >20.5

The magnitudes in the table are not corrected for the strong Galactic
extinction due to the reddening of E(B-V) = 1.02 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB131227A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15622
SUBJECT: GRB 131227A: Xinglong optical observations
DATE:    13/12/27 16:02:49 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), T.-M. Zhang, L.-P. Xin, F. Xiao (NAOC) report:

We observed the field of GRB 131227A (Oates et al., GCN 15616) using
the 2.16m Xinglong telescope, equipped with BFOSC and located in
Heibei, China. We obtained 2x600s R-band images with a mean time of
9.086 hr after the BAT trigger.

At the afterglow position (Zheng et al., GCN 15617), which is within
the XRT error circle (Evans & Goad, GCN 15618), the afterglow has
decayed to have R>21.2 mag, calibrated with nearby USNO B1 field.


GRB_name: GRB131227A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15623
SUBJECT: GRB 131227A: Swift-XRT refined Analysis
DATE:    13/12/27 17:09:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.6 ks of XRT data for GRB 131227A (Oates  et al. GCN
Circ. 15616),  from 63 s to 18.8 ks after the  BAT trigger. The data
comprise 1.8 ks in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. Using 4789 s of PC mode data and 7 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 =
67.37831, +28.88296 which is equivalent to:

RA (J2000): 04h 29m 30.80s
Dec(J2000): +28d 52' 58.7"

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.110 (+0.029, -0.028).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.28 (+0.22, -0.21). The
best-fitting absorption column is  4.4 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.93 (+0.22, -0.21)
and a best-fitting absorption column of 4.9 (+1.2, -1.1) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.9 x 10^-11 (8.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.9 (+1.2, -1.1) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 5.3 sigma
Photon index:      1.93 (+0.22, -0.21)

If the light curve continues to decay with a power-law decay index of
1.110, the count rate at T+24 hours will be 3.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.9 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/00582184.

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


GRB_name: GRB131227A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15624
SUBJECT: GRB 131227A: Gemini-North Redshift
DATE:    13/12/27 18:44:22 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (ORAU/NASA-GSFC) and S.B. Cenko (NASA-GSFC)
report on behalf of a larger collaboration:

"On December 27.42 UT (~ 5.1 hr after the Swift trigger) we
began observing the afterglow of GRB 131227A (Oates et al.
GCN 15616, Zheng et al. GCN 15617) with the GMOS spectrograph
mounted on the Gemini-North telescope.

Under poor seeing conditions the afterglow was marginally
detected in our i-band acquisition image.
Nevertheless, we performed a spectroscopic sequence of 2x900s
spectra with GMOS and the R400 grating, covering the 4400-8600A
wavelength range.

Clear evidence of continuum flux is detected beyond 7600A, while
no flux is present in either spectra nor in a coadded spectrum
blueward of this wavelength.
No other obvious emission or absorption features are present in
the spectrum, though the signal-to-noise ratio is not extremely
high.

If this break is due to Lyman-alpha, the implied GRB redshift
would be z~5.3.
We caution, however, that this line of sight is subject to high
galactic extinction (A_V= 2.8).

We thank the Gemini staff for performing these observations under
challenging conditions, in particular Marie Lemoine-Busserolle."


GRB_name: GRB131227A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15625
SUBJECT: GRB 131227A: P60 Limits
DATE:    13/12/27 19:05:01 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA/GSFC) and D. A. Perley (Caltech) report on behalf of a
larger collaboration:

We observed the location of the optical afterglow (Zheng et al., GCN
15617) of the Swift GRB 131227A (Oates et al., GCN 15616) with the robotic
Palomar 60 inch telescope.  Observations were obtained in the r', i', and
z' filters beginning at 05:59 UT on 2013 Dec 27 (~ 1.24 hours after the
Swift trigger time).  We do not detect any sources at the location of the
KAIT optical afterglow.  Using nearby point sources from the USNO-B1
catalog for reference, we calculate an upper limit of r > 21.0 mag at a
mean epoch of 1.50 hr after the Swift trigger.


GRB_name: GRB131224A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15626
SUBJECT: GRB 131224A: 5.8 GHz VLA observations
DATE:    13/12/27 23:35:41 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the field of the INTEGRAL short-duration GRB 131224A
(Mereghetti et al., GCN 15607) with the Karl G. Jansky Very Large Array
(VLA). We obtained two sets of 1-hour observations beginning on 2013 Dec
24.907 UT and 2013 Dec 26.971 UT (0.202 and 2.267 days post-burst,
respectively) at a mean frequency of 5.8 GHz. We find no evidence for
variability within the INTEGRAL error circle to a 3-sigma limit of 33
microJy at the time of the two observations.

We thank the VLA staff for quickly executing these observations."


GRB_name: GRB131229A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15627
SUBJECT: GRB 131229A: Swift detection of a burst
DATE:    13/12/29 06:55:46 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. J. Page (UCL-MSSL), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 06:39:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 131229A (trigger=582374).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 85.236, -4.431 which is 
   RA(J2000)  =  05h 40m 57s
   Dec(J2000) = -04d 25' 52"
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 25 sec.  The peak count rate
was ~27,000 counts/sec (15-350 keV), at ~13 sec after the trigger. 

The XRT began observing the field at 06:40:57.9 UT, 93.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 85.2327, -4.3962 which is equivalent to:
   RA(J2000)  = +05h 40m 55.85s
   Dec(J2000) = -04d 23' 46.3"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 125 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 3.18e-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. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6
mag. No correction has been made for the expected extinction corresponding
to E(B-V) of 0.29. 

Burst Advocate for this burst is M. J. Page (m.page AT 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: GRB131229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15628
SUBJECT: GRB 131229A: P60 nondetection
DATE:    13/12/29 07:15:30 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

The robotic Palomar 60-inch telescope automatically responded to GRB 
131229A (Page et al., GCN 15627) and began a sequence of 60-second image 
starting at 06:44:54 UT, 5.5 minutes after the burst.

In the initial r-band image we identify no sources within the XRT error 
circle down to a limiting magnitude of R > 20.5.  No source in the error 
circle is detected in the i- or z-band filters either.

We do detect a source not present in USNO B1.0 well north of the XRT 
error circle at RA=05:40:55.702, dec=-04:23:21.11 (J2000).  It does not 
appear to be fading in images taken so far.

Further P60 observations are ongoing.  NIR observations are encouraged.


GRB_name: GRB131229A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15629
SUBJECT: GRB 131229A: KAIT Optical Upper Limit
DATE:    13/12/29 07:54:23 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 131229A (Page et al.,
GCN 15627) starting at 06:41:34 UT, 130 s after the burst.
Observations were performed with an automatic sequence in the
V, I, and clear(roughly R) filters, and the exposure time was
20 s per image. Compared to the DSS image, we do not detect
new sources within XRT error circle. Typical limiting magnitude
of our single clear image is about 19.4. We marginally detected
the source mentioned by Perley (GCN 15628) in our single clear
image with mag around 19.3, and confirming its non-changing
brightness.

[GCN OPS NOTE(29dec13): Per author's request, the "110 s after the burst"
was changed to "130".]


GRB_name: GRB131229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15630
SUBJECT: GRB 131229A: Deep Gemini-South Imaging
DATE:    13/12/29 10:22:22 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), A. Cucchiara (NASA/GSFC), and N. R. Tanvir (U.
Leicester) report:

We imaged the position of GRB 131229A (Page et al., GCN 15627) using 
GMOS-S on the Gemini-South 8m telescope in i- an z-bands starting at 
07:33:07.5 UT (54 minutes after the GRB).  A total of 6 x 180s of 
imaging was acquired in each filter.

Sources detected in the reduced stack inside or close to the (onboard,
5" radius) XRT error circle (with J2000 positions) include:

A (05:40:55.85, -04:23:40.6), a point source north of the error circle
B (05:40:55.70, -04:23:43.4), an extended source
C (05:40:55.92, -04:23:45.9), a faint, marginally detected source

No statement about variability or association with the GRB can be made
at this time.  All of these sources are fainter than the P60 and USNO
limits.

An image of the field is posted to:
http://www.astro.caltech.edu/~dperley/gcn/131229a/131229a_gmos.png


GRB_name: GRB131229A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15631
SUBJECT: GRB 131229A: Enhanced Swift-XRT position
DATE:    13/12/29 16:54:35 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 7358 s of XRT Photon Counting mode data and 16 UVOT
images for GRB 131229A, 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 = 85.23169, -4.39629 which is equivalent
to:

RA (J2000): 05h 40m 55.61s
Dec (J2000): -04d 23' 46.6"

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: GRB131227A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15632
SUBJECT: GRB 131227A: GROND Upper Limits
DATE:    13/12/29 17:07:39 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed the field of GRB 131227A (Swift trigger 582184; Oates et al.,
GCN 15616) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2m MPG telescope at La Silla Observatory
(Chile).

Observations started at 02:10 UT on December 28th, around 21.4 hrs after
the GRB trigger, and lasted for 2 hours. They were performed at an average
seeing of 1".0 and at an average airmass of 2.

At the position of the optical afterglow reported by Zheng et al. (GCN
15617) and Cucchiara et al. (priv. comm., see also GCN 15624) we do not
detect any source down to 3-sigma AB limiting magnitudes of

g' > 25.7,
r' > 25.6,
i' > 24.8,
z' > 24.6,
J > 21.8,
H > 21.1, and
K > 19.7.

We do detect a compact source to the north-east, at

RA (J2000) = 04:29:30.90
Dec. (J2000) = +28:53:00.3

with an uncertainty of 0".3 and AB magnitudes

r' = 24.28 +/- 0.1,
i' = 24.19 +/- 0.1,
z' = 22.82 +/- 0.1, and
J  = 20.66 +/- 0.4.

It is undetected to above-mentioned limits in the other filters. The
relationship of this source to the afterglow is unclear.

The given limits and magnitudes are derived based on calibrating the
images 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)= 1.02 mag in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB131229A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15633
SUBJECT: GRB 131229A: Swift/UVOT Upper Limits
DATE:    13/12/29 18:18:09 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB131229A
159 s after the BAT trigger (Page et al., GCN Circ. 15627).
No optical afterglow consistent with the XRT enhanced position
(Evans et al. GCN Circ. 15631) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

u_FC               159          408          246         >19.9
u                  159         6481          639         >20.4
v                 4434        18141         1889         >20.6
b                 4023        16459         2164         >21.6
w1                4844         6275          393         >19.8
w2                4230        17366         1279         >20.5

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


GRB_name: GRB131229A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15634
SUBJECT: GRB 131229A: Swift-XRT refined Analysis
DATE:    13/12/29 18:56:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.9 ks of XRT data for GRB 131229A (Page  et al. GCN
Circ. 15627),  from 80 s to 29.7 ks after the  BAT trigger. The data
comprise 465 s in Windowed Timing (WT) mode (the first 12 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 15631).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.04 (+/-0.06), followed by a break at T+488 s to an
alpha of 1.34 (+0.09, -0.06).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+/-0.07). The
best-fitting absorption column is  7.9 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 1.8 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.06 (+0.16, -0.15)
and a best-fitting absorption column of 8.6 (+1.2, -1.1) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.2 x 10^-11 (1.1 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.6 (+1.2, -1.1) x 10^21 cm^-2
Galactic foreground: 1.8 x 10^21 cm^-2
Excess significance: 10.4 sigma
Photon index:      2.06 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.34, the count rate at T+24 hours will be 0.010 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.2 x
10^-13 (1.1 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/00582374.

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


GRB_name: GRB131229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15635
SUBJECT: GRB 131229A: Swift-BAT refined analysis
DATE:    13/12/29 19:15:46 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), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), M. J. Page (UCL-MSSL),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+443 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 131229A (trigger #582374)
(Page, et al., GCN Circ. 15627).  The BAT ground-calculated position is
RA, Dec = 85.236, -4.401 deg, which is 
   RA(J2000)  =  05h 40m 56.6s 
   Dec(J2000) = -04d 24' 04.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows many overlapping peaks
starting at ~T-1 sec, peaking at ~T+14 sec, and ending at ~T+17 sec
with a long low-level tail exteding out to ~T+430 sec, at which point
the BAT data stops due to entering the SAA.  T90 (15-350 keV) is
13.86 +- 0.43 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.08 to T+27.04 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.02 +- 0.03.  The fluence in the 15-150 keV band is 6.6 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+13.55 sec in the 15-150 keV band
is 10.7 +- 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/582374/BA/


GRB_name: GRB131229A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15636
SUBJECT: GRB 131229A: GROND observations
DATE:    13/12/29 19:23:16 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

J. F. Graham, P. Schady, D. A. Kann and J. Greiner (all MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 131229A (Page et al., GCN #15627) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG telescope at La Silla Observatory (Chile). 

Observations started at 07:02 UT on 29th December, 23 mins after the GRB trigger. They were performed at an average seeing of 1.7" and at high airmass.

Source B from Perley et al. (GCN #15630) is clearly detected within a 1440s exposure stacked H-band image (mid-time 07:45UT) with an AB magnitude of 20.1+/-0.2, and marginally detected in z' and J. However, we note that this source lies 1.5" outside the refined XRT position. 

In 3x8min stacked images centred 53 mins after the trigger, we do not detect a source within the refined Swift-XRT error circle down to the following upper limits (AB magnitudes):
g' > 24.2,
r' > 24.0,
i' > 23.4,
z' > 23.2,
J > 21.3,
H > 20.7, and
K > 19.4.

The given optical and NIR limits are calibrated against GROND zeropoints and 2MASS field stars in g'r'i'z and JHK respectively, and are not corrected for the Galactic foreground extinction corresponding to a reddening of E(B-V)=0.29 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB131229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15637
SUBJECT: GRB 131229A: Magellan upper limit
DATE:    13/12/30 07:01:04 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

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

We observed the field of GRB 131229A (Page et al., GCN 15627) using LDSS3 on the 
6.5 m Magellan Clay telescope starting 21 minutes after the BAT trigger. Initial 
r' and i' images in 0.8" seeing revealed no clear counterpart, consistent with 
the upper limits reported by other groups (Perley, GCN 15628; Zheng et al., GCN 
15629; Perley et al., GCN 15630; Graham et al., GCN 15636; de Pasquale et al., 
GCN 15633). We then obtained a sequence of 7x180s z'-band images starting at 
t=+34 min after the trigger. The sources labeled A and B by Perley et al. (GCN 
15628) are visible outside of the enhanced XRT error circle (Evans et al., GCN 
15631). However, a stack of our images reveals no sources within the enhanced 
XRT error circle. We set a 3-sigma upper limit of z'>24.3 mag (AB) at a midpoint 
of t=+49 minutes.


GRB_name: GRB131229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15638
SUBJECT: GRB 131229A: CARMA 3mm observations
DATE:    13/12/30 08:02:56 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

We observed the position of GRB 131229A (Page et al., GCN 15627) with
the Combined Array for Research in Millimeter Astronomy between 05:39:00 
and 07:28:46 UT (0.958-1.034 days post-GRB) at a mean frequency of 93 
GHz.  Conditions were excellent during the observation.

A preliminary examination of the observations reveals no source at the 
location of the XRT error circle (Evans et al., GCN 15631) down to a 
limit of approximately 0.6 mJy.

We thank the CARMA observers B. A. Zauderer and A. Dhabal and the CARMA 
staff for assistance with the observation.


GRB_name: GRB131229A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15639
SUBJECT: Konus-Wind observation of GRB 131229A
DATE:    13/12/31 14:32:55 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long-duration GRB 131229A (Swift-BAT trigger 582374: Page et al., 
GCN 15627) triggered Konus-Wind at T0=23970.560 s UT (06:39:30.560).

The burst light curve shows a multi-peaked structure with a total 
duration of ~17 s. The emission is seen up to ~1.5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB131229_T23970/

As observed by Konus-Wind, the burst had a
fluence of 2.45(-0.17,+0.18)x10-5 erg/cm2, and a 64-ms peak flux, 
measured from T0+10.976 s, of 1.07(-0.15,+0.15)x10-5 erg/cm2/s (both in 
the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+13.056 s) is best fit 
in the 20 keV - 1.5 MeV range by a power law with exponential cutoff 
model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep),
alpha = -0.65(-0.10,+0.11), and
Ep = 352(-28,+34) keV (chi2 = 51.9/60 dof).

The spectrum near the maximum count rate (measured from T0+8.448 to 
T0+13.056 s) is best fit in the 20 keV - 1.5 MeV range by a power law 
with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep), 
alpha = -0.43(-0.10,+0.11), and
Ep = 366(-24,+28) keV (chi2 = 58.6/60 dof).

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


GRB_name: GRB131231A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15640
SUBJECT: GRB 131231A: Fermi-LAT detection of a burst
DATE:    13/12/31 18:38:00 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), J. L. Racusin (NASA/GSFC), D. Kocevski
(NASA/GSFC) and J. McEnery (NASA/GSFC), report on behalf of the Fermi-LAT
team:

At 04:45:16.08 on Dec 31, 2013, Fermi LAT detected high energy emission
from GRB 131231A, which was also detected by Fermi-GBM (trigger
410157919/131231198).

The best LAT on-ground location is found to be RA, Dec 10.585,
-1.845 (J2000) with an error radius of 0.149 deg (90% containment,
statistical error only), this was 40 deg from the LAT boresight at the time
of the trigger.  The GRB was detected at high enough peak flux in the GBM
detectors to trigger an autonomous repoint of the spacecraft, which kept
the source in the LAT field of view for 900 seconds.

The data from the Fermi LAT are temporally correlated with the GBM emission
with high significance.  More than 37 photons above 100 MeV and more than
11 photons above 1 GeV are observed within 900 seconds. The highest energy
photon is a 9.7 GeV event which is observed at 700 seconds after the GBM
trigger.

A Swift ToO request has been submitted.

The Fermi LAT point of contact for this burst is Eda Sonbas (
edasonbas@yahoo.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: GRB131231A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15641
SUBJECT: GRB 131231A: Nanshan afterglow candidate
DATE:    13/12/31 21:39:24 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), H.-B. Niu, X. Zhang, A. Esamdin, L. Ma (XAO) report:

We observed the LAT field of GRB 131231A (Sonbas et al., GCN 15640)
using the 1m telescope located on Mt. Nanshan, Xinjiang, China,
equipped with a 1.2x1.2 deg^2 CCD camera. We obtained a series of 120s
and 300s frames at the mean time 12:40 UT on 2013-12-31 (i.e., 7.91 hr
after the Fermi trigger).

Within the LAT error circle (RA, Dec 10.585, -1.845 with an error
radius of 0.149 deg, error statistical only) reported in Sonbas et al.
(GCN 15640), no new prominent uncatalogued source is found and the
depth of the Nanshan image is similar to that of DSS II. Given that
the above LAT error is statistical only, we thus inspect that
surrounding region the LAT error circle and discovered a bright
source, not present in both DSS II and SDSS, at coordinates

R.A.=00:42:21.66
Dec.=-01:39:10.79

Err Radius: ~1.5 arcsec

with a magnitude of R~17.6, calibrated with nearby USNO B1 stars.

Follow-up observations are encouraged to check whether the source is
the afterglow of the burst.


GRB_name: GRB131231A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15642
SUBJECT: GRB 131231A: afterglow confirmation from the NOT
DATE:    13/12/31 23:02:02 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani, D. Xu (DARK/NBI), I. R. Losada (Stockholm), F. Duval 
(Stockholm), report on behalf of a larger collaboration:

We observed the afterglow candidate of GRB 131231A (Sonbas et al., GCN 
15640; Xu et al., GCN 15641) using the 2.56m Nordic Optical Telescope 
(NOT) equipped with MOSCA. Observations started at 22:05:40 UT on 2013 
Dec 31 (i.e., 17.3 hr after the Fermi trigger).

