# GCN_circulars

GRB_name: GRB121229A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14124
SUBJECT: GRB 121229A: Swift-XRT refined Analysis
DATE:    12/12/30 04:13:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 13 ks of XRT data for GRB 121229A (Sonbas  et al. GCN
Circ. 14115),  from 135 s to 68.4 ks after the BAT trigger. The data
comprise 438 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 14121).

The late-time light curve (from T0+3.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.23 (+0.20, -0.22).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.14 (+/-0.05). The
best-fitting absorption column is  1.62 (+0.24, -0.23) x 10^22 cm^-2,
at a redshift of 2.707, in addition to the Galactic value of 1.4 x
10^21 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon
index of 2.14 (+0.33, -0.13) and a best-fitting absorption column
consistent with the Galactic value. The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.4 x
10^-11 (4.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.4 x 10^21 cm^-2
Intrinsic column:    0 (+8.4, -0) x 10^21 cm^-2 at z=2.707
Photon index:      2.14 (+0.33, -0.13)

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 7.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.6 x
10^-13 (3.7 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00544347.

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


GRB_name: GRB121226A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14126
SUBJECT: GRB 121226A: 5.8 GHz VLA observations
DATE:    12/12/30 17:26:03 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the position of the short-duration GRB 121226A (Krimm et al.,
GCN 14105; Baumgartner et al. GCN 14111) with the Karl G. Jansky Very Large
Array (VLA) beginning on 2012 December 28.54 UT (1.75 days post-burst) at a
mean frequency of 5.8 GHz. In 35-min on source, we detect a faint, 3-sigma
radio source at:

RA (J2000) = 11:14:34.12
DEC (J2000) = -30:24:22.89
with an uncertainty of ~0.2" in each coordinate.

This position is coincident with the XRT and optical positions (Littlejohns
et al., GCN 14112; Castro-Tirado et al., GCN 14114). Further observations
are planned."


GRB_name: GRB130102A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14127
SUBJECT: GRB 130102A: Swift detection of a burst
DATE:    13/01/02 18:27:44 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
F. E. Marshall (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 18:10:53 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130102A (trigger=544784).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 311.464, +49.835 which is 
   RA(J2000)  =  20h 45m 51s
   Dec(J2000) = +49d 50' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As per usual for an image trigger, the TDRSS
lightcurve does not show anything significant. 

The XRT began observing the field at 18:12:50.3 UT, 116.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
311.4233, 49.8174 which is equivalent to:
   RA(J2000)  = 20h 45m 41.60s
   Dec(J2000) = +49d 49' 02.6"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 113 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 7.96
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 5.62e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 125 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. 

We note that this event is at galactic coordinates: l = 88.33 deg, b = 4.22 
deg.  It has the characteristics of a GRB, but could be a galactic transient 
since it is close to the galactic plane. 

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


GRB_name: GRB130102A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14128
SUBJECT: GRB 130102A: IAC80 I-band observations
DATE:    13/01/03 01:21:50 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC) & L. Toribio (IAC), report on behalf of a larger
collaboration:

"We observed the Swift/XRT location of GRB 130102A (Page et al., GCNC
14127) using the 82cm IAC80 telescope at the Observatorio del Teide
(Tenerife, Spain). We took a set of I-band images on Jan 2.7924--2.8340 UT
(0.84--1.83 hours post burst). No optical source brighter than I~21 (Vega)
is detected inside the XRT error circle."


GRB_name: GRB130102A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14129
SUBJECT: GRB 130102A: Enhanced Swift-XRT position
DATE:    13/01/03 05:22:38 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 1933 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130102A, 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 = 311.42346, +49.81764 which is equivalent
to:

RA (J2000): 20h 45m 41.63s
Dec (J2000): +49d 49' 03.5"

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

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

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


GRB_name: GRB130102B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14130
SUBJECT: GRB 130102B: MAXI/GSC detection
DATE:    13/01/03 05:48:37 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

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

At 2013-01-02T04:41:42 UT, the MAXI/GSC nova alert system triggered 
on a bright uncatalogued X-ray transient source.
The transient emission started at 04:41:42 and lasted at least 
45 seconds within the 74 second long triangular transit response 
of MAXI/GSC. We identify this event as GRB 130102B.

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

 (R.A., Dec) = (309.58 deg, -72.38 deg ) = (20 38 20, -72 22 36)(J2000)

with a 90% C.L. statistical error of 0.2 deg and an additional systematic 
uncertainty of 0.2 deg (90% containment radius). The 4-10 keV flux was 
320 +- 40 mCrab.

There was no significant excess flux in the previous transit at 03:09UT 
and in the next transit at 06:15 UT$B!!(Bwith an upper limit of 20 mCrab for each.


GRB_name: GRB130102A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14131
SUBJECT: GRB 130102A: Swift-XRT refined Analysis
DATE:    13/01/03 06:27:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 130102A (Page  et al. GCN
Circ. 14127),  from 109 s to 24.6 ks after the BAT trigger. The data
comprise 66 s in Windowed Timing (WT) mode (the first 5 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 14129).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.33 (+0.21, -0.20). At T+456 s  the decay
steepens to an alpha of 5.5 (+1.9, -1.2) before breaking again at T+924
s to a final decay with index alpha=0.88 (+0.31, -0.28).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+0.4, -0.3). The
best-fitting absorption column is  1.13 (+0.34, -0.29) x 10^22 cm^-2,
in excess of the Galactic value of 8.0 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 5.8 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.13 (+0.34, -0.29) x 10^22 cm^-2
Galactic foreground: 8.0 x 10^21 cm^-2
Excess significance: 1.9 sigma
Photon index:      2.0 (+0.4, -0.3)

If the light curve continues to decay with a power-law decay index of
0.88, the count rate at T+24 hours will be 5.2 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x
10^-14 (6.4 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/00544784.

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


GRB_name: GRB130102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14132
SUBJECT: GRB 130102A: MASTER-Net  optical observations 
DATE:    13/01/03 08:05:28 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,  A.Kuznetsov, V.V.Chazov, D.Denisenko

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  GRB130102A (Page et. al. GCN14127)   104 
sec after GRB time at 2013-01-02 18:12:37 UT in 
two  polarizations. On our first (20s exposure) set we haven't found 
optical transient  within SWIFT  error-box.
The 5-sigma upper limit has been about 17.9 mag

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located near Blagoveschensk was pointed to the  GRB130102A (Page et. al. 
GCN 14127)   107
sec after GRB time at 2013-01-02 18:12:40 UT in
two  diagonal polarizations. On our first (20s exposure) set we haven't 
found optical transient  within SWIFT  error-box.
The 5-sigma upper limit has been about 13.9 mag. The low limit is the 
resultsa of the high zenit distance.

We note that there are no objects in any catalogs 10" around center of 
the Swift XRT error box (Osborne et. al. GCN 14129).

The message may be cited.


GRB_name: GRB130102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14133
SUBJECT: GRB 130102A: Swift-BAT refined analysis
DATE:    13/01/03 14:19:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130102A (trigger #544784)
(Page, et al., GCN Circ. 14127).  The BAT ground-calculated position is
RA, Dec = 311.435, 49.838 deg which is 
   RA(J2000)  =  20h 45m 44.4s 
   Dec(J2000) = +49d 50' 16.4" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.
 
The mask-weighted light curve shows a peak starting at ~T+10 sec, peaking 
at ~T+22 sec, and ending around T+180 sec.  There is a possibility
of emission out to at least T+230 sec.  T90 (15-350 keV) is 77.5 +- 18.2 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+12.51 to T+100.43 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.39 +- 0.18.  The fluence in the 15-150 keV band is 7.2 +- 0.9 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+23.54 sec in the 15-150 keV band
is 0.4 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/544784/BA/


GRB_name: GRB130102A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14134
SUBJECT: GRB 130102A: P60 Observations
DATE:    13/01/03 19:26:41 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

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

We have imaged the field of GRB130102A (Page et al., GCN 14127) with the
robotic Palomar 60 inch telescope (P60).  Observations began at 01:56 on
2013 January 3 (~ 7.8 hours after the Swift trigger), and were obtained
under poor seeing conditions in the r', i', and z' filters.

We do not detect any sources within the enhanced XRT error localization
(Osborne et al., GCN 14129).  Using nearby point sources from the AAVSO
Photometric All-Sky Survey (APASS) for calibration, we measure limiting
magnitudes of r' > 20.9, i' > 20.5 at this time.  We note that these
limits do not include a correction for the large Galactic extinction along
this line of sight.


GRB_name: GRB130102B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14135
SUBJECT: Konus-Wind observation of GRB 130102B
DATE:    13/01/04 15:49:03 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long GRB 130102B localized by MAXI/GSC (Higa et al., GCN 14130) was 
detected by Konus-Wind in the waiting mode.

The burst light curve shows a single pulse with a total duration of ~30 s.

As observed by Konus-Wind, the burst had a fluence of (3.46 +/-
0.28)x10^-6 erg/cm2 (in the 20 - 1400 keV energy range).

Fitting the K-W 3-channel time-integrated spectrum (from T0(MAXI)-21 s 
to T0(MAXI)+11 s) by a simple power-law model yields a power law index 
of 2.85 +/- 0.17.

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/GRB130102B/


GRB_name: GRB130102A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14136
SUBJECT: GRB 130102A: Swift/UVOT Upper Limits
DATE:    13/01/04 22:36:12 GMT
FROM:    Tyler Pritchard at PSU  <tapritchard@astro.psu.edu>

T. A. Pritchard (PSU) and K. L. Page (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130102A
126 s after the BAT trigger (Page et al., GCN Circ. 14127).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 14129)
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           126          276          147         >21.1
u_FC               284          534          246         >20.4
white              126         7587          844         >22.4
v                  614        12045         1343         >20.9
b                  540         7382          549         >20.8
u                  284         7177          775         >20.5
w1                 664         6972          549         >20.2
m2                 639        12641          934         >20.7
w2                 590         7794          568         >20.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.90 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130102B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14137
SUBJECT: GRB 130102B: MASTER synchronous observations 
DATE:    13/01/05 14:27:55 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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

MASTER-ICATE robotic very wide field cameras (FOV=2x384 square degrees,
D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located
in Argentina (Observatorio Astronomico Felix Aguilar,
http://93.180.27.230:8080/) were imaging the sky area of MAXI/GSC GRB 
130102B (M. Higa et al., GCN 14130) before, during and after trigger time 
with 2 sec exposures without time gap. Elevation of center of GRB error 
box at the moment of MAXI/GSC trigger was 16 deg.

We have covered the whole interval of gamma-ray activity by KONUS-WIND 
(Golenetski et al., GCN 14135) which corresponds to T-20 sec to T+10 sec 
from MAXI/GSC trigger time.

We haven't found optical transient within MAXI/GSC error box on our 2-s
frames and on the coadded image made of 15 frames and total exposure of 30 
seconds. The 3-sigma upper limit (with the reference to V magnitudes from 
Tycho-2 catalog) has been about 10.0 mag on single images and 11.5 mag on 
coadded image.

The reduction of the whole data set is continuing.

This message can be cited.


GRB_name: GRB121225B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14138
SUBJECT: GRB 121225B: Suzaku WAM observation of the prompt emission
DATE:    13/01/09 05:46:16 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long, IPN localized GRB 121225B (K. Hurley et al., GCN 14103) was 
detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers 
an energy range of 50 keV - 5 MeV at 10:01:03.165 UT (=T0).

The observed light curve shows double-peaked structure starting at 
T0-16s, ending at T0+70s with a duration (T90) of about 53 seconds. The 
fluence in 100 - 1000 keV was 4.80(+0.19/-0.25)x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+9s was 8.50 photons/cm^2/s in the 
same energy range.

Preliminary result shows that the time-averaged spectrum from T0-16s to 
T0+70s is well fitted by a single power-law with a photon index of 
2.17(+0.07/-0.07) (chi^2/d.o.f = 32.8/30).
All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

----
The light curves with 1-sec time resolution for this burst are appeared at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB121226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14139
SUBJECT: Short GRB 121226A: TNG observation of the host galaxy
DATE:    13/01/14 22:19:49 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), P. D'Avanzo (INAF/OABr), A. Melandri 
(INAF/OABr), S. Covino (INAF/OABr), A. Fiorenzano (INAF/TNG), L. Di 
Fabrizio (INAF/TNG), and G. Andreuzzi (INAF/TNG) report on behalf of the 
CIBO collaboration:

We observed the optical counterpart (Castro-Tirado et al., GCN 14114) of 
the short GRB 121226A (Krimm et al., GCN 14105) with the TNG telescope 
located in the Canary Islands. A total two hour exposure in the SDSS r 
filter was acquired, with mean time 2013 Jan 11.227 UT (15.4 days after 
the GRB). Sky conditions were good and the seeing was 1.1", despite the 
large airmass (around 2).

Consistent with the position reported by Castro-Tirado et al. (GCN 
14114) and Fong et al. (GCN 14126), we clearly detect an object with 
r(AB) = 24.68 +- 0.15. Photometric calibration was carried out by 
observing a standard field at similar airmass (for reference, we find r 
= 19.35 for the USNO star at RA = 11:14:33.12, Dec = -30:23:51.2). 
Coupled with the measurement by Castro-Tirado et al. (GCN 14114), 
obtained ~0.5 days after the GRB, our observation suggests that the 
object is the host galaxy of the GRB, with negligible afterglow 
contribution at both epochs. We note that the radio detection (Fong et 
al., GCN 14126) makes the association with the GRB secure.

The coordinates of the object as measured in our image are (J2000, 
astrometry calibrated against USNO-B1):

RA = 11:14:34.125
Dec = -30:24:22.88

with an estimated uncertainty of 0.3". We note the presence of two 
further, nearby objects, roughly 2" S and 4" NE of the optical/radio 
counterpart. A finding chart is available at the following URL:

http://www.astro.ku.dk/~malesani/GRB/121226A/GRB121226A_finder_TNG.jpg


GRB_name: GRB130122A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14140
SUBJECT: GRB 130122A: Swift detection of a burst with an optical counterpart
DATE:    13/01/22 23:57:00 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
N. Gehrels (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU)
and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team:

At 23:44:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130122A (trigger=546731).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 194.218, +59.015 which is 
   RA(J2000)  =  12h 56m 52s
   Dec(J2000) = +59d 00' 55"
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 30 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 23:46:06.3 UT, 116.9 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 194.28337, 59.01331 which
is equivalent to:
   RA(J2000)  = 12h 57m 08.01s
   Dec(J2000) = +59d 00' 47.9"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 121 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 9.34
x 10^19 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 121 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  = 12:57:08.34 = 194.28476
  DEC(J2000) = +59:00:53.9  =  59.01496
with a 90%-confidence error radius of about 1.10 arc sec. This position is 6.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.95. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.01. 

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


GRB_name: GRB130122A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14141
SUBJECT: GRB 130122A: T100 observations
DATE:    13/01/23 11:43:08 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), T. Guver (Sabanci Univ.), O. Uysal
(Akdeniz Univ./TUG), E. Gogus (Sabanci Univ.), H. Kirbiyik (TUG) report on
behalf of a larger collaboration

We observed the field of Swift GRB 130122A (Lien et al. GCN#14140)
with the 1.0 meter T100 telescope (TUBITAK National Observatory,
Antalya - Turkey), starting January, 23, 00:50 UT (~ 1 hour after
the trigger). Observations were carried out in the R filter
under moderate weather conditions. The afterglow is clearly detected in
stacked (4x300s) R band images and consistent with UVOT coordinates
reported by Lien et al. GCN#14140.

There is ~10 arcsec offset between afterglow candidate and SDSS
J125709.02+590053.1
and USNO-B1 1490-0209231 (RA= 12:57:09.00, Dec = +59:00:53.35) objects.
Using USNO-B1 star USNO-B1 1490-0209196 (RA= 12:56:56.61, Dec= +59:02:39.11)
in the field magnitude of the OT were estimated 20.8 +/- 0.2.

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


GRB_name: GRB130122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14142
SUBJECT: GRB 130122A: MASTER-Net early marginal detection of the OT 
DATE:    13/01/23 13:47:18 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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  GRB130122A  28 sec s after 
notice time and 91 sec after GRB time at 2013-01-22 23:45:40 UT in two 
polarizations.
The weather conditions were not very good and continuosly deteriorated. 
On our first (20s exposure) double set we marginally find an optical 
transient at the Swift UVOT position (Lien et al., GCN 14140) with 
unfiltered magnitude 16.8+-0.3 (m = 0.8R + 0.2B from USNO-B).

This message may be cited.


GRB_name: GRB130122A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14143
SUBJECT: GRB 130122A: Enhanced Swift-XRT position
DATE:    13/01/23 15:18:43 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 488 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130122A, 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 = 194.28517, +59.01455 which is equivalent
to:

RA (J2000): 12h 57m 8.44s
Dec (J2000): +59d 00' 52.4"

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: GRB130122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14144
SUBJECT: GRB 130122A: Xinglong optical upper limit
DATE:    13/01/23 19:50:21 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

L.P. Xin (NAOC), D. Xu (DARK/NBI), Z.Y. Wu, J.Y. Wei, Y.L. Qiu, T.M.
Zhang, J. Wang, J.S. Deng, C. Wu, X.H. Han (NAOC) report on behalf of
a larger collaboration:

We began to observe the field of GRB 130122A (Lien et.al. GCN 14140)
using the Xinglong 2.16m telescope located in Heibei Province, China
at 18:14:12 UT on 2013-01-23. We obtained 5x300s R-band images in a
poor seeing, with a median time of 19.7 hr after the BAT trigger.

The afterglow is not detected in the stacked image, down to a 3sigma
limit of R~20.2 mag, calibrated with nearby USNO B1 stars.

This message may be cited.

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


GRB_name: GRB130122A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14145
SUBJECT: GRB 130122A: Swift-XRT refined Analysis
DATE:    13/01/23 20:57:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.6 ks of XRT data for GRB 130122A (Lien  et al. GCN
Circ. 14140),  from 102 s to 29.4 ks after the BAT trigger. The data
comprise 76 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 14143).

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

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.67 (+0.21, -0.20). The
best-fitting absorption column is  6.3 (+5.3, -4.6) x 10^20 cm^-2, in
excess of the Galactic value of 9.3 x 10^19 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.3 x 10^-11 (4.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.3 (+5.3, -4.6) x 10^20 cm^-2
Galactic foreground: 9.3 x 10^19 cm^-2
Excess significance: 1.9 sigma
Photon index:      1.67 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
1.27, the count rate at T+24 hours will be 1.3 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.4 x
10^-14 (6.1 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/00546731.

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


GRB_name: GRB130122A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14146
SUBJECT: GRB 130122A: Swift-BAT refined analysis
DATE:    13/01/24 00:58:49 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130122A (trigger #546731)
(Lien, et al., GCN Circ. 14140).  The BAT ground-calculated position is
RA, Dec = 194.307, 59.003 deg, which is 
   RA(J2000)  =  12h 57m 13.8s 
   Dec(J2000) = +59d 00' 09.2" 
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.
 
The mask-weighted light curve shows a single roughly FRED-like peak
starting at ~T+0 sec, peaking at ~T+10 sec, and ending at ~T+100 sec.
T90 (15-350 keV) is 64 +- 36 sec (estimated error including systematics).
 
The time-averaged spectrum from T-12.6 to T+67.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.24.  The fluence in the 15-150 keV band is 7.4 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+10.92 sec in the 15-150 keV band
is 0.4 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/546731/BA/


GRB_name: GRB130122A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14147
SUBJECT: GRB 130122A: RATIR Detection
DATE:    13/01/24 04:58:33 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico Ramirez&#8208;Ruiz (UCSC), Jos&#233; A. de
Diego (UNAM), Leonid Georgiev (UNAM), Jes&#250;s Gonz&#225;lez (UNAM),
Carlos Rom&#225;n-Z&#250;&#241;iga (UNAM), Neil Gehrels (GSFC), and Harvey
Moseley (GSFC) report:

Through intermittent clouds and in poor seeing conditions, we observed the
field of GRB 130122A (Lien, et al., GCN 14140) with the Reionization and
Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold
Johnson Telescope at the Observatorio Astron&#243;mico Nacional on Sierra
San Pedro M&#225;rtir.  Between 2013 Jan 23.30 to 2013 Jan 23.52 UTC (7.6
to 12.7 hours after the BAT trigger), we obtained approximately 45 minutes
of useful data in the r', i', Z, Y, and J bands.

In comparison with SDSS DR8 and 2MASS, we derive the following detection
and upper limits (3-sigma) in the AB magnitude system for a source
spatially coincident with the UVOT position (GCN 14140):

 r' >20.7
 i' 21.1 +/- 0.2
 Z  >20.3
 Y  >20.2
 J  >18.2

These magnitudes are not corrected for Galactic extinction in the direction
of the GRB.  Continued observations are planned.

We thank the staff of the Observatorio Astron&#243;mico Nacional in San
Pedro M&#225;rtir.


GRB_name: GRB130122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14148
SUBJECT: GRB 130122A: optical observations
DATE:    13/01/24 10:05:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU/IKI), V. Linkov (ISON-Kislovodsk),  I. Molotov (KIAM), 
V. Kouprianov (GAO), A. Pozanenko (IKI),  report on behalf of larger 
collaboration:

We observed the field of  GRB 130122A (Lien  et al., GCN 14140) with 
SANTEL-400AN (0.4-m f/3)  telescope of ISON-Kislovodsk observatory. 
Observations started on  Jan. 22 (UT) 23:44  and we obtained  several 
unfiltered images  of 60 s and 100 s exposures. Initial part of our 
observations were carried under unfavorable weather conditions. Starting on 
Jan.23 (UT) 00:14:14 we clearly detect optical afterglow of GRB 130122A 
(Lien  et al., GCN 14140; Sonbas et al., GCN 14141; Gorbovskoy  et al., GCN 
14142) in single images of 60 s exposure. A  preliminary photometry of 
stacked  images is based  on USNO-B1.0 (R2)  nearby  stars:

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

00:14:14  0.00899  8x60    none      18.0 +/-0.1
00:47:45  0.04474   100     none      18.5 +/- 0.5
01:02:07  0.05579  4x60    none       >17.3 


GRB_name: GRB130122A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14149
SUBJECT: GRB 130122A: Swift/UVOT Detection
DATE:    13/01/24 12:16:16 GMT
FROM:    Patricia Schady at MPE/Swift  <msslba@googlemail.com>

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

The Swift/UVOT began settled observations of the field of GRB 130122A 121 s
after the BAT trigger (Lien et al., GCN Circ. 14140). A source consistent
with the XRT position reported in (Beardmore et al., GCN Circ. 14143) is
seen in the initial exposures.

The preliminary UVOT position is:
    RA  (J2000) =  12:57:08.30 = 194.28459 (deg.)
    Dec (J2000) = +59:00:53.5  =  59.01487 (deg.)
with an estimated uncertainty of 0.53 arc sec. (radius, 90% confidence).

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

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

white_FC           121          271          148         18.75 Â± 0.09
white              559          579           19         18.57 Â± 0.23
v                  609          629           19        >17.9
b                  535          555           19         18.35 Â± 0.32
u                  279          529          246         18.49 Â± 0.14
uvw1              3974         5610          393        >20.9
uvm2              5205         5404          197        >20.0
uvw2              4795         4995          197        >20.4

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: GRB130122A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14150
SUBJECT: GRB 130122A: CARMA 3mm Observations
DATE:    13/01/25 01:31:32 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

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

"We observed the position of GRB 130122A (Lien et al.;
GCN 14140) beginning 2013 Jan 23.47 (dt=0.48 d) with the
Combined Array for Research in Millimeter Astronomy.  At
a mean frequency of 85 GHz with 78 m integration, we do not
detect significant millimeter emission at the Swift/UVOT
position (Breeveld et al.; GCN 14149) to a 3-sigma limit
of ~0.9 mJy.

We thank the CARMA observatory staff for their support."


GRB_name: GRB130122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14152
SUBJECT: GRB 130122A: RTT150 optical observations
DATE:    13/01/28 12:20:09 GMT
FROM:    Irek Khamitov at TUG  <irekk@tug.tug.tubitak.gov.tr>

A. Galeev (KFU/AST), I. Khamitov (TUG),
I. Bikmaev, N. Sakhibullin (KFU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
H. Kirbiyik (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

The field of the optical afterglow of GRB 130122A (Lien et al., GCN 14140)
was observed with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, 
TUBITAK National Observatory, Turkey) in partially cloudy conditions.
Using the TFOSC instrument we obtained BVR images by 300s starting at 
January 23, 02:38:31 UT, i.e. 2.91 hours after the burst. The afterglow is 
clearly detected in all images.

On our images we find the optical transient at the coordinates with 
uncertainty of 0.1 arcsec:
  R.A. (J2000) =  12 57 08.317
  Dec. (J2000) = +59 00 53.62

Using the same USNO-B1 star reported by Sonbas et al. (GCN 14141) as a 
reference, we estimated the R-magnitudes of the afterglow:

T-T0,  Mag. +/- Mag.err
(hour)
2.95  19.88 +/- 0.13
3.06  20.07 +/- 0.10
3.17  19.94 +/- 0.20
3.28  20.00 +/- 0.09
3.33  19.79 +/- 0.13

The combined image of the field can be found at:
http://hea.iki.rssi.ru/grb/130122a/indexeng.html

This message may be cited.


GRB_name: GRB130127A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14154
SUBJECT: GRB 130127A: Fermi GBM detection
DATE:    13/01/28 18:54:47 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 17:50:23.93 UT on 27 January 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130127A (trigger 381001826 / 130127743).

The on-ground calculated location, using the GBM trigger
data, is RA = 251.1, DEC = -17.1 (J2000 degrees,
equivalent to 16 h 44 m, -17 d 04'), with an uncertainty
of 8.5 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 27 degrees.

The GBM light curve shows a bright short peak and a fainter
tail, with a duration (T90) of about 0.45 s (50-300 keV).

The time-averaged spectrum from T0-0.064 s to T0+0.064 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.03 +/- 0.29 and
the cutoff energy, parameterized as Epeak, is 770 +/- 190 keV
(Castor statistics 751 for 725 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(4.9 +/- 0.4)E-07 erg/cm^2. The 64-msec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 7.4 +/- 0.9 ph/s/cm^2.

A Band function fits the spectrum equally well
(Castor statistics 750.29 for 724 d.o.f.) with Epeak= 700 +/- 210 keV,
alpha = 0.03 +/- 0.34 and beta = -2.4 +/- 0.7.


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


GRB_name: GRB130131A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14156
SUBJECT: GRB 130131A: Swift detection of a burst
DATE:    13/01/31 14:06:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Grupe (PSU), B. N. Barlow (PSU), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), S. T. Holland (STScI),
J. A. Kennea (PSU), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), C. Pagani (U Leicester),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), R. L. C. Starling (U Leicester) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 13:56:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130131A (trigger=547407).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 171.108, +48.069 which is 
   RA(J2000)  =  11h 24m 26s
   Dec(J2000) = +48d 04' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two peak: 1 5-sec peak
at T+0 sec and a 100-sec peak at T+50 sec. 
with a total duration of about 60 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 13:57:20.5 UT, 58.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 171.12193, 48.07520 which
is equivalent to:
   RA(J2000)  = 11h 24m 29.26s
   Dec(J2000) = +48d 04' 30.7"
with an uncertainty of 4.4 arcseconds (radius, 90% containment). This
location is 40 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 1.45
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.22e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 67 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.01. 

Burst Advocate for this burst is D. Grupe (dxg35 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130131A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14157
SUBJECT: GRB 130131A - UKIRT afterglow candidate
DATE:    13/01/31 16:23:37 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), T.  Wold (JACH)
report on behalf of a larger collaboration:

We observed the field of GRB 130131A (Grupe et al. GCN 14166)
with the WFCAM camera on UKIRT, beginning approximately 54 mins
after the BAT trigger.

Within the XRT error circle we detect a single, bright point source
at position:

11 24 30.39
+48 04 33.3
(J2000, uncertainty ~0.5")

Provisional Vega magnitudes (relative to a nearby 2MASS source) are K=16.4,
J=19.4, indicating a rather red source.

Further observations and analysis are ongoing.


GRB_name: GRB130131A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14158
SUBJECT: GRB 130131A - Faulkes Telescope North Observations
DATE:    13/01/31 16:27:53 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

F.J. Virgili (LJMU), C. Guidorzi (U. Ferrara), and A. Melandri 
(INAF-OAB) report:

"The 2-m Faulkes Telescope North robotically followed up GRB 130131A
(Swift trigger 547407, Grupe et al. GCN 14156) 2.88 min after the GRB 
trigger time. No optical counterpart is detected
within the XRT error circle to the following conservative limits:

Midtime from GRB    Exposure    Filter    Magnitude
       (min)                        (s)
-------------------------------------------------
       3.4                       3x10s         R        >19.2
       28.9                      720s          R        >20.6
       33.7                      700s          i'        >20.1
-------------------------------------------------

Magnitudes are calibrated with nearby USNOB-1 and SDSS stars."


GRB_name: GRB130131B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14159
SUBJECT: GRB 130131B: Swift detection of a burst
DATE:    13/01/31 19:21:30 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), S. T. Holland (STScI), J. A. Kennea (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and B.-B. Zhang (PSU) report on behalf of
the Swift Team:

At 19:10:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130131B (trigger=547420).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 173.952, +15.036 which is 
   RA(J2000)  =  11h 35m 48s
   Dec(J2000) = +15d 02' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two peaks
with a total duration of about 5 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 19:11:58.3 UT, 109.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 173.95398, 15.03873 which
is equivalent to:
   RA(J2000)  = 11h 35m 48.96s
   Dec(J2000) = +15d 02' 19.4"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 11 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 (2.81 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.8
(+2.32/-2.04) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 113 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 M. H. Siegel (siegel AT swift.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130131A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14160
SUBJECT: GRB 130131A: Enhanced Swift-XRT position
DATE:    13/01/31 21:29:21 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 574 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130131A, 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 = 171.12621, +48.07589 which is equivalent
to:

RA (J2000): 11h 24m 30.29s
Dec (J2000): +48d 04' 33.2"

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: GRB130131B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14161
SUBJECT: GRB 130131B: Zadko observatory - Gingin optical observations
DATE:    13/01/31 22:37:58 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (IRAP-CNRS-OMP), 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 130131B detected by SWIFT
(trigger 547420) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 70.2s after the GRB trigger
(43.4s after the notice). The elevation of the field decreased from
43 degrees above horizon but gibbous moon was at 23 degrees
away from the GRB position.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT at the XRT position (Siegel et al.
GCNC 14159) with a limiting magnitude of:
t0+70.2s to t0+130.2s : R > 15.6

The second image is 30.0s exposure in tracking mode:
t0+149s to t0+179s : R > 16.5

An image follow-up continued until 1.5h after the
GRB showing no optical transcient at the limiting
magnitude 16.5. The gibbous moon prevents to obtain
deeper limiting magnitudes.

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


GRB_name: GRB130131B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14162
SUBJECT: GRB 130131B: TAROT Calern observatory optical observations
DATE:    13/01/31 22:39:23 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 130131B detected by SWIFT
(trigger 547420) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 1.2h after the GRB trigger
because the GRB occured when the field of view was
under the local horizon. At the start of the observations,
the elevation of the field increased from 10 degrees
above horizon and gibbous moon was at 25 degrees away
from the GRB position.

We co-added a series of exposures. No optical transcient
was detected at the XRT position (Siegel et al. GCNC 14159)
with a limiting magnitude of:
t0+1.3h - 2.2h : R > 17.1

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


GRB_name: GRB130131A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14163
SUBJECT: GRB 130131A: Swift-BAT refined analysis
DATE:    13/01/31 23:03:50 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
D. Grupe (PSU), H. A. Krimm (GSFC/USRA), A. Lien (GSFC/ORAU),
C. B. Markwardt (GSFC), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+903 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130131A (trigger #547407)
(Grupe, et al., GCN Circ. 14156).  The BAT ground-calculated position is
RA, Dec = 171.091, 48.064 deg which is 
   RA(J2000)  =  11h 24m 21.9s 
   Dec(J2000) = +48d 03' 51.0" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows two separated peaks: (1) starting at ~T-5 sec,
peaking at ~T+1 sec, and ending at ~T+15 sec, and (2) T+35, T+47, and ~T+65 sec.
T90 (15-350 keV) is 51.6 +- 2.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.95 to T+52.15 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.12 +- 0.32.  The fluence in the 15-150 keV band is 3.1 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.04 sec in the 15-150 keV band
is 0.7 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/547407/BA/


GRB_name: GRB130131B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14164
SUBJECT: GRB 130131B: Swift-BAT refined analysis
DATE:    13/01/31 23:16:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Lien (GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), G. Sato (ISAS), M. H. Siegel (PSU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-119 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130131B (trigger #547420)
(Siegel, et al., GCN Circ. 14159).  The BAT ground-calculated position is
RA, Dec = 173.957, 15.033 deg which is 
   RA(J2000)  =  11h 35m 49.6s 
   Dec(J2000) = +15d 01' 59.3" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 51%.
 