The afterglow candidate noted by Xu et al. (GCN 15641) has decayed to 
R=18.6, using the same calibration. We thus suggest that this source is 
very likely the afterglow of GRB 131231A. The coordinates of the 
afterglow can be refined to

R.A. = 00:42:21.665
Dec. = -01:39:10.61

with an error of 0.3".

We also wish a happy new year to everyone.


GRB_name: GRB131231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15643
SUBJECT: GRB 131231A: iPTF optical afterglow candidate coincident with Nanshan detection
DATE:    13/12/31 23:07:42 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), and M. M. Kasliwal
(Carnegie Observatories) report on behalf of the intermediate Palomar
Transient Factory (iPTF) collaboration:

Upon receiving the final GBM localization for GRB 131231A, we
selected ten fields to observe with the Palomar 48-inch Oschin
telescope (P48) covering 62 deg^2, most of the 1-sigma GBM error
circle. Due to the short remaining visibility window at Palomar, we
obtained only one epoch of images of five of the ten fields covering
30 deg^2. This includes ~90% of the LAT error localization (Sonbas et
al., GCN 15640).

Sifting through 50 candidate variable sources near the LAT error
circle using standard iPTF vetting procedures, at 1.45 hours after
the burst we identify multiple uncatalogued sources, including
iPTF13ekl at R=15.7 mag, at the coordinates
 RA(J2000)  =  00h 42m 21.67s
 DEC(J2000) = -01d 39' 11.0"

This position coincides with the Nanshan optical afterglow candidate
at 7.91 hours after the burst (Xu et al., GCN 15641). There are no
coincident sources in SDSS and no associated minor planets in the IAU
Minor Planet Center database at this location.

Despite the low ecliptic latitude of -5.7 deg, the two coincident
optical detections separated by 6.46 hours strongly disfavor a solar
system origin. These two observations fit a power-law decay with an
index of alpha=-1.03, suggesting that the source is indeed associated
with the GRB trigger.

See <http://www.its.caltech.edu/~lsinger/iptf/Fermi410157919.pdf> for
a depiction of the LAT error circle in relation to the P48 optical
candidates, with iPTF13ekl highlighted, and a selection of the P48
fields observed.


GRB_name: GRB131231A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15644
SUBJECT: GRB 131231A: Fermi GBM detection
DATE:    14/01/01 00:42:48 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 04:45:16.083 UT on December 31 2013, the Fermi Gamma-Ray
Burst Monitor triggered and located 
GRB 131231A (trigger 410157919/131231198). 
This GRB was detected in a ground analysis by 
the Fermi LAT (Sonbas et al. GCN 15640).  
It was also detected in optical follow-up observations
of the GBM position by DARK/NBI (Xu et al. GCN 15641) 
and iPTF (Singer et al. GCN 15643), and confirmed by NOT 
observations of the Fermi LAT position (Malesani et al. GCN 15642). 
The on-ground calculated location from GBM is consistent 
with the positions reported from these follow-up observations.

The trigger resulted in an Autonomous Repoint Request (ARR) 
that was accepted and the LAT slewed to the GBM in-flight 
location. The initial angle from the LAT boresight is 38 deg
from Fermi/GBM position.  

The GBM light curve consists of a single large peak preceded 
by a smaller peak which resulted in the trigger.  The 
duration (T90) of the burst was about 31 s (50-300 keV).
The time-averaged spectrum from T0+.003 s to T0+56 s is 
best fit with a Band function  with Epeak = 146 +/- 3 keV, 
alpha = -1.10 +/- 0.01 and beta = -2.14 +/- 0.01.

The event fluence (10-1000 keV) in this time interval is
 (2.51 +/- 0.01)E-06 erg/cm^2. The 1.0-sec peak photon flux 
measured starting from T0+22 s in the 10-1000 keV band
is 67.3 +/- 0.8 ph/s/cm^2.

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


GRB_name: GRB131231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15645
SUBJECT: GRB 131231A: VLT/X-shooter redshift
DATE:    14/01/01 02:36:10 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Xu (DARK/NBI), D. Malesani (DARK/NBI), N. R. Tanvir (Univ. 
Leicester), V. D'Elia (ASI/ASDC), A. de Ugarte Postigo (IAA/CSIC and 
DARK/NBI), T. Kruehler (ESO), J. P. U. Fynbo (DARK/NBI) report on behalf 
of a larger collaboration:

We observed the optical counterpart of the Fermi/LAT GRB 131231A (Sonbas 
et al., GCN 15640; Jenke & Xiong, GCN 15644; Xu et al., GCN 15641) with 
the ESO VLT equipped with the X-shooter spectrograph. The mean time of 
our observation is 2014 Jan 1.04 UT, that is 20.2 hr after the GRB. The 
spectrum covers the wavelength range 3200 to 18,000 AA.

The trace of the afterglow is well visible in all arms. We detect 
several absorption features which we interpret as due to Fe II, Mg II, 
Ca H and K, all at a common redshift z = 0.642 (wavelength solution 
based on archival calibration lamps). Emission lines corresponding to 
the [O III] doublet are also detected at the same redshift.

We acknowledge excellent support from the observing staff in Paranal, in 
particular Steffen Mieske.


GRB_name: GRB131231A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15646
SUBJECT: GRB 131231A: MDM afterglow observation
DATE:    14/01/01 08:13:16 GMT
FROM:    Jules Halpern at Columbia U.  <jules@astro.columbia.edu>

J. P. Halpern (Columbia U.) reports:

I observed the afterglow of GRB 131231A (Sonbas et al., GCN 15640;
Xu et al., GCN 15641) using the 1.3m McGraw-Hill telescope of the
MDM Observatory on 2014 January 1, from 01:40 to 03:18 UT.
Nineteen 5-minute exposures were obtained in the R-band.
Conditions were photometric, and the Landolt standard-star field
around PG0231+051 was used for calibration.  The afterglow magnitudes
measured for the first and last exposures of the sequence are:

                --------------------------------
                 Jan 1 UT  t-t0(hr)   R    +/-
                --------------------------------
                  01:40     20.92   18.48  0.02
                  03:18     22.55   18.61  0.02
                --------------------------------

The following stars in field were calibrated, and can be used for
comparison:

           -----------------------------------------
            Star  R.A.(2000)   Decl.(2000)      R
           -----------------------------------------
             A    00 42 30.4    -01 36 13     16.07
             B    00 42 11.7    -01 37 29     17.95
             C    00 42 15.9    -01 39 08     17.92
             D    00 42 20.0    -01 41 53     17.22
             E    00 42 28.8    -01 40 16     17.96
           -----------------------------------------


GRB_name: GRB131231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15647
SUBJECT: GRB 131231A : xinglong TNT optical observation
DATE:    14/01/01 13:10:54 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 131231A  (Sonbas et al., GCN 15640;
Xu et al., GCN 15641,15645; Malesani et al., GCN 15642; Singer et al. GCN 15643;
Halpern GCN 15646) with Xinglong 0.8-m TNT telescope at 10:29:40 (UT) , 
Jan. 1th, at 2014, about 29.73 hours after the burst.  
12*300 sec B,V,R-band images were obtained. 

The optical afterglow (Xu et al., GCN 15641)   was  clearly detected 
with a magnitude of 18.97+/-0.1 mag in R band, calibrated by USNO B1.0 R2mag 
at the mean time of 29.73 hours after the burst.

Compared with the report by Halpern GCN 15646, the brightness of this afterglow
decayed for 0.36 mag during the epoch between 22.55 hours and 29.73 hours after the burst.

This message may be cited.


GRB_name: GRB131231A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15648
SUBJECT: GRB 131231A: Swift-XRT observations
DATE:    14/01/01 17:39:26 GMT
FROM:    Vanessa Mangano at PSU  <vxm22@psu.edu>

V. Mangano (PSU), K. Page (U. Leicester), D. Malesani (DARK/NBI) 
report on behalf of the Swift-XRT team:

We have analysed 4.0 ks of XRT data for the Fermi/LAT-detected burst:
GRB 131231A,  from 52.1 ks to 62.5 ks after the  Fermi/LAT trigger. The
data are entirely in Photon Counting (PC) mode. 
An X-ray source is detected at a position consistent with the optical afterglow 
(Xu et al., GCN 15641) at a mean count rate of 0.4 ct/s.
The refined XRT position is RA, Dec = 10.5904, -1.6519  which is equivalent to:

RA (J2000): 00 42 21.70
Dec(J2000): -01 39 06.7

with an uncertainty of 3.5 arcsec (radius, 90% confidence). This
position is 695 arcsec from the Fermi/LAT position and 4 arcsec
from the optical afterglow.

The light curve can be modelled with a power-law decay with an
index of alpha=1.6 (+/-0.7). 

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.86 (+0.13, -0.13). The
best-fitting absorption column at the redshift of 0.642 (Xu et al., GCN 15645)
is  1.4 (+0.7, -0.6) x 10^21 cm^-2, in excess of the Galactic value of 
2.6 x 10^20 cm^-2 (Kalberla et al. 2005). 
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced 
from this spectrum  is 3.0 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. 

Further ToO observations have already been scheduled for today.

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


GRB_name: GRB131227A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15649
SUBJECT: GRB 131227A: KAIT light curve analysis
DATE:    14/01/01 20:55:53 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

We analyzed the early time KAIT data of GRB 131227A (Oates et al., GCN
15616). The afterglow is easily detected in our clear and I band
images, but not in V band images (single or co-added). After correcting
for the large Galactic extinction (A_V = 2.8 mag, A_I = 1.5 mag;
Schlegel et al., 2011, ApJ, 737, 103), we found the afterglow had a
color of (V - I) > 1.2 mag at early times (~200 s - 900 s). This is
consistent with the spectral break around 7600 A reported by Cucchiara &
Cenko (GCN 15624), but still not so constraining to say the break is
caused by Lyman-alpha.

Due to lack of emission below 7600 A (either because of extinction
or Lyman-alpha break), we calibrated the KAIT clear image to the i'
band. Our preliminary result shows the afterglow decays as a power law
with alpha = -0.99. The late time upper limit reported by Kann et al.
(GCN 15632) is below the extrapolation of the line. 

The preliminary light curve can be found at the following link:
http://128.32.15.133/kait/grb/131227A/GRB131227A.png


GRB_name: GRB131231A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15650
SUBJECT: GRB 131231A: P60 observations
DATE:    14/01/02 05:09:18 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

We imaged the location of GRB 131231A with the Palomar 60-inch (P60) 
robotic telescope on UT 2014-01-01 between 03:28:31 and 04:22:05, and 
again on 2014-01-02 between 01:56:28 and 02:37:12. Observations were 
taken in the g, r, i, and z filters during each epoch.

The afterglow (Xu et al., GCN 15641) is well-detected in individual 
exposures in all bands.  Both nights were photometric and we calibrated 
the field using an observation of the nearby standard field SA92.

Some photometry of the GRB afterglow in the gri bands (all on the 
SDSS/AB system) is:

r = 18.84 +/- 0.02  (t = 0.965 d)
i = 18.72 +/- 0.02  (t = 0.970 d)
g = 19.14 +/- 0.02  (t = 0.982 d)

r = 19.77 +/- 0.03  (t = 1.886 d)
i = 19.64 +/- 0.04  (t = 1.893 d)
g = 20.06 +/- 0.03  (t = 1.907 d)

The power-law temporal decay index in all bands is approximately alpha=1.3.


We also give gri magnitudes of the five nearby calibration stars 
presented by Halpern (GCN 15646) for reference:

star  RA          dec       R         g      r      i
  A    00:42:30.4 -01:36:13  16.07     16.86  16.28  16.11
  B    00:42:11.7 -01:37:29  17.95     19.50  18.24  17.66
  C    00:42:15.9 -01:39:08  17.92     19.16  18.20  17.85
  D    00:42:20.0 -01:41:53  17.22     17.62  17.48  17.58
  E    00:42:28.8 -01:40:16  17.96     18.76  18.18  18.02


GRB_name: GRB131229A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15651
SUBJECT: GRB 131229A: Fermi GBM detection
DATE:    14/01/02 20:50:44 GMT
FROM:    Narayana Bhat at U Alabama/Huntsville/GBM  <Narayana.Bhat@nasa.gov>

A. von Kienlin (MPE) and P. N. Bhat (UAH)
report on behalf of the Fermi GBM Team:

"At 06:39:24.48 UT on 29 December 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 131229A (trigger 409991967 / 20131229277),
which was also detected by the Swift/BAT
(Page et al. 2013, GCN 15627 and Konus-Wind Golenetskii et al. 2013, GCN 15639).
The GBM on-ground location is consistent with the Swift/XRT position (Evans et al. 2013, GCN 15631) .

The angle from the Fermi LAT boresight is 84 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 13 s (50-300 keV).
The time-averaged spectrum from T0+0.002 s to T0+16.096 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.71 +/- 0.02 and
the cutoff energy, parameterized as Epeak, is 382.0 +/- 11.6 keV.

The event fluence (10-1000 keV) in this time interval is
(2.64 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+13.216 s in the 10-1000 keV band
is 24.0+/-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: GRB131231A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15652
SUBJECT: GRB 131231A: Gemini-South Redshift
DATE:    14/01/02 21:09:59 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (ORAU/NASA-GSFC) reports on behalf

of a larger collaboration:


"On January 1.09 UT (~21.5 hours after the trigger) we observed

the afterglow of GRB 131231A (Sombas et al. GCN 15640, Xu et

al. GCN 15641, Malesani et al. 15642, Singer et al. GCN 15643)

with the Gemini South telescope equipped with the GMOS

camera.


A series of spectroscopic observations in Nod & Shuffle more, was

carried out using the R400 grating covering the 6000-10000 A

wavelength range at an average airmass of 2.1.


The resulting spectra show absorption features from CaH+K,

as well as emission lines from forbidden [OII]3727 and

[OIII]4959,5007 transitions at the common redshift of z=0.6439,

consistent with the one reported by Xu et al. (GCN 15645).


We thank the Gemini staff for performing these observations,

in particular E. Marin and E. Wenderoth."


GRB_name: GRB140102A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15653
SUBJECT: GRB 140102A: Swift detection of a burst with optical counterpart
DATE:    14/01/02 21:27:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

L. M. Z. Hagen (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. B. Cenko (GSFC), D. Grupe (PSU), S. T. Holland (STScI),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (INAF-OAB/PSU), C. A. Swenson (PSU), T. N. Ukwatta (MSU)
and B.-B. Zhang (UAH) report on behalf of the Swift Team:

At 21:17:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140102A (trigger=582760).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 211.902, +1.331 which is 
   RA(J2000) = 14h 07m 37s
   Dec(J2000) = +01d 19' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a total duration of about 8 sec.  The peak count rate
was ~55,000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 21:18:34.3 UT, 56.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 211.9190, 1.3333 which is equivalent to:
   RA(J2000)  = +14h 07m 40.56s
   Dec(J2000) = +01d 19' 59.9"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 61 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 7.00e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 65 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 14:07:40.65 = 211.91936
  DEC(J2000) = +01:19:59.7  = 1.33325
with a 90%-confidence error radius of about 0.74 arc sec. This position is 1.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.98 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03. 

Burst Advocate for this burst is L. M. Z. Hagen (lea.zernow.hagen 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: GRB131224B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15654
SUBJECT: GRB 131224B detected in ground analysis of Swift-BAT data
DATE:    14/01/02 23:45:09 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings and D. M Palmer (Los Alamos) report on behalf of the
Swift-BAT team:

At 03:25:08 while Swift was executing a pre-planned slew, BAT detected a rate
increase.  In ground analysis, a significant source was found at RA, Dec
163.722, -14.177 which is
RA (J2000)       10h 54m 53.3s
Dec (J2000)     -14d 10' 36"
with an estimated 90% confidence error radius of 3 arcmin.  This location
was about 95% coded in the BAT field of view during the burst.

The mask-weighted lightcurve shows two symmetrical peaks, the second peak
about 1/3 the size of the first, each about 4 seconds long and separated by
a gap of about 2 seconds.  T90 is about 9 seconds.

The average spectrum over 11 seconds is well fit by a simple power-law
function with a photon index of 2.09 +- 0.20.  The fluence was
(2.6 +- 0.3) x 10^-7 ergs/cm^2.  Errors are 90% confidence.

Because this burst was noticed a week after it occurred, there is no followup
planned with Swift.


GRB_name: GRB140102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15655
SUBJECT: GRB 140102A: Early optical observations from Nanshan
DATE:    14/01/03 00:07:27 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), X. Zhang, C.-H. Bai, H.-B. Niu, A. Esamdin, L. Ma
(XAO) report:

We observed the field of GRB 140102A (Hagen et al., GCN 15653) using
the 1m telescope located on Mt. Nanshan, Xinjiang, China, equipped
with a 1.2x1.2 deg^2 CCD camera. Observations started at 21:27:51 UT
on 2014-01-02 (i.e., 614s after the BAT trigger). All frames are in R
filter.

We find a decaying afterglow at the UVOT position, beginning with
R~16.3 mag at a mean time of 674s post-burst. The afterglow is
decaying roughly as F(t) ~ t^-1 up to ~7000s post-burst, possibly with
fluctuations in between. Observations are ongoing.

Photometry is calibrated with nearby stars: SDSS J140740.98+011949.8
and SDSS J140742.47+012010.4.


GRB_name: GRB140103A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15656
SUBJECT: GRB 140103A: Swift detection of a burst
DATE:    14/01/03 00:55:31 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. Mangano (PSU), S. D. Barthelmy (GSFC), D. Grupe (PSU),
S. T. Holland (STScI), J. A. Kennea (PSU), D. M. Palmer (LANL),
T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU), C. A. Swenson (PSU)
and T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 00:30:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140103A (trigger=582773).  Swift slewed after 100 sec to the burst. 
The BAT on-board calculated location is 
RA, Dec 232.131, +37.749 which is 
   RA(J2000)  =  15h 28m 31s
   Dec(J2000) = +37d 44' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 15 sec.  The peak count rate
was ~1400 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 00:33:31.6 UT, 168.3 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 171 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
0.01. 

Burst Advocate for this burst is V. Mangano (vxm22 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: GRB140102A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15657
SUBJECT: GRB 140102A: Enhanced Swift-XRT position
DATE:    14/01/03 03:46:44 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 2356 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140102A, 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 = 211.91916, +1.33314 which is equivalent
to:

RA (J2000): 14h 07m 40.60s
Dec (J2000): +01d 19' 59.3"

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: GRB140102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15658
SUBJECT: GRB 140102A: I-band observations from IAC80 and 1.23m CAHA telescopes
DATE:    14/01/03 09:15:08 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA/CSIC-UPV/EHU), V. Terron (IAA/CSIC), E. Gomez (IAC), J. Cepa (IAC), M. Fernandez (IAA/CSIC), report on behalf of a larger collaboration:

We observed the GRB140102A optical afterglow (Hagen et al., GCN 15653; Xu et al., GCN 15655) in the I-band using the 1.23m CAHA and IAC80 telescopes. The images were acquired on Jan 3.2569-3.2670 UT and Jan 3.2719-3.2942 UT, respectively. The afterglow is clearly detected with I~20.5 (vega), calibrated against the USNO B1.0 catalog.


GRB_name: GRB140102A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15659
SUBJECT: GRB 140102A: Fermi-LAT detection of a burst
DATE:    14/01/03 12:02:52 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), G. Vianello (Stanford University) and F. Longo
(University and INFN, Trieste) report on behalf of the Fermi-LAT team:

The Fermi Large Area Telescope (LAT) detected emission from GRB 140102A,
also detected by Swift (Hagen et al., GCN 15653) and GBM (trigger
140102887) at 21:17:37.64 UT on January 02, 2014.