The mask-weighted light curve shows a single pulse starting at ~T-1 sec,
peaking at ~T+0.5 sec, and ending at ~T+10 sec.  T90 (15-350 keV) is
4.30 +- 0.26 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.28 to T+4.37 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.15 +- 0.20.  The fluence in the 15-150 keV band is 3.4 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.28 sec in the 15-150 keV band
is 1.0 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/547420/BA/


GRB_name: GRB130131B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14165
SUBJECT: GRB 130131B: Enhanced Swift-XRT position
DATE:    13/02/01 00:46:27 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 2472 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 130131B, 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 = 173.95566, +15.03818 which is equivalent
to:

RA (J2000): 11h 35m 49.36s
Dec (J2000): +15d 02' 17.5"

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: GRB130131A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14166
SUBJECT: GRB 130131A: MITSuME Okayama optical upper limits
DATE:    13/02/01 00:50:07 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 130131A (Grupe et al., GCNC 14156)
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 2013-01-31 14:53:53 UT (~58 min after the burst).
We did not find any new point source within the enhanced XRT circle
(Evans et al., GCNC 14160) 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
------------------------------------------------------
0.10111    16:21:58    9000.0   >20.5  >20.5  >19.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130131B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14167
SUBJECT: GRB 130131B: MITSuME Okayama optical upper limits
DATE:    13/02/01 01:00:50 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 130131B (Siegel et al., GCNC 14159)
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 2013-01-31 19:11:04 UT (~57 sec after the burst).
We did not find any new point source within the enhanced XRT circle
(Goad et al., GCNC 14165) 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
------------------------------------------------------
0.03838    20:05:23    4800.0   >19.8  >19.9  >19.2
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130131A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14168
SUBJECT: GRB 130131A: Swift-XRT refined Analysis
DATE:    13/02/01 02:07:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.2 ks of XRT data for GRB 130131A (Grupe  et al. GCN
Circ. 14156),  from 64 s to 18.8 ks after the  BAT trigger. The data
comprise 235 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 14160).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.1 (+0.4, -0.3).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.44 (+/-0.07). The
best-fitting absorption column is  3.17 (+/-0.19) x 10^21 cm^-2, in
excess of the Galactic value of 1.4 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.21 (+0.21, -0.20)
and a best-fitting absorption column of 2.4 (+/-0.6) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (6.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.4 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^20 cm^-2
Excess significance: 6.5 sigma
Photon index:      2.21 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
1.1, the count rate at T+24 hours will be 2.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.3 x
10^-14 (1.6 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/00547407.

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


GRB_name: GRB130131B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14169
SUBJECT: GRB 130131B: Swift/UVOT Upper Limits
DATE:    13/02/01 03:17:28 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 130131B
114 s after the BAT trigger (Siegel et al., GCN Circ. 14159).
No optical afterglow consistent with the XRT position
is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(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           114          264          147         >20.9
u_FC               327          577          246         >20.2
white              114         6416          449         >22.0
v                 3871         5506          393         >19.8
b                  583         6325          413         >20.5
u                  327         6120          639         >21.0
w1                4281         5915          393         >20.4
m2                4076         5710          393         >20.6
w2                5101         5301          197         >21.1

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: GRB130131B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14170
SUBJECT: GRB 130131B: IAC80 I-band observations
DATE:    13/02/01 04:09:46 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA/CSIC-UPV/EHU), L. Monteagudo Narvion (IAC), D. Malesani
(DARK/NBI), S. Schulze (PUC, MCSS), report on behalf of a larger
collaboration:

"We observed the GRB 130131B (Siegel et al., GCNC 14159) at the Swift/XRT
location reported in Goad et al. (GCNC 14165) with the 82cm IAC80
telescope at the Observatorio del Teide (Tenerife, Spain). I-band images
with a total exposure time of 13x250s were taken on Feb 1.0135-1.0832 UT
(5.2-6.8 hours post burst). No object brighter than I~21.2 mag (Vega,
calibrated against USNO B1.0 and not corrected for Galactic Extinction)
was detected inside the XRT error circle (Goad et al., GCNC 14165)."


GRB_name: GRB130131A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14171
SUBJECT: GRB 130131A: VLA 5.8 Ghz Detection
DATE:    13/02/01 11:22:34 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

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

"We observed the position of GRB 130131A (Grupe et al.;
GCN 14156) beginning 2013 Feb 1.28 (dt=0.7 d) at a
mean frequency of 5.8 Ghz with the Karl G. Jansky Very
Large Array.  We detect a source consistent  with the
enhanced Swift-XRT position (Evans et al.; GCN 14160)
with a flux of 38 (+/- 11) uJy.  The position of this radio
source is

 RA (J2000)    11:24:30.4  (+/- 0.2)
DEC (J2000)   +48:04:33.0  (+/- 1.5).

Follow-up observations at multiple frequencies are in progress.
We thank the VLA staff for their support."


GRB_name: GRB130131A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14172
SUBJECT: GRB 130131A: CARMA 3mm Observations
DATE:    13/02/01 12:56:17 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

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

"We observed the position of GRB 130131A (Grupe et al., GCN 14156) with
the Combined Array for Research in Millimeter Astronomy beginning
2013 Feb 1.3 UT (0.7 d post-burst) at a mean frequency of ~85 GHz.
Coincident with the Swift-XRT position (Evans et al., GCN 14160) and
the VLA 5.8 GHz position (Laskar et al., GCN 14171), we report
a preliminary detection of a radio source with a flux of ~0.5 mJy.
Further analysis is in progress.

We thank the CARMA staff for their support."


GRB_name: GRB130131B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14173
SUBJECT: GRB 130131B: GROND Upper limits
DATE:    13/02/01 14:07:31 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

F.Knust, K.Varela, J.Greiner (all MPE Garching) report on behalf of the
GROND team:

We observed the field of GRB 130131B (Swift trigger 547420; Siegel et al.,
GCN 14159) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 04:00 UT on February 1st, 9 hrs after the GRB
trigger, only 27 deg away from the moon. They were performed at an average
seeing of 2.9â€ and at an average airmass of 1.6.

We do not detect a source within the Swift-XRT error circle reported by
Goad et al. (GCN 14165) down to 3-sigma AB limiting magnitudes

g' > 23.4,

r' > 23.7,

i' > 23.4,

z' > 23.3,

J > 21.2,

H > 20.5 and

K > 19.7

The given limits 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)= 0.03mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130131B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14174
SUBJECT: GRB 130131B: VLT/X-shooter acquisition camera limits
DATE:    13/02/01 14:16:07 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

S. Schulze (PUC, MCSS), Z. Cano (U. Iceland), J. Hjorth, D. Malesani,
J. P. U. Fynbo, D. Xu (DARK/NBI) and N. R. Tanvir (U. Leicester) report 
on behalf of a larger collaboration:

We observed GRB 130131B (Siegel et al., GCN Circ. 14159) with ESO/VLT
X-shooter. Our observation began at 5:49 UT on 1 February, i.e. 10.7 hours
post burst. We imaged the field with the acquisition camera in the r' and z' bands
for 3x100 and 4x100 seconds, respectively.

We found no optical counterpart within the revised Swift/XRT X-ray error circle
reported in Goad et al. (GCN Circ. 14165) down to a limiting magnitudes of 
approximately 23.2 and 22.7 mag in r' and z' band, respectively. These 
measurements are given in the AB system and not corrected for foreground 
extinction.

We thank the ESO staff at Paranal, and in particular Maja Vuckovic and 
Stephane Brillant for quickly performing the observations.


GRB_name: GRB130131A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14175
SUBJECT: GRB 130131A - UKIRT confirmation of afterglow
DATE:    13/02/01 14:27:41 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), T.  Wold (JACH)
report on behalf of a larger collaboration:

We re-observed the field of GRB 130131A with the WFCAM camera on
UKIRT, beginning approximately 20.5 hr post-burst.  The source reported
by us previously (GCN 14157) is no longer detected in our provisional
reduction, indicating a fading of at least 2 mag in the K-band.  This confirms
the source as the afterglow of the GRB (consistent also with the radio detection
by Zauderer et al. GCN 14171).

We also report that the afterglow was faintly visible in a Z-band image
taken at UKIRT 2hr post-burst (in morning twilight), indicating that this
is likely not an extreme redshift event.


GRB_name: GRB130131B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14176
SUBJECT: GRB 130131B: Swift-XRT refined Analysis
DATE:    13/02/01 19:21:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 3.1 ks of XRT data for GRB 130131B (Siegel  et al. GCN
Circ. 14159),  from 117 s to 6.4 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN. Circ 14165).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.15 (+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 2.2 (+/-0.3). The
best-fitting absorption column is  4.2 (+1.3, -1.1) x 10^21 cm^-2, in
excess of the Galactic value of 2.8 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.9 x 10^-11 (7.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.2 (+1.3, -1.1) x 10^21 cm^-2
Galactic foreground: 2.8 x 10^20 cm^-2
Excess significance: 5.6 sigma
Photon index:      2.2 (+/-0.3)

If the light curve continues to decay with a power-law decay index of
1.15, the count rate at T+24 hours will be 1.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.7 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/00547420.

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


GRB_name: GRB130131A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14177
SUBJECT: GRB 130131A: RAPTOR Limits During Gamma-Ray Emitting Interval
DATE:    13/02/01 19:23:05 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

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

The RAPTOR network of robotic optical telescopes made observations of Swift
trigger 547407 (Grupe, et al., GCN 14156).  The burst location was within
the field of our wide-field monitor located in Maui, HI, which began a 10 s
integration of the location at 13:56:20.65 UT, 1.4 s before the Swift trigger
time and during the gamma-ray emitting interval.  During the period that the
BAT was detecting gamma-ray emission, from ~T-5 s to ~T+65 s (Palmer,
et al., GCN 14163), we have a total of four 10 s exposures with limiting
magnitudes of R~9.4 in moderate moonglow.  We do not detect the optical
counterpart (Tanvir et al., GCN 14157; Virgili et al., GCN 14158) in any of
our images.  Our 3-sigma limiting magnitudes are based on a comparison of
our unfiltered image to the Tycho-2 V-band catalog.


GRB_name: GRB130131A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14178
SUBJECT: GRB 130131A: RATIR optical and infrared upper limits
DATE:    13/02/01 23:07:03 GMT
FROM:    Ori Fox at UCB  <ofox@berkeley.edu>

Ori Fox (UCB), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander 
Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃˆ A. de
Diego (UNAM), Leonid Georgiev (UNAM), JesË™s GonzÂ·lez (UNAM),
Carlos RomÂ·n-ZË™Ã’iga (UNAM), Neil Gehrels (GSFC), and Harvey
Moseley (GSFC) report:

Under good weather conditions, we observed the field of GRB 130131A 
(Grupe, et al., GCN 14156) with the Reionization and Transients Infrared 
Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at 
the Observatorio AstronÃ›mico Nacional on Sierra San Pedro MÂ·rtir. An 
extremely red (K=16.4, J=19.4) afterglow candidate was detected by 
Tanvir, et al. (GCN 14157). We obtained approximately 2.83 hrs (ri) and 
1.07 hrs (ZYJH) of data from 2013 February 1.25 to 2023 February 1.42 
UTC (16.0 to 20.0 hrs after the BAT trigger)

We detect no source within the XRT error circle (Evans et al; GCN 14160) 
or at the position of the UKIRT source (GCN 14157). In comparison with 
SDSS DR8 and 2MASS, we derive the following upper limits (3-sigma) in 
the AB magnitude system:

r' > 23.8
i' > 23.3
Z > 22.2
Y > 21.8
J > 21.9
H > 21.5

The limits are consistent with the suggested fading of at least 2 mag in 
K-band (GCN 14175) measured at 20.5 hours.

These magnitudes are not corrected for Galactic extinction in the direction
of the GRB.

We thank the staff of the Observatorio AstronÃ›mico Nacional in San
Pedro MÂ·rtir.

-- 
Please make note of the new email address.
http://astro.berkeley.edu/~ofox/website/Homepage.html


GRB_name: GRB130131B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14179
SUBJECT: GRB 130131B: RATIR Upper Limits
DATE:    13/02/02 14:51:20 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico Ramirezâ€Ruiz (UCSC), Jos&eacute; A. de Diego
(UNAM), Leonid Georgiev (UNAM), Jes&uacute;s Gonz&aacute;lez (UNAM), Carlos
Rom&aacute;n-Z&uacute;&ntilde;iga (UNAM), Neil Gehrels (GSFC), and Harvey
Moseley (GSFC) report:

We observed the field of GRB 130131B (Siegel et al., GCN 14159) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron&oacute;mico
Nacional on Sierra San Pedro M&aacute;rtir. Between 2013 February 1.42 and
2013 February 1.54 UTC (14.86 to 17.70 hrs after the BAT trigger), we
obtained 1.96 hrs exposure in the r and i bands and 0.73 hrs exposure in
the Z, Y, J, and H bands.

We detect no source within the XRT error circle (Goad et al., GCN 14165).
In comparison with SDSS DR8 and 2MASS, we derive the following upper limits
(3-sigma) in the AB magnitude system:

 r' > 23.8
 i' > 23.1
Z > 22.1
Y > 21.7
J  > 21.8
H > 21.4

These magnitudes are not corrected for Galactic extinction in the direction
of the GRB.

We thank the staff of the Observatorio Astron&oacute;mico Nacional in San
Pedro M&aacute;rtir.


GRB_name: GRB130131A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14180
SUBJECT: GRB 130131A: Swift/UVOT Upper Limits
DATE:    13/02/02 15:19:38 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 130131A
68 s after the BAT trigger (Grupe et al., GCN Circ. 14156).
No optical afterglow consistent with the optical position (Tanver et al.,
GCN Circ 14157) or XRT position (Evans et al., GCN Circ. 14160)
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            68          217          147         >21.8
u_FC               280          529          246         >20.8
white               68         7570          839         >22.5
v                  609        18681         1378         >21.0
b                  535         7369          549         >21.7
u                  280        13670         1434         >22.0
w1                 658        12906         1434         >21.7
m2                1932        18851         1263         >21.3
w2                 758        17768         1336         >22.0

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: GRB130206A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14181
SUBJECT: GRB 130206A: Swift detection of a burst
DATE:    13/02/06 19:43:58 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

M. De Pasquale (UCL-MSSL), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), S. R. Oates (UCL-MSSL),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and V. N. Yershov (UCL-MSSL) report on
behalf of the Swift Team:

At 19:36:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130206A (trigger=547918). 
The BAT on-board calculated location is 
RA, Dec 140.375, -58.160 which is 
   RA(J2000) = 09h 21m 30s
   Dec(J2000) = -58d 09' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked 
structure with a total duration of about 50 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~4 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+48.5
minutes. There will be no XRT or UVOT data until this time. 

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


GRB_name: GRB130131A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14182
SUBJECT: GRB 130131A: optical observation in Mondy observatory
DATE:    13/02/06 20:27:48 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 130131A (Grupe et al., GCN 14156) 
with AZT-33IK telescope of Sayan observatory (Mondy). We took several 
images in R-filter of 60 s exposure on Jan. 31, between (UT) 
14:12:36-15:36:53 under favorable weather conditions with a FWHM of 
about  2.5". In the stacked images we detected a source which is 
coincident with the source reported by Tanvir et al. (GCN 14157). The 
photometry based on SDSS DR8 is the following:

  t_start,      T0+ (mid), filter,  exp.,   OT+/-err      UL (3 sigma)
  (UT)          d                   s

  14:12:36      0.01640    R       10x60    22.5 +/-0.35  22.4
  14:12:36      0.04053    R       79x60    23.4 +/-0.25  23.5

Taken coincidence with source detected in IR (Tanvir et al. GCN 14157) 
and fading nature of the source we suggest that we detect OT of GRB 
130131A. The detection in R filter confirms that the GRB 130131A is not
an extreme redshift event (Tanvir et al. GCN 14175). Also we compared 
fluxes in X-ray and optic at ~0.016 days after trigger and found that 
the GRB 130131A can be considered as  optically dark burst following the 
both criteria (Jakobsson et al., 2004; van der Horst et al., 2009).

The stars used for photometry and assumed R mags:

J112419.01+480710.6 11:24:19.01 +48:07:10.7 R = 18.93
J112414.86+480528.8 11:24:14.86 +48:05:28.9 R = 18.77
J112419.60+480357.4 11:24:19.61 +48:03:57.5 R = 20.32

The finding chart of the stacked image can be found in 
http://grb.rssi.ru/GRB130131A/GRB130131A_130131_AZT33IK.png


GRB_name: GRB130206A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14183
SUBJECT: GRB 130206A: Swift-XRT observations
DATE:    13/02/06 21:22:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 130206A at 20:27:46.2 UT,
3077.7 seconds after the BAT trigger. No source was detected in 1.9 ks
of promptly downlinked data. We are waiting for the full dataset to
detect and localise the XRT counterpart.


GRB_name: GRB130206A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14184
SUBJECT: Swift GRB 130206A - analysis of Swift/UVOT initial data.
DATE:    13/02/06 22:32:32 GMT
FROM:    Patricia Schady at MPE/Swift  <msslba@googlemail.com>

M. De Pasquale (MSSL-UCL) on behalf of the Swift/UVOT team reports:

UVOT took a finding chart exposure of 150 seconds with the White
filter starting 3080 seconds after the BAT trigger. No credible
candidates have been identified in the initial data products. The
8'x8' region for the list of sources generated on-board covers about
86% of the BAT error circle. The list of sources is typically complete
to about 18 mag.

The GRB occurred in a crowded field only 5.8 deg from the Galactic Plane.

No correction has been made for the expected extinction corresponding to
E(B-V) of 0.49.


GRB_name: GRB130206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14185
SUBJECT: GRB 130206A: Zadko observatory - Gingin optical observations
DATE:    13/02/06 22:44:26 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 (IRAP-CNRS-OMP), 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 130206A detected by SWIFT
(trigger 547918) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 106s after the GRB trigger
(73s after the notice). The elevation of the field
decreased from 48 degrees above horizon and weather
conditions were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT in the BAT error box with a
limiting magnitude of:
t0+106s to t0+166s : R > 16.5

The second image is 30.0s exposure in tracking mode:
t0+187s to t0+217s : R > 18.3

We co-added a series of images in tracking mode:
t0+187s to t0+482s : R > 20.1

The analysis was made by substraction with images
acquired one hour later.

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

N.B. Galactic coordinates are lon=278.0587 lat=-5.8228
and the corresponding galactic absorption in R band
should be about 1.1 mag (Schlegel et al. 1998).

This message may be cited.


GRB_name: GRB130206A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14186
SUBJECT: GRB 130206A, Swift-BAT refined analysis
DATE:    13/02/07 13:51:11 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), M. De Pasquale (UCL-MSSL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D.
M. Palmer (LANL), T. Sakamoto (AGU), 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 130206A (trigger #547918)
(De Pasquale, et al., GCN Circ. 14181).  The BAT ground-calculated position is
RA, Dec = 140.387, -58.193 deg which is
     RA(J2000)  =  09h 21m 32.9s
     Dec(J2000) = -58d 11' 35.6"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 52%.

The mask-weighted light curve shows two clusters of peaks. The first runs from
approximately T-10 sec to T+15 sec and the second from T+20 sec to T+60 sec,
though the count rate does not return to baseline between the two clusters.
Each of these clusters consists of multiple sub-peaks.  There is also some
low-level emission extending out to T+150 sec. T90 (15-350 keV) is
128.0 +- 50.6 sec (estimated error including systematics).

The time-averaged spectrum from -12.78 to 147.21 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.17.  The fluence in the 15-150 keV band is 2.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+42.72 sec in the 15-150 keV band is
0.3 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/547918/BA/


GRB_name: GRB130131B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14187
SUBJECT: GRB 130131B: optical upper limit in Mondy observatory
DATE:    13/02/07 15:20:15 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 130131B (Siegel et al., GCN 
14159) with AZT-33IK telescope of Sayan observatory (Mondy) on Jan. 31 
between (UT) 19:51:32-20:51:58. We took several images in R-filter of 60 
s exposure. Within enhanced XRT position (Goad et al., GCN 14165) we do 
not detect any source in a combined image. Photometry is based on nearby 
SDSS DR8 stars.

UT start,    t-t0           filter      Exp.   OT      UL (3 sigma)
             (mid, days)                (s)

19:51:32     0.04973        R          60x60   n/d     22.5


GRB_name: GRB130206A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14188
SUBJECT: GRB 130206A: XRT and UVOT follow-up observations.
DATE:    13/02/07 20:22:53 GMT
FROM:    MSSL Swift/UVOT team at MSSL/Swift  <msslba@googlemail.com>

Andy Beardmore (Univ. Leicester), A. Breeveld (MSSL-UCL) and M. De
Pasquale (MSSL-UCL) on behalf of the Swift team, report:

The Swift-XRT began observing the field of GRB130206A (De Pasquale et al.,
GCN Circ. 14181) in photon counting  mode at 2013-02-06 20:28 UT, 3090 s
after the trigger. In 10.3 ks of data we find a faint source at RA, Dec =
140.37670, -58.19362 which is equivalent to

RA  (J2000) = 09h 21m 30.41s
Dec (J2000) = -58d 11' 37.0"

with an uncertainty of 5.6 arcseconds (radius, 90% confidence). The
source is located 20 arcseconds from the BAT refined position
(Stamatikos et al, GCN Circ, 14186), within the BAT error circle.

The source is detected at a count rate of 0.0017 Â± 0.0006 count/s. We
cannot tell if it is fading at this time.

The Swift/UVOT began settled observations of the field of GRB130206A
3081 s after the BAT trigger.
No optical afterglow consistent with the XRT position is detected in the
initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(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       3081          3231           147         >21.4
white             3081        16409         2114         >23.1
v                   4062        22199         1319         >20.3
b                   3445        15497         1278         >22.3
u                   3239        28222           634         >21.2
w1                4473         27971         1082         >21.0
m2                4268        27065         1312         >20.7
w2                3857         32412         2546         >21.3

The magnitudes in the table are not corrected for the strong Galactic
extinction due to the reddening of E(B-V) = 0.48 in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB130206A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14189
SUBJECT: GRB 130206A: Fermi GBM observation
DATE:    13/02/07 22:21:38 GMT
FROM:    Adam Goldstein at Fermi-GBM/UAH  <adam.m.goldstein@msfc.nasa.gov>

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

At 19:36:30.45 UT on 06 February 2013, the Fermi Gamma-Ray 
Burst Monitor triggered and located GRB 130206A 
(trigger 381872193 /130206817) which was also detected by 
the Swift/BAT (De Pasquale et al. 2013, GCN 14181).  The GBM 
on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 19 degrees.

The GBM light curve consists of three overlapping pulses 
with a duration (T90) of about 91 s (50-300 keV). The 
time-averaged spectrum from T0=-1.5 s to T0+85.6 s is 
adequately fit by a power law function with an exponential 
high-energy cutoff.  The power law index is -1.1 +/- 0.2 and 
the cutoff energy, parameterized as Epeak, is 132.6 +/- 34.0 keV.

The event fluence (10-1000 keV) in this time interval is 
(3.3 +/- 0.4)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.8 s in the 10-1000 keV band is 
2.1 +/- 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: GRB130206A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14190
SUBJECT: GRB 130206A: Fermi LAT Observations
DATE:    13/02/07 23:11:00 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

J. L. Racusin (NASA/GSFC), G. Vianello (Stanford), N. Omodei (Stanford), and D. Kocevski (NASA/GSFC), report on behalf of the Fermi-LAT team:

The Fermi Large Area Telescope (LAT) observed GRB 130206A, detected by Fermi-GBM (Goldstein et al., GCN 14189) and Swift-BAT (De Pasquale et al., GCN 14181).

The burst location was within the LAT field of view at an angle of ~19.4 degrees to the LAT boresight, and had a zenith angle of 69 degrees. No significant excess is seen using standard analysis procedures.  The burst exited the nominal LAT field of view roughly ~600 s after the GBM trigger.  

We estimate the 95% confidence upper limits in the energy range of 100 MeV - 10 GeV, assuming spectral index of -2.1, over the time interval 0-40 s:
F(100MeV-10GeV)  < 3.7e-05 (ph/cm^2/s)
                                    <1.5e-02  (MeV/cm^2/s)
                                    <2.4e-08 (erg/cm^2/s)

Using the non-standard LAT Low Energy (LLE) data selection, >60 counts above background were observed in a single FRED like pulse, peaking ~15 s after the GBM trigger.  This corresponds to a significance of 2.9 sigma without taking into account trial factors, and therefore does not constitute a clear detection. On the other hand, the putative signal shows good correlation with the low-energy (GBM) light curve. Such faint signal is constituted by low energy gamma-rays, below 75 MeV, and therefore has insufficient spatial resolution to provide a reliable LAT localization. Indeed, no events were observed above 75 MeV using the standard analysis classes.

The Fermi LAT point of contact for this burst is Judith Racusin (judith.racusin@nasa.gov).

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


GRB_name: GRB130206A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14191
SUBJECT: GRB 130206A: GROND Observations
DATE:    13/02/08 19:20:31 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

F. Knust (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 130206A (Swift trigger 547918; De Pasquale
et al.,GCN 14181) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla
Observatory (Chile).

The first observations started at 01:10 UT on 07 Feb 2013, 6.5 hrs after
the GRB trigger, and a second epoch was taken at 7:47 UT on 8 Feb 2013.
These observations were performed at an average seeing of 1.4/1.0 arcsec
and at an average airmass of 1.3/1.4.

We detect three sources within the 5.6 arcsec Swift-XRT error circle
(Beardmore et al., GCN 14188), at positions:

Source 1
RA (2000.0) = 09h 21m 30.45s
Decl. (2000.0) = -58d 11' 34.7"

Source 2
RA (2000.0) = 09h 21m 30.10s
Decl. (2000.0) = -58d 11' 36.5"

Source 3
RA (2000.0) = 09h 21m 30.14s
Decl. (2000.0) = -58d 11' 41.2"

with an uncertainty of 0.5" in each coordinate.

For the aforementioned three sources, the preliminary photometry does
not show any variability. Image subtraction between the two epochs
has revealed no residuals either.

Based on exposures of 42 min in g'r'i'z' and  54 min in JHK,
we do not detect the afterglow  within the 5.6" XRT error circle
to the following  3-sigma upper limits (AB system):


g' > 24.7,
r' > 24.6,
i' > 23.8,
z' > 23.8,
J > 21.6,
H > 21.2 and
K > 20.6

The given limits are derived based on calibrating the images against GROND
zeropoints and 2MASS field stars and are not corrected for the Galactic
foreground extinction corresponding to a reddening of E_(B-V)= 0.5 in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14192
SUBJECT: GRB 130122A: PTF P48 optical upper limits
DATE:    13/02/09 15:33:37 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (UC Berkeley), and D. A. Brown
(Syracuse) report on behalf of a larger collaboration:

We have imaged the 3-sigma Swift UVOT error circle (P. Evans, GCN
14143) of GRB130122A (Swift546731, S. Barthelmy, GCN 14140) with the
Palomar 48 inch Oschin telescope (P48) as part of the Palomar
Transient Factory (PTF).  Images were obtained in the Mould R filter
at 2013-01-23 at 06:27:39 and 07:11:25 UTC, 6.7 and 7.5 hours after
the trigger.

With sporadic cloud cover and a bright moon, we find no point source,
fading or otherwise, to 5-sigma limiting magnitudes of 19.1 and 18.4.


GRB_name: GRB130131B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14193
SUBJECT: GRB 130131B: MITSuME Akeno Optical upper limits
DATE:    13/02/10 13:58:00 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

M. Hayashi, T. Yoshii, R. Usui, Y.Aoki, S. Kurita,
Y. Saito, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed GRB 130131B (Siegel et al., GCNC 14159) 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 2013-01-31 19:10:57 UT (~49 sec after
the burst). And we could not find any new point source within the XRT
error circle in all the three bands.
The results of photometry (3 sigma upper limits) are listed below.

The photon flux were calibrated against GSC2.3 catalog.

T0+[sec]   MID-UT   T-EXP[sec]    g'           Rc          Ic
-------------------------------------------------------------------------------------------
     70       19:12:07       60        >16.4   >16.4   >16.2
    178      19:13:55      240       >17.4   >17.6   >17.4
   1183     19:30:40      1320      >18.6   >19.0   >18.9
   2769     19:57:06     4200       >19.1   >19.6   >19.5
-------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130131A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14194
SUBJECT: GRB 130131A: MITSuME Akeno Optical upper limits
DATE:    13/02/10 14:00:06 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

M. Hayashi, T. Yoshii, R. Usui, Y.Aoki, S. Kurita,
Y. Saito, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed GRB 130131A (Grupe et al., GCNC 14156) 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 2013-01-31 13:57:11 UT ( ~49 sec after
the burst). And we could not find any new point source within the XRT
error circle in all the three bands.
The results of photometry (3 sigma upper limits) are listed below.

The photon flux were calibrated against GSC2.3 catalog.

T0+[sec]   MID-UT   T-EXP[sec]    g'           Rc          Ic
-------------------------------------------------------------------------------------------
     33       13:57:44      60        >17.6   >17.8   >17.1
    159      13:59:51      270      >18.5   >18.6   >18.0
   1105     14:15:46      1440     >19.0   >19.4   >18.9
   7119     15:56:00      9540     >19.9   >20.6   >19.8
-------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130211A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14195
SUBJECT: GRB 130211A: Swift detection of a burst
DATE:    13/02/11 03:58:20 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 03:36:32 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130211A (trigger=548276).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 147.523, -42.339 which is 
   RA(J2000)  =  09h 50m 05s
   Dec(J2000) = -42d 20' 18"
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 20 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 03:38:26.0 UT, 113.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 147.53605,
-42.34244 which is equivalent to:
   RA(J2000)  = 09h 50m 08.65s
   Dec(J2000) = -42d 20' 32.8"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 36 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.16
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 7.98e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 125 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. 
Results 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 0.54. 

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


GRB_name: GRB130211A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14196
SUBJECT: GRB 130211A: GROND detection of the afterglow
DATE:    13/02/11 09:50:35 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

F. Knust, J. Greiner, and V. Sudilovsky (all MPE Garching) report on 
behalf of
the GROND team:

We observed the field of GRB 130211A (Swift trigger 548276; Oates et al.,
GCN 14195) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 03:45 UT on 11.02.2013, 9 min after the GRB trigger.
They were performed at a seeing improving over time from 3" to 1.2", and at
an average airmass of 1.0.

We find one variable source inside the 4.0" error circle, at coordinates
RA (2000.0) = 09:50:08.736
Decl (2000.0) = -42:20:32.64
with an error of 0.3".

Based on 1500s exposure in g'r'i'z' and 1200s in JHK started at 06:09 UT,
we estimate preliminary AB magnitudes of:

g' >  25.3 mag,
r' =  23.5 +- 0.1 mag,
i' =  22.2 +- 0.1 mag,
z' =  21.7 +- 0.1 mag,
J =  20.6 +- 0.2 mag,
H =  20.1 +- 0.2 mag, and
K >  19.5 mag.

Given magnitudes are calibrated against GROND zeropoints (g'r'i'z') as well
as 2MASS field stars (JHK) and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=0.53 mag in
the direction of the burst (Schlegel et al. 1998).

After correcting for the expected foreground extinction, the spectral 
energy distribution of this source
is well-fit by a power-law with slope b~1.4. The reduced flux in g' and 
r' imply a redshift of z~4.3.


GRB_name: GRB130211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14197
SUBJECT: GRB 130211A: Swift-BAT refined analysis
DATE:    13/02/11 13:32:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
S. R. Oates (UCL-MSSL), D. M. Palmer (LANL), T. Sakamoto (AGU),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130211A (trigger #548276)
(Oates, et al., GCN Circ. 14195).  The BAT ground-calculated position is
RA, Dec = 147.524, -42.330 deg which is 
   RA(J2000)  =  09h 50m 05.7s 
   Dec(J2000) = -42d 19' 47.1" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 40%.
 
The mask-weighted light curve shows multiple, weak, overlapping peaks
starting at ~T-10 sec, peaking at ~T-2 sec, and ending at ~T+30 sec.
T90 (15-350 keV) is 25.1 +- 6.3 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.56 to T+32.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.81 +- 0.24.  The fluence in the 15-150 keV band is 6.4 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-1.58 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/548276/BA/


GRB_name: GRB130211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14198
SUBJECT: GRB 130211A: Swift-XRT refined Analysis
DATE:    13/02/11 18:58:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), O.M. Littlejohns (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), A. Melandri (INAF-OAB), B.
Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC), J.A. Kennea (PSU), M.C.
Stroh (PSU) and S.R. Oates report on behalf of the Swift-XRT team:

We have analysed 9.2 ks of XRT data for GRB 130211A (Oates  et al. GCN
Circ. 14195),  from 120 s to 29.1 ks after the BAT trigger. The data
comprise 201 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
147.53616, -42.34237 which is equivalent to:

RA (J2000): 09 50 08.68
Dec(J2000): -42 20 32.5

with an uncertainty of 3.6 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=2.85 (+0.27, -0.23).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.55 (+/-0.14). The
best-fitting absorption column is  5.9 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 2.2 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 2.5 x 10^-11 (2.3 x 10^-10) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      5.9 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: 15.9 sigma
Photon index:      3.55 (+/-0.14)

If the light curve continues to decay with a power-law decay index of
2.85, the count rate at T+24 hours will be 1.3 x 10^-7 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.3 x
10^-18 (3.1 x 10^-17) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00548276.