The GRB was detected at high enough peak flux in the GBM detectors to
trigger an autonomous repoint of the spacecraft. The source was 47 deg from
the LAT boresight at the time of the trigger, and then was kept close to
the boresight of the LAT up to 1200 seconds after the trigger. It entered
again the LAT field of view from T0+3400 to T0+7000 s.

Only the first couple of hundreds seconds of LAT data have been processed.
They show an excess temporally and spatially correlated with the emission
detected by Swift and by the GBM with very high significance. More than 20
photons above 100 MeV and more than 5 photons above 1 GeV are observed
within the first ~650 seconds. The highest energy photon is a 8 GeV event
which is observed 520 seconds after the GBM trigger.

The best LAT on-ground location is found to be RA, Dec 211.88, 1.36 (J2000)
with an error radius of 0.25 deg (90% containment, statistical error only),
which is 0.05 deg from the afterglow candidate detected and localized by
Swift/UVOT (GCN 15653).

The Fermi LAT point of contact for this burst is Eda Sonbas (
edasonbas@yahoo.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: GRB140103A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15660
SUBJECT: GRB 140103A: MASTER-Net optical observations
DATE:    14/01/03 12:05:21 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy,  V. Lipunov, D.Denisenko, V.Kornilov, 
D.Kuvshinov, N.Tyurina,  P.Balanutsa,  A.Kuznetsov
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  GRB140103A 22 sec after notice 
time and 303 sec after trigger time at 00:35:54 UT. On our first (60s 
exposure) set we haven't found optical transient  within SWIFT error-box 
(V. Mangano et. al. GCN 15656).

The 5-sigma upper limit has been about 18.5 mag on first image and 21.2 
mag on coadd of 20 images with total exposure 3600 sec and avagare time 
01:18:38 UT i.e. 2890 sec after trigger.

The message may be cited.


GRB_name: GRB140102A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15661
SUBJECT: GRB 140102A: Swift-XRT refined Analysis
DATE:    14/01/03 12:27:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U.
Leicester), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), P.
D'Avanzo (INAF-OAB) and L.M.Z. Hagen report on behalf of the Swift-XRT
team:

We have analysed 6.9 ks of XRT data for GRB 140102A (Hagen  et al. GCN
Circ. 15653),  from 47 s to 25.3 ks after the  BAT trigger. The data
comprise 3.0 ks in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 15657).

The late-time light curve (from T0+5.4 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.72 (+0.16, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.85 (+/-0.03). The
best-fitting absorption column is  1.31 (+/-0.09) x 10^21 cm^-2, in
excess of the Galactic value of 2.7 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.93 (+0.17, -0.16)
and a best-fitting absorption column of 9.0 (+4.1, -3.7) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (4.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.0 (+4.1, -3.7) x 10^20 cm^-2
Galactic foreground: 2.7 x 10^20 cm^-2
Excess significance: 2.8 sigma
Photon index:      1.93 (+0.17, -0.16)

If the light curve continues to decay with a power-law decay index of
1.72, the count rate at T+24 hours will be 6.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.6 x
10^-13 (3.2 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/00582760.

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


GRB_name: GRB140102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15662
SUBJECT: GRB 140102A, Swift-BAT refined analysis
DATE:    14/01/03 14:07:40 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), L. M. Z. Hagen (PSU), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), 
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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140102A (trigger #582760)
(Hagen, et al., GCN Circ. 15653).  The BAT ground-calculated position is
RA, Dec = 211.915, 1.332 deg which is 
  RA(J2000)  =  14h 07m 39.5s 
  Dec(J2000) = +01d 19' 54.8" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.

The mask-weighted light curve shows many overlapping peaks starting 
at ~T-0.2 sec, peaking at ~T+0.7 sec and ending at ~T+5 sec with a long 
tail emission out to T+200 sec.  T90 (15-350 keV) is 65 +- 15 sec (estimated 
error including systematics).

The time-averaged spectrum from T-0.15 to T+131.22 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.38 +- 0.04.  The fluence in the 15-150 keV band is 7.7 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.97 sec in the 15-150 keV band
is 29.8 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/582760/BA/


GRB_name: GRB140102A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15663
SUBJECT: GRB 140102A: MAXI/GSC detection
DATE:    14/01/03 14:11:53 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Kimura (JAXA), T. Sakamoto (AGU), S. Nakahira (JAXA), 
S. Ueno, H. Tomida, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, M. Morii, M. Serino, J. Sugimoto, T. Takagi, 
A. Yoshikawa, M. Matsuoka (RIKEN), 
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii, Y. Tachibana (Tokyo Tech), 
A. Yoshida, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, M. Sasaki, D. Uchida (Osaka U.), 
H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, M. Higa (Chuo U.), 
M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada, Y. Morooka (Miyazaki U.),
K. Yamaoka (Nagoya U.) 
report on behalf of the MAXI team:

The MAXI/GSC Nova alert system triggered a bright uncatalogued 
X-ray transient source at 21:19:54 UT on 2014-01-02.  Assuming that 
the source flux was constant over the transit, we obtain the source position at 

(R.A., Dec) = (211.813 deg, 1.477 deg) = (14 07 15, +01 28 37) (J2000) 

with a statistical 90% C.L. elliptical error region in long and short radii of 
0.46 deg and 0.35 deg respectively.  The roll angle of long axis from the north 
direction is 40.0 deg counterclockwise.  There is an additional systematic 
uncertainty of 0.1 deg (90% containment radius).  This uncatalogued X-ray 
source is temporary and positionally coincident with the Swift detected 
GRB 140102A (Hagen et al. GCN #15653).   

Using the data available from 21:16 to 21:23 UT, the MAXI/GSC spectrum 
is created from T0(BAT)+58.2 sec to T0(BAT)+219.2 sec (T0(BAT) is the trigger 
time of the Swift/BAT).  An absorbed power-law model gives an acceptable 
fit to the data.  The best fit photon index is 2.7 (-0.8/+1.0).  The unabsorbed 
2-20 keV flux is 2.3 (-0.8/+0.9) x 10^-9 erg/cm2/s.  All the quoted errors 
are at the 90% confidence level. 

There was no significant excess flux in the previous transit at 
19:47 UT and in the next transit at 22:53 UT with an upper limit 
of ~20 mCrab for each.


GRB_name: GRB140103A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15664
SUBJECT: GRB 140103A, Swift-BAT refined analysis
DATE:    14/01/03 14:14:10 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC),  J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), V. Mangano (PSU), 
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-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140103A (trigger #582773)
(Mangano, et al., GCN Circ. 15656).  The BAT ground-calculated position is
RA, Dec = 232.114, 37.752 deg which is 
  RA(J2000)  =  15h 28m 27.2s 
  Dec(J2000) = +37d 45' 08.4" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 48%.

The mask-weighted light curve shows two peaks.  The first weak peak starts 
at ~T-13 sec, peaks at ~T-11 sec and ends at ~T-6 sec.  The second peak starts 
at ~T-4 sec, peaks at ~T+1 sec and ends at ~T+9 sec.  T90 (15-350 keV) is 
17.3 +- 1.9 sec (estimated error including systematics).

The time-averaged spectrum from T-12.52 to T+6.94 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.6 +- 0.2.  The fluence in the 15-150 keV band is 6.0 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.39 sec in the 15-150 keV band
is 2.1 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 


GRB_name: GRB140102A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15665
SUBJECT: GRB 140102A: GROND observations
DATE:    14/01/03 15:03:39 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

M. Tanga (MPE Garching), S. Klose (TLS Tautenburg), and J. Greiner (MPE 
Garching) report on behalf of the GROND team:

We observed the field of GRB 140102A (Hagen et al., GCN 15653) 
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 
405) mounted at the 2.2m MPG telescope at La Silla Observatory (Chile).

Observations started at 07:51 UT on Jan 03, about 10.5 hrs after the GRB 
trigger. The afterglow discovered by Hagen et al. (see also Gorosabel et 
al., GCN 15658; Xu et al., GCN 15655) is detected in all optical bands. At 
a mean time of 08:19 UT, we measure the following preliminary AB 
magnitudes:

g'= 21.6 +/- 0.1,
r'= 21.4 +/- 0.1,
i'= 20.9 +/- 0.1,
z'= 21.0 +/- 0.1,
J = 20.7 +/- 0.3,
H = 20.6 +/- 0.4,
K > 19.3,

calibrated against SDSS and 2MASS field stars.

After correcting for a Galactic reddening of E(B-V)=0.03 mag (Schlegel et 
al. 1998), the spectral slope defined by g'r'z'JH is ~ 0.7, with no 
evidence for host extinction.

The SED fit shows a slight excess in i'-band flux. It could be due to 
emission line(s) from the underlying host, though we cannot say anything 
about an underlying galaxy due to the bad image quality (FWHM ~ 2.5"). We 
note, however, the presence of a galaxy just 4" East of the afterglow.


GRB_name: GRB140103A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15666
SUBJECT: GRB 140103A: Swift-XRT refined analysis
DATE:    14/01/03 15:17:05 GMT
FROM:    Vanessa Mangano at PSU  <vxm22@psu.edu>

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

We have analysed 5.1 ks of XRT data for GRB 140103A (Mangano  et al.
GCN Circ. 15656),  from 172 s to 8.5 ks after the  BAT trigger. The
data comprise 2.6 ks in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. 
A faint X-ray source at the level of 0.05 counts/s is detected during 
PC mode observation.
The refined XRT position is RA, Dec = 232.08747, +37.75917 
which is equivalent to:

RA (J2000): 15 28 20.99
Dec(J2000): +37 45 33.0

with an uncertainty of 3.6 arcsec (radius, 90% confidence).

The 2.5 ks PC observation show a small scale flare and WT mode data are 
background dominated due to bright earth contamination and highly scattered.
At present time we cannot asses if the source is fading.
Further observations have been scheduled.

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


GRB_name: GRB140102A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15667
SUBJECT: Konus-Wind observation of GRB 140102A
DATE:    14/01/03 15:53:48 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 140102A
(Swift-BAT trigger 582760: Hagen et al., GCN 15653, Barthelmy et al., GCN 15662;
Fermi LAT detection: Sonbas et al., GCN 15659;
MAXI/GCS detection: Kimura at al., GCN 15663)
triggered Konus-Wind at T0=76656.245 s UT (21:17:36.245).

The burst light curve shows a multi-peaked structure from ~T0-0.5 s to ~T0+4 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140102_T76656/

As observed by Konus-Wind, the burst
had a fluence of (2.0  0.2)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.192 s,
of (1.3  0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+10.496 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.05  0.14,
the high energy photon index beta = -2.68  0.30,
the peak energy Ep = 185  19 keV,
chi2 = 120/97 dof.

The spectrum near the maximum count rate
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.75  0.27,
the high energy photon index beta = -3.05  0.73,
the peak energy Ep = 200  31 keV,
chi2 = 85.8/69 dof.

All the quoted values are preliminary.


GRB_name: GRB131229A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15668
SUBJECT: GRB 131229A: Suzaku WAM observation of the prompt emission
DATE:    14/01/03 16:01:44 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-u.ac.jp>

T. Yasuda, M. Tashiro, Y. Terada, S. Koyama, S. Takeda, Y. Ishida,
H. Ueno, S. Sugimoto, T. Nagayoshi (Saitama U.), M. Yamauchi,
N. Ohmori, M. Akiyama, R. Kinoshita (Univ. of Miyazaki), M. Ohno,
K. Takaki, T. Kawano, R. Nakamura, S. Furui,
Y. Fukazawa (Hiroshima U.), K. Yamaoka (Nagoya U.),
S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), W. Iwakiri(RIKEN),
Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa, 
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report:


The long GRB 131229A (Swift/BAT trigger #582374; M. J. Page et al., GCN 15627) triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 06:39:29.971 UT (=T0). 

The observed light curve shows a multi-peaked structure starting at T0-6 s, ending at T0+13 s with a duration (T90) of about 12 s. The fluence in 100 - 1000 keV was 2.35 (+0.28/-0.30) x10^-5 erg/cm^2. The 1-s peak flux measured from T0+9 s was 13.7 (+0.8/-0.8) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-6 s to T0+13 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       1.05 (+0.67/-0.80), and
Epeak       405 (+78/-156) keV (chi^2/d.o.f. = 8.2/10).

All the quoted errors are at statistical 90% confidence level.

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


GRB_name: GRB140102A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15669
SUBJECT: GRB 140102A: Fermi/GBM Observation
DATE:    14/01/03 16:46:14 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang and Narayana Bhat (UAH/CSPAR) report on behalf of the Fermi GBM Team:

"At 21:17:37.81 UT on January 02 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140102A (trigger 410390260/
140102887). This GRB also triggered Swift (Hagen et al. GCN 15653) and 
Konus-Wind (Golenetskii et al, GCN 15667) and was detected by Fermi/LAT 
(Sonbas et al. GCN 15659) and in several ground follow-up observations 
(Xu et al GCN 15655; Gorosabel et al, GCN 15658; Kimura et al, GCN 15663 
and Tanga et al, 15665). The GBM on-ground calculated location is consistent 
with the Swift/XRT position and those obtained with follow-up observations.

The trigger resulted in an Autonomous Repoint Request (ARR) that was 
accepted and the spacecraft slewed to the GBM in-flight location. The 
initial angle from the LAT boresight was 47 deg from the Fermi/GBM 
position.

The GBM light curve consists of two major bright overlapping peaks. The 
duration (T90) of the burst was about 3.6 s (50-300 keV). The time-averaged 
spectrum from T0+0.4 s to T0+4 s is best fit with  a Band function with 
Epeak = 186 +/- 5 keV, alpha = -0.71 +/- 0.02  and beta = -2.49 +/- 0.07.

The event fluence (10-1000 keV) in this time interval is
(1.78 +/- 0.03)E-05 erg/cm^2. The 1.0-sec peak photon flux measured 
starting from T0+1.98 s in the 10-1000 keV band is 49.7 +/- 0.5 ph/s/cm^2.

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


GRB_name: GRB131231A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15670
SUBJECT: Konus-Wind observation of GRB 131231A
DATE:    14/01/03 17:15:47 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 131231A
(Fermi-LAT detection: Sonbas, et al., GCN 15640;
Fermi-GBM observation: Jenke & Xiong, GCN 15644)
triggered Konus-Wind at T0=17132.361 s UT (04:45:32.361).

The light curve shows a broad mult-peaked pulse from ~T0-13 s to ~T0+35 s.
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/GRB131231_T17132/
Note: periodic 'dips' in the count rate are due
to the GRB source occultation by the s/c structure.

As observed by Konus-Wind, the burst
had a fluence of (1.55  0.05)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+7.488 s,
of (2.14  0.13)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+34.303 s)
is best fit in the 35 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.28  0.04,
the high energy photon index beta = -2.47  0.05,
the peak energy Ep = 163  6 keV,
chi2 = 93.8/95 dof.

The spectrum near the maximum count rate
(measured from T0+5.888 s to T0+8.448 s)
is best fit in the 35 keV - 10 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.76  0.09,
and the peak energy Ep = 226  14 keV,
chi2 = 94.3/82 dof.

Assuming the redshift z=0.644 (Xu, et al., GCN 15645;
Cucchiara, GCN 15652),
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is (1.7  0.1)x10^53 erg,
the peak luminosity L_iso is (3.9  0.2)x10^52 erg/s,
and the rest-frame peak energy Ep,i = (270  10) keV

All the quoted results are preliminary.


GRB_name: GRB140103A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15671
SUBJECT: GRB 140103A: Swift/UVOT Upper Limits
DATE:    14/01/03 18:13:02 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 140103A
172 s after the BAT trigger (Mangano et al., GCN Circ. 15656).
No optical afterglow consistent with the XRT position (Mangano et al.,
GCN Circ 15666) 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           172          321          147         >20.8
white              172         2581          361         >21.5
v                  406         2631          252         >19.1
b                  506         2557          233         >19.9
u                  480         2704          252         >19.5
w1                 456         2680          252         >19.6
m2                6760         8396          393         >20.0
w2                 382         2607          252         >19.9

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: GRB131231A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15672
SUBJECT: GRB 131231A: Fermi GBM correction to GCN 15644
DATE:    14/01/03 19:03:04 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

P. Jenke (UAH) reports on behalf of the Fermi GBM team:

"The quoted fluence (10-1000 keV) in GCN 15644 (P. Jenke et al) 
was in fact the time integrated average energy flux for this burst.  The actual 
fluence (10-1000 kev) for this event is (1.400 +/- 0.001)E-4 ergs/cm^2."


GRB_name: GRB131231A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15673
SUBJECT: GRB 131231A: Swift/UVOT Observations of the Optical Afterglow 
DATE:    14/01/03 19:47:04 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and
V. Mangano (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began observations of the field of GRB 131231A 136.5 ks
after the Fermi/LAT trigger (Sonbas et al., 2013, GCNC 15640).  The
preliminary UVOT position is

     RA (J2000)  00:42:21.66  =  10.59025 (deg)
    Dec (J2000) -01:39:10.6   =  -1.65294 (deg)

with an estimated uncertainty of 0.43 arcsec (radius, 90% confidence,
statistical + systematic).  We detect the optical afterglow at the
position reported by Xu et al. (2013, GCNC 15641).  Preliminary UVOT
photometry is presented below.

------------------------------------------------------
Filter      TSTART     TSTOP    Exposure     Mag   Err
------------------------------------------------------
u          246,875   248,554        1652   19.57  0.10
white      136,762   138,942        1650   19.37  0.05
white      228,985   231,172        1639   20.07  0.07
------------------------------------------------------

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

The white observations yield a power-law decay index of alpha ~ 1.25
between 1.6 and 2.7 days.  This is consistent with that found by
Perley et al. (2014, GCNC 15650) between 1.0 and 1.9 days.  The
power-law decay index in the X-ray band at this time is alpha ~ 1.6
(Mangano et al. 2014, 15648), suggesting that there may be a cooling
break between the optical and X-ray regimes.


GRB_name: GRB140102A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15674
SUBJECT: GRB 140102A: P60 observations
DATE:    14/01/03 21:35:47 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:

We imaged the location of Swift GRB 140102A (Hagen et al., GCN 15653), 
also detected by the Fermi/LAT (Sonbas et al., GCN 15659) with the 
Palomar 60-inch (P60) robotic telescope on UT 2014-01-03 between 12:01 
and 12:45 UT, in the g, r, i, and z filters.

The afterglow is marginally detected in individual exposures, and 
clearly detected after stacking all of the observations in each filter. 
Photometry of the stacks relative to SDSS stars in the field gives 
magnitudes (at a common midpoint of approximately 12:23 UT, t=0.63 days 
after the trigger) of:

g = 22.08 +/- 0.10
r = 21.59 +/- 0.09
i = 21.37 +/- 0.10

[GCN OPS NOTE(07jan14):  Changed the "130102A" in the first line
to "140102A".]


GRB_name: GRB140103A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15675
SUBJECT: GRB 140103A: P60 Observations
DATE:    14/01/03 23:46:00 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko (NASA/GSFC) and D. A. Perley (Caltech) report on behalf of a larger collaboration:

We imaged the field of GRB140103A (Mangano et al., GCN 15656) with the robotic Palomar 60 inch telescope.  Observations were obtained in the i filter at a median time of 11:40 UT on 2014 January 3 (11.15 hr after the Swift trigger time).  We do not detect any sources within the XRT localization (Mangano, GCN 15666).  Using several nearby point sources from SDSS for reference, we calculate an upper limit of i > 22.9 mag at this time.