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


GRB_name: GRB130211A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14199
SUBJECT: GRB 130211A: Swift/UVOT Upper Limits
DATE:    13/02/11 21:58:48 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130211A
125 s after the BAT trigger (Oates et al., GCN Circ. 14195).
No optical afterglow consistent with the optical position
(Knust et al. GCN Circ. 14196) 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           125          275          147         >21.8
white              125        17061         1076         >22.9
v                 4470        22933         1646         >21.7
b                 3854        16303         1278         >22.4
u                  284        29091          650         >21.3
w1                4880        28760         1082         >21.8
m2                4674        27853         1175         >21.6
w2                4265        22020         1968         >22.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.53 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14200
SUBJECT: GRB 121123A: optical observations
DATE:    13/02/13 16:34:45 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

Yu. Krugly (Institute of Astronomy of Kharkiv National University), 
R.Inasaridze, O. Kvaratskhelia(Abastumani Astrophysical Observatory), 
I. Molotov (KIAM), A. Pozanenko (IKI)  report on behalf of  larger GRB 
follow-up collaboration:

We observed the field of the Swift GRB 121123A (Helder et al., GCN 
13982) with AC-32 (0.7m Maksutov) telescope of Abastumani Observatory, 
starting on Nov. 23 (UT) 15:18. We took several unfiltered images of 180 
s exposure. We clearly detected the afterglow (Helder et al., GCN 13982; 
Zhao et al., GCN 13983) in every  single image. The photometry of the 
stacked images is based on USNO-B1.0 stars (R2):

Start,    T0+,        Filter,   Exp.,  OT
(UT)      (mid),days

15:18:28  0.2229      none      4x180  19.01 +/- 0.10
15:33:10  0.2337      none      4x180  18.96 +/- 0.09
15:48:15  0.2448      none      4x180  18.88 +/- 0.08
16:02:57  0.2551      none      4x180  19.17 +/- 0.11
16:02:57  0.2642      none      4x180  18.94 +/- 0.10
16:28:40  0.2729      none      4x180  19.06 +/- 0.11


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14201
SUBJECT: GRB 121128A: optical observations
DATE:    13/02/13 16:37:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

Yu. Krugly (Institute of Astronomy of Kharkiv National University), 
R.Inasaridze, O. Kvaratskhelia(Abastumani Astrophysical Observatory), 
I. Molotov (KIAM), A. Pozanenko (IKI)  report on behalf of  larger GRB 
follow-up collaboration:

We observed the field of the Swift Swift GRB 121128A (Oates et al., GCN 
14007)with AC-32 (0.7m Maksutov) telescope of Abastumani Observatory, 
starting on Nov. 28 (UT) 15:28. We took several unfiltered images of 300 
s exposure. We detected the afterglow (Oates et al., GCN 14007; Japelj 
et al., GCN 14008) in stacked images. The photometry of a the stacked 
image is based on USNO-B1.0 stars (R2):

Start,    T0+,        Filter,   Exp.,  OT
(UT)      (mid),days

15:27:50  0.4479      none      9x300  20.24 +/- 0.12
16:18:59  0.4853      none      8x300  20.35 +/- 0.16
17:09:58  0.5208      none      8x300  20.38 +/- 0.18
18:01:17  0.5544      none      9x300  20.55 +/- 0.22
18:46:44  0.5871      none      8x300  20.84 +/- 0.36


GRB_name: GRB130131B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14202
SUBJECT: GRB 130131B: CTIO 0.9-m optical upper-limits
DATE:    13/02/13 18:57:53 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

D. Caldern Espinoza, B. Indahl, L. Paredes Alvarez, C. Kaleida (CTIO), and F. J. Virgili (LJMU) report:

"As part of the REU/PIA student program at the Cerro Tololo Inter-American Observatory (CTIO) we observed
GRB 130131B (Siegel et al., GCN 14159) with the SMARTS 0.9-m telescope beginning 11.6 hrs after the Swift
trigger.  No optical counterpart is detected within the XRT error circle to the following conservative limits:

Midtime of exposure     Exposure time     Filter     Magnitude
--------------------------------------------------------------------------
      12.7 hr               7x450s            R        > 20.7
      12.8 hr               7x450s            V        > 20.3
--------------------------------------------------------------------------

Magnitudes are calibrated using nearby USNOB-1 (R-band) and NOMAD (V-band) stars."


GRB_name: GRB130206A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14203
SUBJECT: Swift GRB130206A: late XRT observations.
DATE:    13/02/14 21:58:20 GMT
FROM:    MSSL Swift/UVOT team at MSSL/Swift  <msslba@googlemail.com>

M. De Pasquale (MSSL-UCL), A. Beardmore (Univ. Leicester) report, on behalf
of the Swift team:

The X-ray source described in GCN circ. 14188 (Beardmore et al. 2013) is not
detected anymore in XRT observations performed between 33 and 550 ks after
the trigger, for a total of 35.2 ks of integration time. The 3 sigma upper limit is
0.00089 count/s, appreciably lower than the count rate observed in previous
observations.

Because of the fading behaviour of this source, we conclude it was likely
the X-ray afterglow of GRB130206A.

We also note that successive analysis of late data has reduced the error circle
radius of the source to 4.6'' (90% confidence level).


GRB_name: GRB130215A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14204
SUBJECT: GRB 130215A: Swift detection of a burst
DATE:    13/02/15 01:50:26 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (NASA/GSFC) and B. Sbarufatti (INAF-OAB/PSU) report on
behalf of the Swift Team:

At 01:31:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130215A (trigger=548760).  Swift did not slew because of Moon constraint. 
The BAT on-board calculated location is 
RA, Dec 43.479, +13.371 which is 
   RA(J2000)  =  02h 53m 55s
   Dec(J2000) = +13d 22' 14"
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 40 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 14:00 UT on 2013 February 18. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB130215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14205
SUBJECT: GRB 130215: ROTSE-III Detection of Optical Counterpart
DATE:    13/02/15 01:54:24 GMT
FROM:    Heather Flewelling at IfA/Hawaii  <flewelling.heather@gmail.com>

W. Zheng (UC Berkeley), H. Flewelling (IfA/Hawaii), report on behalf of the
ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 130215
(Swift trigger 548760). The first image was at 01:43:07.3 UT, 697.1 s after
the burst (8.3 s after the GCN notice time). The unfiltered images are
calibrated relative to USNO A2.0. We detect a new object, not visible in
the DSS (second epoch), with coordinates:

     02:54:00.7      +13:23:43.7    (J2000), with positional uncertainty of
1" or better

start UT     mag     mlim(of image)
----------------------------------
01:43:07.3     14.2     16.2


A jpeg image is available at
http://www.rotse.net/images/gsb548760_3b00_img.jpg Note that the object
marked 8 is the candidate in question.

Continuing observations are in progress.


GRB_name: GRB130215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14206
SUBJECT: Skynet Observations of GRB130215
DATE:    13/02/15 02:55:19 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

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

Skynet began observing the field of GRB130215A (Swift trigger 548760, GCN 
14204) in BVRI beginning ~12 minutes after the burst using four of the 
PROMPT telescopes located at CTIO in Chile, and the DSO-14 telescope and 
Morehead telescope in North Carolina, USA.  A bright, fading source is 
detected at the position reported by the ROTSE group (GCN 14205.)

Calibrating to several nearby USNO B1.0/NOMAD stars, we find the following 
initial magnitudes:

Filt    Time    Mag
B       15.4m 15.4 
V 15.4m 14.5
R       13.0m 13.8
I       15.5 13.3


The object has set in Chile, but further observations from the Northern 
hemisphere telescopes are ongoing.


GRB_name: GRB130215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14207
SUBJECT: GRB 130215A: Redshift estimate
DATE:    13/02/15 02:57:36 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick), M. Fumagalli (Carnegie Observatory/
Princeton University), report on behalf of a larger collaboration 
reports:

On February 15.1 UT (~50 minutes after the BAT trigger) we observed 
the field of GRB 130215A (D'Elia et al., GCN 14204, Zheng et al GCN 
14205) using the KAST Spectrograph on the Lick Shane 3-m telescope.  

The optical candidate is clearly detected.
We obtained a 2x600s spectrum, covering the wavelength range 3500-8000A

The spectrum reveals strong absorption lines of MgII2796, MgII2803,
MgI2853, FeII2586, FeII2600, and Ca H&K.  
A provisional reduction gives a redshift of z=0.597, which we believe 
is most likely the redshift of this burst.
 
We thank the Lick Observatory staff for their prompt support.


GRB_name: GRB130215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14208
SUBJECT: GRB 130215A: ROTSE-III data analysis
DATE:    13/02/15 04:07:03 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

W. Zheng (UC Berkeley), H. Flewelling (IfA/Hawaii), T. Guver (Sabanci
U), F. Yuan (Australian National University), report on behalf of the
ROTSE collaboration: 

Further analysis of ROTSE-IIIb data revealed that the OT of GRB 130215A
(Swift trigger 548760; D'Elia et al., GCN 14204; Zheng et al GCN 14205;
LaCluyze et al. 14206) peaked around 750s after the burst, followed with
a single power-law decay with index alpha = -1.24 up to ~4ks after the
burst. Observation is on going.
 
Interestingly the GRB is also triggered by Fermi-GBM (trigger
382584689). The GBM trigger arrived ~600s earlier than Swift-BAT trigger
and ROTSE-IIIb responded to GBM trigger at first. A 4x4 tiling follow-up
mode was performed before BAT-trigger interrupted it and a total of 22
images were obtained to GBM trigger. Unfortunately, our effort of the
tiling follow-up still didn't cover the OT location in these images
since the GBM trigger is about 3.78 degree away, just a bit away from
one of the corner. 


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14209
SUBJECT: GRB 130215A: P60 Observations
DATE:    13/02/15 04:15:55 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

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

We imaged the location of the Swift GRB130215A (D'Elia et al., GCN 14204)
with the robotic Palomar 60 inch telescope.  Images were obtained in the
SDSS r', i', and z' filters beginning at 02:29 UT on 2013 Feb 15 (~ 1 hr
after the Swift trigger).

We detect a bright point source at the location of the optical counterpart
(Zheng et al., GCN 14205) in all filters.  Using several nearby point
sources from the USNO-B1 for reference, we measure a magnitude of R = 15.9
at this time.

Observations are ongoing.


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14210
SUBJECT: GRB 130215A: CARMA 3mm detection
DATE:    13/02/15 06:21:53 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and G. Keating (UC Berkeley) report on behalf of 
a larger collaboration:

We began observations of the position of GRB 130215A (D'Elia et al., GCN 
14204) with the Combined Array for Research in Millimeter Astronomy at a 
frequency of 93 GHz (3mm) starting at 03:28 UT, 1.95 hours after the 
burst.  Observations continued until 05:03 UT (midpoint t=2.73 hours.)

A provisional reduction of the data shows a strong detection of a source 
consistent with the location of the optical afterglow (Zheng et al., GCN 
14205).  We estimate a preliminary flux at this time of 2.99 +/- 0.39 
mJy.  Follow-up observations are planned.

We thank the CARMA staff for executing these rapid observations.


GRB_name: GRB130215A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14211
SUBJECT: GRB 130215A: REM NIR observations
DATE:    13/02/15 06:38:27 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, D. Fugazza, V. d'Elia,  on behalf of the REM team report:

We imaged the field of GRB130215A (D'Elia et al., GCN 14204) with the
REM NIR camera with the J, Hand Ks filters.
Observations started at 2013/02/15 01:43:21, i.e. about 12 min after
the prompt event.
The optical counterpart detected by ROTSE-IIIb (Zheng et al., GCN
14205) was well detected and still fairly bright at H=11.6+-0.1
(preliminary calibration) at the beginning of our observations.

[GCN OPS NOTE(14may13): Per author's request, the line
"2013/02/15 01:38:40, i.e. about 7 min"
was changed to 
"2013/02/15 01:43:21, i.e. about 12 min", due to a clock error correction.]


GRB_name: GRB130215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14212
SUBJECT: GRB 130215A: RATIR Optical and NIR Observations
DATE:    13/02/15 10:48:09 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Antonino Cucchiara (UCSC), William H. Lee (UNAM),
Alexander Kutyrev (GSFC), Alan M. Watson (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Eleonora Troja (GSFC), Enrico Ramirezâ€Ruiz (UCSC), JosÃ© A. de Diego
(UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga
(UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 130215A (D'Elia et al.; GCN 14204) 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 2013/02 15.13 to 2013/02 15.18 UTC (1.58 to
2.88 hours after the BAT trigger) through intermittent clouds, obtaining a
total of 25 minutes of useful exposure in the r' and i' bands and 19
minutes of useful exposure in the Z and J bands.

We detect the optical counterpart discovered by ROTSE (Zheng et al.; GCN
14205).   In comparison with USNO-B1 and 2MASS, we derive the following
magnitudes in the AB system:

  r' = 17.86 +/- 0.05
  i' = 17.10 +/- 0.04
  Z = 16.86 +/-0.04
  J = 16.67 +/- 0.04

These magnitudes are not corrected for Galactic extinction in the direction
of the GRB.  Compared to the earlier observation at Palomar (Cenko et al;
GCN 14209), our r band magnitude implies a temporal fade by >1 mag on a
timescale of 2 hours, with a corresponding power law fade f ~ t^(-1.5)
between 1 and 3 hours after the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14213
SUBJECT: GRB 130215A: TAROT La Silla observatory optical observations
DATE:    13/02/15 11:08:54 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@gmail.com>

Gendre B. (Artemis/IRAP), Dereli, H. (Artemis/OCA), Atteia J.L. 
(IRAP-CNRS-OMP), Boer M. (UNS-CNRS-OCA), Klotz A. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130215A detected by SWIFT (trigger 548760,
D'Elia et al., GCN 14204) with the TAROT robotic telescope located at 
the European Southern Observatory, La Silla observatory, Chile.

The observations started 15.5s after the GCN notice (704.3s after the
SWIFT trigger). The elevation of the field decreased from 20 degrees 
above horizon and weather conditions were good.

At the position reported by Zheng et al. (GCN 14205) we clearly detect
the afterglow between 704s and 5481 seconds after the trigger. We also
confirm the peak in the light curve around 750s post-trigger announced
by Zheng et al. (GCN 14208).

We obtained the following magnitudes, calibrated with three different
USNO-B1 objects (statistical 3 sigma errors are of the order of
0.1-0.2), and not corrected for galactic extinction.


MidTime (s) R mag
719 13.8
1192 14.4
1795 15.0
2723 15.7
4439 16.3

N.B. Galactic coordinates are lon=163.0747 lat=-39.7685 and the galactic 
extinction in R band is 0.3 magnitudes estimated from D. Schlegel et al. 
1998ApJ...500..525S.


This message may be cited.


GRB_name: GRB130215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14214
SUBJECT: GRB 130215A: Swift-BAT refined analysis
DATE:    13/02/15 13:03:30 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),
V. D'Elia (ASDC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130215A (trigger #548760)
(D'Elia, et al., GCN Circ. 14204).  The BAT ground-calculated position is
RA, Dec = 43.486, 13.387 deg which is 
   RA(J2000)  =  02h 53m 56.7s 
   Dec(J2000) = +13d 23' 13.6" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 8%.
 
The mask-weighted light curve starts at ~T-10 sec, peaks at ~T+10 sec,
and slowly returns to baseline at ~T+170 sec.
T90 (15-350 keV) is 65.7 +- 10.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-5.83 to T+73.38 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.59 +- 0.14.  The fluence in the 15-150 keV band is 5.4 +- 0.5 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+11.16 sec in the 15-150 keV band
is 2.5 +- 0.7 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/548760/BA/

We note that the BAT trigger occurred during a telemetry downlink session
during which the real-time TDRSS messages (that GCN uses) are buffered on-board
until the end of the downlink.  For this trigger the minimum bufferring delay
to the ground was 692 sec.


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14215
SUBJECT: GRB 130215A: Xinglong optical observations
DATE:    13/02/15 13:14:33 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI) and T.M. Zhang (NAOC) report on behalf of a larger
collaboration

We observed the field of GRB 130215A (D'Elia et al., GCN 14204) using
the Xinglong 2.16m telescope, located in Heibei China and equipped
with the BFOSC camera. Observations started at 10:57:59 UT on
2013-02-15 (i.e., 9.941 hr after the BAT trigger), and 3x300s R-band
and I-band frames were obtained, respectively.

The optical afterglow (Zheng et al., GCN 14205; LaCluyze et al., GCN
14206; Cenko, GCN 14209; Butler et al., GCN 14212; Gendre et al., GCN
14213) is clearly detected in each of our images. Compared with the
measurements in previous GCN reports, it decayed to R=19.1 mag at the
mean time of 10.08 hr post-trigger, in the staked image and calibrated
with nearby USNO B1 stars.

We thank Feng Xiao for carrying out these observations.


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14216
SUBJECT: GRB 130215A: iTelescope T11 observations
DATE:    13/02/15 13:46:08 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@varkaus.fi>

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

T11 (iTelescope Observatory, Mayhill, New Mexico) TEL T11 0.50-m/6.8
astrograph (0.50 m) f/6.5 and FLI ProLine PL11002M CCD camera were
used to detect GRB 130215A optical afterglow. The observations were
started at 2013-02-15 02:20:23 (UT) and stopped at 2013-02-15 03:22:20
(UT). Three unfiltered, two photometric R filter and two photometric V
filter observations with different exposure times were made.
The afterglow was detected at following position RA 02:54:00.73 and
DEC +13:23:43.4.

The following magnitudes were obtained from the observations using
NOMAD1 1034-0036172 (R = 14.220, V = 15.030) as the comparison:

Tmid(s)+T0     Filter         Exp (sec)     Mag          Mag err   Limit
2993              unfiltered       120          15.56CR     0.02     19.66
3156              unfiltered       120          15.70CR     0.03     19.66
4595              Rc                 300          16.44R        0.04     19.22
4936              Rc                 300          16.54R        0.05     19.32
5586              V                   300          17.27V        0.05     19.92
5910              V                   300          17.34V        0.06     19.92
6500              unfiltered       300           16.62CR      0.03     19.64

-- 
*************************************************************************
Viesti on tarkastettu roskapostinsuodatus- ja virustorjuntaohjelmistolla.
*************************************************************************


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14217
SUBJECT: GRB 130215A: GMG optical observation
DATE:    13/02/15 14:56:14 GMT
FROM:    Xiao-hong Zhao at Yunnan Obs  <zhaoxiaohong78@gmail.com>

X.-H. Zhao (YNAO), J.-M. Bai 
(YNAO) report on behalf of 2.4m telescope group:

We observed the field of GRB 130215A (D'Elia et al., GCN 14204) with 2.4m Gao-Mei-Gu (GMG) telescope. Observations
started at 11:59:03 UT on 2013-02-15 (i.e., 10.46 hrs after the burst) and 5x300s R-band images were obtained. The optical afterglow of this burst was clearly detected in each image. The mag is R~19.2 calibrated with USNO B1 stars. 
   
We thank the GMG staff, especially Wen-Bo Xu, De-Qing Wang for
performing these observations.


GRB_name: GRB130215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14218
SUBJECT: GRB 130215A: RAPTOR Measurements
DATE:    13/02/15 17:56:46 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 548760 (D'Elia, et al., GCN 14204).  Our narrow-field
instruments in Los Alamos, NM USA, began imaging at 01:43:07.0 UT, 696.8 s
after the Swift BAT trigger.  We detect the optical counterpart initially
reported by the ROTSE team (Zheng, et al., GCN 14205).  Our unfiltered images
are calibrated to the USNO-B1 r-band.  The following table gives a sample of
our observations.

T-Start  Exp-Time   Mag +/- error
------------------------------------
696.85     5.0      13.73 +/- 0.014
725.35     5.0      13.70 +/- 0.015
762.35     5.0      13.74 +/- 0.014
796.75     10.0     13.80 +/- 0.009
927.55     10.0     13.98 +/- 0.010
1089.9     30.0     14.13 +/- 0.006


GRB_name: GRB130215A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14219
SUBJECT: GRB 130215A: Fermi GBM detection
DATE:    13/02/15 21:10:57 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

George Younes (USRA) and P. N. Bhat (UAH)
report on behalf of the Fermi GBM Team:

"At 01:31:26.02 UT on 15 February 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130215A (trigger 382584689 / 130215063).
which was also detected by the Swift/BAT (D'Elia et al. 2013, GCN 14204)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 86 degrees.

The GBM light curve consists of single FRED like pulse
with a duration (T90) of about 140 s (50-300 keV).
The time-averaged spectrum from T0-7.0 s to T0+124 s is
adequately fit by a Band function with Epeak= 155 +/- 63 keV,
alpha = -1.0 +/- 0.2 and beta = -1.60 +/- 0.03.

The event fluence (10-1000 keV) in this time interval is
(2.02 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+10.56 s in the 10-1000 keV band
is 3.5 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB130215A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14220
SUBJECT: GRB 130215A: MITSuME Okayama Optical Observation
DATE:    13/02/15 21:25:50 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 130215A (D'Elia et al., GCN 14204)
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 2013-02-15 10:40:36 UT (~9.2 h after the burst).
We detected the previously reported afterglow (Zheng et al., GCNC 14205)
in Rc and Ic bands.

Photometric results and 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  Rc_err   Ic  Ic_err
-----------------------------------------------------------------------
0.39422    10:59:09    4080.0    >20.3   19.5  0.2    18.4  0.2
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130215A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14221
SUBJECT: GRB 130215A: GROND Detection of the Optical/NIR Afterglow
DATE:    13/02/16 03:38:47 GMT
FROM:    Fabian Knust at MPE/GROND  <fabian.knust@hotmail.de>

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

We observed the field of GRB 130215A (Swift trigger 548760; D'Elia et al., GCN 14204) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory (Chile).

Observations started at 00:50 UT on 16.02.13, 23.3 hrs after the GRB trigger They were performed at an average seeing of 1".8 and at an average airmass of 1.98.

We detect a point source in most bands at position:

RA (J2000) = 02:54:00.70

Dec. (J2000) = +13:23:43.4

with an uncertainty of 0".4, close to the position reported by Zheng et al. (GCN 14205).

Based on the first 13 min of total exposures in g'r'i'z' and 14 min in JHK, we estimate preliminary magnitudes (all in AB system) of

g' = 21.0 +- 0.1 mag,

r' = 20.5 +-0.1 mag,

i' = 20.2 +- 0.1 mag,

z' = 19.9 +- 0.1 mag,

J = 19.4 +- 0.2 mag,

H = 19.0 +- 0.1 mag

and

K > 18.0 mag.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.16 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14222
SUBJECT: GRB 130215A: P200 NIR observations
DATE:    13/02/16 10:11:26 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports:

I observed the location of GRB 130215A (D'Elia et al., GCN 14204) with 
the Wide-Field Infrared Camera (WIRC) on the Palomar 200-inch telescope 
on 2013-02-16 UT between 02:14 and 03:17.  A series of nine 60-second 
images each were taken in Ks, J, and H filters, followed by a second 
series in Ks.  High winds were present and seeing significantly degraded 
over the course of the observations.

The optical/NIR afterglow (Zheng et al., GCN 14205, Covino et al., GCN 
14211) is well-detected in a preliminary reduction of the Ks-band 
images.  Photometry (calibrated relative to 2MASS standards in the 
field) gives the following magnitudes:

t_mid=24.89 hours : Ks = 17.23 +/- 0.05 mag (19.07 AB)
t_mid=25.65 hours : Ks = 17.34 +/- 0.08 mag (19.18 AB)

Further observations are planned.


GRB_name: GRB130216A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14223
SUBJECT: GRB 130216A: Swift detection of a burst
DATE:    13/02/16 22:33:11 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC),
J. A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 22:15:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130216A (trigger=548927).  Swift did not slew because 
of the Moon observing constraint. 
The BAT on-board calculated location is 
RA, Dec 67.898, +14.665 which is 
   RA(J2000)  =  04h 31m 36s
   Dec(J2000) = +14d 39' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a small precursor 
peak at T-6 sec, and then the main peak at T+2 sec
with a total duration of about 20 sec.  The peak count rate
was ~10,000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 13:16 UT on 2013 February 20. There will thus be no XRT
or UVOT data for this trigger before this time. 

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: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14224
SUBJECT: GRB 130216A: OSN I-band observations
DATE:    13/02/16 23:56:39 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

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

"Following the detection of GRB 130216A by Swift (Melandri et al. GCN
Circ. 14223), we are carrying out I-band observations with the 1.5m OSN
telescope at Sierra Nevada Observatory starting 32 min post burst. We do
not find any new or varying optical source within the 3 radius Swift/BAT
error cirle down to I about 20. Observations are ongoing.

This message can be quoted.


GRB_name: GRB120118B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14225
SUBJECT: GRB 120118B: host observations and redshift determination
DATE:    13/02/17 01:46:52 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani, Thomas Kruehler (DARK/NBI), Daniel Perley (Caltech), 
Johan P. U. Fynbo, Dong Xu, Bo Milvang-Jensen (DARK/NBI), Paolo Goldoni 
(APC, CEA/Irfu), Steve Schulze (PUC and MCSS), report on behalf of the 
X-shooter GTO GRB collaboration:

We observed the field of GRB 120118B (Littlejohns et al., GCN 12852) 
with the Keck I telescope located on Mauna Kea. Observations were 
carried out on 2013 Feb 10 (389 days after the GRB), using the LRIS 
instrument, simultaneously in the g and I bands, for a total exposure 
time of 750 and 720 s, respectively. Consistent with the latest XRT 
position (Osborne et al. GCN 12857; see also 
http://www.swift.ac.uk/xrt_positions/), we detect a bright, slightly 
extended object (I = 23.8, Vega), which we consider to be the GRB host 
galaxy. Its coordinates are (J2000):

RA = 08:19:29.047
Dec = -07:11:05.14

This position is consistent with that of the tentative near-infrared 
counterpart reported by D'Avanzo & Palazzi (GCN 12870).

A spectrum of this source was taken on 2013 Feb 13 with the ESO VLT 
equipped with the X-shooter spectrograph, covering the wavelength range 
3000-20500 AA. The seeing was 0.6". In the NIR arm, we detect several 
emission lines, interpreted as [O III] (5007), [Ne III] (3869), and 
hints for [O III] (4959) and [O II] (3727) at a common redshift z = 
2.943. The weakness/lack of other prominent lines usually seen in GRB 
host spectra is readily explained by their location in non-favorable 
parts of the spectrum. In the UVB arm, the host continuum is detected 
down to ~4750 AA, which corresponds to the onset of the Lyman alpha 
forest at z = 2.943.

At z = 2.94 the host is a fairly luminous galaxy at 2000  rest-frame, 
roughly 0.5 mag brighter than L* at that redshift (e.g. Gabasch et al. 
2004, A&A, 421, 41). The properties of this object are akin to those of 
Lyman-break galaxies.

We acknowledge excellent support from the observing staff at Mauna Kea 
and Paranal, in particular Cedric Ledoux and Andrea Mehner.


GRB_name: GRB130216B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14226
SUBJECT: GRB 130216B: Burst found in ground analysis of BAT data
DATE:    13/02/17 03:41:21 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

At 18:58:12 Swift-BAT rate-triggered on GRB 130216B (BAT trigger 548918). No
significant source was found in onboard processing.  This was the same event
as Fermi GBM trigger 382733894. In ground analysis, a significant unknown
source was found at RA, Dec 58.875, +2.040, which is:

RA (J2000)   03h 55m 30.1s
Dec (J2000)  02d 02m 24s

with a 90% error radius of approximately 2 arcmin.

This position is within 2 arcmin of a low-redshift galaxy, 2MASX J03553770+0202484.

The burst had two peaks each about 2 seconds long, the first weaker, with a
total duration about 4 seconds long. A Swift TOO request has been submitted,
but the source is in Sun constraint at the present time.


GRB_name: GRB130215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14227
SUBJECT: GRB 130215A: Additional P200 NIR observations
DATE:    13/02/17 10:56:45 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports:

I re-observed the location of GRB 130215A with the Wide-Field Infrared 
Camera (WIRC) on the Palomar 200-inch telescope on 2013-02-17 UT between 
02:09 and 02:37 and between 04:29 and 04:56.  Images were again taken in 
J, H, and Ks-bands; transmission and seeing conditions were good.

The NIR afterglow remains well-detected in the most recent images. 
Photometry of the Ks-band images gives the following magnitudes (Vega):

t_mid=48.75 hours : Ks = 17.57 +/- 0.05 mag
t_mid=51.07 hours : Ks = 17.60 +/- 0.07 mag

Relative to the previous night (GCN 14222), these observations show 
remarkably little fading (decay index alpha~0.4 between 25-50 hours, 
compared to alpha~1.5 earlier;  Butler et al., GCN 14212).  This could 
indicate contribution from a bright host galaxy, but no obvious 
extension of the source is seen (in 1" seeing).  Alternatively it could 
indicate a bump, plateau or flare in the light curve.  Further 
observations with WIRC are not planned, but observations elsewhere are 
encouraged to constrain further evolution of the afterglow.


GRB_name: GRB130216A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14228
SUBJECT: GRB 130216A: TAROT La Silla observatory optical observations
DATE:    13/02/17 13:53:05 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@gmail.com>

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

We imaged the field of GRB 130216A detected by SWIFT (trigger 548927, 
Melandri et al., GCN 14223) with the TAROT robotic telescope (D=25cm) 
located at the European Southern Observatory, La Silla observatory, Chile.

The observations started 1.96h after the GRB trigger. The elevation of 
the field decreased from 44 degrees above horizon and weather conditions
were good.

The date of trigger : t0 = 2013-02-16T22:15:24.620

The first image is trailed with a duration of 180.0s (see the 
description in Klotz et al., 2006, A&A 451, L39). We do not detect any 
OT with a limiting magnitude of: t0+7048.3s to t0+7228.3s : R > 15.1

The second image is 180.0s exposure in tracking mode: t0+7238.9s to 
t0+7418.9s : R > 16.2

We co-added a series of exposures: t0+7238.9s to t0+8399.0s : R > 17.7

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

N.B. Galactic coordinates are lon=181.8416 lat=-22.2057 and the galactic 
extinction in R band is 0.3 magnitudes estimated from D. Schlegel et al. 
1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14229
SUBJECT: GRB 130216A: Swift-BAT refined analysis
DATE:    13/02/17 13:55:37 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130216A (trigger #548927)
(Melandri, et al., GCN Circ. 14223).  The BAT ground-calculated position is
RA, Dec = 67.901, 14.670 deg, which is 
   RA(J2000)  =  04h 31m 36.2s 
   Dec(J2000) = +14d 40' 10.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 54%.
 
The mask-weighted light curve shows two peaks.  There is an initial small peak
centered on ~T-6 sec with a duration of about 4 sec.  The second peak starts
at ~T-3 sec, peaks at ~T+2 sec, and ends at ~T+10 sec.
T90 (15-350 keV) is 6.5 +- 1.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.16 to T+4.31 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.35 +- 0.04.  The fluence in the 15-150 keV band is 3.1 +- 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 6.5 +- 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/548927/BA/


GRB_name: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14230
SUBJECT: GRB 130216A: P200 NIR Observations
DATE:    13/02/17 14:01:31 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (UC Berkeley) report:

We imaged the BAT position of GRB 130216A (Melandri et al., GCN 14223; 
Barthelmy et al., GCN 14299) on 2013-02-17 (UT) in Ks-band at two 
different epochs: 9 one-minute exposures between 02:56 and 03:08 
followed by 18 one-minute exposures between 05:46 and 06:13.  The FOV 
covers the entire BAT error circle.

No new sources are seen in the field relative to the 2MASS catalog. 
Digital image subtraction of the two epochs gives a limit on variability 
of Ks >~ 18.7 mag (5 sigma) between 4.77 and 7.74 hours after the BAT 
trigger.


GRB_name: GRB130216B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14231
SUBJECT: GRB 130216B: P200 NIR Observations
DATE:    13/02/17 14:01:42 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (UC Berkeley) report:

We imaged the BAT position of GRB 130216B (Cummings et al., GCN 14226) 
on 2013-02-17 (UT) in Ks-band at two different epochs: 10 one-minute 
exposures between 04:11 and 04:26 followed by 11 one-minute exposures 
between 05:27 and 05:45.  The FOV covers the entire BAT error circle.

No new sources are seen in the field relative to the 2MASS catalog. 
Digital image subtraction of the two epochs gives a limit on variability 
of Ks >~ 18.6 mag (5 sigma) between 9.33 and 10.63 hours after the BAT 
trigger.   In particular, we do not identify any variable sources or 
pointlike objects at the location of the 2MASS galaxy mentioned by 
Cummings et al, which our observations resolve into a highly-inclined 
spiral galaxy (major axis diameter ~40 arcsec).


GRB_name: GRB130216B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14232
SUBJECT: GRB 130216B BAT refined analysis
DATE:    13/02/17 19:42:32 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
  
Using the data set from T-0 to T+10 sec, we report further analysis of BAT
GRB 130216B (trigger #548918) (Cummings, GCN Circ. 14226).  The BAT ground-
calculated position is RA, Dec 58.866, +2.036, which is:
RA (J2000)   03h 55m 27.9s
Dec (J2000)  02d 02m 10s
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11%.
  
The mask-weighted light curve shows two peaks, the smaller from T+0 to T+2 and
the larger from T+2 to T+4.  Each is symmetrical in time.  T90 (15-350 keV) is
3.7 +- 0.5 sec (estimated error including systematics).
  
The time-averaged spectrum from T+0 to T+4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.77 +- 0.08.  The fluence in the 15-150 keV band is 1.3 +- 0.3 x 10^-6  erg/cm2.
The 1-sec peak photon flux measured from T+2.5 sec in the 15-150 keV band
is 7.4 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Because this burst was not located in onboard processing, the full burst
response was not initiated and not all of the normal data products are
available.  A Swift TOO to determine the position of the x-ray afterglow has
been approved,  and will take place once the source comes out of constraint on
February 19th.


GRB_name: GRB130216A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14233
SUBJECT: GRB 130216A: MITSuME Ishigakijima upper limits
DATE:    13/02/18 01:13:02 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130216A (Melandri et al., GCNC 14223)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical Observatory.

The observation started on 22013-02-17 14:30:07 UT (~16.2 h after the burst).
We did not find any new point source within the refined BAT error circle
(Barthelmy et al., GCNC 14229) 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
------------------------------------------------------
0.69477    14:55:52    1560.0   >20.1  >19.7  >18.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14234
SUBJECT: GRB 130216A: possible early detection at 15 GHz
DATE:    13/02/18 01:44:14 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

T.D. Staley, R.P. Fender (Univ. of Southampton), A.J. van der Horst,
A. Rowlinson (Univ. of Amsterdam), D.J. Titterington, K.J.B. Grainge
(MRAO) report on behalf of the 4 Pi Sky / AMI team:

"We observed the BAT position of GRB 130216A (Melandri et al., GCN 14223;
Barthelmy et al., GCN 14229) with the AMI Large Array at 15 GHz on
February 16, for one hour starting at 22:28 UT, i.e. 13 minutes after
the burst. The beam FWHM covers the entire BAT error circle.
We detect a source at >10 sigma significance consistent with the
location of the BAT trigger. Further observations are planned to
confirm if this is indeed very early radio emission from GRB 130216A.

These observations were triggered via the system described in
Staley et. al (2013, MNRAS, 428, 3114)."


GRB_name: GRB130216B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14235
SUBJECT: GRB 130216B: Fermi GBM observation
DATE:    13/02/18 04:17:03 GMT
FROM:    Vandiver Chaplin at UAH/Fermi-GBM  <chapliv@email.uah.edu>

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

"At 18:58:11.70 UT on 16 Feb 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130216B (trigger 382733894 / 130216790),
which was also located in Swift/BAT ground analysis (Cummings 2013, GCN 14226).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 93 degrees.

The GBM light curve shows a single pulse
with a duration (T90) of about 15 s (50-300 keV).
The time-averaged spectrum from T0-2.5 s to T0+6.8 s is fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.7 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 119 +/- 16 keV.

The event fluence (10-1000 keV) in this time interval is
(4.8 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.0 s in the 10-1000 keV band
is 15.5 +/- 0.5 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 91 +/- 21 keV, alpha = -1.6 +/- 0.1 and beta = -2.2 +/- 0.2.


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


GRB_name: GRB130216A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14236
SUBJECT: GRB 130216A: Fermi GBM observation
DATE:    13/02/18 04:18:14 GMT
FROM:    Vandiver Chaplin at UAH/Fermi-GBM  <chapliv@email.uah.edu>

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

"At 22:15:21.42 UT on 16 Feb 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130216A (trigger 382745724 / 130216927),
which was also detected by the Swift/BAT (Melandri et al. 2013, GCN 14223).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 71 degrees.

The GBM light curve consists of two peaks at T0 and T0+4 s,
with a duration (T90) of about 7 s (50-300 keV).
The time-averaged spectrum from T0-0 s to T0+6.7 s is
best fit by a Band function with Epeak = 152 +/- 13 keV,
alpha = -0.7 +/- 0.1, and beta = -2.6 +/- 0.3.


The event fluence (10-1000 keV) in this time interval is
(6.231 +/- 0.255)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.5 s in the 10-1000 keV band
is 9.2 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB130215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14237
SUBJECT: GRB 130215A: Continued RATIR Optical and NIR Monitoring
DATE:    13/02/18 09:24:53 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 (UCSC),
Eleonora Troja (GSFC), 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 continue to observe the field of GRB 130215A (D'Elia et al.; GCN 14204)
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 2013/02 18.13 to 2013/02
18.21UTC (73.5 to 75.5 hours after the BAT trigger), we obtained a
total of 1.40
hours exposure in the r' and i' bands and 0.53 hours of exposure in the Z,
Y, J, and H bands.

In comparison with USNO-B1 and 2MASS, we derive the following AB
magnitudes, not corrected for Galactic extinction in the direction of the
GRB, for the afterglow:

  r'  21.92 +/- 0.09
  i'  20.92 +/- 0.07
  Z   20.21 +/- 0.12
  Y   20.38 +/- 0.15
  J   20.37 +/- 0.13
  H   19.59 +/- 0.11

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


GRB_name: GRB130216A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14238
SUBJECT: GRB 130216A: MASTER-Net early observations 
DATE:    13/02/18 11:19:43 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-VWF robotic telescope (MASTER-Net: http://observ.pereplet.ru) in 
Kislovodsk was pointed to the GRB130216A 15 sec after notice time and 31 
sec after GRB time at 2013-02-16 22:15:52.273 UT using FERMI coordinates 
(V.Chaplin et. al. GCN14236).  We observ  SWIFT error-box by very wide 
field cameras (FOV=400 sq. deg. d=8.2 cm) and  haven't found optical 
transient on images with 5-sigma upper limit has been about 8 mag.

MASTER II  robotic telescope  located in Kislovodsk was pointed to the 
GRB130216A 23 sec  after notice time and 582 sec after GRB time at 
2013-02-16 22:25:06.231 UT. On our first (120s exposure) set we haven't 
found optical transient  within SWIFT error-box (A. Melandri  et. al. 
GCN14223).
The 5-sigma upper limit has been about 14.0 mag

All bservations were made on high (z>85 deg.) zenith distances and in bad 
weather condition .

The message may be cited.


GRB_name: GRB130216B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14239
SUBJECT: GRB 130216B: MASTER-Net early observation
DATE:    13/02/18 11:22:50 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-VWF robotic telescope (MASTER-Net: http://observ.pereplet.ru) in 
Kislovodsk was pointed to the GRB130216A  12 sec  after notice time and 53 
sec after GRB time at  2013-02-16 18:59:04.829  UT using FERMI coordinates 
(V.Chaplin et. al. GCN14235).  We observ SWIFT error-box ( J. R. Cummings 
et al. GCN14232 )  by very wide field cameras (FOV=400 sq. deg.) and 
haven't found optical transient on images with 5-sigma upper limit has 
been about 10 mag.

Observations were made in bad weather condition at zenith distanse z=70 
deg.

The message may be cited.


GRB_name: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14240
SUBJECT: GRB 130216A: Further Swift-BAT refined analysis
DATE:    13/02/18 14:57:39 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. Sakamoto (AGU) and S. D. Barthelmy (GSFC) reports on behalf of the Swift-BAT team:

Due to a issue in our automatic pipeline analysis script of the BAT data, we only reported 
the result based on a simple power-law fit at the spectral analysis section of the BAT refined 
circular (GCN Circ. 14229).  However, this GRB had an enough signal-to-noise ratio in 
the spectrum to obtain Epeak by the BAT data alone.  Therefore, we would like to update the 
spectral analysis part of the circular to:

"The time-averaged spectrum from T-6.16 to T+4.31 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.80 +- 0.20, 
and Epeak of 123.7 +- 27.1 keV (chi squared 47.17 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.0 +- 0.1 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+1.11 sec in the 15-150 keV band is
6.5 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.35 +- 0.04 (chi squared 72.98 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. "

We want to thank Alex Kann for pointing this out.  


GRB_name: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14241
SUBJECT: GRB 130216A: Further Swift-BAT refined analysis
DATE:    13/02/19 03:08:35 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. Sakamoto (AGU) and S. D. Barthelmy (GSFC) reports on behalf of the Swift-BAT team:

Due to a issue in our automatic pipeline analysis script of the BAT data, we only reported 
the result based on a simple power-law fit at the spectral analysis section of the BAT refined 
circular (GCN Circ. 14229).  However, this GRB had an enough signal-to-noise ratio in 
the spectrum to obtain Epeak by the BAT data alone.  Therefore, we would like to update the 
spectral analysis part of the circular to:

"The time-averaged spectrum from T-6.16 to T+4.31 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.80 +- 0.20, 
and Epeak of 123.7 +- 27.1 keV (chi squared 47.17 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.0 +- 0.1 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+1.11 sec in the 15-150 keV band is
6.5 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.35 +- 0.04 (chi squared 72.98 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. "

We want to thank Alex Kann for pointing this out.  


GRB_name: GRB130216B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14242
SUBJECT: GRB 130216B: Swift/XRT observations
DATE:    13/02/20 19:37:55 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

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

We have analysed 1.9 ks of XRT data for GRB 130216B (Cummings GCN Circ.
14226; Chaplin GCN Circ. 14235), from 247.9 ks to 277.3 ks after the BAT
trigger. The data are all in Photon Counting (PC) mode. No bright X-ray
afterglow is detected inside the refined BAT error circle (Cummings et al.
GCN Circ. 14232). The 3sigma upper limit is of 9.3 x 10^-3 cts/s.

This corresponds to an observed 0.3-10 keV flux of 3.6 x 10^-13 erg/cm2/s
(assuming a typical GRB spectrum with photon spectral index of 2). If we
consider the Galactic absorption in this direction (1.3 x 10^21 cm^-2;
Kalberla et al. 2005) this corresponds to an unabsorbed flux of 4.7 x
10^-13 erg/cm2/s.

We note that there is a flux excess (SNR~2) at the edge (but inside) of
the 1.5 arcmin radius BAT error circle, at the following position: RA,
Dec=58.84993, +2.05183 which is equivalent to

RA (J2000): 03h 55m 23.98s
Dec (J2000): +02d 03' 06.6"

with an uncertainty of 8.6 arcsec (radius, 90% confidence). The count rate
at this position is (2.5 +/- 1.4) x 10^-3 cts/s.


GRB_name: GRB130219A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14243
SUBJECT: GRB 130219A: Fermi GBM detection
DATE:    13/02/20 19:53:04 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 18:35:51.73 UT on 19 February 2013, the Fermi Gamma-ray 
Burst Monitor (GBM) triggered and located GRB 130219A (trigger 
382991754 / 130219.775).  The on-ground calculated location, 
using the Fermi GBM trigger data, is RA = 303.7, DEC = +40.8  
(J2000 degrees, equivalent to J2000 20h 14m, +40d 49'), with a 
statistical uncertainty of 1.2 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 85 degrees.

The GBM light curve shows two distinct peaks with a total duration 
(T90) of about 96 s (50-300 keV). The spectrum is taken over the 
peaks, from T0+0.003 to T0+3.328 s and T+66.817 to T0+101.634, 
and is well fit by a Comptonized model with Ep = 396.0 +/- 21.0 and
alpha = -1.11 +/- 0.02.  This yields a fluence (10-1000 keV) in this
time interval of ï»¿(3.18 +/- 0.05)E-05 erg/cm^2.

This interval is equally well fit to a Band function with
Ep = 343.1 +/- 25.5, alpha = -1.08 +/- 0.02, and
beta = -2.28 +/- 0.15.  This yields a fluence (10 - 1000 keV) over this
interval of (3.11 +/- 0.05)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: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14244
SUBJECT: GRB 130215A: PTF P48 optical detection
DATE:    13/02/21 06:08:29 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (UC Berkeley), and D. A. Brown
(Syracuse) report on behalf of a larger collaboration:

We have imaged the 3-sigma Swift BAT error circle (S. Barthelmy, GCN
14214) of GRB130215A (Swift548760, S. Barthelmy, GCN 14204) with the
Palomar 48 inch Oschin telescope (P48) as part of the Palomar
Transient Factory (PTF).

Images were obtained in the Mould R filter on 2013-02-15 at 02:35:05
and 04:05:52 UTC, 1.1 and 2.6 hours after the trigger. We detect a
fading point source that is absent in the USNO B-1 catalog at
magnitudes of 16.38 and 17.59 at
    RA(J2000)  =   2h 54m 00.73s
    DEC(J2000) = +13d 23' 43.0"
, matching the ROTSE-IIIb position (GCN 14205, Zheng & Flewelling).

Assuming a power-law decay, these two P48 observations give us an index
alpha=-1.25, consistent with the index of alpha=-1.24 reported by ROTSE
analysis (GCN 14208, Zheng et al.).


GRB_name: GRB130215A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14245
SUBJECT: GRB 130215A: Suzaku WAM observation of the prompt emission
DATE:    13/02/21 09:10:52 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long GRB 130215A (Elia et al GCN14204; George et al GCN14219) was
detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 01:31:25.437 UT (=T0).

The observed light curve shows a single peak with a duration (T90) of
about 46.0 seconds. The fluence in 100 - 1000 keV was
1.04 (+0.13/-0.13) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+1 s was
0.69 (+0.28/-0.36) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-7 s to
T0+55 s is well fitted by a single power-law with a photon index of
1.61 (+0.08/-0.07) (chi2/d.o.f = 13.9/14).

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: GRB130219A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14246
SUBJECT: IPN Triangulation of GRB 130219A
DATE:    13/02/21 16:50:12 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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,

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

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

The long-duration GRB 130219A was observed by Fermi (GBM: trigger
382991754, Collazzi, GCN Circ. 14243), Konus-Wind, INTEGRAL (SPI-ACS), 
Suzaku (WAM), Swift (BAT), AGILE (MCAL), and MESSENGER (GRNS), at about 
66950 s UT (18:35:50). 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
    ---------------------------------------------
    Corners:
    311.189 (20h 44m 45s) +51.497 (+51d 29' 50")
    307.440 (20h 29m 46s) +48.611 (+48d 36' 41")
    296.804 (19h 47m 13s) +37.410 (+37d 24' 35")
    296.474 (19h 45m 54s) +37.565 (+37d 33' 53")
    ---------------------------------------------
The error box area is about 2.5  sq. deg, and its maximum dimension is 
17.4 deg (the minimum one is 9 arcmin).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130219_T66950/IPN/


GRB_name: GRB130216A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14247
SUBJECT: GRB 130216A: Swift/XRT observations
DATE:    13/02/21 18:03:58 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB) reports on behalf of the Swift team:

We have analysed 8 ks of XRT data for GRB 130216A (Melandri et al.,  
GCN Circ. 14223), from 317.7 ks to 347.4 ks after the BAT trigger. The  
data are all in Photon Counting (PC) mode. No X-ray afterglow is  
detected inside the refined BAT error circle (Sakamoto & Berthelmy,  
GCN Circ. 14240). The 3sigma upper limit is of 4.7 x 10^-3 cts/s.

This corresponds to an observed 0.3-10 keV flux of 1.8 x 10^-13 erg/ 
cm2/s (assuming a typical GRB spectrum with photon spectral index of  
2). If we consider the Galactic absorption in this direction (1.5 x  
10^21 cm^-2; Kalberla et al. 2005) this corresponds to an unabsorbed  
flux of 2.4 x 10^-13 erg/cm2/s.


GRB_name: GRB130216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14248
SUBJECT: GRB 130216A: possible radio counterpart is steady field source
DATE:    13/02/21 20:15:01 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

A.J. van der Horst (U. of Amsterdam), R.D.E. Saunders (MRAO),
K.J.B. Grainge (U. of Manchester), R.P. Fender, T.D. Staley
(U. of Southampton), A. Rowlinson, R.A.M.J. Wijers (U. of Amsterdam)
report on behalf of a large collaboration:

"We have observed the Swift/BAT error circle of GRB 130216A (GCN 14229)
at multiple epochs with the AMI Large Array and the Westerbork Synthesis
Radio Telescope, at 15 and 4.8 GHz respectively. The radio source we
reported in GCN 14234 was clearly detected at all epochs at this
position: RA, Dec (J2000) = 04:31:34, +14:39:36 (+/- 2 arcsec).
Our flux density measurements are given in the table below.

Epoch              Delta T      Freq.     Flux density
==============     ========     =======   ============
Feb 16.94-16.98    0.03 days    15 GHz    0.78 +/- 0.08 mJy
Feb 18.55-19.01    1.86 days    15 GHz    0.80 +/- 0.04 mJy
Feb 19.51-19.59    2.62 days    4.8 GHz   1.11 +/- 0.09 mJy
Feb 19.86-19.99    3.00 days    4.8 GHz   1.15 +/- 0.06 mJy
Feb 20.50-20.64    3.64 days    4.8 GHz   0.92 +/- 0.07 mJy
Feb 20.91-20.99    4.02 days    4.8 GHz   1.09 +/- 0.08 mJy

The source is constant in flux between our observing epochs and also
within the 11-hour AMI observation. The spectral index between 4.8
and 15 GHz is -0.3. There is no significant polarization detected
in the combined Westerbork data, with a 3-sigma upper limit of 15%.

 From these observations we conclude that this source is not the
counterpart of GRB 130216A, but possibly a radio galaxy or AGN.
Based on the combined 9C and 10C Surveys of Radio Sources
(see, e.g., Davies et al. 2011, MNRAS, 415, 2708), we estimate that
the probability for a source as bright or brighter than the one we
detect to occur by chance inside the Swift/BAT error circle is 2%.

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


GRB_name: GRB130216B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14249
SUBJECT: GRB 130216B: Suzaku WAM observation of the prompt emission
DATE:    13/02/22 05:17:37 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The GRB 130216B  (Cummings 2013, GCN 14226) was triggered the Suzaku
Wide-band  All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 2013/02/16 18:58:13.41 UT (=T0).

The observed light curve shows a double-peaked structure starting at
T0-3.0 s and ending at T0+4.5 s with a duration (T90) of about
7.44 seconds. The fluence in 100 - 1000 keV was
1.81 (+0.21/-0.35) x 10^-6 erg/cm^2. The 1-s peak flux measured from
T0 was 2.62 (+0.46/-0.62) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1.0 s
to T0+6.5 s is well fitted by a single power-law with a photon index
of 2.93 (+0.68/-0.35) (chi^2/d.o.f = 12.5/14).

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: GRB130219A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14250
SUBJECT: Konus-Wind observation of GRB 130219A
DATE:    13/02/22 11:01:58 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense GRB 130219A
(Fermi GBM detection: Collazzi, GCN 14243;
IPN detection and localization: Hurley et al., GCN 14246)
triggered Konus-Wind at T0=66950.352.048s UT (18:35:50.352)

The burst started with a soft precursor
at ~T0-0.5s which was followed, after ~65 sec of quiescence,
by a harder intense emission pulse.
A total duration of the burst is ~117 s.
The emission in the main emission episode is seen up to ~8 MeV.

As observed by Konus-Wind, the burst
had a fluence of (4.2  0.4)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+81.152 s,
of (2.4  0.2)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The energy spectrum of the precursor (measured T0 to T0+8.444 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model,
for which:
alpha = +0.11  0.45,
and Ep = 95  8 keV,
chi2 = 57.2/60 dof.

The time-integrated spectrum of the main emission episode
(measured T0+67.792 to T0+105.984 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 = -1.08  0.07,
the high energy photon index beta = -2.12  0.11,
the peak energy Ep = 280  35 keV,
chi2 = 90.8/96 dof.

The spectrum at the maximum count rate
(measured T0+79.984 to T0+81.408 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 = -1.10  0.05,
the high energy photon index beta = -3.1  0.2,
the peak energy Ep = 365  15 keV,
chi2 = 81.3/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130219_T66950/

All the quoted results are preliminary.


GRB_name: GRB130219A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14253
SUBJECT: GRB 130219A: Suzaku WAM observation of the prompt emission
DATE:    13/03/01 10:21:18 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long GRB 130219A (Collazzi, GCN 14243; Hurley et al., GCN 14246) was
detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 2013/02/19 18:35:51.73 UT (=T0).

The observed light curve exhibited two separated pulses; which are
the 1st short pulse from T0+1 s to T0+3 s,
and the following 2nd long pulse from T0+74 s to T0+96 s,
with a total duration of 96 s. The fluence in 100 - 1000 keV was
2.06 (+0.16/-0.36) x 10^-5 erg/cm^2. The 1-s peak flux measured from
T0+81 s was 5.03 (+0.57/-0.72) photons/cm^2/s in 100 - 1000 keV.

Preliminary result shows that the time-averaged spectrum from T0-2s to
T0+98s is marginally described as a power-law with exponential cutoff
model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 1.23(-0.45 +0.39), and
Epeak 502(-96 +151) keV (chi^2/d.o.f. = 33.2/24).

On the other hand, the two separate pulse spectra are well fitted
by different models. The 1st pulse spectrum is well fitted by a single
power-law with a photon index of 2.12(+0.57/-0.37) (chi^2/d.o.f = 21.6/25).
The 2nd pulse spectrum is well fitted by a GRB Band model:
  the low-energy photon index alpha: -1.16(-0.35 +0.49),
  the high-energy photon index beta: -2.5(fixed),
  and the peak energy Epeak: 515(-84, +145) keV (chi^2/d.o.f = 26.1/24).

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: GRB130216A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14254
SUBJECT: GRB 130216A: Swift/UVOT Upper Limit
DATE:    13/03/01 22:02:14 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began observations of the field of GRB 130216A
3.67 days after the BAT trigger (Melandri et al., GCN Circ. 14223).
The observations were delayed because of an observing constraint
due to the Moon. No new source is seen inside the refined BAT
error circle (Barthelmy et al. GCN Circ. 14229).

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

Filter         T_start(s)   T_stop(s)      Exp(s)        Mag
w1              317224       346946         7959        >22.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.49 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14255
SUBJECT: GRB 121128A: optical upper limit in Maidanak observatory
DATE:    13/03/04 20:09:12 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (SAI MSU), A. Sergeev (Institute of Radio 
Astronomy of NASU),  O. Burhonov (UBAI), I. Molotov (KIAM) report on 
behalf of larger GRB follow-up collaboration:

We observed  the field of Swift  GRB 121128A  (Oates et al., GCN 14007) 
with AZT-22 telescope of Maidanak observatory starting on Nov. 30  (UT) 
13:47:48 under mean seeing (FWHM) of about 1 arcsec. We obtained several 
images of 180 s exposure in R  filter.  The optical afterglow
(Oates et al., GCN 14007; Japelj et al., GCN 14008) is not detected in 
our  images. A photometry of the stacked image is based on nearby 
USNO-B1.0 stars:

t_start, T0+ (mid), filter, exp.,   OT,  Upper Limit(3sigma)
(UT)     d                  s

13:47:48 2.37924    R      15x180   n/d  23.7


GRB_name: GRB121128A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14256
SUBJECT: GRB 121128A: optical observations in Mondy observatory
DATE:    13/03/04 20:20:57 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We report revised results of our observations in Mondy observatory (GCNs 
14019, 14024) of the afterglow of GRB 121128A (Oates et al., GCN 14007; 
Japelj et al., GCN 14008). We re-processed data obtained on Nov. 28,29 
and Dec. 02 based on full data set obtained.

Nov. 28
  t_start, filter, exp,      T-t0,   OT,  err
  UT               s         d

  10:27:30 R     4*30+16*60 0.23024 19.79 0.05
  10:46:51 R    10*60       0.24047 19.85 0.04
  10:56:58 R    10*60       0.24751 19.78 0.04
  11:07:06 R    10*60       0.25454 19.96 0.05
  11:17:14 R    8*60+12*40  0.26674 19.95 0.05
  11:42:14 R    25*40       0.28132 20.07 0.05
  11:59:13 R    30*40       0.29429 20.12 0.05
  12:19:36 R    30*40       0.30845 20.06 0.04
  12:39:58 R    30*40       0.32259 20.24 0.05
  13:00:21 R    64*40       0.34488 20.32 0.04

Nov. 29
  t_start, filter, exp,      T-t0,   OT,  UL(3sigma)
  UT               s         d

10:16:58  R      6220      1.27406 n/d  23.3

Dec. 02
  t_start, filter, exp,      T-t0,   OT,  UL(3sigma)
  UT               s         d
10:47:17  R      4920      4.32854 n/d  21.2

The photometry is based on following reference stars

  1442-0304687 20:02:23.58 +54:16:58.9 16.67
  1442-0304744 20:02:29.58 +54:16:57.0 18.66
  1442-0304807 20:02:36.33 +54:17:58.9 18.20
  1443-0305750 20:02:37.10 +54:18:34.6 17.72
  1443-0305710 20:02:32.72 +54:18:46.9 17.25

The combined light curve of our observations (this circular, GCN 14201 
and GCN 14255) can be found at
http://grb.rssi.ru/GRB121128A/GRB121128A_lc2.PNG

Non-filtered photometry of Abastumani observatory (GCN 14201) is 
corrected to the R as d(C-R)=-0.034. One can see non-monotonous behavior 
of the lc between 0.4 -- 0.4 days after trigger, and probable jet brake 
between 0.6 and 1.3 days.


GRB_name: GRB130305A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14257
SUBJECT: GRB 130305A found in ground analysis of Swift/BAT data
DATE:    13/03/05 17:49:08 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (NASA/GSFC UMBC/CRESST) and D. M. Palmer (LANL) report on behalf
of the Swift/BAT team:

At 11:39:16, BAT triggered on GRB 130305A (trigger #550329).  No source was
found on board.  This burst was also detected by Fermi (trignum=384176354)
and INTEGRAL (TRIGGER_NUM:    6794,   Sub_Num: 0).  In ground analysis of the
BAT scaled-map data, a significant source was found on the edge of the BAT
FOV (2.25% coded) at RA, Dec 116.765, +52.025, which is:

RA (J2000)  07h 47m 03.6s  
Dec (J2000) 52d 01m 29s

with an estimated 90% uncertainty radius of 3.5 arcmin.

The GRB was a single symmetrical peak about 20 seconds long.  A Swift TOO request
has been approved to detect the afterglow position.


GRB_name: GRB130228A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14258
SUBJECT: GBM trigger 383712005 (GRB 130228A?) : Possible high-energy photon emission in Fermi/LAT data
DATE:    13/03/05 18:55:53 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

WeiKang Zheng (UC Berkeley) and Carl Akerlof (Umich), report on behalf
of the ROTSE collaboration (the authors are not affiliated with the
Fermi Collaboration),

We report the possible high-energy photon emission in Fermi/LAT data
correlated with GBM trigger 383712005 (02:40:02 UT on Feb. 28, 2013,
probably GRB 130228A) as a follow-up of a routine search in GBM trigger
catalogs using our LAT data processing pipeline. The GBM trigger
location (RA = 265.830, Dec = 55.930) was about 24 degree from the LAT
boresight, and the zenith angle was about 45 degrees.

A standard matched filter technique analysis (Akerlof et al. 2010, 2011,
2013, Zheng et al. 2012a,b), which uses a duration data of 47.5s
after the trigger, did not reveal confident signal in LAT data. However,
if extending the duration to 150s, the matched filter analysis gives a
weight value of 10.53, not high enough to claim a firm detection
compared to standard case, but is clearly higher than background. This
kind of delayed LAT high energy photon emission is quite common in GRB.
The new GRB location estimated by the matched filter technique is Ra =
255.46, Dec = 55.02 with uncertainty ~0.5 degree, this is ~6 degrees
away from the GBM trigger location. ~7 photons above 100 MeV were
detected within 150s, with the highest energy of ~692 MeV at 133s after
the burst.

A maximum likelihood analysis focusing on the new GRB location gives a
TS value of 31.0 over the same time window of 150s after the trigger.
This supports the above finding from matched filter analysis.

The photon information can be found in the following link including the
skymap:
http://www.rotse.net/LAT/GBMTriggers/383712005/383712005_res.html


GRB_name: GRB130305A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14260
SUBJECT: GRB 130305A: Fermi LAT Detection
DATE:    13/03/05 22:54:38 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

S. Guiriec (NASA/GSFC/NPP), J. L. Racusin (NASA/GSFC),
G. Vianello (Stanford) and D. Kocevski (NASA/GSFC/NPP)
report on behalf of the Fermi-LAT team:

The Fermi Large Area Telescope (LAT) detected emission from GRB 130305A at
 approximately 11:39:11 UT on March 5th, 2013, while in Target Of
Opportunity
(i.e., pointing) mode observing the Crab (ATEL #4855). GRB 130305A was
detected
by Fermi-GBM (GBM trigger 130305486/384176354)
and Swift-BAT (Cummings et al., GCN #14257).

The burst location was within the LAT field of view at an angle of ~41
degrees to
the LAT boresight, and ~100 degrees from the zenith, placing it very close
to
the Earth's limb, which is a very bright source of gamma rays. No
significant excess is
seen using standard analysis procedures (>100 MeV) neither in the prompt
phase nor
in a search for extended emission when the burst position was no longer
occulted
from ~1500 to 5000 s.

Using the non-standard LAT Low Energy (LLE) data selection,
>550 counts above background were detected in a single FRED like pulse,
peaking
between 5 and 10 s after the GBM trigger and coinciding with the time of
the GBM emission, with a significance of ~10.7 sigma. This detection is due
to
low energy gamma-rays, below 75 MeV, and therefore has insufficient spatial
resolution
to provide a reliable LAT localization.

A GBM circular on GRB 130305A is forthcoming.

The Fermi LAT point of contact for this burst is Sylvain Guiriec
(sylvain.guiriec@nasa.gov)


GRB_name: GRB130305A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14261
SUBJECT: GRB 130305A: Fermi GBM observation
DATE:    13/03/06 00:34:45 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Hoi-Fung Yu (MPE) and Shaolin Xiong (UAH)
report on behalf of the Fermi GBM Team:

"At 11:39:11.37 UT on 05 March 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130305A (trigger 384176354 / 130305486),
which was also detected by the Fermi/LAT (S. Guiriec et al., GCN 14260) and
the Swift/BAT (Cummings et al., GCN 14257).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is about 44 degrees.

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

The GBM light curve shows single pulse with a tail
with a duration (T90) of about 29 s (50-300 keV).
The time-averaged spectrum from T0-0 s to T0+30 s is best fit by
a Band function with Epeak = 640 +/- 23 keV,
alpha = -0.67 +/- 0.02, and beta = -2.4 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(5.7 +/- 0.07)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.2 s in the 10-1000 keV band
is 25.4 +/- 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: GRB130305A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14262
SUBJECT: Konus-Wind observation of GRB 130305A
DATE:    13/03/06 12:14:28 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense GRB 130305A
(Swift-BAT trigger #550329: Cumings & Palmer, GCN 14257;
Fermi-LAT detection: Guiriec et al., GCN 14260;
Fermi-GBM observation: Yu and Xiong, GCN 14261)
triggered Konus-Wind at T0=41953.135s UT (11:39:13.135)

The light curve shows a bright hard pulse with
a total duration of ~30 s followed by a weaker
hard emission tail out to ~T0+250 s.
The emission in the main bursting episode is seen up to 12 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130305_T41953/

As observed by Konus-Wind, the main pulse
had a fluence of (8.5  0.6)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.480 s,
of (1.6  0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+36.096 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 = -0.81  0.04,
the high energy photon index beta = -2.5  0.2,
the peak energy Ep = 640  45 keV,
chi2 = 83.7/95 dof.

The spectrum at the maximum count rate (measured from T0 to T0+11.520 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 = -0.72  0.04,
the high energy photon index beta = -2.8  0.2,
the peak energy Ep = 655  30 keV,
chi2 = 89.5/96 dof.

The spectrum of the emission tail (measured from T0+36.096 to T0+224.512 s)
is best fit in the 20 keV - 10 MeV range by the simple power-law model
with a rather hard photon index of (-1.4  0.1), chi2 = 71.7/89 dof.
The emission in this time interval is seen up to 9 MeV
and the 20 keV - 10 MeV energy fluence is (3.3  1.1)x10-5 erg/cm2.

All the quoted results are preliminary.


GRB_name: GRB130305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14263
SUBJECT: GRB 130305A: Swift/XRT detection of the afterglow
DATE:    13/03/06 15:50:04 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani (DARK/NBI), Bin-Bin Zhang (PSU), David N. Burrows 
(PSU), Dirk Grupe (PSU), report on behalf of the Swift-XRT team:

The Swift spacecraft observed the ground-discovered BAT GRB 130305A 
(Cummings & Palmer, GCN 14257), also detected by Fermi GBM and LAT (Yu & 
Xiong, GCN 14261; Guiriec et al., GCN 14260), Konus/Wind (Golenetskii et 
al., GCN 14262) and INTEGRAL SPI-ACS.

We have analysed 1.8 ks of XRT data, from 31.0 ks to 47.2 ks after the 
Swift/BAT trigger. The data are entirely in photon counting (PC) mode. 
An X-ray source is detected within the Swift/BAT error circle. The XRT 
position is RA, Dec = 116.74762, +52.03332 which is equivalent to:

RA (J2000) = 07 46 59.43
Dec(J2000) = +52 01 60.0

with an uncertainty of 3.8 arcsec (radius, 90% confidence). This 
position is 49 arcsec from the Swift/BAT position.

A spectrum formed from the PC mode data can be fitted with an absorbed 
power-law with a photon spectral index of 2.0 (+0.7, -0.6). The 
best-fitting absorption column is  4.1 (+3.6, -2.5) x 10^21 cm^-2, in 
excess of the Galactic value of 4.8 x 10^20 cm^-2 (Kalberla et al. 
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion 
factor deduced from this spectrum  is 4.3 x 10^-11 (7.3 x 10^-11) erg 
cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:         4.1 (+3.6, -2.5) x 10^21 cm^-2
Galactic foreground: 4.8 x 10^20 cm^-2
Excess significance: 2.4 sigma
Photon index:         2.0 (+0.7, -0.6)

Further observations by Swift are ongoing. The results of the XRT-team 
automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020234.

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


GRB_name: GRB100615A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14264
SUBJECT: GRB 100615A: HST host detection and X-shooter redshift 
DATE:    13/03/06 17:46:42 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler, D. Malesani, D. Xu, J. P. U. Fynbo (DARK/NBI), A. J. Levan
(U. Warwick), N. R. Tanvir (U. Leicester), V. D'Elia (ASDC, INAF) and 
D. Perley (Caltech) report on behalf of the X-shooter GTO GRB collaboration:

The field of GRB 100615A (Swift trigger 424733, D'Elia et al., GCN 10841) 
was observed with the Hubble Space Telescope and WFC3
(filters F606W and F160W) under proposal ID 11840 (PI: A. J. Levan).
Observations were carried out on 2010 Dec 16 (154 days after the GRB),
for a total exposure time of 1128 s and 1208 s, respectively.
In the HST images, we detect a single, resolved object (F160W = 24.1 AB mag)
consistent with the Chandra X-ray position (Butler et al., GCN 10915),
which we consider to be the GRB host galaxy. 

Its coordinates are (J2000):

RA = 11:48:49.34
Dec = -19:28:51.8

A spectrum of this source was taken on 2013 Mar 05 with the ESO VLT
equipped with the X-shooter spectrograph, covering the wavelength range
3000-20500 AA. The seeing was 0.8". In the VIS and NIR arm,
we detect several emission lines, interpreted as the doublet of
[O II](3726, 3729), [Ne III](3869),  [O III](4959), [O III](5007) and Halpha 
at a common redshift of z = 1.398.

At this redshift, the afterglow data imply a very high host exinction
along the GRB sight-line (A_V > 10-15, see D'Elia & Stratta 2011, A&A, 532, A48,
their Figure 4). The intrinsic soft X-ray absorption column measured
from Swift/XRT data (Margutti et al., GCN 10847) at z = 1.398 is
N_{H,X} = 1.07 (+0.13, -0.12) x 10^23 cm^-2. This is similarly at the high end
of measured column densities, even among dark bursts
(e.g., Kruehler et al., 2012, ApJ, 758, 46, their Figure 5). In
contrast, the host of GRB 100615A is rather blue (F606W - F160W \sim 1
AB mag) and does not show obvious signs of heavy dust content.

We acknowledge excellent support from the observing staff at Paranal,
in particular Giacomo Beccari and Emanuela Pompei.