GRB_name: GRB131231A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15676
SUBJECT: GRB 131231A, Optical Observations
DATE:    14/01/04 12:00:42 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

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

The Fermi-LAT detected GRB 131231A (Sonbas et al., GCN 15640;
Xu et al., GCN 15641) was monitored  with the 1.04m and 1.3m
telescopes at ARIES Nainital starting at 2014-01-01 13:15:13 (UT).
Several images in R_c and I_c pass-bands were obtained.

The optical afterglow was clearly detected in individual frames.
The preliminary photometry of the first R_c frame (exposure time
300 sec) yields afterglow magnitude to be 19.2+-0.1 mag.

The nearby USNO stars have been used for calibrate.

This massage may be cited.


GRB_name: GRB140102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15677
SUBJECT: GRB 140102A, Optical Observations
DATE:    14/01/04 12:02:35 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

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


We observed GRB 140102A (Swift trigger 582760, Hagen et al. 2014,
GCNC 15653) field with the 1.3m telescope at ARIES, Nainital starting
~ 1.5 hours after the burst. Several frames in V,R_c and I_c pass-bands
were obtained in clear sky conditions.

The candidate optical afterglow (Hagen et al. 2014, GCNC 15653; Xu et al.
2014, GCNC 15655) was clearly seen in our frames. The
photometry of the first R_c frame yields afterglow brightness to be ~ 19
mag.

The nearby USNO stars have been used for calibrate.

This massage may be cited.


GRB_name: GRB140104A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15678
SUBJECT: GRB140104A : Xinglong TNT observation.  A bright star is located nearby
DATE:    14/01/04 16:41:59 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 140104A  (  trigger number 582894) 
with Xinglong 0.8-m TNT telescope at 10:55:20 (UT) , 
Jan. 4th, 2014, about 7 min after the burst notice recived.  

Optical observations shows that there is a very bright stars near XRT postion
of the burst. The coordiantes and the brightness of the bright star 
(as noticed by XRT postion notice ) are :
RA =  03:36:47, 
DEC=00:35:16, 
R=5.37 mag, 

Since the nearby bright star is totally satuated in our images, 
no statement about the afterglow of this burst 
could be made right now. 

This message may be cited.


GRB_name: GRB131231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15680
SUBJECT: GRB 131231A: CARMA 3mm detection
DATE:    14/01/05 01:15:53 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

We observed the position of GRB 131231A (Sonbas et al., GCN 15640; Jenke 
and Xiong, GCN 15644) with the Combined Array for Research in Millimeter 
Astronomy between 2013-01-01 23:54:54 UT and 2013-01-02 02:02:17 UT 
(1.798-1.887 days post-GRB) at a mean frequency of ~93 GHz, under good 
conditions.

We identify a weak source consistent with the optical localization (Xu 
et al., GCN 15651; Singer et al., GCN 15643) in the reduced map.  The 
afterglow flux at this time is measured to be 0.85 +/- 0.25 mJy.

We thank observers B. A. Zauderer and M. Balokovic and the CARMA staff 
for executing the observation.


GRB_name: GRB131231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15681
SUBJECT: GRB 131231A : Lulin Optical Observations
DATE:    14/01/05 01:36:03 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

K.Y. Huang (NTNU), Y. Urata (NCU) on behalf of EAFON report:

We observed the optical afterglow of GRB131231A (Xu et al., GCN 15641)
using the Lulin One-meter Telescope (LOT) with g, r, i, and z
filters. The monitoring observation was made on the night of 1, 2 and
4, Jan, 2014. Based on nearby stars reported by Halpern (GCN15646) and
Perley (GCN15650), we made photometry of the GRB afterglow. The
temporal decay index alpha remains ~1 including the latest epoch. Some
of photometry is summarized below.

epoch(d) g-mag g-err
1.259    19.6  0.1
2.247    20.3  0.1
4.377    20.9  0.1


GRB_name: GRB140103A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15682
SUBJECT: GRB 140103A: Lulin Optical r-band Observations
DATE:    14/01/05 01:37:12 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

K.Y. Huang (NTNU), Y. Urata (NCU) on behalf of EAFON report:

We observed the field of GRB 140103A (Mangano et al., GCN 15656) with
r filter using the Lulin One-meter Telescope (LOT). The observation
was started at 2014-01-03T20:48 and ended at 21:37 (20.7 hr after the
trigger at the mid). We do not detect any sources within the XRT
localization (Mangano et al., GCN 15666) brighter than 22.5.


GRB_name: GRB131209A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15683
SUBJECT: GRB 131209A: Further Swift XRT  observations 
DATE:    14/01/05 03:06:33 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (Swift MOC, PSU)  reports on behalf of the 
Swift team:

We report on further Swift XRT observations of the field of the 
FERMI/LAT-discovered GRB 131209A (Vianello et al., GCN circ. 
15587). As reported in GCN circular 15592 (Grupe & Breeveld) 
there was one uncatalogued X-ray source found within the IPN error
box reported by Hurley et al. (GCN circ. 15588). We followed this
source  with Swift on 2013-December 17. This observation 
suggested a decaying source with a decay slope of about 1. 
Although this is a rather flat decay slope during the normal decay 
phase of a GRB X-ray afterglow, it is not uncommon (e.g. Grupe et 
al. 2013, ApJS, 209, 20). Nevertheless, it is also consistent with
a variability by a factor of 2.5 which is quite common for an AGN
(e.g. Grupe et al. 2010, ApJS, 187, 64). Therefore the data were
not conclusive. We therefore performed two additional observations
which were performed on 2014-January 02 and 03. During the
2014-January 02 observation the source had brightened again to a
count rate in the XRT of (6.4+2.2-1.7)e-3 counts s^-1 and then 
dropped again down to (1.8+1.1-0.8)e-3 counts s^-1 during the
January 03 observation. These observations suggest that the
uncatalogued source in the IPN error box is not the X-ray
afterglow of GRB 131209A. The rapid X-ray variability may suggest
that this is either a Narrow Line Seyfert 1 Galaxy or a blazar if
this is a background AGN. 


This report is an official product of the Swift team. 


GRB_name: GRB140104B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15684
SUBJECT: GRB 140104B: Fermi-LAT detection of a burst
DATE:    14/01/05 07:33:20 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford University), J. McEnery (NASA/GSFC), and E.
Sonbas (Adiyaman Univ.), report on behalf of the Fermi-LAT team:

Starting at 17:32:03.15 on Jan. 4, 2014, Fermi LAT detected high
energy emission from GRB 140104B, which was also detected by Fermi-GBM
(trigger 410549526).

The best LAT on-ground location is found to be R.A., Dec 218.81, -8.90
deg (J2000) with an error radius of 0.22 deg (90% containment,
statistical error only), which was 25 deg from the LAT boresight at
the time of the trigger.

The data from the Fermi LAT show a significant increase in the event
rate within 10 deg of the GBM location after the GBM trigger that is
spatially and temporally correlated with the GBM emission with high
significance. The highest-energy photon is a 1.8 GeV event which is
observed ~800 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi LAT point of contact for this burst is Eda Sonbas
(edasonbas@yahoo.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.

[GCP OPS NOTE(06jan14): Per author's request, name of the burst
in the subject line was corrected by removing the "731" ending.]


GRB_name: GRB140102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15685
SUBJECT: GRB 140102A: BOOTES-4 early optical observations
DATE:    14/01/05 15:29:18 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

S. Guziy (Nikolaev Univ. Obs., Ukraine), J. Gorosabel (UPV/EHU-IAA/CSIC,
Spain), A. J. Castro-Tirado, R. Cunniffe, M. Jelnek, S. Jeong, O.
Lara-Gil, R. Snchez-Ramrez, J. C. Tello (IAA-CSIC Granada, Spain), P.
Kubnek FZU-CAS, Czech Rep.), S. B. Pandey (ARIES, India), Y. Fan, X.
Zhao, J. Bai, Ch. Wang, Y. Xin (Yunnan National Astronomical Observatory,
China) and Ch. Cui (Beijing National Astronomical Observatory, China), on
behalf of a larger collaboration, report:

"Following the detection of GRB 140102A by Swift (Hagen et al., GCNC
15653) and Fermi (Sonbas et al. GCNC 15659), the robotic 0.6m MET
telescope at the BOOTES-4 station, in Lijiang Astronomical Observatory
(China) responded to the event with the first images being obtained 30s
post-burst. At the position of the optical afterglow detected by
Swift/UVOT we detect a source
rapidly decaying in brightness, with R = 14.0 about 70s after the burst
trigger time. Detailed analysis of the whole BOOTES-4 dataset is ongoing."

[GCN OPS NOTE(07jan14): Per author's request, the "130102A" in the first line
was corrected to "140102A".]


GRB_name: GRB140104B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15687
SUBJECT: GRB 140104B: Fermi GBM observation
DATE:    14/01/05 18:42:56 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

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

"At 17:32:03.15 UT on 04 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140104B (trigger 410549526 / 140104731),
which was also detected by the ground analysis of Fermi/LAT
(Vianello et al. 2014, GCN 15684)
The GBM on-ground location is consistent with the LAT position.

The GBM light curve consists of multiple pulses
with a duration (T90) of about 190 s (50-300 keV).
The time-averaged spectrum from T0 to T0+200 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.23 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 280 +/- 40 keV.

The event fluence (10-1000 keV) in this time interval is
(3.2 +/- 0.2)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+190.7 s in the 10-1000 keV band
is 5.7 +/- 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: GRB140105A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15688
SUBJECT: GRB 140105A: Fermi GBM detection
DATE:    14/01/05 21:39:05 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) and Valerie Connaughton (UAH)
report on behalf of the Fermi GBM Team:

"At 01:33:01.01 UT on 05 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140105A (trigger 410578384 / 140105065).

The on-ground calculated location, using the GBM trigger
data, is RA = 208.22, DEC = 50.17 (J2000 degrees,
equivalent to 13 h 53 m, 50 d 10 '), with an uncertainty
of 6 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 72 degrees.

The optical afterglow candidates reported by iPTF (Singer et al.
GCN 15686) lie within the 1-sigma (statistical and systematic)
uncertainty region surrounding the GBM localization.

The GBM light curve consists of weak pulses
with a duration (T90) of about 0.8 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.64 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.98 +/- 0.11 and
the cutoff energy, parameterized as Epeak, is 1200 +/- 500 keV.

The event fluence (10-1000 keV) in this time interval is
(8.7 +/- 0.6)E-7 erg/cm^2. The 64 ms peak photon flux measured
starting from T0 in the 10-1000 keV band is 8.2 +/- 1.2 ph/s/cm^2.

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


GRB_name: GRB140102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15689
SUBJECT: LOAO R-band Observation of GRB 140102A 
DATE:    14/01/06 02:52:23 GMT
FROM:    Changsu Choi at Seoul Nat U  <changsu@astro.snu.ac.kr>

Changsu Choi, Myungshin Im (CEOU/SNU), Hyun-Il Sung (KASI), and Yuji Urata
(NCU), on behalf of EAFON

 

We observed the field of GRB 140102A (Hagen et al., GCN 15653) in R-band
using the 1-m telescope at Mt. Lemmon Optical Observatory (LOAO) in Arizona,
US

 

The observation started at 2014-01-03 13:01:40 UT, or about 15.34 hours
after the BAT alert.

We marginally identify the afterglow in a stacked image with a total
exposure time of ~ 45min. The approximate magnitude of the object is R(Vega)
= 21.5 +- 0.3 mag, calibrated against R1-mag of USNO-B1 stars in the
vicinity. 

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


GRB_name: GRB140102A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15690
SUBJECT: GRB 140102A: Swift/UVOT Detection
DATE:    14/01/06 03:33:36 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

L. M. Z. Hagen (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140102A 65 s
after the BAT trigger (Hagen et al., GCN Circ. 15653). We detect a fading
source consistent with the XRT position (Goad et al. GCN Circ. 15657) that
is detected in all but the bluest UVOT filters.

The preliminary UVOT position is:
    RA  (J2000) =  14:07:40.65 = 211.91939 (deg.)
    Dec (J2000) = +01:19:59.8  =   1.33329 (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 (fc)          65          215          147         16.07 +/- 0.03
white              557         2215          322         18.38 +/- 0.05 
white             6222         7858          393         20.08 +/- 0.21
v                  607         2265          194         18.21 +/- 0.23
b                  533         2191          175         18.50 +/- 0.15
u (fc)             278          527          245         16.90 +/- 0.05
u                  681         2166          155         17.97 +/- 0.14
w1                 657         2142          175         19.10 +/- 0.33 
m2                 631         2117          175        >19.34
w2                6428         8034          364        >19.96

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: GRB140104B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15691
SUBJECT: GRB 140104B:  Swift XRT  observations 
DATE:    14/01/06 03:39:41 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (Swift MOC, PSU)  reports on behalf of the 
Swift team:

We report on the Swift observations of the field of the Fermi GBM
and LAT detected GRB 140104B (Xiong, GCN Circ. 15687, G. Vianello
GCN Circ. 15684, respectively).  Swift started observing the 
field of GRB 140104B at 2014-January-05 08:55, 15.5 hours after 
the GBM trigger for a total of 4073s. The XRT field
covered the inner part of the GBM error circle reported by Xiong.
We found four faint X-ray sources in the XRT. The first source is
a star already present in the DSS, the other three sources are
know sources: the star TYC 5564-19-1, the AGN HE 1432-0838, and
the starburst galaxy IRAS F14325-0837. No other X-ray source was 
found.  The 3-sigma upper limit at the center of the field is 
1.4e-3  counts s^-1.

This report is an official product of the Swift team. 


GRB_name: GRB140103A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15693
SUBJECT: GRB 140103A: Swift XRT afterglow confirmation
DATE:    14/01/06 19:17:38 GMT
FROM:    Vanessa Mangano at PSU  <vxm22@psu.edu>

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

We have analysed 6.9 ks of XRT data for GRB 140103A (Mangano  et al.
GCN Circ. 15656),  from 153 s to 59.7 ks after the  BAT trigger. The
data comprise 2.6 ks in Windowed Timing (WT) mode (the first 7 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode.
We confirm that the X-ray source reported in Mangano et al. GCN Circ. 
15666 is the afterglow of GRB 140103A. Its light curve can now be 
modelled with an initial power-law decay with an index of 
alpha=0.18 (+0.17, -0.19), followed by a break at T+3221 s to
an alpha of 1.18 (+0.51, -0.28).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.6 (+0.5, -0.4). The
best-fitting absorption column is  2.5 (+1.9, -1.3) x 10^21 cm^-2, in
excess of the Galactic value of 1.3 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 2.7 x 10^-11 (6.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      2.5 (+1.9, -1.3) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^20 cm^-2
Excess significance: 3.0 sigma
Photon index:      2.6 (+0.5, -0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00582773.

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


GRB_name: GRB140105A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15694
SUBJECT: GRB 140105A:  Swift XRT  observations 
DATE:    14/01/06 22:05:49 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (Swift MOC, PSU)  reports on behalf of the 
Swift team:

We report on the Swift XRT observations of the field of the
Fermi GBM detected GRB 140105A (Xiong & Connaughton GCN Circ. 
15688). We followed three of the four afterglow candidates 
reported by Singer et al. (GCN circular 15686). We did not find 
an X-ray source in any of these observations. Below is a summary 
of the XRT observations:

iPTF14ai: target ID 20338, T-exp=3939s, 
          Tstart = 2014-01-05 19:46
          3sigma ul = 1.5e-3 counts/s
   
iPTF14ae:  target ID 20339, T-exp=3962s
          T-start = 2014-01-05 23:01
          3sigma ul = 1.53-3 counts/s
          Note that the bright source in the XRT image
   is the Seyfert 1 galaxy SBS 1343+537.
   
iPFT14x:  target ID 20340, T-exp=3077s
          T-start = 2014-01-06 08:56
          3sigma ul = 2.8e-3 counts/s
   
   
Note that Swift was not able to observe the field of the forth
source, iPTF14ac, because the star tracker did not lock onto the
target and caused Swift to go into a safehold. 

This report is an official product of the Swift team.         
   


GRB_name: GRB140105A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15696
SUBJECT: GRB 140105A: continued iPTF observations and rejection of optical candidates
DATE:    14/01/07 06:03:23 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton),
S. B. Cenko (NASA/GSFC), E. Bellm (Caltech), and Y. Cao (Caltech) report
on behalf of the intermediate Palomar Transient Factory (iPTF)
collaboration:

We have continued to observe four optical transients (Singer et al.,
GCN 15686) in the Fermi GBM error circle for GRB 140105A (Xiong &
Connaughton, GCN 15688) with the Palomar 48-inch Oschin telescope
(P48), the robotic Palomar 60-inch (P60), and the Palomar 200-inch
(P200) equipped with the Double Beam Spectrograph (DBSP).

At 33 hours after the burst, with the P48 we obtain the following
host-subtracted magnitudes in the Mould R filter:
 iPTF14x,  R = 20.0
 iPTF14ac, R = 20.3
 iPTF14ae, R = 20.5

With the P60, at 34 hours after the burst, we obtain the following
magnitude in the SDSS system:
 iPTF14ai, r = 20.4

We obtained spectra of all four with the P200. iPTF14x resembles a
Type II supernova. Our spectra for iPTF14ac, iPTF14ae, and iPTF14ai
show a mostly featureless continuum.

The lack of significant optical fading in any of the four candidates
strongly argues against association with the GRB.


GRB_name: GRB140105A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15697
SUBJECT: GRB 140105A: HCT Observations
DATE:    14/01/07 12:28:25 GMT
FROM:    G.C. Anupama at IIA,Bangalore  <gca@iiap.res.in>

V. Bhalerao (IUCAA), Vaidehi S. Paliya (IIA), G. C. Anupama (IIA), and 
C. S.
Stalin (IIA) report:

We undertook followup observations of the four optical transients 
(Singer et
al., GCN 15686) in the Fermi GBM error circle for GRB 140105A (Xiong &
Connaughton, GCN 15688) with the 2-m Himalayan Chandra Telescope (HCT). 
We
obtained two 300s exposures of each field, under non-photometric 
conditions.

20 hours after the burst, we obtain the following unsubtracted 
magnitudes in
the R band:
iPTF14ae = 20.1 +- 0.1
iPTF11ai = 19.8 +- 0.2
iPTF11x  = 19.1 +- 0.3

iPTF11ac is contaminated by a nearby star, and we can only place a limit 
that
R > 18.4 mag. We concur with Singer et al. (GCN 15696) that the lack of 
fading
rules out these candidates as counterparts to GRB 140105A.

We thank the iPTF team for alerting us about this event.


GRB_name: GRB140108A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15699
SUBJECT: GRB 140108A: Swift detection of a burst
DATE:    14/01/08 17:29:05 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. L. Racusin (NASA/GSFC), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB),
J. A. Kennea (PSU), A. Melandri (INAF-OAB), D. M. Palmer (LANL),
M. H. Siegel (PSU), E. Sonbas (NASA/GSFC/Adiyaman Univ.),
E. Troja (NASA/GSFC/UMCP) and T. N. Ukwatta (MSU) report on behalf of
the Swift Team:

At 17:18:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140108A (trigger=583338).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 325.178, +58.766 which is 
   RA(J2000)  =  21h 40m 43s
   Dec(J2000) = +58d 45' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks at
T+5, T+35, and T+85 sec with a total duration of about 120 sec.  
The peak count rate was ~8000 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 17:19:51.1 UT, 68.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 325.1106, 58.7437 which is equivalent to:
   RA(J2000)  = +21h 40m 26.54s
   Dec(J2000) = +58d 44' 37.3"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 149 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 3.34e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 78 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 large, but uncertain extinction expected. 