GRB_name: GRB130305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14265
SUBJECT: GRB 130305A: P60 Observations
DATE:    13/03/06 19:51:49 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

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

We imaged the location of the Swift (Cummings et al., GCN 14257), Fermi
(Guiriec et al., GCN 14260; Yu et al., GCN 14261), and Konus (Golenetskii
et al., GCN 14262) GRB 130305A with the robotic Palomar 60 inch telescope.
Observations were obtained in the g', r', and i' filters beginning at 2:47
UT on 2013 Mar 6 (~ 15.1 hr after the Swift-BAT trigger).

We do not detect any sources within the Swift-XRT error circle (Malesani
et al., GCN 14263) in any filter.  Using nearby point sources from SDSS
for reference, we calculate limiting magnitudes of g' > 22.8, r' > 22.2,
and i' > 21.7 at this time.


GRB_name: GRB130306A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14266
SUBJECT: GRB 130306A: Swift detection of a burst
DATE:    13/03/07 00:07:17 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. H. Siegel (PSU), B. N. Barlow (PSU), S. D. Barthelmy (GSFC),
N. Gehrels (NASA/GSFC), D. Grupe (PSU), D. Malesani (DARK/NBI),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), D. M. Palmer (LANL) and
B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 23:51:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130306A (trigger=550457).  Swift did not slew because
of a Moon constraint.  The BAT on-board calculated location is 
RA, Dec 279.478, -11.692 which is 
   RA(J2000)  =  18h 37m 55s
   Dec(J2000) = -11d 41' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT real-time TDRSS light curve shows nothing
significant as is typical for image triggers. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 05:58 UT on 2013 March 08. There will thus be no XRT or
UVOT data for this trigger before this time. 

We note that this burst was strongly detected by Fermi GBM
in a 4.096 second trigger at T-216 seconds (Trigger 384306448) at
a location consistent with the BAT location.  Swift was
slewing at the time of the Fermi Trigger, detecting the afterglow
of the GRB in its first 64 second image trigger after the slew ended. 

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


GRB_name: GRB130305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14267
SUBJECT: GRB 130305A: RATIR Observations
DATE:    13/03/07 01:47:52 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico 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 130305A (Cummings, et al., GCN 14257) 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 2013/03 6.12 to 2013/03 6.13 UTC (15.11 to
15.50 hours after the BAT trigger), obtaining a total of 0.31 hours
exposure in the r' and i' bands.

For a source within the Swift-XRT error circle (Malesani, et al., GCN
14263), in comparison with USNO-B1, we derive the following upper limits
(3-sigma) in the AB magnitude system:

  r'  > 23.4
  i'  > 23.1

These magnitudes 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: GRB130305A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14268
SUBJECT: GRB 130305A: Swift/UVOT Upper Limit
DATE:    13/03/07 12:34:13 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (MSSL-UCL), Daniele Malesani (DARK/NBI), Bin-Bin Zhang 
(PSU), S. R. Oates (MSSL-UCL) and M. De Pasquale (MSSL-UCL) report on 
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130305A 
30975s after the BAT trigger discovered in ground analysis (Cummings et 
al., GCN Circ. 14257).
No optical afterglow consistent with the XRT position (Malesani et al., 
GCN Circ. 14263) is detected in the initial UVOT exposures. Preliminary 
3-sigma upper limit 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                30975        59030         3890         >21.4

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.05 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB130306A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14269
SUBJECT: GRB 130306A: MASTER-Net pre-Swift alert observation
DATE:    13/03/07 15:05:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Denisenko, D.Kuvshinov, 
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  GRB130306A 59 sec after Fermi 
trigger num 384306448 at 2013-03-06 23:48:24.313 UT, i.e. 157 sec before 
Swift  trigger time (Siegel et. al. GCN14266).
The observations started on very high zenith distance about 85 deg.

SWIFT error box (Siegel et. al. GCN14266) got on the edge of our FOV.  On 
our first (10s exposure) set we haven't found optical transient  within 
SWIFT error box. The 5-sigma upper limit has been about 13 mag.

Next time we pointed to BAT position at 2013-03-06 23:52:44.60 UT by 
SWIFT alert. On our first (20s exposure) set we haven't found optical 
transient  within SWIFT error-box  with upper limit 15.2m. On coadd image 
of 8 sets with total exposure 420 sec upper limit is 17.0m (5-sigma).

Galactic extinction in the direction of GRB 130306 is A_R=3.7, A_I=2.7
(from to Schlegel et al., 1998) and A_R=3.0, A_I=2.1 (according to
Schlafly et al., 2011).

The message may be cited.


GRB_name: GRB130306A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14270
SUBJECT: GRB 130306A: Fermi GBM observation
DATE:    13/03/08 02:56:56 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 23:47:25.57 UT on March 6 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130306A (trigger 384306448 / 130306991),
which was also detected by the Swift/BAT (Siegel et al. 2013, GCN 14266)
The GBM on-ground location is consistent with the Swift position.

The GRB is observed at high angles to all GBM NaI detectors and the angle
from the LAT boresight is 166 degrees.

The GBM light curve consists of 3 main peaks with a duration of about
60 s with a plateau starting about 20 s before trigger and a tail
extending to about 100s after trigger."


GRB_name: GRB130307A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14271
SUBJECT: GRB 130307A: Fermi GBM detection
DATE:    13/03/08 05:19:20 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

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

"At 03:01:44.47 UT on March 7 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130307A (trigger 384318107 / 130307126).

The on-ground calculated location, using the GBM trigger
data, is RA = 153.7, DEC = 18.3 (J2000 degrees,
equivalent to +10h 12m, +18d 16'), with an uncertainty
of 3.3 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 67 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.
An IPN triangulation will be issued in a forthcoming circular.

The GBM light curve consists of a single pulse
with a duration (T90) of about 0.4 s (50-300 keV).
The time-averaged spectrum from T0-0.64 s to T0+0.032 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.78 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 1670 +/- 350 keV
(Castor statistics 816 for 728 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(1.43 +/- 0.05)E-06 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+0.064 s in the 10-1000 keV band
is 9.9 +/- 1.1 ph/s/cm^2.

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


GRB_name: GRB130305A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14272
SUBJECT: GRB 130305A: Gemini-North upper limit
DATE:    13/03/08 06:03:09 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick Observatory), S. B. Cenko 
(UC Berkeley), D. Perley (Caltech) report on behalf of 
a large collaboration:

"On March 7.21 UT we observed the field of GRB 130305A 
(Cummings & Palmer, GCN 14257; Yu & Xiong, GCN 14261; 
Guiriec et al., GCN 14260) with the Gemini-North telescope
equipped with the GMOS camera.

We obtained 14x180s exposures, for a total integration time
of 42 minutes (T_mid = T0+1.70 days). No clear object is 
detected within the XRT error circle down to r' > 26.1 mag.

Nevertheless we note the presence of several galaxies
just outside the current XRT error circle (2.7 arcsec radius), 
in particular of a relatively bright object in the S-W direction, 
which seems to show a distorted morphology 
(https://www.dropbox.com/s/pyir6g8mqd658xn/GRB130305A.jpeg). 
The galaxy coordinates are

RA: 07:46:58.9  (J2000)
Dec: +52:01:55.72 (J2000)


We thank the Gemini staff for performing this observations,
in particular J. Rhee."


GRB_name: GRB111123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14273
SUBJECT: GRB 111123A: Keck-I host detection and VLT/X-shooter redshift
DATE:    13/03/08 10:59:57 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu, D. Malesani, T. Kruehler, J. P. U. Fynbo (DARK/NBI), D. A.
Perley (Caltech), P. Goldoni (APC/Univ. Paris 7 and SAp/CEA), L. Kaper
(U. Amsterdam), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI), N. R.
Tanvir (U. Leicester) report on behalf of the X-shooter GTO GRB
collaboration:

We observed the field of GRB 111123A (Stamatikos et al., GCN 12587)
using the Keck-I telescope equipped with the LRIS instrument.
Observations were carried out on 2013 February 10 (~444 days after the
burst), simultaneously in the g and I bands, for a total exposure time
of 750 and 720 s, respectively.

An extended source with g=25.83 (AB) and I = 23.55 (Vega) is detected
at the position of the optical and NIR afterglow (Xu et al., GCN
12589; Fugazza et al., GCN 12593), where the positional error radius
of the optical afterglow has been reduced from ~1.0" to ~0.3" through
a refined analysis. We thus consider the source to be the host galaxy
of GRB 111123A.

A spectrum of this source was taken on 2013 March 07 with the ESO VLT
equipped with the X-shooter spectrograph, featuring NIR/VIS/UVB three
arms and covering the wavelength range 3000-25000 AA. The exposure
time was 4x600 s. In the NIR arm, we detect four emission lines,
interpreted as [O III] (5007), [NeIII] (3869), [O II] (3727), and
Hbeta (a marginal detection), all at a common redshift z = 3.1516. In
the UVB arm, the host continuum is detected down to ~5100 AA, thus
corresponds to the onset of the Lyman alpha forest at the proposed
redshift.

We acknowledge excellent support from the observing staff at Mauna Kea
and Paranal, in particular Emanuela Pompei, Claudio Melo, and Andres
Pino.


GRB_name: GRB130305A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14274
SUBJECT: GRB 130305A: Optical Observations
DATE:    13/03/08 12:03:05 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

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

We observed the LAT detected GRB 130305A error-box (Cummings & Palmer GCN
14257; Guiriec et al. GCN 14260; Yu & Xiong GCN 14261) using 1.04m
telescope
at ARIES Nainital on 2013:03:05, 18:28:30 UT, ~6.8 hours after the
Swift/BAT detection.

Four frames in R_c pass-band 300sec each were acquired in good sky
conditions.
In the co-added image (4x300 sec), we did not detect any optical transient
within the XRT error circle (Malesani et al. GCN 14263) down to a limiting
magnitude of 21 mag. The photometry was performed in comparison to nearby
USNO- B1 stars.

This massage could be cited.


GRB_name: GRB130306A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14275
SUBJECT: Konus-Wind observation of GRB 130306A
DATE:    13/03/08 16:33:09 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The very long-duration GRB 130306A
(Swift-BAT trigger #550457: Siegel et al., GCN 14266;
Fermi-GBM observation: Pelassa, GCN 14270)
triggered Konus-Wind at T0=85669.636s UT (23:47:49.636)

The light curve shows a multi-pulse emission which
started ~270 s before the trigger, peaked at ~T0+10s,
and, after ~T0+110s, passed into a long tail
out to ~400 s after the trigger.
The total duration of the burst is ~700 s.
The emission is seen up to 5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130306_T85669/

As observed by Konus-Wind, the burst
had a fluence of (2.9  0.05)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+8.768 s,
of (6.1  0.6)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum
(measured from T0 to T0+116.224 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model,
for which:
alpha = -1.50  0.05,
and Ep = 212  10 keV,
chi2 = 53.8/59 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+11.774 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model,
for which:
alpha = -1.34  0.04,
and Ep = 410  30 keV,
chi2 = 64.7/71 dof.

The spectrum of the emission tail
(measured from T0+116.224 to T0+402.944 s)
is best fit in the 20 keV - 5 MeV range
by the simple power-law model with
the photon index -2.3  0.1, chi2 = 65.1/75 dof.
The emission in this time interval is seen up to 4 MeV
and the 20 keV - 10 MeV energy fluence
is (2.7  0.3)x10-5 erg/cm2.

All the quoted results are preliminary.


GRB_name: GRB130305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14276
SUBJECT: GRB 130305A: Further Swift-XRT Observations
DATE:    13/03/08 16:40:57 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

Bin-Bin Zhang (PSU), Daniele Malesani (DARK/NBI), Dirk Grupe (PSU),
David N. Burrows (PSU) and Kim L. Page (U. Leicester) report on behalf
of the Swift-XRT team:

We have analyzed 16 ks of XRT data for the Swift/BAT-detected burst:
GRB 130305A,  from 31.0 ks to 210.2 ks after the  Swift/BAT trigger.
The data are entirely in Photon Counting (PC) mode. We confirm that 
the X-ray source reported in Malesani et al. GCN 1426  is fading.  
The light curve can be modeled with  a power-law decay with a decay
index of alpha=2.4 (+0.5, -0.4).

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020234.

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


GRB_name: GRB130305A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14277
SUBJECT: GRB 130305A BAT refined circular
DATE:    13/03/08 22:35:16 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), D. Malesani (DARK/NBI),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)

Using 11 seconds of event data covering part of the burst, we present
further analysis of GRB 130305A (Cummings and Palmer, GCN # 14257).  This
was a ground-detected burst on the edge of the BAT field of view.  The
best BAT position is RA, Dec 116.774, +52.037, which is:

RA (J2000)   07h 47m 05.8s
Dec (J2000)  52d 02m 11s

with an estimated uncertainty radius of 1.8 arcmin (90% containment).  This
position is 1.0 arcmin from the XRT afterglow position (Malesani et al,
GCN # 14263).

The BAT mask-weighted lightcurve does not show more detail than the raw
lightcurve due to the extreme partial coding (2.5%).  There is a single
peak, approximately symmetrical, a total of about 20 seconds long.  Note,
however, the much longer duration mentioned at high energy by the
Konus-Wind team (Golenetskii et al., GCN # 14262.

The following spectral results appear to cover about 90% of the total flux
of the burst, based on the raw lightcurve excess over constant background.
Again, the partial coding makes the uncertainty of the fit parameters large.
A fit to a simple power law function has a photon index of 0.78 +/- 0.20.
This is harder than most other BAT-detected long GRBs.  The fluence from
15-150 keV was (4.8 +/- 1.8) x 10^-6 ergs/cm^2.

[GCN OPS NOTE(08mar13):  Per author's request, the word "draft" was removed
from the Subject-line.]


GRB_name: GRB130228A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14278
SUBJECT: IPN triangulation of GRB 130228A
DATE:    13/03/09 00:08:01 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

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

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

D. M. Smith, J. McTiernan, R. Schwartz, and W. Hajdas, on behalf of the
RHESSI 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, A. von Kienlin,
and A. Rau, on behalf of the Fermi GBM team, report:

GRB 130228A was detected by the Fermi GBM (trigger 383712005),
Konus-Wind, RHESSI, Suzaku WAM, Swift BAT (outside the coded FoV),
and MESSENGER GRNS.  We have triangulated it to a preliminary,
3 sigma error box whose coordinates are:


             RA(2000)         Dec(2000)
Center:  256.8792 = 17 h 07 m 31 s +57.9767 = 57 d 58 m 36 s
Corners: 257.9210 = 17 h 11 m 41 s +74.5340 = 74 d 32 m 03 s
         256.9529 = 17 h 07 m 49 s      +36.0592 = 36 d 03 m 33 s
         255.7015 = 17 h 02 m 48 s      +76.3736 = 76 d 22 m 25 s
         256.3030 = 17 h 05 m 13 s      +38.7303 = 38 d 43 m 49 s

and whose area is 22.7 sq. deg.  This error box may be improved.

The minimum distance between the edge of the error box and the
edge of the 0.5 degree radius LAT error circle (Zheng and Akerlof,
GCN 14258) is about 1.5 arcminutes.  Thus the two localizations
are consistent if the LAT error circle radius is a roughly one
sigma confidence region.

Maps have been posted at ssl.berkeley.edu/ipn3/130228.


GRB_name: GRB130306A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14279
SUBJECT: GRB 130306A: Swift-BAT refined analysis
DATE:    13/03/09 01:15:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), A. Lien (NASA/GSFC/ORAU).  T. Sakamoto (GSFC/UMBC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), G. Sato (ISAS), M. H. Siegel (PSU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-160 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130306A (trigger #550457)
(Siegel, et al., GCN Circ. 14266).  The BAT ground-calculated position is
RA, Dec = 279.475, -11.682 deg, which is 
   RA(J2000)  =  18h 37m 54.1s 
   Dec(J2000) = -11d 40' 55.0" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11%.
 
This burst was already active when it came into the BAT FoV during a slew
at T-160 sec.  There were several peaks until ~T-130 sec, then a long
relatively smooth decay out past T+900 sec (when the data ends).
 
The time-averaged spectrum from T-159.5 to T+154.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.05.  The 1-sec peak photon flux (during the period of BAT viewing)
measured from T-152.73 sec in the 15-150 keV band is 7.3 +- 0.8 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/550457/BA/


GRB_name: GRB130306A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14280
SUBJECT: GRB 130306A: MITSuME Ishigakijima upper limits
DATE:    13/03/10 08:25:23 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130306A (Siegel et al., GCNC 14266)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2013-03-07 19:28:07 UT (~19.6 h after the burst).
We did not find any new point source within the refined BAT error circle
(Barthelmy et al., GCNC 14279) in all the three bands.

Three sigma upper limits of the OT are listed below. We used
GSC2.3(for g' and Rc) and USNO-B1(for Ic) catalog for flux calibration.

T0+[day]   MID-UT   T-EXP[sec]    g'     Rc     Ic
------------------------------------------------------
0.84918    20:13:51    4560.0   >20.6  >19.5  >18.4
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130131A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14281
SUBJECT: GRB 130131A: JCMT SCUBA-2 sub-mm observations
DATE:    13/03/11 01:49:17 GMT
FROM:    Ian Smith at Rice U  <ian@spacsun.rice.edu>

I.A. Smith (Rice U.), R.P.J. Tilanus (Leiden Observatory), N.R. Tanvir 
(U. of Leicester), D.A. Frail (NRAO) report:

We observed the location of GRB 130131A (Grupe et al., GCN Circ. 14156) 
twice using the SCUBA-2 sub-millimeter continuum camera on the James 
Clerk Maxwell Telescope.  The first observation started at 14:36 UT on 
2013-01-31, corresponding to 40 minutes after the burst trigger.  It 
lasted 2.0 hours in good weather conditions.  The second observation 
started at 12:40 UT on 2013-02-01, corresponding to 0.95 days after 
the burst trigger.  It lasted 2.1 hours in good weather conditions.  
No source was significantly detected in the individual or combined 
observations at the VLA location (Laskar et al., GCN Circ. 14171).  
The combined RMS was 2.2 mJy/beam at 850 microns and 18.2 mJy/beam at 
450 microns.

We thank Iain Coulson, Jim Hoge, Callie McNew, Alexander Karim, and 
William Montgomerie for their prompt support of these observations.


GRB_name: GRB130310A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14282
SUBJECT: GRB 130310A: Fermi-LAT detection and localization
DATE:    13/03/11 07:36:13 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

S. Guiriec (NASA/GSFC/NPP), G. Vianello (Stanford)
and M. Ohno (Hiroshima U.)
report on behalf of the Fermi-LAT team:

The Fermi Large Area Telescope (LAT) detected emission from
GRB 130310A (GBM trigger 130310840/384638984) at approximately
20:09:44 UT on March 10th, 2013, about 3s after Fermi-GBM trigger time.

The burst location was outside the LAT nominal field of view, at an angle
of ~79 degrees from the LAT boresight, and ~50 degrees from the Zenith.

Using the non-standard LAT Low Energy (LLE) data selection, featuring
a large effective area and a larger field of view below 100 MeV but a much
larger PSF with respect to the standard classes, we clearly detect
the prompt emission of the GRB (significance > 10 sigma above the
background). With this selection and in this energy range the GRB shows
a single FRED-like pulse, peaking ~3 s after the GBM trigger in good
coincidence with the peak of the GBM emission.

The high peak flux of the burst triggered an Autonomous Repointing
Request (ARR) starting about 50s after the trigger time, which placed
the GRB within the LAT nominal field of view for standard data
classes (~65 deg) approximately 200 s after the trigger.
Using the P7SOURCE_V6 class we detect ~18 photons between 100 MeV
and 3 GeV in the time interval 200 s - 800 s from the trigger, clearly clustered
in a point source ~4.8 deg away from the best GBM position and with
a significance larger than 5 sigma. Our best localization is:

R.A., Dec = 142.34, -17.23 (J2000)
90 % containment radius (statistical only) = 0.45 deg.

A GBM circular on GRB 130310A is forthcoming.

The Fermi LAT point of contact for this burst is Sylvain Guiriec
(sylvain.guiriec@nasa.gov)


GRB_name: GRB130310A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14283
SUBJECT: GRB 130310A: Fermi GBM detection
DATE:    13/03/11 08:48:12 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) and Vandiver Chaplin (UAH)
report on behalf of the Fermi GBM Team:

"At 20:09:41.50 UT on 10 March 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130310A (trigger 384638984 / 130310840),
which was also detected by the Fermi/LAT (Guiriec et al. 2013, GCN 14282)
The GBM on-ground location is consistent with the LAT position.
At the time of triggering the angle from the Fermi LAT boresight was
79 degrees. GBM generated a Autonomous Repointing
Request (ARR) due to the high peak flux of this GRB, causing
Fermi to reorient so that the LAT could better observe this GRB.

The GBM light curve consists of a precursor and a FRED pulse
with a duration (T90) of about 2.4 s (50-300 keV).
The time-averaged spectrum from T0+4.1 s to T0+5.0 s is
adequately fit by a Band function with Epeak = 2.1 +/- 0.2 MeV,
alpha = -1.01 +/- 0.02, and beta = -2.27 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(1.4 +/- 0.02)E-5 erg/cm^2. The 0.064 sec peak photon flux measured
starting from T0+4.1 s in the 10-1000 keV band is 170 +/- 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: GRB130310A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14284
SUBJECT: IPN triangulation of GRB 130310A
DATE:    13/03/11 13:10:43 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

V. Connaughton, M. Briggs, and C. Meegan, 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

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


The short-duration, hard-spectrum, intense GRB 130310A (Fermi/LAT 
detection: Guiriec,  Vianello, Ohno, GCN 14282; Fermi/GBM detection: 
Xiong and Chaplin, GCN 14283) has been also observed by Konus-Wind, 
Suzaku (WAM), INTEGRAL (SPI-ACS), MESSENGER (GRNS), and Mars Odyssey 
(HEND), so far, at about 72585 s UT (20:09:45).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
     ---------------------------------------------
      RA(2000), deg                 Dec(2000), deg
     ---------------------------------------------
    Center:
     141.905 (09h 27m 37s) -17.431 (-17d 25' 53")
    Corners:
     141.722 (09h 26m 53s) -16.780 (-16d 46' 50")
     141.801 (09h 27m 12s) -17.435 (-17d 26' 06")
     142.093 (09h 28m 22s) -18.072 (-18d 04' 18")
     142.008 (09h 28m 02s) -17.428 (-17d 25' 40")
     ---------------------------------------------
The error box area is 465 sq. arcmin, and its maximum
dimension is 80 arcmin (the minimum one is 12 arcmin; the minimum 
annulus width is 11 arcmin).

This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130310_T72588/IPN/

The center of the LAT position (Guiriec,  Vianello, Ohno, GCN 14282) is 
0.46 deg from the box center.


GRB_name: GRB130310A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14285
SUBJECT: Konus-Wind observation of GRB 130310A
DATE:    13/03/11 14:14:12 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short hard intense GRB 130310A
(Fermi-LAT detection: Guiriec et al., GCN 14282;
Fermi-GBM detection: Xiong and Chaplin, GCN 14283
IPN triangulation: Golenetskii et al., GCN 14284)
triggered Konus-Wind at T0=72588.897s UT (20:09:48.897)

The light curve shows a bright hard FRED-like structure
with a total duration of ~3 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/GRB130310_T72588/

As observed by Konus-Wind, the burst
had a fluence of (3.0  0.3)x10-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.000s,
of (3.6  0.2)x10-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (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 = -1.03  0.05,
the high energy photon index beta = -1.85  0.15,
the peak energy Ep = 855  270 keV,
chi2 = 85.8/97 dof.

The spectrum at the maximum count rate (measured from T0 to T0+0.064 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 = -0.87  0.13,
the high energy photon index beta = -1.62  0.28,
the peak energy Ep = 2600  1400 keV,
chi2 = 27.9/26 dof.

All the quoted results are preliminary.


GRB_name: GRB130131B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14286
SUBJECT: GRB 130131B: host detection and redshift
DATE:    13/03/11 14:20:28 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Johan P. U. Fynbo, Dong Xu, Daniele Malesani, Thomas Kruehler 
(DARK/NBI), Dan A. Perley (Caltech), Valerio D'Elia (ASDC, INAF), report 
on behalf of the X-shooter GTO GRB collaboration:

We observed the field of GRB 130131B (Siegel et al., GCN 14159) using 
the Keck-I telescope equipped with the LRIS instrument. Observations 
were carried out on 2013 February 10 (9.62 days after the burst), 
simultaneously in the g and I bands, for a total exposure time of 750 
and 720 s, respectively.

A source with g = 25.7 (AB) and I = 24.9 (Vega) is detected inside the 
enhanced XRT error circle (which has a radius of 1.8"; Goad et al., GCN 
14165), at coordinates:

R.A.(J2000) = 11:35:49.31
Dec.(J2000) = +15:02:18.0

We consider this object to be the likely host galaxy of GRB 130131B.

A spectrum of this source was taken on 2013 March 9 with the ESO VLT 
equipped with the X-shooter spectrograph, covering the wavelength range 
3000-20000 AA. The exposure time was 8x900 s. In the NIR arm, we detect 
three emission lines, interpreted as [O III] (4960, 5007) and [O II] 
(3727), all at a common redshift z = 2.539. In the UVB arm, the host 
continuum is detected down to ~4400 AA, which corresponds to the onset 
of the Lyman alpha forest at the proposed redshift.

We acknowledge excellent support from the observing staff at Mauna Kea 
and Paranal, in particular Emanuela Pompei, Claudio Melo, and Thomas 
Rivinius.


GRB_name: GRB130306A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14287
SUBJECT: GRB 130306A: Swift Detection of a Possible Afterglow
DATE:    13/03/11 15:07:32 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

GRB 130306A: Swift Detection of a Possible Afterglow

M. H. Siegel (PSU), David N. Burrows (PSU) and Dirk Grupe (PSU)
report on behalf of the Swift team:

On 8 March 2013 the Swift spacecraft performed a delayed observation of the
BAT-detected burst GRB 130306A (Siegel et al., GCN 14266), which was also
detected by Fermi GBM (Pelassa, GCN 14270) and Konus/Wind (Golenetskii et al.,
GCN 14275).

We have analyzed 5.1 ks of XRT data, from 146 to 163 ks after the Swift/BAT
trigger.   The data are entirely in photon counting (PC) mode. 
An X-ray source is detected within the Swift/BAT error circle. The XRT 
position is RA, Dec = 279.46147, -11.68123 which is equivalent to:

RA (J2000) = 18 37 50.75
Dec(J2000) = -11 40 52.4

with an uncertainty of 4.0 arcsec (radius, 90% confidence).  We do not detect
any fading over the time span of the Swift observations.

The Swift/UVOT began settled observations of the field of GRB 130306A 146 
ks after the Swift/BAT trigger.  No optical afterglow consistent with the XRT position
is detected in the initial UVOT exposures. Preliminary 3-sigma upper limit 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

uvw1         145609      162770         4707         >22.2

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.15 in the direction of the 
burst (Schlegel et al. 1998).

Further observations are planned to determine if the source is fading.


GRB_name: GRB130310A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14288
SUBJECT: Swift XRT observations of GRB 130310A
DATE:    13/03/12 03:12:58 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/PSU), D. N. Burrows (PSU), J. L. Racusin
(NASA/GSFC), C. J. Mountford (U Leicester), N. Gehrels (NASA/GSFC) report
on behalf of the Swift team:

Swift performed 3 pointings of 1.5 ks each to cover the IPN error box for
GRB 130310A (Golenetskii et al., GCN #14284). A single, uncatalogued
source is detected at coordinates:

   RA/Dec (J2000) = 09 27 36.35   -17 06 16.1
   RA/Dec (J2000) = 141.901   -17.1044

Error radius (arcsec) = 3.6 (90% confidence level)

The source is inside the IPN error box, and 0.44 degrees from the Fermi
LAT position (Guiriec et al., GCN #14282), just inside the LAT error
circle.

The countrate is 7.60E-03 +/- 2.5E-03 c/sec
At present is not possible to tell if the source is fading.

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


GRB_name: GRB130310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14289
SUBJECT: GRB 130310A: optical observations
DATE:    13/03/12 08:00:05 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick Observatory), S. B. Cenko 
(UC Berkeley), D. Perley (Caltech) report on behalf of 
a large collaboration:

"On March 12.4 UT we observed the field of the short-hard 
GRB 130313A (GCN 14282, 14283, 14284, 14285 and 14288) 
with the Gemini-South telescope equipped with the GMOS camera.

We obtained 5x180s exposures, for a total integration time
of 15 minutes (T_mid = T0+1.22 days). 


A snapshot of our imaging campaign can be seen here:
https://www.dropbox.com/s/jqt714c44b7ngei/0310A_rband.jpeg
We note the presence of two irregular objects (marked as "G1" adn "G2") 
within the current XRT error circle (3.6 arcsec radius, GCN 14288).

The coordinates of this objects are:

"G1"
RA: 09:27:36.34  (J2000)
Dec: -17:06:18.92 (J2000)

"G2"
RA: 09:27:36.46  (J2000)
Dec: -17:06:13.80 (J2000)


Using 3 USNO-B1 stars we estimate a preliminary 
brightness for "G1" of r' = 25.05 +- 0.15 and for
"G2" r'=23.80 +- 0.10.

At this point the nature of these objects as well as the relation with 
GRB 130313A afterglow is still uncertain. Further observations
are encouraged.

We thank the Gemini staff for performing this observations,
in particular J. Thomas-Osip"


GRB_name: GRB130310A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14290
SUBJECT: Swift XRT RETRACTION of GRB 130310A afterglow detection 
DATE:    13/03/12 14:44:15 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/PSU), D. N. Burrows (PSU), P. E. Evans (U
Leicester), E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift team:

Upon further analysis of the Swift XRT observations of the IPN error box
for GRB 130310A (Svinkin et al., GCN #14284) we RETRACT the detection of a
candidate afterglow reported by Sbarufatti et al., GCN #14288.

Further analysis is ongoing.

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


GRB_name: GRB100424A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14291
SUBJECT: GRB 100424A: Keck host detection and VLT/X-shooter redshift
DATE:    13/03/12 16:07:54 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani, D. Xu, J. P. U. Fynbo, T. Kruehler (DARK/NBI), D. A. Perley 
(Caltech), S. D. Vergani (CNRS/GEPI), P. Goldoni (APC/IRFU-CEA), report 
on behalf of the GRB GTO X-shooter collaboration:

We observed the field of GRB 100424A (Hoversten et al., GCN 10667) using 
the Keck-I telescope equipped with the LRIS instrument. Observations 
were carried out on 2010 July 8.2 UT (74.5 days after the burst), 
simultaneously in the g and I bands, for a total exposure time of 35 and 
32 min, respectively.

Consistent with the position of the NIR afterglow (Cenko et al., GCNs 
10682, 10690, 10692), we detected a source with g = 26 (AB) and I = 24.4 
(Vega). We consider this object to be the host galaxy of GRB 100424A.

A spectrum of this source was taken on 2013 March 11.3 UT with the ESO 
VLT equipped with the X-shooter spectrograph, covering the wavelength 
range 3000-25000 AA. The exposure time was 8x600 s. In the NIR arm, we 
detect four emission lines, that we interpret as [O III](4959), [O 
III](5007), Hbeta, and [O II](3727), all at a common redshift of z = 
2.465. In the UVB arm, we also detect weak Lyalpha in emission at the 
same redshift.

We acknowledge excellent support from the observing staff at Mauna Kea 
and Paranal, in particular Thomas Rivinius and Claudio Melo.


GRB_name: GRB130307A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14292
SUBJECT: IPN Triangulation of GRB 130307A
DATE:    13/03/12 17:05:12 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

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

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

The short-duration GRB 130307A was observed by Fermi (GBM: trigger
384318107, Pelassa, GCN Circ. 14271), Konus-Wind, INTEGRAL (SPI-ACS), 
Swift (BAT), AGILE (MCAL), and MESSENGER (GRNS), at about 10904 s UT 
(03:01:44). 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:
     155.996 (10h 23m 59s) +22.998 (+22d 59' 53")
    Corners:
     154.692 (10h 18m 46s) +22.026 (+22d 01' 32")
     155.790 (10h 23m 10s) +23.534 (+23d 32' 02")
     157.288 (10h 29m 09s) +23.852 (+23d 51' 08")
     156.204 (10h 24m 49s) +22.463 (+22d 27' 46")
     ---------------------------------------------
The error box area is about 1.6  sq. deg, and its maximum dimension is
3.0 deg (the minimum one is 1.3 deg).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130307_T10908/IPN/


GRB_name: GRB130313A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14293
SUBJECT: GRB 130313A: Swift detection of a short burst
DATE:    13/03/13 16:36:56 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B.P. Gompertz (U Leicester), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU), V. D'Elia (ASDC),
S. T. Holland (STScI), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester),
C. A. Swenson (PSU) and E. Troja (NASA/GSFC/UMCP) report on behalf of
the Swift Team:

At 16:08:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130313A (trigger=550906).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 236.423, -0.362 which is 
   RA(J2000)  =  15h 45m 42s
   Dec(J2000) = -00d 21' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 0.2 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 16:09:29.2 UT, 78.1 seconds after
the BAT trigger. No source was detected in 737 s of promptly downlinked
data, which covered 93% of the BAT error circle. 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 81 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
0.10. 

Burst Advocate for this burst is B.P. Gompertz (bpg6 AT le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14294
SUBJECT: GRB 130313A: MASTER-Net optical observations
DATE:    13/03/13 16:47:08 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

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.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  GRB130313A 27 sec after 
notice and 45 sec after GRB time at 2013-03-13 16:08:56.268 UT in two 
polarizations. On our first (10s exposure) set we haven't found optical 
transient  within SWIFT error-box (ra=15 45 39 dec=+00 21 34 r=0.05 d).
The 5-sigma upper limit has been about 15.0 mag.

MASTER II  robotic telescope 
located in Tunka was pointed to the  GRB130313A 85 sec after GRB time at 
2013-03-13 16:09:36.11 UT in two polarizations. On our first (20s 
exposure) set we haven't found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 13.3 mag. Such a low limit is 
connected to large zenith distance of observed field (z>85 deg).

The observations are continued.
The message may be cited.


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14295
SUBJECT: GRB 130313A: Zadko observatory - Gingin optical observations
DATE:    13/03/13 18:15:55 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 (IRAP-CNRS-OMP), 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 130313A detected by SWIFT
(trigger 550906) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 52.3s after the GRB trigger
(34.2s after the notice). The elevation of the field increased from
19 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any optical transcient with a limiting
magnitude of:
t0+52.3s to t0+112.3s : R > 17.2

The second image is 30.0s exposure in tracking mode:
t0+130s to t0+160s : R > 18.6

We co-added a series of exposures:
t0+131s to t0+320.0s : R > 19.3

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

This message may be cited.


GRB_name: GRB130313A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14296
SUBJECT: GRB 130313A: Swift-BAT refined analysis
DATE:    13/03/13 19:48:15 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), B.P. Gompertz (U Leicester),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+180 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130313A (trigger #550906)
(Gompertz, et al., GCN Circ. 14293).  The BAT ground-calculated position is
RA, Dec = 236.438, -0.355 deg, which is 
   RA(J2000)  =  15h 45m 45.1s 
   Dec(J2000) = -00d 21' 18.0" 
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.
 
The mask-weighted light curve shows a single pulse starting at ~T+0.0,
peaking at ~T+0.1 sec, and ending at ~T+0.2 sec.  T90 (15-350 keV) is
0.26 +- 0.09 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.02 to T+0.23 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.37 +- 0.36.  The fluence in the 15-150 keV band is 3.1 +- 0.7 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.36 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/550906/BA/


GRB_name: GRB130313A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14297
SUBJECT: GRB 130313A: Swift-XRT detection of a possible X-ray afterglow
DATE:    13/03/13 20:08:27 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

B.P. Gompertz & K.L. Page (U. Leicester) report on behalf of the Swift-XRT
team:

Swift-XRT started observing the field of the short GRB 130313A 78 s after
the BAT trigger (Gompertz et al., GCN Circ. 14293). Using 662 s of XRT
Photon Counting mode data, we find a possible weak source at a position of
RA, Dec = 236.41005, -0.36874, which is equivalent to:

RA (J2000): 15h 45m 38.41s
Dec (J2000): -00d 22' 07.5"

with an uncertainty of 5.3 arcsec (radius, 90% confidence). This is 1.9
arcmin from the BAT refined position (Barthelmy et al., GCN Circ. 14296),
within the error circle.

It is not possible to determine if the source is fading at this time.

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


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14298
SUBJECT: GRB 130313A: Weihai optical upper limit
DATE:    13/03/13 20:36:40 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We imaged the field of GRB 130313A (Gompertz et al., GCN 14293) with
the 1m telescope located in Weihai, Shandong Province, China.
Observations started at 17:41:25 UT on 2013-03-13 (i.e., 1.554 hr
after the BAT trigger) and 5x600s R-band images were obtained.

No optical source is detected within the XRT error circle (Gompertz &
Page, GCN 14297) in the stacked image, down to a limit of R>20.5 mag
calibrated with nearby USNO B1 stars.

We thank Chang-Ming Zhang for carrying out these observations.


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14299
SUBJECT: GRB 130313A: simultaneous and follow-up optical observations at  BOOTES-3 and BOOTES-4
DATE:    13/03/13 23:25:34 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

J. C. Tello (IAA-CSIC Granada), S. Guziy (Mykolaiv Nat. Univ.), O.
Lara-Gil, R. Cunniffe, M. Jelinek (IAA-CSIC), J. Gorosabel
(UPV/EHU-IAA/CSIC), P. Kubanek (IP AS CR), Y. Fan, X. Zhao, J. Bai, C. Wang,
Y. Xin (Yunnan Nacional Astronomical Observatory), Ch. Cui (Beijing
National Astronomical Observatory), W. Allen (Vintage Lane Obs.), Ph. Yock
(Auckland Univ.) and A. J. Castro-Tirado (IAA-CSIC), on behalf of a larger
collaboration, report:

Following the detection of GRB 130313A by Swift (Gompertz et al. GCNC
14293), both the 0.6m BOOTES-3/YA and BOOTES-4/MET robotic telescopes in
Lijiang (China) and Blenheim (New Zealand) responded automatically to the
trigger alert. Due to poor atmospheric/environmental conditions in both
places, not deep limits were obtained: R > 15 (at BOOTES-3) with an
unfiltered 60 second exposure beginning at 16h35m29s UT (27 minutes after
the burst) and R > 18.5 (at BOOTES-4) beginning at 18h12m39s UT (2 hours
after the burst). In addition to these late limits, the CASANDRA-3
wide-field system at BOOTES-3 took unfiltered images (36 seconds exposure
each) beginning at 16h06m44s UT (87 seconds before the burst), 16h07m40s
UT (31 seconds before the burst) and 16h08h36s UT (25 seconds after the
burst). No credible transient is observed down to a limiting magnitude of
R > 8.5.


GRB_name: GRB130313A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14300
SUBJECT: GRB 130313A: Swift-XRT refined Analysis
DATE:    13/03/14 04:27:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.1 ks of XRT data for GRB 130313A (Gompertz  et al.
GCN Circ. 14293),  from 85 s to 18.7 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The refined XRT
position is RA, Dec = 236.41004, -0.36897 which is equivalent to:

RA (J2000): 15 45 38.41
Dec(J2000): -00 22 08.3

with an uncertainty of 4.8 arcsec (radius, 90% confidence). We cannot
determine at the present time whether the source is fading.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+3.4, -4.0). The
best-fitting absorption column is  consistent with the Galactic value
of 5.9 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 7.0 x 10^-11 (7.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+1.7, -0) x 10^23 cm^-2
Galactic foreground: 5.9 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.6 (+3.4, -4.0)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00550906.

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


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14301
SUBJECT: GRB 130313A: NOT optical upper limit
DATE:    13/03/14 05:00:30 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), S. Schulze  (PUC and MCSS), N. R. Tanvir (U.
Leicester), H. Dahle, N. Groeneboom (U. Oslo), and J. P. U. Fynbo (DARK/NBI), report
on behalf of a larger collaboration:

We imaged the field of GRB 130313A (Gompertz et al., GCN 14293) using
the 2.5m Nordic Optical Telescope (NOT) equipped with the ALFOSC
instrument, located on La Palma, Canary Islands. Observations started
at 02:16:32 UT on 2013-03-14 (i.e., 10.139 hr after the BAT trigger)
and 12x300s SDSS_i-band images were obtained in good seeing of ~0.7".

No object was found within the refined XRT error circle (Osborne et
al., GCN 14300) in the stacked image, down to a limit of i>23.4 mag,
calibrated with nearby SDSS stars.

[GCN OPS NOTE(14mar13): Per author's request, NG was added to the author list.]


GRB_name: GRB130313A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14302
SUBJECT: GRB130313A: Optical observations from GTC
DATE:    13/03/14 06:55:45 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), 
J. Gorosabel (IAA-CSIC), R. Sanchez-Ramirez (IAA-CSIC), J. P. U. Fynbo 
(DARK/NBI) and N. Tanvir (U. Leicester) report:

We have observed the field of the short GRB 130313A (Gompertz et al., 
GCN 14293) using the 10.4m GTC. Observations started at 5:22 UT 
(13.23 hr after the burst) and were performed in the r-band in good conditions 
and a seeing of ~0.8". The combined 8x120s exposure covers the complete 
refined BAT error box (Barthelmy et al., GCN 14296).

We detect a point-like source at the edge of the suggested X-ray afterglow 
(Osborne et al., GCN 14300) for which we estimate a preliminary magnitude 
of r=26.3+/-0.4, as compared with SDSS stars (we note that the photometry is
complicated by a nearby bright star). This object is located at the following 
coordinates (J2000, +/-0.5"):

S1:
R.A.: 15:45:38.45
Dec.: -00:22:03.5

There are two other marginally detected sources consistent with the XRT error 
box, one unresolved at:

S2:
R.A.: 15:45:38.21
Dec.: -00:22:10.3

And one extended:

S3:
R.A.: 15:45:38.64
Dec.: -00:22:04.7

A finding chart with these sources can be found at:
http://www.iaa.es/~deugarte/GRBs/130313A/130313A_GTC.jpg

Further observations in search for variability will be needed to determine the relation 
of any of these sources with GRB 130313A.


GRB_name: GRB130215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14303
SUBJECT: GRB 130215A: Detection of the SN with the 10.4m GTC
DATE:    13/03/14 13:30:03 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), 
J. Gorosabel (IAA-CSIC, UPV/EHU), R. Sanchez-Ramirez (IAA-CSIC), 
G. Leloudas (OKC, Stockholm), Z. Cano (U. Iceland), D. Xu (DARK/NBI), 
K. Wiersema (U. Leicester), J.P.U. Fynbo, D. Malesani, J. Hjorth (DARK/NBI), 
P. Jakobsson (U. Iceland), O.E. Hartoog (U. Amsterdam) report on behalf of 
a larger collaboration:

We have observed the optical counterpart of GRB 130215A (D'Elia et al., 
GCN 14204, Zheng et al., GCN 14205) with the 10.4 m GTC telescope 
equipped with the OSIRIS imager and spectrograph. A spectroscopic 
observation was performed on 12 March 2013 at a mean time of 20:52 UT, 
25.8 days after the burst, corresponding to 16.2 days after the burst in the 
rest frame, considering a redshift of z=0.597 (Cucchiara et al. GCN 14207). 
The total exposure was 3x1200s using a low resolution grating (R~600) 
covering a wavelength range 5000-10000 A. Due to its current location, 
observations had to be carried out at high airmass, between 1.6 and 2.2. 
There were thin cirrus but seeing was very good, at 0.6".

At this epoch, the spectrum presents undulations typical of SN spectra, 
including a prominent bump at ~8200 A. Using SNID (Blondin & Tonry 2007, 
ApJ, 666, 1024), we have compared the spectrum to a series of SN templates. 
The spectrum gives a good match to a number of SNe Ic, including 
broad-lined and normal events such as SN 2002ap and SN 1994I, around 
maximum light or slightly after. By leaving the redshift unconstrained we 
obtain the same template fit and derive a redshift of z=0.58+/-0.02, fully 
consistent with the absorption line redshift.

We acknowledge excellent support from the GTC staff, in particular 
Carlos A. Alvarez Iglesias. 


GRB_name: GRB130313A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14305
SUBJECT: GRB 130313A: Fading X-ray Afterglow
DATE:    13/03/14 14:09:00 GMT
FROM:    Ben Gompertz at U.of Leicester  <bpg6@leicester.ac.uk>

B. P. Gompertz&  K. L. Page (U. Leicester) report on behalf of the
Swift-XRT team:

Continuing Swift observations of GRB 130313A (Gompertz et al., GCN Circ.
14293) have shown the X-ray source identified by Gompertz&  Page (GCN
Circ. 14297) and Osborne et al. (GCN Circ. 14300) has faded. The first
snapshot of data contains 10 counts in 326 seconds, giving a count rate of
0.012  0.004 count s^-1, while later data provide an upper limit of
0.0025 count s^-1, corresponding to a single count in 22 ks of data. The
souurce has faded and we therefore confirm that this is the X-ray
afterglow of GRB 130313A.

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


GRB_name: GRB130313A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14306
SUBJECT: GRB 130313A: Swift-BAT Spectral lag analysis
DATE:    13/03/14 14:46:53 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

J. Norris (BSU), T. Sakamoto (AGU), S. D. Barthelmy (GSFC), N. Gehrels (GSFC)

We report the spectral lag analysis for GRB 130313A (GCN Circ. 14293 & 14296)
based on the BAT data. Using 8-ms binned light curve, the spectral lag 
for the 15-25 keV to 50-100 keV bands is 9.2 (+11.5/-7.7) msec.  
These lag values place this burst in the short burst category. There is no evidence 
for extended emission.  


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14307
SUBJECT: GRB 130313A: TNG optical observations
DATE:    13/03/14 15:45:14 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, S. Covino, A. Melandri (INAF/OAB), C. P. Padilla Torres, G.
Andreuzzi (INAF/TNG) report on behalf of the CIBO collaboration:

We observed the field of GRB 130313A (Gompertz et al., GCN 14293) with the
TNG telescope located in the Canary Islands. A total 1800 s exposure in
the SDSS r filter was acquired, with mean time 2013 Mar 14.2314 UT (13.4
hours after the GRB). Sky conditions were good and the seeing was 0.9".

No clear optical afterglow is detected inside the refined XRT error circle
(Osborne et al. GCN 14300; Gompertz et al., GCN 14305) down to a limiting
magnitude r~25 mag (3sigma c.l.; calibrated against nearby SDSS stars). In
particular, we do not detect the 3 optical sources reported by de Ugarte
Postigo et al. (GCN 14302).


GRB_name: GRB130313A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14308
SUBJECT: GRB 130313A: RATIR Optical and NIR Observations
DATE:    13/03/14 15:56:30 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico 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 the short-duration GRB 130313A (Gompertz, et al.,
GCN 14293) 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 March 14.30 to
2013 March 14.52 UTC (14.96 to 20.25 hours after the BAT trigger),
obtaining a total of 3.5 hours exposures in the r' and i' bands and 1.5
hours of exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (Osborne et al., GCN 14293;
Gompertz et al., GCN 14305), in comparison with SDSS DR8 and 2MASS, we
derive the following upper limits (3-sigma) in the AB magnitude system:

  r'  > 23.6
  i'  > 23.3
  Z   > 22.3
  Y   > 22.0
  J   > 21.8
  H   > 21.3

These magnitudes 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: GRB130305A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14309
SUBJECT: GRB 130305A: TLS Tautenburg observations
DATE:    13/03/15 00:20:12 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

B. Stecklum, D. A. Kann and C. Hoegner (TLS Tautenburg) report:

Following the announcement of the ground-detection of the bright GRB
130305A by Swift BAT (Cummings & Palmer 2013, GCN 14257), which was also
detected by Fermi LAT (Guiriec et al. 2013, GCN 14260), Fermi GBM (Yu &
Xiong 2013, GCN 14261) and Konus-Wind (Golenetskii et al. 2013, GCN
14262), we initiated observations with the 1.34m Schmidt telescope of the
Thueringer Landessternwarte Tautenburg under excellent weather conditions
at 18:11 UT, 22 minutes after the GCN notice.

We obtained 6 x 600 sec exposures in the Rc band, centered 0.29299 days
after the GRB. At the position of the XRT afterglow (Malesani et al. 2013,
GCN 14263, Zhang et al. 2013, GCN 14276), we detect no source down to a 2
sigma upper limit of Rc > 23.2. Photometric calibration was obtained with
respect to several SDSS stars in the field, using the transformations of
Lupton (2005).

This upper limit is deeper than the one obtained by Kumar & Pandey (2013,
GCN 14274) at a similar time and earlier than several other reported
observations (Cenko 2013, GCN 14265; Butler et al. 2013, GCN 14267;
Breeveld et al. 2013, GCN 14268). We detect all the surrounding sources
seen in the deep Gemini image (Cucchiara et al. 2013, GCN 14272).

A second observation was attempted a day later, but due to inclement
weather conditions only a single 600 sec image could be successfully
obtained. It is significantly shallower than the stack of the first night
and shows no changes.

This message may be cited.


GRB_name: GRB130310A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14310
SUBJECT: GRB 130310A : Suzaku WAM observation of the prompt emission
DATE:    13/03/15 10:55:37 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

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

The bright short GRB (Fermi-LAT detection ; Guiriec et al., GCN14282;
Sbarufatti et al., GCN 14288) triggered by the Suzaku Wide-band All-sky
Monitor (WAM)
which covers an energy range of 50 keV - 5 MeV at 20:09:45 UT (=T0).

The observed light curve shows a single peak structure starting at
T0 s, ending at T0+1 s with a duration (T90) of about 0.3 seconds.
The fluence in 100 - 1000 keV was 7.78 (-1.13, +2.72) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0 s was 14.34(-1.37,+2.30)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+1 s is well fitted by GRB Band model:
the low-energy photon index alpha: -1.13 (-0.25, +0.16),
                      beta        : -2.07 (-0.32, +0.19)
and the peak energy Epeak: 1000 (-442, +639) keV (chi^2/d.o.f = 43.2/44).
All the quoted errors are at statistical 90% confidence level.

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


GRB_name: GRB130315A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14311
SUBJECT: GRB 130315A: Swift detection of a burst
DATE:    13/03/15 12:59:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

P. A. Evans (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
B.P. Gompertz (U Leicester), J. A. Kennea (PSU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
M. H. Siegel (PSU), R. L. C. Starling (U Leicester) and
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team:

At 12:45:32 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130315A (trigger=551126).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 157.542, -51.810 which is 
   RA(J2000)  =  10h 30m 10s
   Dec(J2000) = -51d 48' 36"
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 40 sec.  The peak count rate
was ~1100 counts/sec (15-350 keV), at ~10 sec after the trigger. 
There is a possible flare at T+160 sec. 

The XRT began observing the field at 12:48:13.7 UT, 160.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 157.54648, -51.79244 which
is equivalent to:
   RA(J2000)  = 10h 30m 11.16s
   Dec(J2000) = -51d 47' 32.8"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 63 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.27
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.10e-08 erg cm^-2 s^-1 (0.2-10
keV). 

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 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
0.36. 

Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130315A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14312
SUBJECT: GRB130315A BOOTES-3 optical limit
DATE:    13/03/15 14:43:14 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C. Tello, R. Snchez-Ramirez, M. Jelinek (IAA-CSIC Granada), J. Gorosabel
(UPV/EHU-IAA/CSIC), W. Allen (Vintage Lane Obs.), Ph. Yock (Auckland
Univ.), P. Kubanek (IP AS CR & IAA-CSIC), and A. J. Castro-Tirado
(IAA-CSIC) report on behalf of a larger collaboration:

  "We observed the field of GRB 130315A (Evans et al., GCNC 14311),
detected by Swift/BAT, with the 0.6m Yock-Allen robotic telescope
(BOOTES-3) located in Blenheim, New Zealand. Unfiltered images were
obtained starting 13:21:02UT (35m after the burst, limited by clouds). An
exposure of 30 seconds revealed no uncatalogued sources down to a magnitude
of RMag~16.5 when compared to the USNO-B1 catalogue."


GRB_name: GRB130305A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14313
SUBJECT: GRB 130305A: PTF P48 optical upper limits
DATE:    13/03/15 19:28:32 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (UC Berkeley), and D. A. Brown
(Syracuse) report on behalf of a larger collaboration:

We have imaged the 3-sigma Swift XRT error circle (D. Malesani, GCN
14263) of GRB130305A (Fermi384176354, J. R. Cummings, GCN 14257) with
the Palomar 48 inch Oschin telescope (P48) as part of the Palomar
Transient Factory (PTF).  Images were obtained in the Mould R filter
at 2013-03-06 at 05:13:35 and 05:56:17 UTC, 17.6 and 18.3 hours after
the trigger.

We find no point source, fading or otherwise, to 5-sigma limiting
magnitudes of 20.8 and 20.8.


GRB_name: GRB130313A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14314
SUBJECT: GRB 130313A: Swift/UVOT Upper Limits
DATE:    13/03/15 21:41:57 GMT
FROM:    Tyler Pritchard at PSU  <tapritchard@astro.psu.edu>

T. A. Pritchard (PSU) and B. P. Gompertz (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130313A
81 s after the BAT trigger (Gompertz et al., GCN Circ. 14293).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 14300)
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            81          231          147         >20.6
u_FC               293          543          246         >20.3
white               81        17899         2332         >22.4
v                  625        22348         1681         >20.4
b                  550        16987         1327         >21.4
u                  293         6955          697         >20.3
w1                 674         6750          471         >20.9
m2                 649         6545          413         >21.0
w2                 600        18671         2110         >21.5

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).


GRB_name: GRB130315A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14315
SUBJECT: GRB 130315A, Swift-BAT refined analysis
DATE:    13/03/15 21:58:28 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), P. A. Evans (U Leicester) N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), 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 130315A (trigger #551126)
(Evans, et al., GCN Circ. 14311).  The BAT ground-calculated position is
RA, Dec = 157.541, -51.794 deg which is
    RA(J2000)  =  10h 30m 09.9s
    Dec(J2000) = -51d 47' 37.4"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 42%.

The mask-weighted light curve shows two broad peaks, the first starting at
~T-10 sec, peaking at T+10 sec and then slowly declining until ~T+70 sec.  The
rise to the second peak begins almost immediately, with a broad peak around
T+160 sec and falling to background by T+240 sec. Note that a slew took the
source out of the field of view at ~T+650 sec. T90 (15-350 keV) is
233.4 +- 17.5 sec (estimated error including systematics).

The time-averaged spectrum from T-3.30 to T+268.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.81 +- 0.08.  The fluence in the 15-150 keV band is 4.9 +- 0.2 x 10^-6 erg/cm2. 
The 1-sec peak photon flux measured from T+8.41 sec in the 15-150 keV band is 
1.0 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/551126/BA/


GRB_name: GRB130310A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14316
SUBJECT: Swift XRT observations of GRB 130310A
DATE:    13/03/15 22:03:36 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/PSU), D. N. Burrows (PSU), P. E. Evans (U
Leicester) report on behalf of the Swift XRT team:

Swift performed a total of 7 pointings for this burst on March 11th: 4x1ks
covering the Fermi LAT error circle (Guiriec et al., GCN #1482) and 3x1.5
ks covering the IPN error box (Golenetskii et al., GCN #14284). We detect
a total of 5 sources:

#  RA          DEC          Err     counts  rate(counts/ks)
1  09 28 45.9  -17 18 49.5  7.4"    9     11  (+11/-7)
2  09 29 27.0  -17 30 13.8  6.8"    12     13  (+14/-8)
3  09 28 59.0  -17 00 40.8  5.4"    8     9   (+10/-7)
4  09 27 58.9  -17 12 57.9  8.6"    10     11  (+12/-7)
5  09 27 31.7  -17 08 55.3  11.0"   5     4.7 (+6/-4)

The fluxes are computed at the 99% confidence level, following Kraft,
Burrows & Nousek (1991). The background level was computed both generally,
using the 'background' task of XIMAGE on each pointing, and locally, using
the 'sosta' task of XIMAGE, and selecting the highest value.
All sources are inside the LAT error circle, but only source #5 is inside
the IPN error box.

Swift performed another observation in the direction of source #5 on March
13th, with a 3.4 ks exposure. The 99% confidence level upper limit at the
position of source #5 is 4.6E-3 counts/s, which does not give strong
evidence for fading.

No further observations are planned.

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


GRB_name: GRB130315A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14317
SUBJECT: GRB 130315A: Swift-XRT refined Analysis
DATE:    13/03/16 00:59:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 130315A (Evans  et al. GCN
Circ. 14311),  from 167 s to 29.4 ks after the BAT trigger. The data
comprise 337 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
157.54687, -51.79362 which is equivalent to:

RA (J2000): 10 30 11.25
Dec(J2000): -51 47 37.0

with an uncertainty of 3.6 arcsec (radius, 90% confidence).

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

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.49 (+/-0.04). The
best-fitting absorption column is  2.88 (+0.19, -0.18) x 10^21 cm^-2,
in excess of the Galactic value of 2.3 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.1 (+/-0.3) and a
best-fitting absorption column of 3.1 (+1.2, -0.8) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.9 x 10^-11 (6.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+1.2, -0.8) x 10^21 cm^-2
Galactic foreground: 2.3 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.1 (+/-0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00551126.

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


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14318
SUBJECT: GRB 130313A: 5.8 GHz VLA upper limit
DATE:    13/03/16 05:55:06 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the position of the short-duration GRB 130313A (Gompertz et
al., GCN 14293) with the Karl G. Jansky Very Large Array (VLA) beginning on
2013 March 14.44 UT (18.5 hr post-burst) at a mean frequency of 5.8 GHz. In
1 hour of observations, we do not detect any source within the BAT-refined
position (Barthelmy et al., GCN 14296), within the latest XRT position
(Osborne et al., GCN 14300), or in coincidence with any of the reported
optical sources (de Ugarte Postigo et al., GCN 14302). We therefore place a
3-sigma limit of ~60 microJy on the radio counterpart of GRB 130313A at
18.5 hr after the burst."


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14319
SUBJECT: GRB130313A: GTC early optical limits
DATE:    13/03/16 08:10:39 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

J. Gorosabel (UPV/EHU-IAA/CSIC), J.C. Tello, R. Snchez-Ramrez, M.
Jelinek, A. J. Castro-Tirado (IAA-CSIC Granada), report on behalf of a
larger
collaboration:

"We have observed the field of the short duration GRB 130313A (Gompertz et
al., GCN 14293) using the 10.4m GTC in Sloan r,i and z filters with a
seeing of ~1.3", however at an airmass of ~1.4 and with cirruses across
the field. The combined exposure of 12x70 s images with a Sloan i filter
taken starting 02:54:47UT and ending 03:14:58UT (10.7 - 11.1 hours after
the burst) shows no afterglow candidate within the refined XRT uncertainty
circle (Osborne et al., GCN 14300) down to a magnitude of i > 23.5 when
compared to the SDSS Photometric Catalog, Release 6."


GRB_name: GRB130315A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14320
SUBJECT: GRB 130315A: SALT optical observations
DATE:    13/03/16 15:02:46 GMT
FROM:    Timothy Pickering at SALT  <tim@saao.ac.za>

T. E. Pickering, P. Vaisanen, V. van Wyk report on behalf of SALT:

We have observed the field of GRB 130315A (Evans et al. GCN 14311) using the RSS imager/spectrograph at the Southern African Large Telescope (SALT).  The observations began at 17:40 UT, just under 5 hours after the initial Swift trigger.  Imaging was performed using a broadband filter with a blue cutoff at 4600 A and three narrow-band filters centered at 4820 A, 6530 A, and 8175 A. The data were somewhat hampered by scattered clouds and mediocre seeing.  Comparison to a DSS2 red image finds no evidence of a new source within the error circle of the refined XRT position (3.6"; Page et al. GCN 14317).  The limiting magnitude of our best images is roughly ~0.5 mag deeper than the DSS2 image which gives a detection upper limit of r ~ 21 based on comparison with nearby stars in the GSC 2.3.  

This message may be cited.


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14321
SUBJECT: GRB 130313A: optical upper limit in Mondy observatory
DATE:    13/03/16 19:54:28 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 130313A (Gompertz  et al., GCN 
14293) with AZT-33IK telescope of Sayan observatory (Mondy) on March 13 
between (UT) 17:45:47 - 22:55:49. We took several images in R-filter of 90 s 
exposure which cover  partially the refined BAT error box (Barthelmy et al., 
GCN 14296).  Within  XRT position (Gompertz et al., GCN  14297; Osborne et 
al., GCN  14300) we do  not detect any source. Preliminary photometry of 
combined images is following

UT start,    t-t0           filter      Exp.   OT      UL (3 sigma)
             (mid, days)                (s)

17:54:56    0.06737        R          20x90   n/d     20.3
17:54:56    0.17047        R        147x90   n/d     23.3

The photometry is based on two SDSS DR8  stars
SDSS J154537.18-001931.3 RA = 15 45 37.18 Dec = -00 19 31.3 (J2000), R = 
18.95
SDSS J154535.15-001918.8 RA = 15 45 35.15 Dec = -00 19 18.8 (J2000), R = 
16.76 


GRB_name: GRB130313A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14322
SUBJECT: GRB 130313A: optical upper limit in CrAO
DATE:    13/03/16 19:54:45 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 130313A (Gompertz  et al., GCN 
14293) with ZTSh telescope of CrAO observatory (Mondy) on March 14
between (UT) 00:23:52 - 02:11:00. We took several images in R-filter of 60 
s exposure which cover  the  refined BAT error box (Barthelmy et al., GCN 
14296). Within  XRT position (Gompertz et al., GCN  14297; Osborne et al., 
GCN  14300) we do  not detect any source. Preliminary photometry of a 
combined image is following

UT start,    t-t0           filter      Exp.   OT      UL (3 sigma)
             (mid, days)                (s)

00:23:52    0.3818        R     24x60   n/d     22.7

The photometry is based on USNO-B1.0  star
0896-0256107 15:45:37.83 -00:22:18.2 R=16.04


GRB_name: GRB130315A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14323
SUBJECT: GRB 130315A: Swift/UVOT Upper Limits 
DATE:    13/03/16 20:19:38 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

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

     Swift/UVOT began settled observations of the field of GRB 130315A
starting 171 s after the BAT trigger (Evans et al., 2013, GCNC 14311).
We do not detect any new source within the XRT error circle (Page et al.,
2013, GCNC 14317).  Preliminary UVOT 3-sigma upper limits at this
position are presented below.

------------------------------------------------
Filter      TSTART     TSTOP    Exposure     Mag
------------------------------------------------
white (FC)     171       321         147   >21.1 
    u (FC)     330       580         246   >20.3 
------------------------------------------------
    v         4476    23,657        1136   >20.7 
    b         3860    28,925        1685   >21.7 
    u          330    17,889        1443   >21.4 
 uvw1         4887    17,764        1995   >21.3 
 uvm2         4681    16,857        1277   >21.0 
 uvw2         4271    22,898        1279   >21.2 
white          171    29.424        1022   >22.2 
------------------------------------------------

    The quoted upper limits have not been corrected for the Galactic
extinction along the line of sight to this burst of E_{B-V} = 0.32 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 photometry is affected by the presence of a J = 15.4 mag 2MASS
source 10301128-5147395 located 2.3 arcsec south of the XRT position.


GRB_name: GRB130305A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14324
SUBJECT: GRB 130305A: optical upper limit in Mondy observatory
DATE:    13/03/17 15:30:22 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.Volnova (SAI MSU/IKI), R. Burenin(IKI), E. Klunko (ISTP), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed We imaged the location of the Swift (Cummings et al., GCN 
14257), Fermi (Guiriec et al., GCN 14260; Yu et al., GCN 14261), and 
Konus (Golenetskii et al., GCN 14262) GRB 130305A with AZT-33IK 
telescope of Sayan observatory (Mondy) on March 05 between (UT) 20:44:08 
- 22:17:04. We took several images in R-filter of 100 s exposure under 
unfavorable seeing (FWHM) of about 4.2 arcsec.  We do not detect any 
sources within the XRT error circle (Malesani
et al., GCN 14263). A photometry of a combined image is following

UT start,  t-t0       Filter Exp.   OT    UL (3 sigma)
           (mid, days)        (s)

20:44:08  0.41071     R      35x100 n/d   21.4

The photometry is based on  SDSS DR8  star
SDSS J074702.42+520103.3 07:47:02.43 +52:01:03.4 R = 16.94


GRB_name: GRB130315A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14325
SUBJECT: GRB 130315A: GROND afterglow candidate
DATE:    13/03/17 18:11:35 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

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

We observed the field of GRB 130315A (Swift trigger 551126; Evans et
al., GCN 14311) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

First-epoch observations started on March 15, 2013, at 23:51 UT, 11.1
hrs after the GRB trigger. They were performed at an average seeing of
0."7 and at an average airmass of 1.18. No evidence for a fading
afterglow was found.

Second-epoch observations were executed the following night (38.4 hr
after the trigger) under slightly worse observing conditions. A
comparison with the first-epoch images reveales a fading source at the
south-east border of the Swift/XRT error circle (Page et al., GCN 14317)
at coordinates

RA (J2000)  =  10:30:11.54
Dec (J2000) = -51:47:39.8

with an uncertainty of 0."5 in each coordinate.

Based on a total exposure time of 1500 s in r'i'z' at a midtime of
12.8 hrs after the burst, for this source we measure the following
preliminary AB magnitudes:

r' = 22.0 +/- 0.1,
i' = 21.5 +/- 0.1,
z' = 21.1 +/- 0.1.

Between both epochs this object faded by more than 1 magnitude, implying
a decay with alpha > 0.75.

The given magnitudes are calibrated against GROND zeropoints. The
Galactic reddening along the line of sight is E(B-V)= 0.36 mag (Schlegel
et al. 1998).


GRB_name: GRB130305A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14326
SUBJECT: GRB 130305A: Gemini follow-up observations
DATE:    13/03/21 22:13:43 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick Observatory), S. B. Cenko 
(UC Berkeley), D. Perley (Caltech) report on behalf of 
a large collaboration:

"On March 20.31 UT we observed again the field of GRB 130305A 
(Cummings & Palmer, GCN 14257; Yu & Xiong, GCN 14261; 
Guiriec et al., GCN 14260) with the Gemini-North telescope
equipped with the GMOS camera.

We obtained 7x180s exposures, for a total integration time
of 21 minutes (T_mid = T0+13.10 days). 

We compared the coadded image with our pervious observation 
(Cucchiara et al. GCN 14272) and performed an image subtraction 
between the two epochs.

No variable source appears in the subtraction image, in particular 
we note that the galaxy reported in GCN 14272 appears of constant 
brightness.

We estimated a limiting magnitude of r' > 26.0 within the XRT
circle.

We thank the Gemini staff for performing this observation.


GRB_name: GRB130320A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14327
SUBJECT: IPN Triangulation of GRB 130320A (long/very bright)
DATE:    13/03/22 17:11:59 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

The long-duration, very bright GRB 130320A has been observed by 
Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), and AGILE (MCAL), so 
far, at about 25720 s UT (07:08:40).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   192.684 (12h 50m 44s) -14.471 (-14d 28' 15")
  Corners:
   190.889 (12h 43m 33s) -17.026 (-17d 01' 34")
   190.945 (12h 43m 47s) -17.088 (-17d 05' 15")
   195.164 (13h 00m 39s) -10.078 (-10d 04' 40")
   195.128 (13h 00m 31s)  -9.967 ( -9d 58' 00")
  ---------------------------------------------
The error box area is 0.646 sq. deg, and its maximum dimension is
8.2 deg (the minimum one is 5 arcmin).

This box may be improved.