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


GRB_name: GRB140108A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15700
SUBJECT: GRB 140108A: Prompt enhanced Swift-XRT position
DATE:    14/01/08 18:05:49 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 140108A, we find an
enhanced XRT position of the afterglow: RA, Dec: 325.1127, 58.7446
which is equivalent to:
   RA (J2000)  = 21 40 27.04
   Dec (J2000) = +58 44 40.7
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/583338.

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: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15701
SUBJECT: GRB 140108A:  MASTER-Net OT detection 
DATE:    14/01/08 18:08:50 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy,  V. Lipunov, D.Denisenko, V.Kornilov, D.Kuvshinov, N.Tyurina, 
P.Balanutsa,  A.Kuznetsov
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  GRB140108A 22 sec after notice 
time and 39 sec after trigger time at 2014-01-08 17:19:21.913 UT in two 
polarizations. On our first (10s exposure) set we haven't found optical 
transient  within SWIFT error-box ( Racusin et al. GCN 15699 ).
The 5-sigma upper limit has been about 17.0 mag.

MASTER II  robotic telescope located in Blagoveschensk was pointed to the 
GRB140108A 30 sec after notice time and 47 sec after trigger time at 
2014-01-08 17:19:29.211 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 16.0 mag.

The polarizations filters oriented by RA and DEC axis (0 and 90 degrees 
from RA axis) in Kislovodsk, and 45 and 135 degrees from RA axis in 
Blagoveschensk.


The OT candidate apeared in two sites (Blagoveschensk and Kislovodsk) and 
at 2014-01-08 17:19:42 at position:

(J2000) 
RA =  21 40 26.77 
Dec = +58 44 41.4
Error=+-1 arcsc sigma

The message may be cited.


GRB_name: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15702
SUBJECT: GRB 140108A: 1.23m CAHA observations
DATE:    14/01/08 18:17:29 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (UPV/EHU-IAA/CSIC), R. Hueso (UPV/EHU), M. Fernandez (IAA/CSIC) on behalf of a larger collaboration report:

We observed the field of GRB 140108A (Racusin et al., GCN 15699) with the 1.23m CAHA telescope. An object  with I~19 is detected at 17:55 UT coincident with the optical candidate position reported by Gorbovskoy et al.  (GCN 15701). Further observations are in progress.


GRB_name: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15703
SUBJECT: GRB 140108A: D50+BART optical candidate detection
DATE:    14/01/08 18:27:38 GMT
FROM:    Jan Strobl at AI AS CR,Ondrejov  <jan@strobl.cz>

Jan Strobl (1,3), Martin Jelinek (2), Cyril Polasek (1), Michal Jakubec 
(1), Petr Skala (1,3) and Rene Hudec (1,3) (1. AI ASCR Ondrejov, 2. IAA 
CSIC Granada, 3. FEE CTU Prague)

We observed the field of the Swift GRB 140108A (Racusin et al., GCNC 
15699) with the 0.5m telescope D50 and 0.25m telescope BART in Ondrejov 
(Czech Republic), starting at 17:19:20 UT, i.e. 36s after the trigger.

We detect a new variable and uncatalogued object within the XRT 
coordinates

         21:40:26.813 +58:44:40.17 (J2000) +-1".

Preliminary photometry provides brightness of R~18.0 300s after the GRB 
trigger.

This message can be cited.


GRB_name: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15704
SUBJECT: GRB 140108A: Mondy optical observations
DATE:    14/01/08 19:07:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Klunko (ISTP), M. Eselevich(ISTP), A. Volnova (IKI), A. 
Pozanenko(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140108A (Racusin et al., GCN 
15699) with AZT-33IK telescope of Sayan observatory (Mondy) starting 
Jan., 08 (UT) 17:24:55.  We obtained several images in R-filter with 
exposure of 20,60 and 180 seconds. Within the enhanced XRT circle (Evans 
et al., GCN 15700) we detected  optical afterglow (Gorbovskoy et al., 
GCN 15701;  Gorosabel  et al., 15702) The  position of the afterglow 
coincids with  previously reported (Gorbovskoy et al., GCN 15701; Strobl 
et al., 15703). At (UT) 17:32, i.e. ~13.5 min. after GRB trigger the 
R-magnitude of the afterglow is ~19.2.

  The finding chart can be found in 
http://grb.rssi.ru/GRB140108A/GRB140108A_AZT33IK_2014-01-08T_17-30-34.png

Observation is continuing.


GRB_name: GRB140108A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15705
SUBJECT: GRB 140108A: Enhanced Swift-XRT position
DATE:    14/01/08 22:00:31 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 634 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140108A, 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 = 325.11211, +58.74464 which is equivalent
to:

RA (J2000): 21h 40m 26.91s
Dec (J2000): +58d 44' 40.7"

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

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

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


GRB_name: GRB140108A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15706
SUBJECT: GRB 140108A: Swift-XRT refined Analysis
DATE:    14/01/09 08:12:15 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), J. L. Racusin (NASA/GSFC), P. A. Evans (U.
Leicester) report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 140108A (Racusin  et al. GCN
Circ. 15699),  from 58 s to 41.8 ks after the  BAT trigger. The data
comprise 2.4 ks in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 15705).

The light curve shows some initial flaring activity, with the flares
peaking at around 90 and 220 s after the trigger. The underlying
emission can be modelled with a series of power-law decays. The initial
decay index is alpha=2.8 (+/-0.7). At T+184 s  the decay flattens to an
alpha of 0.52 (+/-0.03) before breaking again at T+7014 s to a final
decay with index alpha=1.20 (+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 1.69 (+0.04, -0.03). The
best-fitting absorption column is  consistent with the Galactic value
of 7.0 x 10^21 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a
photon index of 1.91 (+0.16, -0.15) and a best-fitting absorption
column of 9.3 (+1.3, -1.2) x 10^21 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 5.7 x 10^-11 (1.1 x 10^-10) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.3 (+1.3, -1.2) x 10^21 cm^-2
Galactic foreground: 7.0 x 10^21 cm^-2
Excess significance: 3.1 sigma
Photon index:      1.91 (+0.16, -0.15)

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 0.035 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-12 (3.8 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/00583338.

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


GRB_name: GRB140108A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15707
SUBJECT: GRB 140108A: theoretical prediction of redshift and of supernova occurrence
DATE:    14/01/09 11:47:54 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, C.L. Bianco, M. Enderli, M. Kovacevic, M. Muccino, A.V.
Penacchioni, G.B. Pisani, J.A. Rueda, Y. Wang report:

The late Swift/XRT observations of GRB 140108A (1,2) evidences the
fullfillment of the IGC paradigm (3,4). A preliminary overlapping of
its X-ray (0.3-10 keV in rest-frame) luminosity with the one of GRB
090618, namely an IGC prototype (5), gives an estimate of the redshift
of z=0.6 (+/- 0.1) (see Fig. 1
<http://www.icranet.org/images/GCN/GRB140108A.pdf>).

As a consequence, a supernova associated to GRB 140108A is expected to
emerge after 16 (+/- 3) days after the trigger.

Given the spectral parameters of the prompt emission by Swift/BAT
(<http://gcn.gsfc.nasa.gov/notices_s/583338/BA/>), this redshift
estimation leads to an isotropic energy of E_iso ~ 4x10^52 erg.

Continuous monitoring and complementary observations in all possible
wavelengths are encouraged.

References:
(1) Racusin et al., GCN 15699
(2) D'Avanzo et al., GCN 15706
(3) Rueda & R. Ruffini, ApJLett, 758, L7 (2012)
(4) Pisani et al., A&A, 552, L5 (2013)
(5) Izzo et al., A&A, 548, L5 (2012)


GRB_name: GRB140108A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15708
SUBJECT: GRB 140108A: Swift/UVOT Detection
DATE:    14/01/09 12:31:27 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) 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 140108A
78 s after the BAT trigger (Racusin et al., GCN Circ. 15699).
A fading source consistent with the optical position (Gorbovskoy et al. 
GCN Circ. 15701, Strobl et al. GCN Circ. 15703) is 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 finding chart (FC) and other early exposures are:

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

white_FC            78          228          147         20.17  0.20
white              571         1021          189        >21.3
v                  621         1420           97        >18.9
b                  547         1345           78        >19.8
u                  291         1320          304        >20.6
w1                 670         1462           90        >20.3
m2                 646         1444           97        >19.8
w2                 596         1395           83        >20.2

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 1.00 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB140108A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15709
SUBJECT: GRB 140108A: Fermi GBM detection
DATE:    14/01/09 14:10:59 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

G. Younes (USRA/NASA-MSFC) reports on behalf of the Fermi GBM Team:

At 17:18:42.99 UT on 08 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140108A (trigger 410894325/140108721), which was
also detected with Swift (J. L. Racusin et al., GCN 15699). The GBM on-ground
location is consistent with the Swift/XRT location of the burst
(P. Evans et al., GCN 15705). The angle to the Fermi LAT boresight is 87 degrees
from the Swift XRT position.

The GBM light curve consists of a multiple-peak structure with a duration
(T90) of about 95 s (50-300 keV). The time-averaged spectrum from
T0 to T0+105 s is adequately fit by a Comptonized function with Epeak =
240 +/- 23 keV, and an index alpha = -1.24 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(1.905 +/- 0.069)E-05  erg/cm^2. The 1-sec peak photon flux measured
starting from T0+85 s in the 10-1000 keV band is 10.3 +/- 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: GRB140108A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15710
SUBJECT: GRB 140108A: Swift-BAT refined analysis
DATE:    14/01/09 14:22:08 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC),
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-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140108A (trigger #583338)
(Racusin, et al., GCN Circ. 15699).  The BAT ground-calculated position is
RA, Dec = 325.129, 58.749 deg, which is 
   RA(J2000)  =  21h 40m 30.9s 
   Dec(J2000) = +58d 44' 55.3" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.
 
The mask-weighted light curve shows two main peaks; the first starting at
~T-25 sec, peaking at ~T+7 sec, and almost returns to background at T+20 sec.
The second peak starts at ~T+70 sec, peaks at ~T+77 sec, and ends at ~T+110 sec
with some weak emission (2-3 sigma) out to ~T+150 sec.
T90 (15-350 keV) is 97.8 +- 3.3 sec (estimated error including systematics).
 
The time-averaged spectrum from T-24.8 to T+103.3 sec (with 2.5 sec of missing
data in the middle of the 2nd peak) is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 1.60 +- 0.05.
The fluence in the 15-150 keV band is 6.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+6.49 sec in the 15-150 keV band
is 6.1 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/583338/BA/


GRB_name: GRB131231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15711
SUBJECT: GRB 131231A: AAO optical observations
DATE:    14/01/09 16:06:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), G. Inasaridze (AAO), V. 
Zhuzhunadze (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the optical counterpart of the Fermi/LAT GRB 131231A 
(Sonbas et al., GCN 15640; Xu et al. GCN 15641) with AS-32 (0.7m) 
telescope of Abastumani Observatory on Jan. 3, 4, and 5. We obtained 
several unfiltered images of 120 s exposure during each observational 
set. On stacked images we clearly detect the afterglow. The photometry 
based on the reference stars, R-mag, from Halpern (GCN 15646) is following:

Date        T_start   t-t0,     exp,    OT
              (UT)      mid, d    s

2014-01-03  17:08:16  3.54893  33x120  20.26 Â± 0.06
2014-01-04  16:53:04  4.53207  29x120  20.32 Â± 0.08
2014-01-05  15:59:46  5.50061  34x120  20.74 Â± 0.13


GRB_name: GRB140105A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15712
SUBJECT: GRB 140105A:  MASTER-Net early optical observations and time correction
DATE:    14/01/09 17:35:59 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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 VWF robotic very wide field cameras (FOV=2x384 square degrees, 
D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) installed on 
MASTER-II robotic telescope syncronously covered ~15% part of 3 sigma 
FERMI-GBM error box (Xiong et al., GCN 15688). No credible transients have 
been found on our images. The 3 sigma unfiltered upper limit is 10.6.
MASTER-II robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the GRB140105A 21 sec after notice 
time and 45 sec after trigger time at 2014-01-05 01:33:46 UT.

After pointing by FERMI alert we cover 90% of 1-sigma and 70% of 3-sigma 
FERMI-GBM error box.  We didn't find new object in error box on single and 
coadd images. The 3 sigma upper limit on single 5 seconds exposure image 
is 10.6 and 12.0 on coadd of 24 images with total exposure 120 seconds.
The positions of all iPTF optical afterglow candidates (Singer et al., GCN 
15686) are covered by out cameras since 48 sec. after the trigger but 
there are no flares up to 10.6 mag. on their place.

The movie is available here 
http://master.sai.msu.ru/static/GRB/GRB140105A/GRB140105A.gif

The map of error box and our FOV is available at 
http://master.sai.msu.ru/static/GRB/GRB140105A/GRB140105A_map.png

The pointing time informations in our previous telegram Gorbovskoy et al. 
GCN 15692 are not correct. We apologize for this inaccuracy.



The message may be cited.


GRB_name: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15713
SUBJECT: GRB 140108A: Mondy optical upper limit
DATE:    14/01/10 12:39:53 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (IKI), E. Klunko (ISTP), M. Eselevich(ISTP), A.
Pozanenko(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140108A (Racusin et al., GCN
15699) with AZT-33IK telescope of Sayan observatory (Mondy) starting
Jan., 09 (UT) 15:10:20. We obtained several images in R-filter with
exposure of 180 seconds. On the stacked image we do not detected
the optical afterglow (Gorbovskoy et al., GCN 15701; Gorosabel et al.,
15702).

The details of the photometry are the following:

UT start,      t-T0           Filter     Exp.     OT    UL
                (mid, days)               (s)                (3 sigma)
15:10:20    0.94627       R         34*180   n/d    22.0

The photometry is based on 3 USNO-B1.0 stars:

USNO-B id        RA                Dec             R2
1487-0322168   21:40:30.85   +58:43:53.1   18.18
1487-0322049   21:40:20.16   +58:43:58.3   17.96
1487-0322069   21:40:21.62   +58:45:00.6   17.29


GRB_name: GRB140110A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15714
SUBJECT: GRB 140110A: Fermi-LAT detection of a burst
DATE:    14/01/10 13:16:18 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (University & INFN Trieste), E. Sonbas (Adiyaman University),
F. Longo (University & INFN Trieste), and J. Racusin (NASA/GSFC),
report on behalf of the Fermi-LAT team:


Starting at 06:18:37.94 on January 10th, 2014, Fermi LAT detected
high energy emission from GRB 140110A, which was also detected
by Fermi-GBM (trigger 411027520).

The best LAT on-ground location is found to be RA, Dec 28.90, -36.26 (J2000)
with an error radius of 0.50 deg (90% containment, statistical error only).
This was 30 deg from the LAT boresight at the time of the trigger.

Only the first 1300 s of LAT data have been processed.
They show a significant increase in the event rate within 5 degrees
of the GBM location after the GBM trigger that is spatially and temporally
correlated with the GBM emission with high significance.
Around 20 photons above 100 MeV are observed within 200 seconds.
The highest energy photon is a 735 MeV event which is observed
160 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi LAT point of contact for this burst is
Elisabetta Bissaldi (Elisabetta.Bissaldi@ts.infn.it).


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: GRB140110A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15715
SUBJECT: GRB 140110A Tiled Swift observations
DATE:    14/01/10 14:14:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 140110A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00023

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177).

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


GRB_name: GRB140110A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15716
SUBJECT: GRB 140110A: Fermi GBM observation
DATE:    14/01/10 16:10:42 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) and V. Connaughton (UAH)
report on behalf of the Fermi GBM Team:

"At 06:18:37.94 UT on 10 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140110A (trigger 411027520 / 140110263), which was

also detected by Fermi/LAT (Bissaldi et al. 2014, GCN 15714).
The GBM on-ground location is consistent with the LAT position. The angle 
from the Fermi LAT boresight at the time of the trigger is 34 degrees.

The GBM light curve shows a single pulse with a duration (T90) 
of about 9 s (50-300 keV). The time-averaged spectrum from T0-0.524 s to
T0+5.764 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.61 (+0.07/-0.06) and
the cutoff energy, parameterized as Epeak, is 1550 (+300/-250) keV.

The event fluence (10-1000 keV) in this time interval is
(7.1 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+2.69 s in the 10-1000 keV band
is 3.6 +/- 0.2 ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak= 1400(+290/-260)
keV, 
alpha = -0.59 (+0.08/-0.07)  and beta = -2.7 (+0.4/-1.1) .

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


GRB_name: GRB140108A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15717
SUBJECT: GRB 140108A BAT refined analysis update
DATE:    14/01/10 16:28:23 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings reports on behalf of the Swift-BAT team:

There were some small gaps in the data used in the BAT refined analysis
of GRB 140108A (Cummings et. al, GCN circ # 15710).  With a complete
data set, T90 is slightly shorter, 94 +- 4 seconds, the photon index for
the simple power-law fit to the spectrum is slightly larger, 1.62 +- 0.05,
and the total fluence is slightly larger, (7.0 +- 0.2) x 10^-7 ergs/cm^2.
The energy interval is 15-150 keV and uncertainties are 90% confidence.

In the lightcurve, the second peak is a little larger than it looked
before, and is very similar to the first peak.

The updated results have been posted at:
http://gcn.gsfc.nasa.gov/notices_s/583338/BA/


GRB_name: GRB140108A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15718
SUBJECT: GRB 140108A BAT refined analysis update *CORRECTION*
DATE:    14/01/10 17:27:59 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

My apologies; I made a typographical error in the posted update, GCN
Circ. #15717.  The total fluence should be (7.0 +- 0.2) x 10^-6 ergs/cm^2.
The corrected circular text is below:

J. R. Cummings reports on behalf of the Swift-BAT team:

There were some small gaps in the data used in the BAT refined analysis
of GRB 140108A (Cummings et. al, GCN circ # 15710).  With a complete
data set, T90 is slightly shorter, 94 +- 4 seconds, the photon index for
the simple power-law fit to the spectrum is slightly larger, 1.62 +- 0.05,
and the total fluence is slightly larger, (7.0 +- 0.2) x 10^-6 ergs/cm^2.
The energy interval is 15-150 keV and uncertainties are 90% confidence.

In the lightcurve, the second peak is a little larger than it looked
before, and is very similar to the first peak.

The updated results have been posted at:
http://gcn.gsfc.nasa.gov/notices_s/583338/BA/


GRB_name: GRB140110A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15719
SUBJECT: GRB 140110A: OT detection in Swift/UVOT imaging
DATE:    14/01/10 21:31:17 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI) reports

Inspection of the UVOT u-band image of the field1 of the tiled Swift
observations (Evans, GCN 15715) reveals a very bright optical source,
no present at DSS, at coordinates

R.A. = 01:54:57.50
Dec. = -36:16:38.71

Error Circ. ~ 1.5 arcsec

No known minor planet, near-Earth object, and comet would appear at
this position at the UVOT observational time.

Thus this object could be the optical afterglow of GRB 140110A, and
may worth some photometric follow-ups to check its variation.


GRB_name: GRB140110A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15720
SUBJECT: GRB 140110A: Reported UVOT OT not GRB afterglow
DATE:    14/01/10 22:11:38 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea and M. M. Chester (PSU) report on behalf of the Swift team:

The UVOT detected optical transient reported by Xu (GCN 15719) is not 
related to GRB 140110A (Bissaldi et al., GCN 15714). The transient appears 
at different locations in two observations taken by UVOT as part of the 
Swift target-of-opportunity observations of GRB 140110A (Evans, GCN 
15715). We believe that this transient is most likely an optical artifact.


GRB_name: GRB140110A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15721
SUBJECT: GRB 140110A: Swift XRT observations
DATE:    14/01/11 12:03:01 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA), S. Campana (INAF-OAB), D. Malesani (DARK/NBI) 
and P. A. Evans (U. Leicester) report on behalf of the Swift team:

Swift-XRT has observed the error circle of the Fermi/LAT GRB 140110A 
(Bissaldi et al., GCN 15714), also detected by Fermi/GBM (von Kienlin & 
Connaughton, GCN 15716), in a series of observations tiled on the sky. 
The total exposure time is 12.8 ks spread over 7 fields; the maximum 
exposure within the sky observed was 3.9 ks. The observations started 
28.4 ks after the Fermi/LAT trigger. Within these data there are two 
objects (source #1 and source #3) which are in the 1RXS catalogue and 
five sources which are not catalogued in X-rays. At the present time we 
cannot be sure which of these, if any, is the afterglow. However, we 
note that the light curve of source #2, with a mean count rate of (1.23 
 0.27) x 10^-2 ct s^-1, suggests evidence of decay.

Source details:

Source 1
RA:  28.58425  = 01h 54m 20.22s (J2000)
Dec:  -36.49342  = -36d 29' 36.3" (J2000)
Err: 4.4" (radius, 90% confidence)
Exposure time: 1.7 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_1.php

Source 2
RA:  28.53253  = 01h 54m 7.81s (J2000)
Dec:  -36.12000  = -36d 07' 12.0" (J2000)
Err: 5.4" (radius, 90% confidence)
Exposure time: 2.6 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_2.php

Source 3
RA:  28.63188  = 01h 54m 31.65s (J2000)
Dec:  -36.70189  = -36d 42' 06.8" (J2000)
Err: 5.4" (radius, 90% confidence)
Exposure time: 1.5 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_3.php

Source 4
RA:  29.24134  = 01h 56m 57.92s (J2000)
Dec:  -36.06453  = -36d 03' 52.3" (J2000)
Err: 6.2" (radius, 90% confidence)
Exposure time: 1.6 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_4.php

Source 5
RA:  28.36418  = 01h 53m 27.40s (J2000)
Dec:  -36.32146  = -36d 19' 17.3" (J2000)
Err: 5.7" (radius, 90% confidence)
Exposure time: 1.7 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_5.php

Source 6
RA:  28.46195  = 01h 53m 50.87s (J2000)
Dec:  -36.04399  = -36d 02' 38.4" (J2000)
Err: 6.2" (radius, 90% confidence)
Exposure time: 1.0 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_6.php

Source 7
RA:  28.94482  = 01h 55m 46.76s (J2000)
Dec:  -36.43079  = -36d 25' 50.8" (J2000)
Err: 6.2" (radius, 90% confidence)
Exposure time: 2.7 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_7.php

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


GRB_name: GRB140104B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15722
SUBJECT: GRB 140104B: Suzaku WAM observation of the prompt emission
DATE:    14/01/11 15:06:03 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-u.ac.jp>

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


The long GRB 140104B (Fermi-LAT detection: Vianello et al., GCN 15684;
Fermi-GBM observation: Xiong, GCN 15687) triggered the Suzaku Wide-band
All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at
17:32:13.926 UT (=T0).

The observed light curve shows a multi-peaked structure starting at
T0-14 s, ending at T0+200 s with a duration (T90) of about 185 seconds.
The fluence in 100 - 1000 keV was 1.86 (+0.83/-0.77) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+179 s was 1.34 (+0.52/-0.45)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-14 s to T0+200 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 0.42 (+1.17/-1.78), and
Epeak 351 (+75/-102) keV (chi^2/d.o.f. = 12.5/14).

All the quoted errors are at statistical 90% confidence level.

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


GRB_name: GRB140108A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15723
SUBJECT: GRB 140108A: Suzaku WAM observation of the prompt emission
DATE:    14/01/11 15:12:08 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-u.ac.jp>

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


The long GRB 140108A (Swift/BAT trigger #583338; Racusin et al., GCN 15699)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 17:18:48.879 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0-11 s,
ending at T0+104 s with a duration (T90) of about 90 seconds.
The fluence in 100 - 1000 keV was 1.19 (+0.12/-0.50) x 10^-5 erg/cm^2. 
The 1-s peak flux measured from T0+79 s was 4.70 (+0.14/-1.81) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-11 s to T0+104 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.70 (+0.68/-0.85), and
Epeak       427 (+137/-72) keV (chi^2/d.o.f. = 5.8/10).

All the quoted errors are at statistical 90% confidence level.


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


GRB_name: GRB140110A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15724
SUBJECT: GRB 140110A: Swift/UVOT Observations
DATE:    14/01/11 18:28:39 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates  (UCL-MSSL) and M. Stamatikos (OSU) report on behalf of the Swift/UVOT team:

The Swift/UVOT observed the error circle of the Fermi/LAT GRB 140110A 
(Bissaldi et al., GCN Circ. 15714) in a series of u band observations 
tiled on the sky. The total exposure time is 12.7 ks spread over 7 
fields; each field was observed typically for 1.8 ks. Observations 
started 28.4 ks after the Fermi/LAT trigger. At the locations of the 
XRT candidates (Maselli et al., GCN Circ. 15721), we find sources 
2 and 6 lie outside of the UVOT field of view, while the rest are 
consistent with known objects within the USNO-B1 catalogue. 
However, within the UVOT fields we find two uncatalogued sources:

The refined UVOT position for UVOT source 1 is:

    RA (J2000)   1:57:11.98
   Dec (J2000) -36:17:48.2

The refined UVOT position for UVOT source 2 is:

    RA (J2000)   1:55:13.95
   Dec (J2000) -35:54:14.0

both positions have an estimated uncertainty of 0.6 arcsec (radius, 90% confidence). 
At this time we are unable to determine if either of these sources are fading. 

Preliminary magnitudes for the two UVOT uncatalogued sources using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

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

UVOT1    u           28798        30607          1734  19.63 +/- 0.10 
UVOT2    u           30251        63599          1793  19.56 +/- 0.10 

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: GRB140110A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15725
SUBJECT: IPN Triangulation of GRB 140110A
DATE:    14/01/11 21:02:15 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

V. Pal'shin on behalf of the IPN,

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

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

The long-duration GRB 140110A (Bissaldi et al., GCN Circ. 15714; von 
Kienlin & Connaughton, GCN Circ. 15716) has been also observed by Swift 
(BAT), and MESSENGER (GRNS), so far, at about 22718 s UT (06:18:38). The 
burst was outside the coded field of view of the BAT.

We have triangulated this GRB to a GBM-MESSENGER annulus centered at
RA(2000)=299.570 deg (19h 58m 17s)  Dec(2000)=-22.828 deg (-22d 49' 
41"), whose radius is  76.183 Â± 0.140 deg (3 sigma).

This annulus intersects the Fermi-LAT 90% CL error circle (Bissaldi et 
al., GCN Circ. 15714) to form an error box whose area is about 3 times
smaller than that of the LAT error circle, and whose
corners are:
-----------------------------------------------
   RA(2000), deg                 Dec(2000), deg
-----------------------------------------------
    Corners:
    29.211 (01h 56m 51s) -36.693 (-36d 41' 35")
    28.826 (01h 55m 18s) -35.764 (-35d 45' 49")
    28.614 (01h 54m 27s) -35.817 (-35d 49' 00")
    28.999 (01h 56m 00s) -36.754 (-36d 45' 13")
-----------------------------------------------
This box may be improved.

Only one of the reported XRT sources (Maselli et al., GCN Circ. 15721), 
the source 7, is consistent with the IPN annulus and, hence, can be the 
afterglow.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140110_T22717/IPN/


GRB_name: GRB140110A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15726
SUBJECT: GRB 140110A: Swift/UVOT retraction of UVOT candidates
DATE:    14/01/12 13:45:30 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates  (UCL-MSSL) and M. Stamatikos (OSU) report on behalf of the Swift/UVOT team:

We have further investigated source 2 from Oates et al. (GCN 15724). While this source 
is not present in the USNO-B1 catalogue, it is present in the DSS and GSC-2.3 catalogue. 
We therefore retract this source as a potential afterglow candidate for GRB 140110A.

We also note that source 1 is not within the IPN annulus (Hurley et al., GCN 15725) and 
is therefore also unlikely to be the optical afterglow for this GRB.


GRB_name: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15727
SUBJECT: GRB 140108A: Konkoly optical observations 
DATE:    14/01/13 18:20:17 GMT
FROM:    Janos Kelemen at Konkoly Obs/Hungary  <kelemen@konkoly.hu>

J. Kelemen (kelemen at konkoly.hu) on behalf of the GRB OT observing program
at the Konkoly Observatory.

Starting on the evening of 08/01/2014 we observed the field of GRB 140108A
(Racusin et al., GCN 15699) 8802 sec. after the burst, using a 60/90/180 cm
Schmidt telescope located at the Mountain Station of the Konkoly
Observatory, equipped with an Apogee CCD camera through R filter. On the coadded
R images (total exp.time 900 sec) we marginally detected the OT at the
position indicated the finding chart provided by Pozarenko, GCN 15704.
Based on the nearby UCAC-4 stars we provide 22.6 +/- 0.3 magnitude in the R
band for the OT. 

time from GRB.    exp    filter     Mag.      

  8802 s.         900 s     R       22.6 +/-0.3 


GRB_name: GRB140114A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15728
SUBJECT: GRB 140114A: Swift detection of a burst
DATE:    14/01/14 12:23:14 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/UMCP), A. P. Beardmore (U Leicester),
M. G. Bernardini (INAF-OAB), D. N. Burrows (PSU), V. D'Elia (ASDC),
P. A. Evans (U Leicester), D. Malesani (DARK/NBI),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 11:57:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140114A (trigger=583861).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 188.482, +27.926 which is 
   RA(J2000) = 12h 33m 56s
   Dec(J2000) = +27d 55' 35"
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 at least 300 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~118 sec after the trigger. 

The XRT began observing the field at 11:59:46.0 UT, 126 seconds after
the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued
X-ray source with an enhanced position: RA, Dec 188.5214, 27.9514 which
is equivalent to:
   RA(J2000)  = 12h 34m 05.13s
   Dec(J2000) = +27d 57' 05.1"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 155 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 (1.55 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.1
(+3.20/-2.63) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 120 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
0.02. 

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


GRB_name: GRB140114A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15729
SUBJECT: GRB 140114A: P60 Observations
DATE:    14/01/14 13:18:09 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko (NASA/GSFC) reports on behalf of a larger collaboration:  

We imaged the location of GRB140114A (Troja et al., GCN 15728) with the robotic Palomar 60 inch telescope.  Observations were obtained in the r', i', and z' filter beginning at 12:01 UT on 2014 January 14 (~ 3 minutes after the Swift trigger).  The seeing was relatively poor throughout the observations (~ 3").  

We do not detect any emission at the location of the XRT counterpart.  Using several nearby point sources from SDSS for reference, we calculate the following upper limits in coadded images:  

i' > 20.8 mag at a mean epoch of dt ~ 14 min  
r' > 21.2 mag at a mean epoch of dt ~ 15 min
z' > 20.0 mag at a mean epoch of dt ~ 16 min


GRB_name: GRB140102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15730
SUBJECT: GRB 140102A: AAO optical upper limits
DATE:    14/01/14 14:33:36 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

GRB 140102A: AAO optical upper limits

A. Volnova (IKI), R. Inasaridze (AAO), G. Inasaridze (AAO), V.
Zhuzhunadze (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 140102A (Hagen et al., GCN 15653) with
AS-32 (0.7m) telescope of Abastumani Observatory on Jan. 5 and 6. We
obtained several unfiltered images of 120 s exposure during each
observational set. On stacked images in the enhanced XRT circle (Goad
et al., GCN 15657) we do not detect the optical afterglow.


The details of the photometry are the following:

Date             T_start     t-t0,        exp.,      Uplim
                     (UT)        mid, d     s            3 sigma

2014-01-05   00:48:24   2.13972   38x120   22.5
2014-01-06   01:04:20   3.18687   32x120   22.3

The photometry is based on the SDSS reference stars from Xu (GCN 15655)
using gri -> R transformations by Lupton 2005:

N  SDSS_id                     R(Lupton)
1  J140740.98+011949.8   17.59
2  J140742.47+012010.4   17.51


GRB_name: GRB140114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15732
SUBJECT: GRB 140114A: RATIR Optical and NIR Afterglow Detection
DATE:    14/01/14 17:26:26 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
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140114A (Troja et al., GCN 15728) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2014/01 14.50 to 2014/01 14.56 UTC (9.6 to
90.6 minutes after the BAT trigger), obtaining a total of 0.98 hours
exposure in the r and i bands and 0.43 hours exposure in the Z, Y, J, and H
bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9 and 2MASS, we obtain the following detections:

  r     21.92 +/- 0.10
  i     21.31 +/- 0.07
  Z     21.14 +/- 0.12
  Y     20.75 +/- 0.15
  J     20.56 +/- 0.12
  H     20.28 +/- 0.15

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB140114A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15733
SUBJECT: GRB 140114A: Enhanced Swift-XRT position
DATE:    14/01/14 18:56:03 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 2514 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140114A, 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 = 188.52173, +27.95080 which is equivalent
to:

RA (J2000): 12h 34m 5.22s
Dec (J2000): +27d 57' 02.9"

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

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

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


GRB_name: GRB140104B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15734
SUBJECT: GRB 140104B: Further Swift XRT  observations 
DATE:    14/01/14 19:37:50 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (Swift MOC, PSU) and Phil Evans (U Leicester) report
on behalf  of the  Swift team:

We report on further Swift XRT observations of the field of the
Fermi GBM and LAT detected GRB 140104B (Xiong, GCN Circ. 15687, 
G. Vianello GCN Circ. 15684, respectively). 
We detected an uncatalogued X-ray source in the first Swift 
observation of the field of GRB 140104B starting at 15.5 hours
after the Fermi trigger (Grupe, GCN circ 15691) at

Ra-2000  =  14 35 01.0
Dec-2000 = -09 01 40.7

with an uncertainty of 4.0". The XRT count rate of this source
was (8.1+/-1.6)e-3 counts s^-1. Note that we misidentified this
source in the previous circular (15691) with the star TYC
5564-19-1, which however, is 2.2' away from this X-ray position. 

We re-observed this source on 2014-01-14 for 4.6 ks again with
Swift (9.5 days after the trigger). We do not detect this source
in the XRT any more, suggesting that this may be the X-ray
afterglow of GRB 140104B. The 3sigma upper limit at the position
of this source is 1.3e-3 counts s^-1. Note, however, that this is
not conclusive. This source can still be a highly variable
background AGN (see e.g. Grupe et al. 2010, ApJS, 187, 64). 

If this source is the X-ray afterglow of GRB 140104B, the X-ray
spectrum appears to be rather soft. A spectral analysis of the
X-ray data shows that the X-ray photon index is Gamma =
2.7+/-0.68 which is rather steep (see Grupe et al. 2013, ApJS,
209, 20; Evans et al., 2009, MNRAS, 397, 1177). 
The absorption column density is consistent with the
Galactic value (5.63e20 cm^-2). This steep X-ray spectral index
and the steep energy spectral index and the high fluence in the
10-1000 keV band of the burst reported by Xiong (GCN circular 
15687) suggests a low redshift nature of the burst (see Grupe et
al. 2013, ApJ, 209, 20).

However, the steep X-ray photon index of Gamma = 2.7
does not exclude a possible AGN nature of the source. In a 
matter of fact, if this is a background AGN then the steep X-ray 
spectrum suggest that this is most-likely a Narrow Line 
Seyfert 1 galaxy. This is also the type of AGN with the 
strongest X-ray variability  (e.g. Boller et al. 1996, 
Leighly 1999, Grupe et al. 2010). 



This report is an official product of the Swift team. 


GRB_name: GRB140103A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15735
SUBJECT: GRB 140103A: AAO optical afterglow candidate
DATE:    14/01/14 20:23:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), G. Inasaridze (AAO), V.
Zhuzhunadze (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the optical counterpart of the Swift GRB 140103A (Mangano et 
al., GCN 15656) with AS-32 (0.7m) telescope of Abastumani Observatory on 
Jan. 3 and 4. We obtained several unfiltered images of 120 s exposure 
during each observational set. In the refined XRT position (Mangano, GCN 
15666) we do not detect any object in stacked images. However we found a 
fading object which is not present in SDSS catalog. The coordinates of 
the obsjet is (J2000)   RA=15 28 20.73, Dec = +37 45 28.8 with 
uncertainity of  0.3" in each coordinate. The position of the fading 
object is 5.2" from the refined XRT position (Mangano, GCN 15666). Due 
to fading nature of the new object we suggest it as an afterglow of the 
GRB 140103A.

Details of the photometry   is following:

Date        T_start   t-t0,     Filter  Exp.,    OT   err.
               (UT)    mid, d            s
2014-01-03  01:21:18  0.03953  None     5*120  21.14  0.12
2014-01-03  01:34:40  0.05345  None    10*120  21.35  0.12
2014-01-03  02:01:21  0.07662  None    15*120  21.41  0.11
2014-01-04  01:47:48  1.08483  None    34*120  >22.3  (3 sigma)

The photometry is based on SDSS DR9 stars and gri -> R transformations 
(Lupton):

N  SDSS_id              R(Lupton)
1  J152814.09+374706.3  18.20
2  J152819.83+374538.8  15.61

Finding chart and a light curve of the afterglow can be found in
http://grb.rssi.ru/GRB140103A/grb140103A_chart.png
and
http://grb.rssi.ru/GRB140103A/grb140103A_lc.PNG


GRB_name: GRB140114A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15736
SUBJECT: GRB 140114A: KAIT Optical Upper Limit
DATE:    14/01/14 21:58:17 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 140114A (Troja et al.,
GCN 15728) starting at 12:01:57 UT, 257 s after the burst.
Observations were performed with an automatic sequence in the
I and clear (roughly R) filters, and the exposure time was
20 s per image. Within the enhanced XRT error circle (Beardmore
et al., GCN 15733), we do not detect the afterglow reported by
Butler et al. (GCN 15732) in our single images, nor in a co-added
image from the first 5 images. The typical limiting magnitude of
our single clear image is about 19.4. The co-added image limiting
magnitude is 20.6 at a mean time of about 490 s after the burst.


GRB_name: GRB140114A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15737
SUBJECT: GRB 140114A: Swift/UVOT Upper Limits
DATE:    14/01/14 22:18:03 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140114A
120 s after the BAT trigger (Troja et al., GCN Circ. 15728).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 15733) is detected in the initial UVOT
exposures and following summed 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           120          270          147         >20.9
u_FC               278          528          246         >20.2
white              120         1701          411         >21.2
v                  608         1404           97         >18.8
b                  534         1330           78         >19.6
u                  278          528          246         >20.2
w1                 658         1626          117         >19.3
m2                 633         1429           58         >18.6
w2                1013         1379           39         >18.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140114A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15738
SUBJECT: GRB 140114A: Swift-BAT refined analysis
DATE:    14/01/14 22:29:15 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), 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 140114A (trigger #583861)
(Troja, et al., GCN Circ. 15728).  The BAT ground-calculated position is
RA, Dec = 188.498, 27.942 deg, which is 
   RA(J2000)  =  12h 33m 59.6s 
   Dec(J2000) = +27d 56' 31.9" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows one roughly symmetrical peak starting 
at ~T+10 sec, peaking at ~T+100 sec, and ending at ~T+210 sec. There are a few
small peaks riding on top of the main peak.  T90 (15-350 keV) is 139.7 +- 16.4 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+24.2 to T+202.5 sec (with 2.7 sec missing 
in the middle due to data drop outs) is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 2.06 +- 0.09.
The fluence in the 15-150 keV band is 3.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+115.88 sec in the 15-150 keV band
is 0.9 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/583861/BA/


GRB_name: GRB140114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15739
SUBJECT: GRB 140114A: Swift-XRT refined Analysis
DATE:    14/01/15 00:23:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 11 ks of XRT data for GRB 140114A (Troja  et al. GCN
Circ. 15728),  from 118 s to 24.7 ks after the BAT trigger. The data
comprise 449 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN. Circ 15733).