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

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130320_T25724/IPN/


GRB_name: GRB130320A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14328
SUBJECT: Konus-Wind observation of GRB 130320A
DATE:    13/03/24 12:28:11 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The intense long-duration GRB 130320A
(IPN triangulation: Hurley et al., GCN 14327)
triggered Konus-Wind at T0=25724.822s UT (07:08:44.822)

The light curve shows a double-peaked pulse with a total
duration of ~20 s.
The emission is seen up to 5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130320_T25724/
Note: periodic "dips" visible in this light curve are due
to the GRB source occultation by the spacecraft structure.

As observed by Konus-Wind, the burst
had a fluence of (2.6  0.05)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.960 s,
of (1.85  0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum
(measured from T0 to T0+22.784 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model,
for which:
alpha = -0.78  0.05,
and Ep = 295  7 keV,
chi2 = 85.0/93 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+2.048 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model,
for which:
alpha = +0.27  0.06,
and Ep = 364  7 keV,
chi2 = 91.1/98 dof.

All the quoted results are preliminary.


GRB_name: GRB130325A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14329
SUBJECT: GRB 130325A: Fermi GBM detection
DATE:    13/03/25 18:55:30 GMT
FROM:    David Tierney at UCD  <david.tierney@ucd.ie>

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

"At 04:51:54.30 UT on 25 March 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130325A (trigger 385879917 / 130325203).

The on-ground calculated location, using the GBM trigger
data, is RA = 130.71, DEC = -21.12 (J2000 degrees,
equivalent to 08 h 42 m, -21 d 07 '), with an uncertainty
of 2.15 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 51.0 degrees.

The GBM light curve consists of a single bright pulse
with a duration (T90) of 9.7 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+9.216 s is
best fit by a Band function with Epeak = 202.20 (+17.50/-15.60) keV,
alpha = -0.73 (+0.06/-0.05), and beta = -2.18 (+0.09/-0.12).

The event fluence (10-1000 keV) in this time interval is
(8.25 +/- 0.27)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.8 s in the 10-1000 keV band
is 12.9 +/- 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: GRB130315A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14330
SUBJECT: report: GRB 130315A: Zadko observatory - Gingin optical observations
DATE:    13/03/26 14:26:44 GMT
FROM:    Husne Dereli at ARTEMIS/OCA/TAROT/ZADKO  <husne_dereli@yahoo.com>

GRB 130315A: Zadko observatory - Gingin optical observations
------------------------------**------------------------------**----------
H. Dereli (UNS-CNRS-OCA), A. Klotz (IRAP-CNRS-OMP),
D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (IRAP-CNRS-OMP), M. Boer, K. Siellez, O. Bardho (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA)
report:

We imaged the field of GRB 130315A detected by SWIFT
(trigger 551126) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 1.22h after the GRB trigger.
The elevation of the field increased from
65 degrees above horizon and weather conditions
were good.

We co-added a series of unfiltered exposures and we
substracted images taken with the same telescope
4h to 8h later to eliminate contaminations by
foreground stars. We did not detect any optical
transient at the position provided by Schmidl
et al. (GCNC 14325):

t0+1.22h to t0+1.54h : Rlim = 20.4

This limiting magnitude and the detection
of Schmidl et al. (GCNC 14325) implies a
decay with alpha < 0.67. As Schmidl et al.
(GCNC 14325) announced alpha > 0.75 after 12h
we suspect a late rising of a faint afterglow
or a break of the decay.

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


GRB_name: GRB130327A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14331
SUBJECT: GRB 130327A: Swift detection of a burst
DATE:    13/03/27 02:09:19 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), V. Mangano (INAF-IASFPA),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), D. M. Palmer (LANL), M. H. Siegel (PSU) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 01:47:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130327A (trigger=552063).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 91.992, +55.730 which is 
   RA(J2000)  =  06h 07m 58s
   Dec(J2000) = +55d 43' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a weak single peak
with a duration of about 10 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:49:55.0 UT, 141.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 92.0387, 55.7143 which
is equivalent to:
   RA(J2000)  = 06h 08m 09.29s
   Dec(J2000) = +55d 42' 51.5"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 110 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 1.31
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 104 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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 0.13. 

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: GRB130325A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14332
SUBJECT: GRB 130325A: Fermi LAT detection
DATE:    13/03/27 02:12:28 GMT
FROM:    Julie McEnery at NASA/GSFC  <julie.e.mcenery@nasa.gov>

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

The Fermi Large Area Telescope (LAT) detected emission from GRB 130325A
(GBM trigger 130325203/385879917).

This burst was detected over a 1300 s integration following the GBM 
trigger using
the P7SOURCE data class. This burst seems unusual because despite being 
within
the field of view of the LAT at the time of the GBM trigger, it was not 
detected by
the LAT during the prompt phase, which lasted 10 s (GCN 14329).

The best LAT on-ground location is found to be RA, DEC 122.78, -18.90 
(J2000)
with an error radius of 0.25 deg (68% containment, statistical error 
only), this
was 51 deg from the LAT boresight at the time of the trigger and 
triggered an
autonomous repoint of the spacecraft at 04:52:31.48 UT.

A Swift ToO has been submitted.

The Fermi LAT point of contact for this burst is Julie McEnery 
(julie.mcenery@nasa.gov).

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


GRB_name: GRB130327A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14333
SUBJECT: GRB 130327A: PAIRITEL NIR Afterglow Candidate
DATE:    13/03/27 03:39:24 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 130327A (Ukwatta et al., GCN 14331) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2013-Mar-27 02h21m22s UT, ~33.8 minutes after the Swift trigger.  In
mosaics (effective exposure time of ~25 m) taken simultaneously in the J,
H, and Ks filters, we marginally detect a source in the J band within the
XRT error circle (Ukwatta et al., GCN 14331).  Given the minor significance
of the detection in only a single filter, deeper observations are
encouraged to confirm if this possible source is indeed the afterglow of
GRB 130327A.

post burst
t_mid (hr) exp.(hr) filt  Mag
0.91       0.42     J     17.8 +/- 0.4
0.91       0.42     H     > 17.1
0.91       0.42     Ks    > 15.7


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


GRB_name: GRB130327A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14334
SUBJECT: GRB 130327A: RATIR Optical and NIR Observations
DATE:    13/03/27 04:56:14 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (UCSC), Eleonora Troja (GSFC), Enrico 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 130327A (Ukwatta, et al., GCN 14331) 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 2013/03 27.12 to 2013/03
27.17 UTC (1.16 to 2.17 hours after the BAT trigger), obtaining a
total of 0.82 hours exposures in the r' and i' bands and 0.35 hours of
exposure in the Z, Y, J, and H bands.

We detect one uncatalogued source within the XRT error region (GCN
14331), at a position RA , DEC: = 92.03875,  55.71504 (+/-0.5 ",
J2000).  This is 2.7" from the center of the XRT error circle.  In
comparison with USNO-B1 and 2MASS, we derive the following detections
and upper limit (3-sigma) in the AB magnitude system:

r'    21.22 +/- 0.10
i'    21.17 +/- 0.09
Z    20.09 +/- 0.14
Y    19.98 +/- 0.17
J    19.98 +/- 0.23
H     > 20.08

We also detect a second uncatalogued source just outside the XRT error
circle (3.9" from the center) at RA , DEC: 92.03822,  55.71326 (+/-0.5
", J2000):

r'    21.61 +/- 0.14
i'    20.36 +/- 0.05
Z    19.15 +/- 0.06
Y    18.72 +/- 0.06
J    18.70 +/- 0.07
H    18.53 +/- 0.09

We note that this second source has a brightness consistent with the
earlier PAIRITEL measurement (Morgan; GCN 14333).

We thank the staff of the Observatorio Astronmico Nacional in San
Pedro Mrtir.  Further observations are planned.


GRB_name: GRB130327A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14335
SUBJECT: GRB 130327A: Enhanced Swift-XRT position
DATE:    13/03/27 07:49:55 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 1239 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130327A, 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 = 92.03858, +55.71475 which is equivalent
to:

RA (J2000): 06h 08m 9.26s
Dec (J2000): +55d 42' 53.1"

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: GRB130325A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14336
SUBJECT: GRB 130325A Tiled Swift observations
DATE:    13/03/27 08:24:48 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 130325A. Automated analysis of the XRT data will be 
presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00013

Any uncatalogued X-ray sources detected in this analysis will be 
reported on this website. 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: GRB130327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14337
SUBJECT: GRB 130327A: ISON-NM optical upper limit
DATE:    13/03/27 09:59:23 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of  the Swift GRB 130327A (Ukwatta, et al., GCN 
14331) with 0.45-m telescope of ISON-NM observatory  on Mar. 27, 
between (UT) 02:44:04 - 03:27:54.  We took  several unfiltered images of 
30 s exposures.  Within enhanced XRT afterglow position (Osborne et al., 
GCN 14335) we do not detect any new object.  We marginally (S/N~2.5, R~ 
20.3)  detected "second uncatalogued source" (Morgan et al., GCN 14333; 
Butler et al., GCN 14334) at RA , DEC (J2000): 06 08 09.06 +55 42 48.5. 
  A photometry of combined  image is based  on the USNO-B1.0 (R2) 
nearby  stars

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

02:44:04  0.0546        60x30      n/d    20.0


GRB_name: GRB130325A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14338
SUBJECT: Konus-Wind observation of GRB 130325A
DATE:    13/03/27 11:00:30 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 130325A (Fermi-GBM detection: Tierney, GCN 14329;
Fermi-LAT detection: Vianello et al., GCN 14332)
triggered Konus-Wind at T0=17516.880s UT (04:51:56.880)

The light curve shows a single pulse with a total duration of ~8 s.
The emission is seen up to 6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130325_T17516/

As observed by Konus-Wind, the burst
had a fluence of (8.1  1.4)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.704s,
of (3.7  0.4)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.90  0.18,
the high energy photon index beta = -2.4  0.3,
the peak energy Ep = 186  28 keV,
chi2 = 59.8/78 dof.

All the quoted results are preliminary.


GRB_name: GRB130327A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14339
SUBJECT: GRB 130327A: Swift/UVOT Upper Limits
DATE:    13/03/27 14:22:35 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 130327A
104 s after the BAT trigger (Ukwatta et al., GCN Circ. 14331).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 14335)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           104          254          147         >21.2
u_FC               317          567          246         >20.0
white              104         6491          727         >21.8
v                  646         6877          428         >19.8
b                  572         6286          432         >20.7
u                  317         6081          659         >20.4
w1                 695        12014         1111         >21.6
m2                 671        11107         1141         >21.0
w2                 622         6696          452         >21.9

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


GRB_name: GRB130327A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14340
SUBJECT: GRB 130327A: Weihai optical obsevations
DATE:    13/03/27 17:51:32 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of GRB 130327A (Ukwatta et al., GCN 14331) using
the 1m telescope located in Weihai, Shandong Province, China.
Observations started at 11:27:02 UT on 2013-03-27 (i.e, 9.658 hr after
the burst) in a seeing of ~2.8", and 10x360s I-band images were
obtained with a mean time of 10.158 hr post-burst.

Within the enhanced XRT error circle (Osborne et al., GCN 14335), no
credible source is detected in the stacked I-band image, down to a
limit of R>20.2 mag, calibrated with the USNO B1 catalogue.

A source, with R~19.2 mag and somehow extended along NW-SE, is
detected at the position of the "second uncatalogued source" reported
by Butler et al. (GCN 14334), and confirmed in Elenin et al. (GCN
14337). This source might be the one in Morgan (GCN 14333). Since it
is 5.5" away from the center of the enhanced XRT error circle (radius:
1.9") and it's getting brightening significantly, this source is
unlikely related to the afterglow of the burst.

We thank Dayong Ren for carrying out thee observations.


GRB_name: GRB130327A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14341
SUBJECT: GRB 130327A: Swift-XRT refined Analysis
DATE:    13/03/27 19:09:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 130327A (Ukwatta  et al. GCN
Circ. 14331),  from 83 s to 45.1 ks after the  BAT trigger. The data
comprise 902 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN. Circ 14335).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.3 (+0.5, -0.4), followed by a break at T+348 s to an
alpha of 0.22 (+0.07, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.28 (+0.29, -0.13). The
best-fitting absorption column is  consistent with the Galactic value
of 1.3 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.2 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+3.7, -0) x 10^20 cm^-2
Galactic foreground: 1.3 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.28 (+0.29, -0.13)

If the light curve continues to decay with a power-law decay index of
0.22, the count rate at T+24 hours will be 0.012 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.7 x
10^-13 (4.8 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/00552063.

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


GRB_name: GRB130327A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14342
SUBJECT: GRB 130327A: Gemini Observations
DATE:    13/03/27 21:20:55 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

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

"On March 27.25 UT we observed the field of GRB 130327A 
(Ukwatta et al., GCN 14331) with the Gemini-North telescope
equipped with the GMOS camera.

We obtained a 4 minutes i' band image of the field:
the two sources identified by Butler et al. (GCN 14334)
are both detected.

The southern source (#1) is located at
RA: 06:08:09.12 (J2000)
Dec: +55:42:47.98 (J2000)

The northern source (#2) is located inside the XRT revised 
error circle (Osborne et al. GCN 14335) at:

RA: 06:08:09.25 (J2000)
Dec: +55:42:54.39  (J2000)

Using several nearby USNO-B1 stars we estimated i' = 19.81 
+- 0.02, (source #1), and i' = 21.75 +- 0.06 (source #2), 
which is 0.43 mag fainter than the RATIR observations. 

We also obtained a 2x900s spectra of these two sources under cloudy
conditions, covering the 6000-10000A wavelength range: source #1
presents several stellar features, while source #2 presents a noisy 
continuum, but no clear absorption features are identified.

If we assume that source #2 is indeed GRB 130327A afterglow, we can
place an upper limit on the GRB redshift of z < 3.9, based on the 
absence of a Lyman-break features. 
Our acquisition image can be found here:
https://www.dropbox.com/s/ygvcdykmpow6gq5/sources.jpeg

We thank the Gemini staff for performing this observations,
in particular Andre'-Nicolas Chene' "


GRB_name: GRB130327A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14343
SUBJECT: GRB 130327A: Swift-BAT refined analysis
DATE:    13/03/27 21:54:49 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130327A (trigger #552063)
(Ukwatta, et al., GCN Circ. 14140).  The BAT ground-calculated position is
RA, Dec = 91.984, 55.732 deg, which is 
   RA(J2000)  =  06h 07m 56.2s 
   Dec(J2000) = +55d 43' 56.2" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 61%.
 
The mask-weighted lightcurve shows a single peak starting at ~T-5 sec,
peaking at ~T+1 sec, and ending at ~T+8 sec.  T90 (15-350 keV) is
9.0 +- 2.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-4.38 to T+5.62 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.26 +- 0.36.  The fluence in the 15-150 keV band is 2.3 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.62 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/552063/BA/


GRB_name: GRB130327B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14344
SUBJECT: GRB 130327B: gamma-ray detection by AGILE
DATE:    13/03/27 23:24:56 GMT
FROM:    Ettore Del Monte at IASF/INAF  <sa.grb@iaps.inaf.it>

F. Longo (University of Trieste and INFN Trieste), A. Giuliani  
(INAF/IASF Milan), M. Marisaldi (INAF/IASF Bologna), E. Del Monte  
(INAF/IAPS Rome), F. Lazzarotto, I. Donnarumma, Y. Evangelista, M.  
Feroci, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda  
(INAF/IAPS Rome), G. Barbiellini, (INFN Trieste), A. Bulgarelli, F.  
Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Galli  
(INAF/IASF Bologna), A. Chen, S. Mereghetti, F. Perotti, P. Caraveo  
(INAF/IASF Milan), M. Tavani, V. Vittorini, A. Argan, G. Piano, S.  
Sabatini, M. Cardillo (INAF/IASF Rome), G. Pucella (ENEA Frascati), A.  
Pellizzoni, A. Trois (INAF/OA Cagliari), M. Pilia (ASTRON), S.  
Vercellone (INAF/IASF Palermo), P. W. Cattaneo, A. Rappoldi (INFN  
Pavia), P. Picozza, A. Morselli, E. Striani, (INFN Roma-2), M. Prest,  
E. Vallazza (Universita' dell'Insubria), P. Lipari, D. Zanello (INFN  
Roma-1), P. Giommi, C. Pittori, F. Lucarelli, P. Santolamazza, F.  
Verrecchia (ASDC) and G. Valentini (ASI), on behalf of the AGILE Team,  
report:

The AGILE Gamma Ray Imaging Detector (GRID) detected emission from GRB  
130327B, localised by Fermi/GBM  
(http://gcn.gsfc.nasa.gov/other/386065447.fermi). The GRB occurred at  
approximately 28 deg off-axis in the field of view
of the AGILE/GRID.

A preliminary analysis of the AGILE/GRID data in temporal coincidence  
with the GRB shows a significant excess of gamma-ray events above 80  
MeV at the location of the event. Most of the events detected by the  
AGILE/GRID have times between ~ t0 + 9 sec and t0 + 14 sec where t0 is  
27 March 2013 at 08:24:04.05 UT.

The GRB was also detected also by the AGILE/MCAL, operating in the  
energy range 0.5 - 100 MeV.

A more detailed analysis of the AGILE data is in progress.
More observations of this interesting burst are strongly encouraged.

This message may be cited.


GRB_name: GRB130327B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14346
SUBJECT: GRB 130327B: Fermi GBM detection
DATE:    13/03/28 03:35:36 GMT
FROM:    Vandiver Chaplin at UAH/Fermi-GBM  <chapliv@email.uah.edu>

V.Chaplin (UAH) and G. Fitzpatrick (UCD)
report on behalf of the Fermi GBM Team:

"At 08:24:04.05 UT on 27 March 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130327B (trigger 386065447 / 130327350), which was 
also detected by several instruments on-board the AGILE spacecraft 
(Del Monte et al. GCN 14344).

The on-ground calculated location, using the GBM trigger
data, is RA = 214.9, DEC = -74.6 degrees, with an uncertainty
of 1 degree (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 at the GBM trigger
time was 47 degrees. The Fermi Observatory executed a 
maneuver following this trigger and tracked the burst location 
for the next 2.5 hours, subject to Earth-angle constraints.

The GBM light curve consists of multiple spikes on top of a gradual
rise and decay.  The main emission occurs between T0 and T0+35 seconds.
The total duration (T90) is about 62 s (50-300 keV).
The time-averaged spectrum from T0-0.8 s to T0+33 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.57 +/- 0.02 and
the cutoff energy, parameterized as Epeak, is 341 +/- 6.3 keV.

The spectrum also fits a Band function with Epeak = 334 +/- 7 keV,
alpha = -0.56 +/- 0.02, and beta = -3.4 +/- 0.4. 

The event fluence (10-1000 keV) in this time interval is
(5.176 +/- 0.057)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+32.4 s in the 8-1000 keV band
is 12.7 +/- 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: GRB130327B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14347
SUBJECT: GRB 130327B: Fermi-LAT detection of a burst
DATE:    13/03/28 04:29:54 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

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

At 08:24:04 on March 27th, 2013, Fermi LAT detected high energy emission
from GRB 130327B, which was also detected by Fermi-GBM (trigger 386065447 /
130327350 ; Chaplin and Fitzpatrick GCN 14346) and by  AGILE  (Del Monte et
al. GCN 14344).

The best LAT on-ground location is found to be RA, DEC 218.09, -69.51
(J2000) with an error radius of 0.17 deg (68% containment, statistical
error only), this was about 50 deg from the LAT boresight at the time of
the trigger and triggered an autonomous repoint of the spacecraft.

The data from the Fermi LAT show a significant increase in the event rate
within 5 degree of the GBM location after the GBM trigger that is spatially
and temporally correlated with the GBM emission with high significance.
More than 20 photons above 100 MeV are observed within 100 seconds.

A Swift TOO observation has been requested.

The Fermi LAT point of contact for this burst is Julie McEnery (
julie.mcenery@nasa.gov).

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

[GCN OPS NOTE(28mar13): Per author's request, the date in the first sentence
was changed from "28" to "27".]


GRB_name: GRB130327B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14348
SUBJECT: Konus-Wind observation of GRB 130327B
DATE:    13/03/28 09:37:10 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 130327B
(AGILE detection: Longo et al., GCN 14344;
Fermi-GBM detection: Chaplin and Fitzpatrick, GCN 14346;
Fermi-LAT detection: Ohno et al., GCN 14347)
triggered Konus-Wind at T0=30247.662s UT (08:24:07.662)

The light curve shows a multi-peaked structure
with a total duration of ~35 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/GRB130327_T30247/

As observed by Konus-Wind, the burst
had a fluence of (5.6  0.5)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.352s,
of (4.9  0.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+40.704 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 = -0.59  0.08,
the high energy photon index beta = -2.65  0.25,
the peak energy Ep = 278  18 keV,
chi2 = 122/97 dof.

The spectrum at the maximum count rate (measured from T0 to T0+7.936 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 = -0.62  0.13,
the high energy photon index beta = -2.6  0.4,
the peak energy Ep = 314  39 keV,
chi2 = 97.6/92 dof.

All the quoted results are preliminary.


GRB_name: GRB130310A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14350
SUBJECT: GRB 130310A: RATIR Observations
DATE:    13/03/28 15:50:17 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Enrico 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 the Fermi-LAT detected GRB 130310A (Guiriec, et
al., GCN 14282) 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.  Data were
taken in the r' and i' channels for a central 9.8 x 7.3 arcmin^2 portion of
the IPN error region (Golenetskii, et al., GCN 14284), centered on RA, DEC
= 141.90061, -17.10809 (J2000),  in 2 epochs, 1.31-1.47 days after the
Fermi trigger and 3.31-3.45 days after the Fermi trigger.  We reach a
limiting magnitude ~24 (AB) in both channels in both epochs.  Data were
captured in the Z, Y, J, and H bands over a larger field (14.8 x 12.5
arcmin^2), reaching a shallower limit (~22 AB).

Of the XRT candidate afterglows (Sbarufatti, et al., GCN 14316), only
source #5 is contained in our images.  We detect that source in both epochs
at a position RA, DEC = 141.881334, -17.147639 (+/-0.5" J2000):

Epoch 1:
  r' = 23.6 +/- 0.1
  i' = 23.6 +/- 0.2

Epoch 2:
  r' = 23.5 +/- 0.1
  i' = 23.3 +/- 0.2

These magnitudes are in the AB system, not corrected for Galactic
extinction in the direction of the GRB, and calibrated relative to USNO-B1.
 We find that source #5 has remained approximately constant in flux over a
2 day period.  It has not faded and is therefore unlikely to be the
afterglow of GRB 130310A.  This source is not detected in the Z, Y, J, or H
bands. We also note that we have searched for additional fading sources
(delta_mag > 0.5) in all bands and have found none.

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


GRB_name: GRB130306A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14351
SUBJECT: GRB 130306A: Confirmation of the X-ray Afterglow
DATE:    13/03/28 17:32:24 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

Swift performed a follow-up observation of the possible X-ray afterglow of
the BAT-detected GRB 130306A (Siegel et al., GCN Circ. 14287).  A 5 ks
observation took place on 14 March 2013, eight days after the burst.  
The reported source faded by at least a factor of three, from .009
counts s^-1 (observed flux 4.2 x 10^-13 erg cm^-2 s^-1) to an upper
limit of of .003 counts s^-1 (observed flux 1.5 x 10^-13 erg cm^-2 s^-1).
We therefore confirm that this was the X-ray afterglow of GRB 130306A.


GRB_name: GRB130327A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14352
SUBJECT: GRB 130327A: RATIR Optical/NIR afterglow confirmation
DATE:    13/03/29 00:21:46 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

Antonino Cucchiara (UCSC), 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), 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 reobserved the field of GRB 130327A (Ukwatta et al., GCN 14331, 
and Osborne et al., GCN 14335) 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 2013/03 28.13 to 2013/03 28.14 UTC (25.24 to 25.64 hours 
after the BAT trigger), obtaining a total of 0.33 hours exposure in the 
r' and i' bands and 0.14 hours of exposure in the Z, Y, J, and H bands.

The source identified in our previous RATIR observations within the refined XRT 
error circle (Butler et al. GCN 14334), and detected by Gemini (source #2 
in GCN  14342) has faded below our detection limit. We report the following 
3-sigma limits in the AB magnitude system:

 r' > 22.67
 i' > 22.46
 Z > 20.83
 Y > 20.47
 J > 20.07
 H > 19.99

This fading is consistent with the fading reported by Cucchiara et al. 
(GCN 14342). Based on these observations we confirm that this was the 
optical/NIR afterglow of GRB 130327A.

The second source identified outside the refined XRT error circle in the 
first RATIR observation and detected also by Gemini (as source #1 in GCN 14342) 
has not faded. Therefore it is unrelated to GRB 130327A. 


These magnitudes 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.

[GCN OPS NOTE(29mar13): Per author's request, the name in the Subject-line
was changed from "130727A" to "130327A".]


GRB_name: GRB130327B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14353
SUBJECT: Swift/XRT observation of GRB 130327B
DATE:    13/03/29 13:16:30 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA) and V. Mangano (INAF-IASFPA) for the Swift team:

We have analysed 7.9 ks of XRT data for the AGILE/Konus/Fermi-detected burst:
GRB 130327B (Longo et al, GCN 14344; Chaplin & Fitzpatrick, GCN 14346; Ohno et
al, GCN 14347; Golenetskii et al, GCN 14348),  from 110.1 ks to 128.6 ks after
the  Fermi/GBM trigger. The data are entirely in Photon Counting (PC) mode.  An
X-ray source is detected within the Fermi/LAT error circle. The refined XRT
position is RA, Dec = 217.87488, -69.40345 which is equivalent to:

RA (J2000): 14 31 29.97
Dec(J2000): -69 24 12.4

with an uncertainty of 4.1 arcsec (radius, 90% confidence). This
position is 459 arcsec from the Fermi/LAT position.  We cannot
determine at the present time whether the source is fading.

The count rate level is 4 x 10^-3 counts/s.  Further Swift observations have
been scheduled.


GRB_name: GRB130320B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14354
SUBJECT: IPN Triangulation of GRB 130320B (very long/bright)
DATE:    13/03/29 17:53:12 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

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

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

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

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

The very long, bright GRB 130320B was observed by Konus-Wind, Mars 
Odyssey (HEND), INTEGRAL (SPI-ACS), Fermi (GBM trigger 385478797), Swift 
(BAT), AGILE (MCAL), and MESSENGER (GRNS) at about 48247 s UT 
(13:24:07). The burst was outside the coded field of view of the BAT.

The burst shows three emission episodes with a total duration of ~380 s.
The entire burst was observed  by Konus-Wind, INTEGRAL-SPI-ACS, and Mars 
Odyssey (HEND). AGILE (MCAL) observed only the first (main) episode. 
Fermi (GBM) triggered on the second episode while exiting the SAA and 
also observed the third episode. MESSENGER (GRNS) triggered twice: on 
the first and on the third episode. These two episodes were also 
observed by Swift (BAT).

We have triangulated it to a 3 sigma error box whose
coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   195.539 (13h 02m 09s) -71.259 (-71d 15' 34")
  Corners:
   197.046 (13h 08m 11s) -71.078 (-71d 04' 39")
   196.172 (13h 04m 41s) -71.308 (-71d 18' 30")
   194.010 (12h 56m 02s) -71.427 (-71d 25' 38")
   194.909 (12h 59m 38s) -71.208 (-71d 12' 29")
  ---------------------------------------------
The error box area is 431 sq. arcmin, and its maximum dimension is
62 arcmin (the minimum one is 22 arcmin).

The IPN localizations of all three pulses are consistent with a common 
source.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130320_T48251/IPN/

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


GRB_name: GRB130320B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14356
SUBJECT: Konus-Wind observation of GRB 130320B
DATE:    13/03/30 11:59:08 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The very long intense GRB 130320B
(IPN triangulation: Hurley et al., GCN 14354)
triggered Konus-Wind at T0=48251.726s UT (13:24:11.726)

The burst consists of three emission episodes with a total duration of ~380 s.
The first episode (from ~T0-1 to ~T0+15s) shows very bright
multi-peaked pulse with strong hard-to-soft spectral evolution.
The second episode is a single weak soft-spectrum pulse
from T0+135 to T0+175s. The third episode (from ~T0+195 to ~T0+380s)
also shows a single pulse, more intense and harder than the second one.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130320_T48251/

As observed by Konus-Wind, the burst
had a total fluence of (7.8  0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.704s,
of (7.2  1.8)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+384.768 s)
is best fit in the 20 keV - 15 MeV range
by a simple power law with the photon index 2.24  0.03,
chi2 = 85.5/98 dof.

The spectrum at the onset of the burst (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 = -1.0  0.3,
the high energy photon index beta = -2.0  0.3,
the peak energy Ep = 340  190 keV,
chi2 = 23/25 dof.

The average spectrum of the second emission episode
(measured from T0+139.008 to T0+188.160 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model,
for which:
alpha = -1.7  0.3,
and Ep = 46  23 keV,
chi2 = 47/58 dof.

The average spectrum of the third emission episode
(measured from T0+294.656 to T0+384.768 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 = -1.23  0.17,
the high energy photon index beta = -2.25  0.19,
the peak energy Ep = 156  29 keV,
chi2 = 91.6/96 dof.


All the quoted results are preliminary.


GRB_name: GRB130327B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14357
SUBJECT: GRB 130327B: Suzaku WAM observation of the prompt emission
DATE:    13/04/01 12:17:36 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

Y. Ishida, M. Tashiro, Y. Terada, T. Yasuda, H. Ueno, S. Sugimoto
(Saitama U.), K. Yamaoka (Nagoya U.), M. Ohno, T. Kawano, K. Takaki,
R. Nakamura, Y. Fukazawa (Hiroshima U.), M. Yamauchi, M. Akiyama,
N. Ohmori, E. Mochinaga (Univ. of Miyazaki), 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 130327B (Chaplin et al GCN14346) was detected by the the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 08:24:04.751 UT (=T0).

The observed light curve shows double-peaked structure starting at
T0-1s, ending at T0+33s with a duration (T90) of about 30 seconds.
The fluence in 100 - 1000 keV was 3.29(+0.15/-0.21)x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+23s was 2.23 photons/cm^2/s in the
same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1s to
T0+33s is well fitted by a power-law with exponential cutoff model :
   dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
   alpha       0.89(+0.46/-0.56), and
   Epeak       484(+64/-50) keV (chi^2 / d.o.f. = 11.1/13).
All the quoted errors are at statistical 90% confidence level, in which
the systematic uncertainties are 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: GRB130211A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14358
SUBJECT: GRB 130211A: Retraction of afterglow candidate
DATE:    13/04/02 14:04:00 GMT
FROM:    Vladimir Sudilovsky at MPE  <vsudilov@mpe.mpg.de>

V. Sudilovsky and J. Greiner (both MPE Garching) report on behalf of the 
GROND
team:

Based on follow-up observations taken on 2013-03-29 (T+47 days after the 
initial
Swift trigger 548276; Oates et al., GCN 14195) of the source reported in GCN
14196, we retract our classification of this object. Since there is no
significant time variability associated with this source, we conclude 
that it
cannot be the afterglow of GRB 130211A.

The final magnitudes of this source (all AB) are:

g' > 24.0 mag,
r' = 23.5 +/- 0.1 mag,
i' = 22.3 +/- 0.1 mag,
z' = 21.7 +/- 0.1 mag,
J = 20.9 +/- 0.2 mag,
H = 20.5 +/- 0.2 mag, and
K > 20.2 mag.

We note that the large r'-i' color is consistent with the 4000 Angstrom 
break
expected from a galaxy at z~0.8. However, we caution that at this time 
there are
not enough data to make a definitive statement about this source.

Given magnitudes are calibrated against GROND zeropoints (g'r'i'z') as 
well as
2MASS field stars (JHK) and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=0.53 mag 
in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130407A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14359
SUBJECT: GRB 130407A: MAXI/GSC detection
DATE:    13/04/08 03:30:03 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

K. Fukushima, M. Nakajima, H. Negoro (Nihon U.), M. Serino (RIKEN), 
S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa (JAXA), 
T. Mihara, M. Sugizaki, M. Morii, T. Yamamoto, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), 
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Nakano (AGU), 
H. Tsunemi, M. Sasaki (Osaka U.), 
T. Onodera, K. Suzuki (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro (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

At 2013-04-07T23:37:01 UT, the MAXI/GSC nova alert system triggered on 
a bright uncatalogued X-ray transient source.
The transient emission started at and lasted at least 25 seconds
within the 41 second long triangular transit response of
MAXI/GSC. We identify this event as GRB 130407A.

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

 (R.A., Dec) = (248.10 deg, 10.51 deg) = (16 32 23, +10 30 39) (J2000)

with a 90% C.L. statistical error of 0.2 deg and an additional systematic 
uncertainty of 0.1 deg (90% containment radius). The 4-10 keV flux was 
170 +- 30 mCrab.

There was no significant excess flux in the previous transit at 22:04UT 
and in the next transit at 4/8 01:10 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB130407A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14360
SUBJECT: GRB 130407A Tiled Swift observations
DATE:    13/04/08 16:07:35 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
MAXI GRB 130407A. Automated analysis of the XRT data will
be presented online at
http://www.swift.ac.uk/xrt_products/TILED_GRB00014

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website. The probability of finding serendipitous 
sources, unrelated to the MAXI 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: GRB130408A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14361
SUBJECT: GRB 130408A: Swift detection of a burst
DATE:    13/04/08 22:11:30 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Y. Lien (NASA/GSFC/ORAU), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
D. Malesani (DARK/NBI), V. Mangano (INAF-IASFPA),
C. Pagani (U Leicester), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 21:51:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130408A (trigger=553132).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 134.401, -32.361 which is 
   RA(J2000) = 08h 57m 36s
   Dec(J2000) = -32d 21' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 12 sec.  The peak count rate
was ~3914 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 21:54:08.6 UT, 149.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 134.40809, -32.36136 which is
equivalent to:
   RA(J2000)  = 08h 57m 37.94s
   Dec(J2000) = -32d 21' 40.9"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 21 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 1.98
x 10^21 cm^-2 (Kalberla et al. 2005). 

UVOT data analysis is not available at this time. 