The late-time light curve (from T0+5.0 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.50 (+/-0.15).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.22 (+/-0.03). The
best-fitting absorption column is  1.53 (+/-0.07) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.33 (+0.21, -0.20)
and a best-fitting absorption column of 1.3 (+0.5, -0.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.1 x 10^-11 (4.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: 4.5 sigma
Photon index:      2.33 (+0.21, -0.20)

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 0.020 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x
10^-13 (9.6 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/00583861.

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


GRB_name: GRB140114A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15740
SUBJECT: GRB 140114A: ROTSE-III Optical Limits 
DATE:    14/01/15 01:07:06 GMT
FROM:    Farley V. Ferrante at Southern Methodist U/ROTSE  <fferrante@smu.edu>

T. Guver (Istanbul Univ.), F. V. Ferrante (SMU), R. Kehoe (SMU), G. Dhungana
(SMU), and W. Zheng (UC Berkely) report on behalf of the ROTSE GRB team:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
140114A (Swift trigger 583861; Troja et al, GCN 14728), producing images
beginning 22.4 s after the GCN notice time. An automated response took the
first image at 11:59:20.4 UT, 98.1 s after the burst, under fair conditions.
We took 10 5-sec, 10 20-sec and 9 60-sec exposures. These unfiltered
images are calibrated relative to USNO A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle or the XRT error circle; the field is not crowded.
Individual images have limiting magnitudes ranging from 14.0-15.1; we set
the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-t_GRB(s)  Coadd?
---------------------------------------------------------------------------
11:59:20.4   11:59:25.4         5      14.0           98.1            N
11:59:20.4   11:60:20.4        60     15.0           98.1            N


GRB_name: GRB140114A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15741
SUBJECT: GRB 140114A: MITSuME Okayama upper limits
DATE:    14/01/15 04:41:49 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 MITSuME collaboration:

We observed the field of GRB 140114A (Troja et al., GCNC 15728)
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 2014-01-14 14:12:05 UT (~2.2 h after the burst).
We could not detect the previously reported afterglow (Butler et al., GCNC
15732) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.13037    15:05:24    6000.0   >18.9  >19.3  >18.6
0.29802    19:06:49    6300.0   >20.1  >20.3  >19.4
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140114A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15742
SUBJECT: GRB 140114A: Continued RATIR Optical and NIR Observations
DATE:    14/01/15 15:20:07 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
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140114A (Troja et al., GCN 15728) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2014/01 15.32 to 2014/01 15.55 UTC (19.72 to
25.20 hours after the BAT trigger), obtaining a total of 3.36 hours
exposure in the r and i bands and 1.48 hours exposure in the Z, Y, J, and H
bands.

The optical/NIR source detected by RATIR last night (Butler et al., GCN
15732) has now faded below our detection limit.  In comparison with the
SDSS DR9 and 2MASS, we obtain the following upper limits (3-sigma):

  r     > 23.67
  i     > 23.52
  Z     > 22.56
  Y     > 21.98
  J     > 21.87
  H     > 21.33

These magnitudes are in the AB system and are not corrected for
Galactic extinction in the direction of the GRB.


GRB_name: GRB140114A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15743
SUBJECT: GRB 140114A: NOT afterglow observations
DATE:    14/01/15 16:25:02 GMT
FROM:    Zach Cano at U of Iceland  <zcano@mail.com>

Z. Cano (U. Iceland), D. Xu, D. Malesani (DARK/NBI), P. Jakobsson (U Iceland), T. Pursimo (NOT) report on behalf of a larger collaboration:

We observed the field of GRB 140114A (Troja et al., GCN Circ. 15728) with the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC starting at 03:19 UT on 15-Jan-2014. We obtained 12x300 s frames in SDSS-i at a mean time of 15.93 hr after the burst.

The afterglow is clearly detected in the stacked image at coordinates:

RA: 12:34:05.1
Dec: +27:57:02.6

with an uncertainty of 0.5''. This position is 1.4'' from the enhanced XRT position (Beardmore et al., GCN Circ. 15733), and falls within the enhanced XRT error circle. This is presumably the source detected by Butler et al. (GCN Circ. 15732). The afterglow has m(i)=23.19+/-0.16 AB at 15.93 hr post-burst, calibrated with the nearby SDSS stars and not corrected for foreground extinction.


GRB_name: GRB140108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15744
SUBJECT: GRB 140108A: Mondy optical observations, refined analysis
DATE:    14/01/15 17:37:02 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.Volnova (IKI), E. Klunko (ISTP), M. Eselevich(ISTP), A. Pozanenko(IKI) 
report on behalf of larger GRB follow-up collaboration:

We analyzed observations of AZT-33IK telescope of Sayan observatory, 
Mondy (Klunko et al., GCN 15704; Volnova et al., GCN 15713) of the 
Swift GRB 140108A (Racusin et al., GCN 15699).  Using bright time 
interval of the afterglow we calculated coordinates of the OT:

RA(J2000)=   21:40:26.75
RA(J2000)=  +58:44:41.3
with uncertainty of 0.4 arcsec of each coordinate.

The OT coordinates are within the enhanced XRT position (Osborne et al., 
GCN 15705) and compatible with positions reported early (Gorbovskoy et 
al., GCN 15701; Strobl et al., 15703).

The light curve of the afterglow can be found in 
http://grb.rssi.ru/GRB140108A/GRB140108A_lc_preliminary.png.

The photometry is based on USNO-B1.0 stars:
s1 1487-0322168 21:40:30.85 +58:43:53.1 18.18
s2 1487-0322049 21:40:20.16 +58:43:58.3 17.96
s3 1487-0322069 21:40:21.62 +58:45:00.6 17.29
s4 1487-0322305 21:40:41.61 +58:45:28.0 15.73

Maximum of afterglow brightness of R=18.50 +/- 0.08 was detected at 
0.00468 days after GRB trigger. It is also interesting a sharp drop at 
~0.85 days (confirmed by observations reported by Kelemen (GCN 15727)) 
which could be related to a jet break observed in XRT light curve (see 
http://www.swift.ac.uk/xrt_live_cat/00583338/).


GRB_name: GRB140103A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15745
SUBJECT: GRB 140103A: optical upper limit
DATE:    14/01/16 07:41:19 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (IKI), A. Ivanov (KubSU), V. Ivanov (KubSU), V. Lysenko (KubSU),
I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of GRB follow-up
collaboration:

We observed the field of the Swift GRB 140103A (Mangano et al., GCN 15656)
with 0.51-m f/8 telescope of Kuban State University Astrophysical
Observatory on Jan. 3, starting 12 minutes after GRB trigger. We obtained
several images of 30 s exposure in R-band. In the refined XRT position
(Mangano, GCN 15666) we do not detect any object in stacked image. In
particular we do not detected the optical afterglow candidate reported by
Volnova et al. (GCN 15735).

Details of the photometry are following:

Date               T_start      t-t0,           Filter  Exp.,      OT
                        (UT)          mid, d                  s
2014-01-03   00:42:05    0.02314    R        80*30.   >17.2 (3 sigma)


GRB_name: GRB140103A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15746
SUBJECT: GRB 140103A:  MASTER-Net early OT detection
DATE:    14/01/16 15:20:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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 SWIFT GRB 140103A (V. Mangano et. 
al. GCN 15656) 22 sec after notice  time and 303 sec after trigger time at 
00:35:54 UT (Gorbovskoy et al., GCN 15660).
We finaly processed our data and found faint optical afterglow on ours 
coadd images starting from t_0 + 303 sec (exp=240 sec) the position 
reported by Volnova et. al. ( GCN 15744).
The afterglow have a local maximum near 1560 sec after the burst, which, 
in the principle, can be result of long  plato-like X-ray activity.

Out photometry data available at table below.

t_start     t_mid   t_finish  t-t0   Exp.    Mag.  S/N coadd
--------+----------+---------+------+-----+-------+---+-----
00:35:45  00:36:45  00:37:59   458    240   19.4   3.6    3
00:35:45  00:36:45  00:41:50   689    670   20.2   2.6    6
00:40:24  00:42:24  00:44:09   828    430  <20.7   ---    3
00:38:33  00:40:13  00:44:50   869    710   20.3   3.0    5
00:51:29  00:54:29  00:56:23  1562    540   19.8   4.3    3
00:48:06  00:51:06  00:58:08  1667   1080   20.2   3.8    6
01:08:39  01:11:39  02:11:41  6080   6660   22.0   2.5   37

The light curve available here 
http://master.sai.msu.ru/static/GRB/GRB140103A.png


The message may be cited.


GRB_name: GRB140110A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15747
SUBJECT: GRB 140110A: Further Swift-XRT Observation
DATE:    14/01/16 16:36:12 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA), D. Malesani (DARK/NBI) and P. A. Evans (U. 
Leicester) report on behalf of the Swift team:

On 2014 January 15, Swift has returned to observe the field of the Fermi 
GRB 140110A (Bissaldi et al., GCN 15714; von Kienlin & Connaughton, GCN 
15716). Five uncatalogued X-ray sources were listed by Maselli et al. 
(GCN 15721) as a result of the analysis of seven tiled XRT observations 
(Evans, GCN 15715) carried out on January 10. According to Pal'shin et 
al. (GCN 15725), the position of just one of these sources (#7) is 
consistent with the IPN annulus.

During the XRT observation carried out on January 15, which started 455 
ks after the LAT trigger, the source #7 was detected at a mean count 
rate of 2.64 (+1.06, -0.84) x 10^-3 ct s^-1 which is consistent with the 
one [2.61 (+1.25, -0.95) x 10^-3 ct s^-1] corresponding to five days 
earlier. Consequently, this source is unlikely to be the afterglow of 
GRB 140110A. Further details of the XRT analysis carried out on the 
field of GRB 140110A are available at the following link: 
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/.

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


GRB_name: GRB140118A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15748
SUBJECT: GRB 140118A: Swift detection of a burst
DATE:    14/01/18 01:40:21 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. A. Kennea (PSU), V. Mangano (PSU),
C. B. Markwardt (NASA/GSFC), 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 01:32:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140118A (trigger=584136).  Swift did not slew to the burst
because the location is sun-constrained. The BAT on-board calculated 
location is RA, Dec 331.003, -17.948 which is 
   RA(J2000) = 22h 04m 01s
   Dec(J2000) = -17d 56' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a broad triangle-
shaped peak structure with a duration of about 40 sec.  The peak count 
rate was ~1200 counts/sec (15-350 keV), at ~3 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 07:34 UT on 2014 April 03. There will thus be no XRT or
UVOT data for this trigger before this time. 

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


GRB_name: GRB140118A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15750
SUBJECT: GRB 140118A, Swift-BAT refined analysis
DATE:    14/01/18 15:15:04 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

A. Y. Lien (NASA/UMBC), S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), 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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140118A (trigger #584136)
(Krimm, et al., GCN Circ. 15748).  The BAT ground-calculated position is
RA, Dec = 330.999, -17.937 deg which is
    RA(J2000)  =  22h 03m 59.8s
    Dec(J2000) = -17d 56' 14.1"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%. The mask-weighted light curve shows a
double-peaked structure of two triangular shaped peaks.  The first
runs from T-70 to T-20 and the second, stronger peak from T-20 to T+30.
T90 (15-350 keV) is 84.15 +- 10.79 sec (estimated error including systematics).

The time-averaged spectrum from T-73.61 to T+30.87 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.87 +- 0.13.  The fluence in the 15-150 keV band is 2.6 +- 0.2 x 10^-6 erg/cm2. 
The 1-sec peak photon flux measured from T+2.98 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/584136/BA/


GRB_name: GRB140118A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15751
SUBJECT: GRB 140118A: Fermi GBM observation
DATE:    14/01/18 15:47:14 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

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

"At 01:32:07.85 UT on 18 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140118A (trigger 411701530 / 140118064),
which was also detected by the Swift/BAT (Krimm et al., GCN 15748;
Lien et al., GCN 15750).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 90 degrees.

The GBM light curve consists of two separate pulses
with a duration (T90) of about 92 s (50-300 keV).
The time-averaged spectrum from T0-74 s to T0+23 s is
adequately fit by a simple power law function with index -1.89 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(6.0 +/- 0.4)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-2.05 s in the 10-1000 keV band
is 2.5 +/- 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: GRB140118A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15752
SUBJECT: GRB 140118A: RATIR Optical and NIR Observations
DATE:    14/01/18 15:48:58 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
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140118A (Krimm, et al., GCN 15748) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2014/01 18.09 to 2014/01 18.10 UTC (39.6 to
53.4 minute after the BAT trigger), obtaining a total of 7.8 minutes
exposure in the r and i bands and 4.2 minutes exposure in the Z, Y, and J
bands through high airmass.

We detect no new, uncatalogued sources in the refined Swift BAT error box
(Lien et al., GCN 15750).  In comparison with 2MASS, we obtain the
following 3-sigma upper limits:

  r     > 19.93
  i     > 19.37
  Z     > 19.06
  Y     > 18.99
  J     > 18.32

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB131215A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15754
SUBJECT: Konus-Wind observation of GRB 131215A
DATE:    14/01/20 13:29:34 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long GRB 131215A (MAXI/GSC detection and localization:
K. Fukushima et al., GCN 15597) was detected by Konus-Wind
in the waiting mode at about T0(MAXI)= 32900 s UT (09:08:20).

The burst began with a pulse with a duration of about 60 s, followed by 
a less intense emission lasting ~240 s. The total burst duration was 
about 300 s.

As observed by Konus-Wind, the burst had a fluence
of (1.4 +/- 0.3)x10^-5 erg/cm2 (in the 20 - 1200 keV energy range).

Modelling the K-W 3-channel time-integrated spectrum
(from T0(KW) to T0(KW)+300 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields
alpha = -1.28 (-0.27, +0.31), and
Ep = 263 (-87, +234) keV

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB131215A/


GRB_name: GRB140118A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15755
SUBJECT: Correction: MAXI J1421-613: Skynet PROMPT/R-COP observations
DATE:    14/01/20 15:56:15 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, D. Reichart, A. Verveer, T. Spuck, A. LaCluyze, J. Haislip, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

In GCN 15753 (Trotter et al.), we mistakenly conflated the transient 
source MAXI J1421-613 (Baumgartner et al., GCN 15749, Swift trigger 
584155) with GRB 140118 (Krim et al., GCN 15748, Lien et al., GCN 15750, 
Swift trigger 584136). We regret the error, and thank our colleagues who 
pointed it out. A corrected version of our observing report follows:

Skynet observed the Swift-XRT localization of transient source MAXI 
J1421-613 (Baumgartner et al., GCN 15749, Swift trigger 584155) with one 
24" and four 14" telescopes of the PROMPT array at Cerro Tololo, Chile, 
with two 14" telescopes of the PROMPT array at Siding Spring, Australia, 
and with the 14" R-COP telescope at Perth Observatory, Australia.  
Observations began 86s after the trigger, simultaneously in the BVRI 
bands. We detect no uncatalogued optical source in the Swift-XRT error 
circle. In stacks of exposures, we obtain the following upper limits:
Mean Time   Band    Limit
10.8m       I       >19.6
14.9m       R       >19.1
11.7m       V       >19.8
14.9m       B       >19.1
6.94h       I       >17.3
7.10h       R       >16.9
6.02h       V       >20.4
6.04h       B       >20.4

Photometry is calibrated to five APASS-DR7 stars in the field, and has 
not been corrected for the extremely significant Galactic foreground 
extinction corresponding to E(B-V)=10.5 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB140114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15756
SUBJECT: GRB 140114A: optical upper limit
DATE:    14/01/21 08:34:59 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (IKI), R. Inasaridze (AAO), Yu. Krugly (IA KhNU), I. Slyusarev
(IA KhNU), G. Inasaridze (AAO), V. Zhuzhunadze (AAO), I. Slyusarev (IA
KhNU), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB
follow-up collaboration:

We observed the field of Swift GRB 140114A (Troja et al., GCN 15728) on
Jan., 15 with AS-32 (0.7m) telescope of Abastumani Observatory, and AZT-8
(0.7m) telescope of Institute of Astronomy, Kharkiv National University. We
obtained several unfiltered frames with exposures of 120 s (AS-32), and
several frames with filter R with exposure of 120 s (AZT-8). Within the
enhanced XRT circle (Beardmore et al., GCN 15733) we did not detect the
afterglow reported by Butler et al. (GCN 15732).

The details of the photometry are the following:

Telescope  t_start, UT  t-T0, mid, days  Exptime,s Filter Uplim, 3 sigma

AS-32          00:07:23    0.54452                     40*120
None        20.6
AZT-8          00:29:00    0.54720        32*120           R
20.8

The photometry is based on SDSS stars, R mag (R mag obtained using ugriz
transformations in BVRI (Lupton, 2005):

SDSS id                          R
J123415.64+275948.8 16.079 J123342.40+275950.2 15.120


GRB_name: GRB140110A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15757
SUBJECT: GRB 140110A: Second Follow-up Swift-XRT Observation
DATE:    14/01/22 14:29:04 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA) and P. A. Evans (U. Leicester) report on behalf 
of the Swift team:

Swift carried out a second follow-up observation to investigate the 
behaviour of the X-ray source #2 reported by Maselli et al. (GCN 15721) 
as a result of the analysis of tiled observations covering the LAT error 
circle. This source, although outside the error box formed by the 
intersection between the LAT error circle and the IPN annulus reported 
by Pal'shin et al.(GCN 15725), suggested initially a possible fading 
behaviour (Maselli et al., GCN 15721).

The new observation started on January 21, 928 ks after the LAT trigger, 
and had an exposure of 6.3 ks. The source #2 has been detected with a 
mean count rate of (1.24  0.16) x 10^-2 ct s^-1 which is consistent 
with the one (1.23  0.27) x 10^-2 ct s^-1 corresponding to eleven days 
earlier. Therefore, we exclude that it may be the afterglow of GRB 140110A.

The Swift-XRT tiled observations have covered the whole error box 
reported by Pal'shin et al. (GCN 15725) and no credible counterpart for 
the X-ray afterglow has been detected (see also Maselli et al., GCN 15747).

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


GRB_name: GRB140122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15759
SUBJECT: GRB 140122A/Fermi412093190:  MASTER-Net early optical observations
DATE:    14/01/24 13:12:16 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,  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  GRB140122A (Fermi trigger 
412093190) 23 sec after notice time and 50 sec after trigger time at 
2014-01-22 14:20:37.228 UT. On our first (10s exposure) set we haven't 
found optical transient  within 2 sq. degree part in middle part of  FERMI 
error-box (ra=03 36 07 dec=+15 27 00 r=5.26) with 5-sigma upper limit has 
been about 15.5 mag on first single image and 17.0m on coadd image  of 
first 6 sets with total exposure 230 sec.   So small covered area due to 
observations in polaroid bands, which cover only 25% of our FOV.

The coordinates of the MASTER II image centers (2.1 degrees rectangle):

03h 37m 16.9s +15d 34m 55s

03h 34m 11.7s +15d 25m 53s

Also we cover 95% of 1-sigma statistical + systematic FERMI  errorbox 
using MASTER VWF robotic very wide field cameras (FOV=2x384 square 
degrees, D=72mm, f/1.4, 1 pix = 22 arcsec, http://observ.pereplet.ru) 
installed on MASTER-II robotic telescope in  same time.  No credible 
transients have been found on our images. The 3 sigma upper limit on 
single 10 seconds exposure image is 10.5 and 12.0 on coadd of 15 images 
with total exposure 150 seconds.
The positions of first two iPTF optical afterglow candidates (Singer et 
al., GCN15758 ) are covered by out cameras since 50 sec. after the trigger 
but there are no flares up to 12.0 mag. on their place.
The MASTER VWF coverage map available here 
http://master.sai.msu.ru/static/GRB/GRB140122A_map.png

The message may be cited.


GRB_name: GRB140129A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15760
SUBJECT: GRB 140129A: Swift detection of a burst with an optical afterglow
DATE:    14/01/29 03:35:31 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), W. H. Baumgartner (GSFC/UMBC),
M. G. Bernardini (INAF-OAB), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), C. A. Swenson (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 03:23:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140129A (trigger=585128).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 37.869, -1.587 which is 
   RA(J2000) = 02h 31m 29s
   Dec(J2000) = -01d 35' 11"
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 5 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 03:25:52.9 UT, 113.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 37.89128, -1.59554 which
is equivalent to:
   RA(J2000)  = 02h 31m 33.91s
   Dec(J2000) = -01d 35' 43.9"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 85 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 (2.55 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.2
(+1.80/-1.58) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 116 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  = 02:31:33.81 =  37.89087
  DEC(J2000) = -01:35:43.3  =  -1.59536
with a 90%-confidence error radius of about 1.10 arc sec. This position is 1.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.74. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.03. 

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


GRB_name: GRB140129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15761
SUBJECT: GRB 140129A: P60 optical afterglow detection
DATE:    14/01/29 04:15:45 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report on behalf of a 
larger calibration:

The Palomar 60-inch telescope automatically responded to the Swift 
trigger for GRB 140129A (Melandri et al., GCN 15760) and began taking 
images at 03:27:37.8 UT, about 3.6 minutes post-GRB trigger.

We detect a bright source, not present in USNO B1.0, at the following 
location consistent with the Swift XRT and UVOT error circles:

RA  =  02:31:33.78
dec = -01:35:42.88
(J2000)

The source is detected in r, i, and z filters, and fades rapidly from 
r=16.29 to r=19.44 between UT 03:28 and 04:07.


GRB_name: GRB140129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15762
SUBJECT: GRB 140129A: RATIR Optical and NIR Observations
DATE:    14/01/29 04:49:03 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (NASA-GSFC), 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), 
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), 
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM), 
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We began observing the field of GRB 140129A (Melandri, et al., GCN 15760) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir at 2014/01 29.15 (12.6 minutes after the BAT trigger).

For a source within the Swift-XRT error circle, in comparison with the SDSS 
DR9 and 2MASS, we obtain the following detections:

Filter    mag(T0+0.12.6 minutes) mag(12.6 to 44.4 minutes)     
  r   18.05 +/- 0.01  18.80 +/- 0.01
  i   17.85 +/- 0.02  18.67 +/- 0.02
  Z   17.72 +/- 0.03  18.50 +/- 0.03
  Y   17.82 +/- 0.04  18.33 +/- 0.03
  J   17.65 +/- 0.05  18.35 +/- 0.04
  H   17.68 +/- 0.07  18.19 +/- 0.05

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. 
Further observations are underway.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro 
Mrtir.


GRB_name: GRB140129A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15763
SUBJECT: GRB 140129A: ROTSE-III Detection of Optical Counterpart
DATE:    14/01/29 05:14:59 GMT
FROM:    Farley V. Ferrante at Southern Methodist U/ROTSE  <fferrante@smu.edu>

F. V. Ferrante (SMU), W. Zheng (UC Berkeley), R. Kehoe (SMU), G. Dhungana (SMU) report on behalf of the ROTSE GRB team:

The 0.45m ROTSE-IIIb telescope located at McDonald Observatory, Texas, responded to GRB 140129A (Swift trigger 585128; Melandri, et al., GCN 15760). The first image was at 03:24:58.3 UT, 57.0 s after the burst (8.3 s after the GCN notice time). The unfiltered images are calibrated relative to USNO A2.0. We confirm the afterglow candidate reported by UVOT and detect a bright source which fades rapidly from magnitude 14.1 to 16.0 between UT 03:24:58.3 and 03:26:55.7. Continuing observations are in progress.


GRB_name: GRB140129A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15764
SUBJECT: GRB 140129A: Enhanced Swift-XRT position
DATE:    14/01/29 10:29:34 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 4216 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 140129A, 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 = 37.89093, -1.59545 which is equivalent
to:

RA (J2000): 02h 31m 33.82s
Dec (J2000): -01d 35' 43.6"

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: GRB140129B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15765
SUBJECT: GRB 140129B: Swift detection of a burst with an optical afterglow
DATE:    14/01/29 13:07:18 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC),
P. A. Evans (U Leicester), J. A. Kennea (PSU),
A. Y. Lien (NASA/GSFC/ORAU), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), 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 12:51:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140129B (trigger=585149).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 326.763, +26.207 which is 
   RA(J2000) = 21h 47m 03s
   Dec(J2000) = +26d 12' 24"
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 2 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 12:52:16.5 UT, 67.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 326.7574, 26.2065 which
is equivalent to:
   RA(J2000)  = 21h 47m 01.77s
   Dec(J2000) = +26d 12' 23.3"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 18 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 (5.58 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.7
(+2.52/-2.09) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 356 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 21:47:01.67 = 326.75695
  DEC(J2000) = +26:12:22.9  =  26.20637
with a 90%-confidence error radius of about 0.61 arc sec. This position is 1.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.92 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.09. 

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


GRB_name: GRB140129B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15766
SUBJECT: GRB 140129B:  MASTER OT confirmation
DATE:    14/01/29 13:32:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

E. Gorbovskoy, V. Lipunov,  D.Denisenko, V.Kornilov, D.Kuvshinov, 
N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov,
V.V.Chazov
Sternberg Astronomical Institute, Moscow 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 Tunka was pointed to the  GRB140129B  106 sec after 
trigger time at 2014-01-29 12h 52m 55 s UT (expo time = 20 sec). 
On our first (20s exposure) set we  found optical transient 
at the  SWIFT optical transient position. The unfiltered magnitude is 
about ~ 14m.

The message  may be cited.


GRB_name: GRB140129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15767
SUBJECT: GRB 140129A: Swift-XRT refined Analysis
DATE:    14/01/29 15:35:39 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.C. Stroh (PSU), B.P. Gompertz (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), D.N. Burrows (PSU), J.A. Kennea
(PSU) and A. Melandri report on behalf of the Swift-XRT team:

We have analysed 9.3 ks of XRT data for GRB 140129A (Melandri  et al.
GCN Circ. 15760),  from 99 s to 19.2 ks after the  BAT trigger. The
data comprise 45 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by Evans
et al. (GCN. Circ 15764).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.89 (+/-0.03).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+0.13, -0.12). The
best-fitting absorption column is  4.0 (+2.5, -1.4) x 10^20 cm^-2,
consistent with the Galactic value of 2.6 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.6 x 10^-11 (4.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.0 (+2.5, -1.4) x 10^20 cm^-2
Galactic foreground: 2.6 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.94 (+0.13, -0.12)

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 8.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-13 (3.5 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/00585128.

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


GRB_name: GRB140129A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15768
SUBJECT: GRB 140129A: Swift/UVOT Observations
DATE:    14/01/29 16:52:45 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140129A
117 s after the BAT trigger (Melandri et al., GCN Circ. 15760).
A source consistent with the XRT position (Evans et al. GCN Circ. 15764)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  02:31:33.78 =  37.89076 (deg.)
     Dec (J2000) = -01:35:43.4  =  -1.59539 (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              117          267          147 16.51  0.03
v                  605         1250           78 18.69  0.24
b                  531          551           20 17.76  0.14
u                  275          525          246 16.98  0.04
w1                 654        17641         1357 20.77  0.22
m2                5292        13449         1054 >21.2
w2                 753        11858         1102 >22.0

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: GRB140129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15769
SUBJECT: GRB 140129A, Swift-BAT refined analysis
DATE:    14/01/29 17:40:59 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), A. Melandri (INAF-OAB), 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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140129A (trigger #585128)
(Melandri, et al., GCN Circ. 15760).  The BAT ground-calculated position is
RA, Dec = 37.851, -1.594 deg which is
  RA(J2000)  =  02h 31m 24.2s
  Dec(J2000) = -01d 35' 40.1"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 57%.

The mask-weighted light curve shows a single peak structure starts at ~T+1.2 s,
peaks at ~T+2.5 s, and ends at ~ T+4.6 s. T90 (15-350 keV) is 2.99 +- 0.79 sec
(estimated error including systematics).

The time-averaged spectrum from T+1.25 to T+4.62 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.08 +- 0.33.  The fluence in the 15-150 keV band is 1.3 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.91 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/585128/BA/


GRB_name: GRB140129B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15770
SUBJECT: GRB 140129B: Enhanced Swift-XRT position
DATE:    14/01/29 20:37:45 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 1682 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140129B, 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 = 326.75708, +26.20648 which is equivalent
to:

RA (J2000): 21h 47m 1.70s
Dec (J2000): +26d 12' 23.3"

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: GRB140129A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15771
SUBJECT: GRB 140129A: MITSuME Okayama upper limits
DATE:    14/01/30 00:13:58 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 MITSuME collaboration:

We observed the field of GRB 140129A (Melandri et al., GCNC 15760)
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 2014-01-29 09:31:12 UT (~6.1 h after the burst).
We could not detect the previously reported afterglow (Melandri et al.,
GCNC 15760; Perley and Cenko, GCNC 15761) 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
-----------------------------------------------------
0.29723    10:32:00    4020.0   >19.6  >19.7  >18.9
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]


GRB_name: GRB140129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15772
SUBJECT: GRB140129A: RAPTOR Observations of the Early Afterglow
DATE:    14/01/30 00:45:09 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 585128 (Melandri, et al., GCN 15760).  Our narrow-field
instruments in Los Alamos, NM,  began imaging at 03:25:05.19 UT, 65.7 seconds
after the BAT trigger time.  Our RAPTOR-T robotic telescope measured the
counterpart simultaneously in SDSS g', r', i', and z' bands through the first
1000 seconds after the BAT trigger.  In r' band, the counterpart is at
magnitude 14.72 +- 0.04 at T+68.22 seconds.  By T+217.21, the source had
faded to r' magnitude 16.24 +- 0.07, consistent with the P60 observations
(Perley, et al., GCN 15761).  The counterpart fades monotonically during the
observation interval.  Our images were calibrated to the SDSS DR9 catalog.


GRB_name: GRB140129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15773
SUBJECT: GRB 140129A: P200 spectroscopy
DATE:    14/01/30 01:58:46 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), M. Rafelski, D. Masters (IPAC), and J. X. 
Prochaska (UCO/Lick) report:

We obtained spectroscopy of the optical afterglow of GRB 140129A 
(Melandri et al., GCN 15760) with the Double Spectrograph at the 5m 
Palomar Hale telescope beginning at 04:56:25.2 UT, approximately 1.5 
hours after the GRB trigger.  Based on our P60 imaging, the GRB 
afterglow was r~20 mag at this point and the S/N of the spectrum is low, 
although the trace is clearly detected in each of three 600s exposures. 
The spectral range covers from the atmospheric cutoff to 8700 Angstroms.

The spectrum is featureless, showing no significant absorption lines 
over our spectral range (although the EW sensitivity limit is poor). 
The absence of a DLA feature suggests a redshift of z<1.8 (more 
conservatively, the lack of IGM absorption down to the atmospheric 
cutoff indicates z<2.1).


GRB_name: GRB140129B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15774
SUBJECT: GRB 140129B, Swift-BAT refined analysis (probably not a short burst)
DATE:    14/01/30 02:54:55 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
M. G. Bernardini (INAF-OAB), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC),
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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140129B (trigger #585149)
(Bernardini, et al., GCN Circ. 15765).  The BAT ground-calculated position is
RA, Dec = 326.764, 26.215 deg which is
  RA(J2000)  =  21h 47m 03.3s
  Dec(J2000) = +26d 12' 53.1"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a single short peak starts at ~T0, peaks
at ~T+0.7 s, and ends at T+1.6 s. T90 (15-350 keV) is 1.36 +- 0.21 sec
(estimated error including systematics).

The time-averaged spectrum from T+0.08 to T+1.59 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.23 +- 0.33.  The fluence in the 15-150 keV band is 7.1 +- 1.4 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T+0.17 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Although the T90 for this burst is shorter than 2 seconds, the power law index
of the time-averaged spectrum is relatively soft for a short GRB. Therefore, we
suspect that this burst might belong to the long-soft burst category with some
burst emission missed due to background noise and detection limit.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/585149/BA/


GRB_name: GRB140129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15775
SUBJECT: GRB 140129A: CARMA early observations
DATE:    14/01/30 08:47:10 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

We observed the position of GRB 140129A (Melandri et al., GCN 15760) 
with the Combined Array for Research in Millimeter Astronomy starting at 
04:57:21 UT, 94 minutes after the GRB trigger.  Observations continued 
until 06:10:30 UT (source elevation = 19 degrees).  No source is 
detected at the optical afterglow location to a limiting flux of <1.8 
mJy (3 sigma).

We thank C. Hull, N. Volgneau, and the CARMA staff for this rapid 
observation.


GRB_name: GRB140129B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15776
SUBJECT: GRB 140129B:  MASTER OT early light curve
DATE:    14/01/30 08:54:54 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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 Tunka was pointed to the  GRB140129B  78 sec after notice time and 105 
sec after trigger time at 2014-01-29 12:52:54 UT (Bernardini et al., GCN 
15765).
Such a long pointing time is due to internal mount pointing error under 
strong Siberian frost, which was automatically solved. A set of images 
with increasing exposures was obtained with the field at zenith distance 
75 deg and setting. On our first (20s exposure) image we found optical 
transient at the SWIFT optical transient position. 
The unfiltered magnitude is about ~14m (Ivanov et al., GCN 15766).

    Our coordinates measured from the combination of 7 images are 
coincident with Swift UVOT position taking into account the error box 
reported by Bernardini et al., GCN 15765 and Swift-XRT position (Goad et 
al., GCN 15770):


     R.A.        Dec.            Err
21 47 01.71 +26 12 22.8     +/-0.5 arcsec

    The object is visible on 6 images, gradually fading below the detection
limit on the 7th image. The results of our photometry are given in table 
below:

T_start   T-T_trig Tm-T_trig   Exp,s Elevation  Mag
----------------------------------------------------
12:52:54   105        115       20     15.5     14.4
12:54:03   174        189       30     15.3     15.4
12:55:28   259        284       50     15.1     15.9
12:57:15   366        401       70     14.9     16.2
12:59:19   490        540      100     14.6     17.0
13:02:11   662        727      130     14.2     17.3
13:05:28   859        944      170     13.7     17.7
13:09:21  1091       1181      180     12.7     18.0
13:13:20  1330       1540      360     11.6    <18.4    # coadd 2 image

In the table above 'T' is time of exposure beginning, 'Tm' is mid-exposure 
time.
The power law slope is alpha = 1.42.

The GRB140129B duration is small (T_90 < 2 sec, Palmer et al., GCN 15774), 
but spectrum is soft and this burst must be  faint long GRB (Pal'shin, 
privet communication; Palmer et al., GCN 15774).

Animation of seven frames by MASTER-Tunka is uploaded to
http://master.sai.msu.ru/static/GRB/GRB140129B-MASTER-Tunka-anim.gif

The light curve is available here:
http://master.sai.msu.ru/static/GRB/GRB140129B_last.png

Take the opportunity we would like to congratulate our first author from 
Siberia Vladimir  Poleshchuk  with the birth of the grandchild.

The message  may be cited.


GRB_name: GRB140129B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15777
SUBJECT: GRB 140129B: Swift-XRT refined Analysis
DATE:    14/01/30 10:57:45 GMT
FROM:    Maria Grazia Bernardini at INAF/Brera  <grazia.bernardini@brera.inaf.it>

M. G. Bernardini (INAF-OAB) reports on behalf of the Swift-XRT team:

We have analysed 1.8 ks of XRT data for GRB 140129B (Bernardini  et al.
GCN Circ. 15765),  from 322 s to 6.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN. Circ 15770).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.24 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.12 (+0.21, -0.20). The
best-fitting absorption column is  1.1 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 5.6 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 5.6 x 10^20 cm^-2
Excess significance: 1.9 sigma
Photon index:      2.12 (+0.21, -0.20)

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 1.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x
10^-14 (8.3 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/00585149.

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


GRB_name: GRB140102A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15778
SUBJECT: GRB 140102A: MITSuME Akeno Optical observation  
DATE:    14/01/30 14:06:05 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

T. Yoshii, Y. Saito, S. Kurita, Y. Tachibana, K. Ito, R. Usui, T.Tanigawa, Y. Yano,Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 140102A (L. M. Z. Hagen et al., GCN Circular #15653) 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 started on 2014-01-02 21:18:44 UT ( 67sec after the burst).
We detected the previously reported optical afterglow of GRB140102A (D. Xu et al., GCN Circular #15655) in the Ic band.

The measured magnitudes were listed below.

T0+      MID-UT      T-EXP        mag
----------------------------------------------------
67[sec]  21:18:59    30[sec]              Rc = 14.36 $B!^(B 0.4    Ic = 13.01+/-0.17
----------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15779
SUBJECT: GRB 140129A: Continued RATIR Optical and NIR Observations
DATE:    14/01/30 16:17:02 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
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140129A (Melandri, et al., GCN 15760) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2014/01 30.13 to 2014/01 30.23 UTC (23.82 to
26.22 hours after the BAT trigger), obtaining a total of 1.36 hours
exposure in the r and i bands and 0.56 hours exposure in the Z, Y, J, and H
bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9 and 2MASS, we obtain the following detections and upper limits
(3-sigma):

  r     22.67 +/- 0.13
  i     22.32 +/- 0.11
  Z     22.19 +/- 0.27
  Y     21.94 +/- 0.37
  J     > 21.78
  H     > 21.28

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The afterglow has faded by several
magnitudes in all bands since our observations last night (Cucchiara et
al., GCN 15762).

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB140129B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15780
SUBJECT: GRB 140129B: Swift/UVOT Detection
DATE:    14/01/30 19:11:46 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and M. G. Bernardini (INAF-OAB) report on behalf
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140129B
356 s after the BAT trigger (Bernardini et al., GCN Circ. 15765).
A source consistent with the XRT position (Goad et al. GCN Circ. 15770)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  21:47:01.66 = 326.75691 (deg.)
     Dec (J2000) = +26:12:23.0  =  26.20638 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections 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              356          506          147         17.05  0.03
v                  663         5031           72         18.04  0.20
b                  588          608           20         17.90  0.20
u                  562          582           20         17.24  0.17
w1                 538          732           39         17.27  0.16
m2                 513         1089           58         17.57  0.19
w2                 638         1039           58         17.99  0.19

The clear detection in all UVOT filters indicate this burst is at a redshift
of z < ~1.5.

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.09 in the direction of the burst
(Schlegel et al. 1998).