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


GRB_name: GRB130408A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14362
SUBJECT: GRB 130408A: Liverpool Telescope Optical candidate detection
DATE:    13/04/08 22:57:31 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), J. Japelj (U. Ljubljana), F.J. Virgili(LJMU),  
C.G. Mundell (LJMU) report:

The 2-m Liverpool Telescope robotically followed up GRB130408A (Swift  
trigger 553132, Lien et al., GCN 14361) 19.42 min after the GRB  
trigger time observing with SLOAN-gri filters.

The automatic LT-TRAP procedure detected an uncatalogued fading source  
candidate at:

RA=08:57:37.30
Dec=-32:21:38.90    (J2000)

with magnitude R~16.5 mag (vs USNOB1) ~20 min after the burst trigger.  
The object is clearly fading in all filters and we suggest this is the  
optical afterglow of GRB130408A.

Observations and analysis are ongoing.


GRB_name: GRB130408A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14363
SUBJECT: GRB 130408A: Swift/UVOT Detection of the Optical Afterglow
DATE:    13/04/09 00:21:52 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and A. Y. Lien (NASA/GSFC/ORAU) report on behalf
of the UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 155 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
 RA(J2000)  = 08:57:37.30 = 134.40540
 DEC(J2000) = -32:21:38.9  = -32.36081
with a 90%-confidence error radius of about 0.5 arc sec. This position is 8.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.82 with a 1-sigma error of about  0.04. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.26.


GRB_name: GRB130408A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14364
SUBJECT: GRB 130408A: GROND detection of the afterglow
DATE:    13/04/09 00:38:53 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

V. Sudilovsky (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 130408A (Swift trigger 553132; Lien et al.,
GCN 14361) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 23:22 UT on April 8th, 1.5 hrs after the GRB
trigger. They were performed at an average seeing of 1.0 and at an average
airmass of 1.0.

Based integrations of 260s in the optical and 240s in the NIR taken at a
mid-time of UT 23:34, we detect the variable source reported by Melandri
et al. (GCN 14362) and Siegel & Lien (GCN 14363), with preliminary
magnitudes (all AB):

g' = 21.0 +- 0.1,
r' = 19.7 +- 0.1,
i' = 19.1 +- 0.1,
z' = 18.8 +- 0.1,
J = 18.0 +- 0.1,
H = 17.8 +- 0.1, and
K > 17.0.

The large r-g color implies a redshift of z>3. Observations are ongoing.

Given magnitudes are calibrated against GROND zeropoints in g'r'i'z' and
2MASS field stars in JHK. They are not corrected for the Galactic
foreground extinction corresponding to a reddening of E_(B-V)= 0.26 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130408A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14365
SUBJECT: GRB 130408A - VLT/X-shooter redshift determination 
DATE:    13/04/09 01:47:22 GMT
FROM:    Jens Hjorth at U.Copenhagen  <jens@dark-cosmology.dk>

J. Hjorth (DARK), A. Melandri (INAF-OAB), D. Malesani (DARK), 
T. Kruehler (DARK), and D. Xu (DARK) report on behalf of a 
larger collaboration:

We observed the afterglow of GRB 130408A (Lien et al. GCN 14361; 
Melandri et al. GCN 14362; Siegel et al. GCN 14363) with the 
X-shooter spectrograph on the ESO VLT, beginning approximately 
1 h 55 min after the BAT trigger.  

We detect damped Ly-alpha absorption, Ly-alpha forest, the 
Lyman break, and numerous metal lines consistent with 
a redshift of 3.758.

We thank Maria Teresa Ruiz, Avril Day-Jones, Cedric Ledoux,
Leo Rivas, Alex Correa, and Lorenzo Monaco for conducting
the observations.


GRB_name: GRB130408A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14366
SUBJECT: GRB 130408A - Gemini-S/GMOS redshift determination
DATE:    13/04/09 01:47:25 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. Cucchiara (UCSC/UCO Lick Observatory)
and S. B. Cenko (UC Berkeley) report on behalf of a larger collaboration:

We observed the afterglow of GRB 130408A (Lien et al. GCN 14361,
Melandri et al. GCN 14362, Siegel et al. GCN 14363) with the GMOS-S
spectrograph on Gemini-S, beginning approximately 1 hr 56 mins after
the BAT trigger.  The integration was 4x600s and the wavelength
covered approximately 3950-6700A.

We detect numerous lines, including Lyman alpha, beta, gamma,
SII1250, SII1253, CII/CII*1260, SiII*1264, OI1302, SiII/OI*1304, SiII*1309,
CII/CII* 1334/1335, SiIV1394/1402 at a common redshift of z=3.757.

We thank D. Krogsrud for performing the observation.


GRB_name: GRB130408A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14367
SUBJECT: GRB 130408A: Enhanced Swift-XRT position
DATE:    13/04/09 07:40:32 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 573 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 130408A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 134.40543, -32.36089 which is equivalent
to:

RA (J2000): 08h 57m 37.30s
Dec (J2000): -32d 21' 39.2"

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: GRB130408A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14368
SUBJECT: Konus-Wind observation of GRB 130408A
DATE:    13/04/09 09:49:43 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 130408A
(Swift/BAT trigger=553132: Lien et al., GCN 14361)
triggered Konus-Wind at T0=78701.184s UT (21:51:41.194)

The light curve shows a bright pulse from ~T0-0.5 to ~T0+5 s
followed by a much weaker emission pulse peaked around ~T0+12;
a total duration of the burst is ~15 s.
The emission is seen up to several MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130408_T78701/

As observed by Konus-Wind, the burst
had a fluence of (1.2  0.2)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.328s,
of (5.2  0.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated 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 = -0.4  0.2,
the high energy photon index beta = -2.3  0.2,
the peak energy Ep = 211  29 keV,
chi2 = 99.4/97 dof.

The spectrum at 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 = -0.70  0.15,
the high energy photon index beta = -2.3  0.3,
the peak energy Ep = 272  40 keV,
chi2 = 87.7/99 dof.

Assuming redshift z=3.758 (Hjorth et al., GCN 14365; Tanvir et al., GCN 14366),
and a standard cosmology (H_0=70 km/s/Mpc, Omega_M=0.3, Omega_\Lambda=0.7),
we estimate the following cosmological rest-frame parameters of the prompt
gamma-ray emission:
- the isotropic equivalent energy release E_iso = (3.3  0.6)x10^53 erg;
- the peak luminosity L_iso = (5.5  0.5)x10^53 erg/s;
- the peak energy of the time-integrated spectrum Ep_rest = 1.00  0.14 MeV.

All the quoted results are preliminary.


GRB_name: GRB130408A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14369
SUBJECT: GRB 130408A: Swift-XRT refined Analysis
DATE:    13/04/09 10:11:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. Maselli  (INAF-IASFPA), V. Mangano (INAF-IASFPA),
J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester)
and A.Y. Lien report on behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 130408A (Lien  et al. GCN
Circ. 14361),  from 134 s to 28.6 ks after the BAT trigger. The data
comprise 28 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 14367).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.39 (+0.06, -0.07). At T+3999 s  the
decay steepens to an alpha of 8.0 (+0.0, -3.0) before breaking again at
T+4518 s to a final decay with index alpha=0.97 (+0.14, -0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.00 (+0.08, -0.07). The
best-fitting absorption column is  consistent with the Galactic value
of 2.0 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.9 x 10^-11 (5.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.0 x 10^21 cm^-2
Intrinsic column:    0 (+4.9, -0) x 10^21 cm^-2 at z=3.758
Photon index:      2.00 (+0.08, -0.07)

If the light curve continues to decay with a power-law decay index of
0.97, 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 7.8 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/00553132.

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


GRB_name: GRB130408A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14370
SUBJECT: GRB130408A: Swift/UVOT followup observations
DATE:    13/04/09 11:07:36 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 130408A 
134 s after the BAT trigger (Lien et al., GCN Circ. 14361). A bright but 
rapidly fading source is detected in the initial exposures (Siegel and 
Lien, GCN Circ. 14363) with a position consistent with detections by 
Melandri et al., (GCN Circ., 14362), Sudilovsky et al., (GCN Circ., 
14364) and Beardmore et al., (GCN Circ. 14367).

The preliminary UVOT position is:
  RA(J2000)  =    08:57:37.30 = 134.40540
  DEC(J2000) =   -32:21:38.9  = -32.36081
with a 90%-confidence error radius of about 0.5 arc sec.

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

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

white              156          305      147.4          16.80  0.05
white             3708         3900      189.2          20.29  0.22
white             6083        10367      924.3          21.99  0.35
v                  134          145       10.1          15.75  0.15
v                 4201         4400      196.7          19.61  0.35
b                 3503         6078      393.2          >20.84
u                  313         5872      236.2          >20.55
uvw1              4611         4752      139.0          >19.82
uvm2              4405         4605      196.6          >19.75
uvw2              3996        21851     1748.0          >21.56

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.258 in the direction of 
the burst (Schlegel et al. 1998).


GRB_name: GRB130407A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14371
SUBJECT: GRB 130407A: Swift-XRT observations
DATE:    13/04/09 13:20:09 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

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

Swift performed 4 tiled observations of the MAXI detected GRB 130407A (Fukushima et al., GCN 14359) to cover the MAXI error circle. The data are all in Photon Counting (PC) mode. No bright X-ray afterglow is detected in the XRT observations.

The 3sigma upper limit is 1.1 x 10^-2  cts/s. This corresponds to an observed 0.3-10 keV flux of 3.7 x 10^-13  erg/cm2/s, assuming a typical GRB spectrum with photon spectral index of 2. If we consider the Galactic absorption in this direction (4.9 x 10^20  cm^-2; Kalberla et al. 2005) this corresponds to an unabsorbed flux of 4.3 x 10^-13  erg/cm2/s.

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


GRB_name: GRB130408A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14372
SUBJECT: GRB 130408A: Zadko observatory - Gingin optical observations
DATE:    13/04/09 19:16:12 GMT
FROM:    Husne Dereli at ARTEMIS/OCA  <usne.Dereli@oca.eu>

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

We imaged the field of GRB 130408A detected by SWIFT
(trigger 553132) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 13.99h after the GRB trigger.
The elevation of the field increased from
87.5 degrees above horizon and weather conditions
were good.

The co addition of the six images filtered C, g, r
gives one image with an equivalent exposure time
of 540s. We did not detected the afteglow
mentioned in Melandri et al. (GCNC 14362):

t0+13.99h to t0+14.56h : Rlim = 20.5

The limiting magnitude of the zadko image is R~20.5.

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

[GNC OPS NOTE(17apr13):  Per athor's request, the GRB name
was changed from "1130408A" to "130408A".]


GRB_name: GRB130408A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14373
SUBJECT: GRB 130408A, Swift-BAT refined analysis
DATE:    13/04/09 23:45:37 GMT
FROM:    Craig Markwardt at NASA/GSFC  <craigm@milkyway.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (GWU)
(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 130408A (trigger 
#553132) (Lien, et al., GCN Circ. 14361).  The BAT ground-calculated 
position is
RA, Dec = 134.398, -32.363 deg which is
    RA(J2000)  =  08h 57m 35.5s
    Dec(J2000) = -32d 21' 45.9"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment). 
The partial coding was 6%.

T90 (15-350 keV) is 28 +- 13 sec (estimated error including 
systematics).  The mask weighted light curve has a main FRED-like 
component with a rise time of about 2 sec and decline of 5 sec, peaking 
at time T+1 sec, followed by a smaller peak at T+12 sec.  There is 
possible low-level emission out to about T+33 sec.

The time-averaged spectrum from T-0.1 to T+33.5 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 1.28 +- 0.26.  The fluence in the 15-150 keV band is 2.3 +- 
0.4 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+1.12 sec 
in the 15-150 keV band is 4.9 +- 1.0 ph/cm2/sec.  All the quoted errors 
are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/553132/BA/


GRB_name: GRB130408A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14374
SUBJECT: GRB 130408A: SMARTS optical/IR afterglow observations
DATE:    13/04/12 20:46:37 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU), reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 130408A
(GCN 14361, Lien et al.)  over several epochs (with mid-exposure
times of 2013-04-09 00:30 UT, 02:15 UT, 03:41 UT and 2013-04-11
02:24 UT). For each epoch, several dithered images were obtained with
total summed exposure times of 15 min in V and I and 12 min in J
and K.  For the final epoch, total exposure times were 36 min in I
and 30 min in J.

The fading afterglow of GRB 130408A (e.g. GCN 14362, Melandri et al.;
GCN 14363, Siegel et al.; GCN 14364, Sudilovsky et al.) was detected
with the following magnitudes (or 3-sigma limits):

mid-exposure
time
(hours)           I mag             J mag            K mag
2.64611         18.8 +/- 0.1    17.8 +/- 0.1     > 16.1
4.38444         19.6 +/- 0.1    18.6 +/- 0.2    16.8 +/- 0.2
5.82472         20.0 +/- 0.1    18.6 +/- 0.2     > 17.2
52.53694        > 21.5            > 19.6            ...

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

Between about 2.6 hrs and 5.8 hrs post-burst, the GRB afterglow fades
with a decay rate of approximately alpha = 1.4 (where afterglow flux is
proportional to t^-alpha).


GRB_name: GRB130408A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14375
SUBJECT: GRB 130408a: Skynet Optical Observations
DATE:    13/04/15 12:41:15 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

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

Skynet began observing the field of GRB130408A (Swift trigger 553132, GCN 
14361) in BVRI beginning ~93 minutes after the burst using four of the 
PROMPT telescopes located at CTIO in Chile. A fading source is detected at 
the enhanced position reported by the Swift-XRT team (GCN 14367.)

A preliminary light curve of the first two night's data from PROMPT can be 
found at: http://skynet.unc.edu/grb/grb130408a.png


GRB_name: GRB130408A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14376
SUBJECT: GRB 130408A: Suzaku WAM observation of the prompt emission
DATE:    13/04/15 20:47:15 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

K. Takaki, M. Ohno, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa
(Hiroshima U.),
M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno, S. Sugimoto(Saitama
U.),
K. Yamaoka (Nagoya U.), M. Yamauchi, M. Akiyama, N. Ohmori (Univ. of
Miyazaki),
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 130408A (Lien et al., GCN14361) triggered by the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 21:51:38 UT (=T0).

The observed light curve shows a single peak starting at T0-2s, ending
at T0+5s with a duration (T90) of about 7 seconds.
The fluence in 100 - 1000 keV was 7.18(+0.06/-0.15) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0s was 5.42(+1.37/-2.27) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-2s to
T0+5s is well fitted by a single power-law with a photon index of
2.32 (+0.41/-0.34) (chi2/d.o.f = 12.19/13).

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: GRB130418A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14377
SUBJECT: GRB 130418A: Swift detection of a burst with an optical counterpart
DATE:    13/04/18 19:16:51 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. De Pasquale (UCL-MSSL), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), M. M. Chester (PSU),
S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), E. Sonbas (NASA/GSFC/Adiyaman Univ.),
M. C. Stroh (PSU), C. A. Swenson (PSU) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift Team:

At 19:00:53 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130418A (trigger=553847).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 149.043, +13.649 which is 
   RA(J2000) = 09h 56m 10s
   Dec(J2000) = +13d 38' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual with image triggers, the BAT light 
curve shows no significant features. 

The XRT began observing the field at 19:03:03.2 UT, 129.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 149.0377, 13.6654 which is equivalent to:
   RA(J2000)  = +09h 56m 9.05s
   Dec(J2000) = +13d 39' 55.4"
with an uncertainty of 5.3 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. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 138 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 09:56:08.92 = 149.03718
  DEC(J2000) = +13:40:02.8  =  13.66744
with a 90%-confidence error radius of about 0.74 arc sec. This position is 7.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.96 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. 

This source was detected on the first image trigger after it came
within the BAT's field of view, so its start time may be significantly
before the nominal trigger time.  There is no significant fading
in the XRT over the ~300 second XRT observation time.  Thus
it is likely that this is a very long duration event.  The position
of the source is 47 degrees from the Galactic plane, but that
doesn't preclude a nearby source.  Further determination of the
characteristics of the source will await further data analysis. 

Burst Advocate for this burst is M. De Pasquale (m.depasquale 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: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14378
SUBJECT: GRB 130418A: 1.23m I-band observations
DATE:    13/04/18 20:53:45 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA/CSIC-UPV/EHU), S. Perez-hoyos (UPV/EHU), I. Mendikoa
(UPV/EHU), A. Sanchez-Lavega (UPV/EHU), R. Hueso (UPV/EHU), J.F. Rojas
(UPV/EHU), A. de Ugarte Postigo (IAA/CSIC-DARK), report on behalf of a
larger collaboration:

We have observed the field of GRB130418A (de Pasquale et al. 2013; GCN
Circ. 14377) with 1.23m CAHA telescope equipped with PLANETCAM. The
observations started on 19:31 UT with the I-band filter. The optical
afterglow reported by de Pasquale et al. (GCN Circ. 14377) is well
detected with an approximate magnitue of I~15.6.


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14379
SUBJECT: GRB 130418A: Bassano Bresciano Observatory optical observations
DATE:    13/04/18 21:58:31 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

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

We imaged the field of GRB 130418A (de Pasquale et al. 2013; GCN
Circ. 14377) detected by SWIFT(trigger 553847) with the robotic 
telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy.

The observations started 15 min. after the 
GRB trigger,with our schmidt telescope 
D=400 mm F/D=3.

Weather conditions were discrete for moon presence.

We co-added 14 unfiltered CCD exposures of 120s each.

We detect a new source of 16.3 Vmag in the error box given by SWIFT.
We detected the candidate couterpart at the following position (+/- 2 arcsec):

RA (J2000) =  09h 56m 08.90s 
DEC(J2000) = +13Â° 40' 02.8"

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

The message may be cited.


GRB_name: GRB130418A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14380
SUBJECT: GRB 130418A: Redshift from 10.4m GTC
DATE:    13/04/18 22:49:12 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), 
J. Gorosabel (UPV/EHU, IAA-CSIC), R. Sanchez-Ramirez (IAA-CSIC), 
J. P. U. Fynbo (DARK/NBI), N. Tanvir (U. Leicester) and 
C.A. Alvarez Iglesias (IAC-ULL) report:

We have observed the afterglow of GRB 130418A (De Pasquale et al. GCN
14377) with the 10.4m GTC telescope starting at 21:45 UT (2.75 hr after the
burst). Observations consisted of 2x600s using the R1000B grating, with a 
resolution of R~1000 in the range 3600 - 7900 A.

The spectrum shows a high S/N trace, with very weak MgII features at a 
redshift of z = 1.218, which we identify as the redshift of the GRB.

[GCN OPS NOTE(19apr13):  Per author's request, CAAI's affiliation
was changed from GTC to IAC-ULL.]


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14381
SUBJECT: GRB 130418A: TNG optical observations
DATE:    13/04/18 23:45:34 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF/OAB), Avet Harutyunyan, G. Mainella
(INAF/TNG) report on behalf of the CIBO collaboration:

We observed the field of GRB 130418A (De Pasquale et al., GCN 14377) with
the TNG telescope located in the Canary Islands. We obtained a set of
images with the DOLORES camera in the B, V, R and I bands, starting on
2013 Apr 18 at 23:01:02 UT (4.0 hours after the GRB).

The optical afterglow (De Pasquale et al. GCN 14377; Gorosabel et al. GCN
14378; Quadri et al. 14379) is clearly detected in all bands. The measured
R-band magnitude is 18.1 (at t-t0=4.06 h; calibrated against the USNOB1
catalogue).


We acknowledge support from the TNG visiting astronomer F. Borsa.


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14382
SUBJECT: GRB 130418A: TAROT Calern and TAROT la Silla observatory optical observations
DATE:    13/04/19 00:34:28 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 130418A detected by SWIFT
(trigger 553847) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

Continuous observations started 78.7 min after the GRB trigger
due to the dusk. The elevation of the field
decreased from 58 degrees above horizon and weather conditions
were good. Four hours after the TAROT la Silla telescope
(Chile) started to observe.

The afterglow mentioned by De Pasquale (GCNC 14377)
appears clearly in the images.

The following magnitudes are obtained using the star
NOMAD-1 1036-0179295 (ra=149.0472378 dec=+13.6557094
R=14.91) for flux calibration:

  Start   Stop    Rmag
  (min)   (min)
    78.7   84.7  17.34
    88.4   94.4  17.48
    98.2  110.2  17.59
   117.6  141.6  17.91
   156.6  186.6  18.11
   242.1  263.1  18.13

Considering a flux decay power law the corresponding
exponent is alpha=0.65.

Magnitudes are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB130418A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14383
SUBJECT: GRB 130418A: Enhanced Swift-XRT position
DATE:    13/04/19 00:45:26 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 1098 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 130418A, 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 = 149.03689, +13.66721 which is equivalent
to:

RA (J2000): 09h 56m 8.85s
Dec (J2000): +13d 40' 02.0"

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

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

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


GRB_name: GRB130418A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14384
SUBJECT: GRB 130418A: Swift/UVOT Detection and request for continuing coverage
DATE:    13/04/19 01:19:37 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin 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 130418A
138 s after the BAT trigger (De_Pasquale et al., GCN Circ. 14377).
A source consistent with the XRT position (De Pasquale et al.
GCN Circ. 14377) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  09:56:08.88 = 149.03700 (deg.)
    Dec (J2000) = +13:40:02.7  =  13.66741 (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              138          288          146         14.85 +/- 0.05

u                  296          353           56         14.71 +/- 0.04
v                 5634         5834          197         17.69 +/- 0.08
b                 3567         3766          197         17.41 +/- 0.05
w1                6044         6124           78         17.25 +/- 0.11
m2                5839         6039          197         17.61 +/- 0.11
w2                5430         5630          197         18.08 +/- 0.11

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).

Due to a Moon constraint, Swift observations will stop for now. Continuing
acquisition of ground-based data, including ubv photometry will be useful
at this time.


GRB_name: GRB130418A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14385
SUBJECT: GRB130418A: OSN 1.5m fading afterglow detection
DATE:    13/04/19 02:32:19 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C. Tello, R. Sanchez-Ramirez (IAA-CSIC), J. Gorosabel (IAA/CSIC-UPV/EHU),
F. Aceituno (OSN, IAA-CSIC) and A. Castro-Tirado (IAA-CSIC) on behalf of a
larger collaboration report:

We observed the field of GRB130418A reported by De Pasquale et al. (GCNC
14377) with the 1.5 meter telescope at the Sierra Nevada Observatory using
an I band filter, where we clearly detect a fading source coincident with
the UVOT afterglow position.

Preliminary results of an image taken at 21h20m (2.33h after the burst)
with a 300s exposure show the source presented a magnitude of I~17.13 when
compared to the USNO-B1.0 catalogue. Another image taken at 22h45m (3.74h
after the burst) with an exposure time of 60s shows a magnitude of I~17.51
(also preliminarily and when compared to the USNO-B1.0 catalogue).

More images were taken and will continue to be taken when the source rises
again above the local horizon.


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14386
SUBJECT: GRB 130418A: GROND detection of the optical-NIR afterglow 
DATE:    13/04/19 02:58:43 GMT
FROM:    Mohit Tanga at MPE/GROND  <mohit@mpe.mpg.de>

GRB 130418A: GROND detection of the optical-NIR afterglow

M. Nardini (UNIMIB), M. Tanga (MPE Garching), D. A. Kann (TLS Tautenburg)
and J. Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field GRB 130418A (Swift trigger 553847; M. De Pasquale et
al., GCN 14377) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 01:20:33 UT on April 19th, 6.3 hrs after the SWIFT
BAT trigger. They were performed at an average seeing of 1" and at an
average airmass of 1.38.

We detect the optical afterglow inside the 0.7" Swift/UVOT error circle
reported by De Pasquale et al., (GCN 14377) in all 7 bands. Based on the
first 4 min of total exposure we estimate preliminary magnitudes (all in
AB system) of

g' = 18.79 +- 0.03,
r'  = 18.46 +-0.03,
i'  = 18.22 +- 0.03,
z' = 17.95 +- 0.03,
J  = 17.62 +- 0.05,
H = 17.17 +- 0.05 and
K = 16.81 +- 0.11

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


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14387
SUBJECT: GRB 130418A: CARMA 3mm detection
DATE:    13/04/19 03:49:53 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 130418A (De Pasquale et al., GCN 14377) 
with the Combined Array for Research in Millimeter Astronomy at a 
frequency of 93 GHz (3mm) starting at 02:50 UT on 2013-04-19, 7.82 hours 
after the burst.  Observations continued until 03:26 UT (midpoint t=8.12 
hours.)

A source is clearly detected at a position consistent with the location 
of the UV, X-ray, and optical afterglow (De Pasquale et al., GCN 14377; 
Gorosabel et al., GCN 14378; Quardri et al., GCN 14379).  The 
approximate flux at this time is ~3 mJy.  Follow-up observations are 
planned.

We thank the CARMA staff for their support in executing these observations.


GRB_name: GRB130418A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14388
SUBJECT: GRB 130418A: RATIR Optical and NIR Observations
DATE:    13/04/19 05:30:29 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), 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 130418A (De Pasquale, et al., GCN 14377) 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 2013/04 19.14 to 2013/04 19.19 UTC (8.24 to
9.54 hours after the BAT trigger), obtaining a total of 1.07 hours exposure
in the r' and i' bands and 0.45 hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-UVOT error circle (Kuin et al., GCN 14384),
in comparison with SDSS DR8 and 2MASS, we obtain the following detections
in the AB magnitude system:

 r'    18.87 +/- 0.02
 i'    18.77 +/- 0.02
 Z    18.30 +/- 0.02
 Y    18.07 +/- 0.02
 J    18.06 +/- 0.02
 H    17.53 +/- 0.02

These magnitudes are not corrected for Galactic extinction in the direction
of the GRB.  Relative to the GROND detections about 3 hrs earlier (Nardini
et al., GCN 14386), the afterglow has faded by about 0.4 mag in all
optical/NIR bands.  Continued observations are planned.

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


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14389
SUBJECT: GRB 130418A: REM NIR observations
DATE:    13/04/19 05:37:23 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, D. Fugazza, V. d'Elia, on behalf of the REM team report:

We imaged the field of GRB130418A (De Pasquale et al., GCN 14377) with  
the
REM NIR camera equippe with the J, Hand Ks filters.

Observations started at 2013/04/18 23:12:37, i.e. about 4.2 hours after
the prompt event.
The optical counterpart detected by UVOT was well detected at  
H=15.7+-0.1
(preliminary calibration) at the beginning of our observations.


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14390
SUBJECT: GRB130418A: VLT/X-shooter redshift confirmation
DATE:    13/04/19 12:06:21 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler, D. Xu (both DARK), R. Sanchez-Ramirez (IAA-CSIC),
D. Malesani, J. Fynbo (both DARK) and H. Flores (GEPI/Obs. de Paris)
report on behalf of a larger collaboration:

We observed the optical/NIR counterpart (e.g., De Pasquale et al. GCN
14377, Gorosabel et al. GCN 14378) of GRB 130418A (De Pasquale et al.
GCN 14377) with the VLT/X-shooter spectrograph.

Our spectra cover the wavelength range 3000-25000 AA, and were taken
starting on 2013 Apr 18, 23:35:08 UT (4.57 hr after the GRB) for a
total exposure of 20 min.

We identify absorption lines of CIV, FeII and MgII at a common redshift
of z = 1.217 (see also de Ugarte Postigo et al., GCN 14380). The
doublet of CIV (1548, 1550) is also detected in a second absorption
system at z = 1.218. No emission lines are evident in our spectrum.

We thank the VLT staff, in particular Henri Boffin, Dimitri Gadotti and
Alex Correa, for the expert support in obtaining these data.


GRB_name: GRB130419A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14391
SUBJECT: GRB 130419A: Swift detection of a burst
DATE:    13/04/19 13:39:56 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

N. P. M. Kuin (UCL-MSSL), D. N. Burrows (PSU), V. D'Elia (ASDC),
P. A. Evans (U Leicester), S. T. Holland (STScI), J. A. Kennea (PSU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA), M. H. Siegel (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 13:30:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130419A (trigger=553918).  Swift did not slew due to Sun constraint.
The BAT on-board calculated location is 
RA, Dec 355.271, +9.977 which is 
   RA(J2000) = 23h 41m 05s
   Dec(J2000) = +09d 58' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for image triggers, there is no
obvious variation in BAT's immediately-avaialble lightcurve. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 00:33 UT on 2013 May 06. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is N. P. M. Kuin (n.kuin 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.)

[GCN OPS NOTE(05dec14):  By author's request, the "Swift slewed immediately"
sentence in the first paragraph was changed.]


GRB_name: GRB130418A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14392
SUBJECT: GRB 130418A, Swift-BAT refined analysis
DATE:    13/04/19 13:49:19 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), M. De Pasquale (UCL-MSSL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
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 130418A (trigger #553847)
(De Pasquale, et al., GCN Circ. 14377). The BAT ground-calculated position is
RA, Dec = 149.045, 13.674 deg which is
    RA(J2000)  =  09h 56m 10.8s
    Dec(J2000) = +13d 40' 28.2"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.

It appears that BAT triggered on the decay phase of a burst already in progress
when the source position came into the BAT field of view during a pre-planned 
slew. Therefore we do not know the true time of the start of the burst, but it 
was at least 50 seconds before T0, here defined as the trigger time. From T-50 
sec, when the burst became visible, there is a steady decline punctuated by two 
peaks at approximately T-20 and T+50, the first being harder than the second. 
The decay continued to roughly T+300 sec.  The burst location was no longer 
visible after T+450, when another slew took it out of the BAT field. T90 cannot
be determined since BAT did not see the start of the burst, but T90 is at least
300 seconds.

The time-averaged spectrum from T-40.16 to T+285.59 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.07 +- 0.17.  The fluence in the 15-150 keV band is 1.8 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-37.68 sec in the 15-150 keV band
is 0.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.  Note that these values are calculated only for the part of the burst
detected by the BAT, so the fluence should be considered a lower limit.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/553847/BA/


GRB_name: GRB130418A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14393
SUBJECT: GRB 130418A: LOAO Observation
DATE:    13/04/19 14:34:07 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

M. Im (CEOU/SNU), H.-I. Sung(KASI), and Y. Urata (NCU) 
on behalf of EAFON

  We observed the field of GRB 130418A (Pasquale et al., GCN 14377) 
in R, I, and z filters using the 1-m telescope at Mt. Lemmon 
observatory in Arizona, US.

  The observation started at 2013-04-19 03:40 UT, 
or about 8.6 hours after the BAT alert, and continued for
about 45 min. We clearly identify the fading afterglow in
R- and I-band, at the location reported earlier (Gorosabel et al.
GCN 14378; Quadri et al. GCN 14379; de Ugarte Postigo et al. GCN14380; 
D'Avanzo et al. GCN 14381; Klotz et al. GCN14382; Kuin et al.
GCN14384; Tello et al. GCN 14385; Nardini et al. GCN 14386; 
Perley et al. GCN 14387; Butler et al. GCN 14388; Covino et al.
GCN 14389; Kruehler et al. GCN 14390). On the other hand,
the detection in z-band is marginal.

  Preliminary magnitudes of the afterglow, calibrated against 
a USNO B-1 star at RA=140.047350 and Dec=+13.655828 are given below:

   T(mid, UT)         Mag
04-19 03:58:26     R=18.95 +- 0.07
04-19 04:04:16     I=18.18 +- 0.08

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


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14394
SUBJECT: GRB 130418A: T18 and T21 optical observations
DATE:    13/04/19 15:49:18 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

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

We have detected GRB 130418A optical afterglow at iTelescope observatories
T18 and T21. Four unfiltered and three photometric V filter images with 300 sec exposure time were made at T18 (AstroCamp Observatory, Nerpio, Spain) 0.32-m/8.0 Astorgraph and KAF-6303E CCD. Two unfiltered and four photometric V filter images with 600 sec exposure time were made at T21 (Mayhill, New Mexico) 0.43-m/6.8 astrograph and FLI ProLine PL6303E CCD.

The afterglow was detected at following position RA 09:56:08.94 and DEC +13:40:02.9.

The following magnitudes were obtained from the observations using 
NOMAD1 1036-0179295 (V= 14.750, R = 14.910) as the comparison:

Tmid(sec) +T0     Filter         Exp time      Mag          Mag err. 
3119                     unfiltered     300         16.200CR     0.026
3406                     unfiltered     300         16.305CR     0.027
3758                     unfiltered     300         16.381CR     0.027
4118                     unfiltered     300         16.496CR     0.030
4835                      V               300         16.895V        0.082
5195                      V               300         16.979V        0.081
5546                      V               300         16.983V        0.085

6432                     V                 600         17.320V       0.075
7093                     V                 600         17.342V       0.077
8026                     unfiltered      600         17.328CR     0.044
8691                     unfiltered      600         17.519CR     0.053
9742                     V                 600         17.775V       0.123
11059                   V                 600         17.752V       0.193


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14395
SUBJECT: GRB 130418A: T21 optical observation
DATE:    13/04/19 16:59:36 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

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

We have detected GRB 130418A optical afterglow at iTelescope observatory 
T21 (Mayhill, New Mexico) 0.43-m/6.8 astrograph and FLI ProLine PL6303E 
CCD. One unfiltered image with 600 sec exposure time was made.

The afterglow was detected at following position RA 09:56:08.87 and DEC 
+13:40:02.7.

The following magnitude was obtained from the image using NOMAD1 
1036-0179295 (R = 14.910) as the comparison:

Tmid(h) +To     Filter         Exp.time   Mag          Mag err. 
10.96               unfiltered    600          19.018       0.277


GRB_name: GRB130419B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14397
SUBJECT: GRB 130419B (Swift trigger Trigger 553930): MASTER-Net optical observations
DATE:    13/04/19 18:31:58 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB130419B 41 sec after 
notice time and 120 sec after GRB time at 2013-04-19 17:26:37.875 UT. On 
our first (20s exposure) set we haven't found optical transient  within 
SWIFT error-box (ra=13 34 34 dec=+37 14 24 r=0.066667).
The 5-sigma upper limit has been about 16.48mag
The analysis and determination of a limit it is complicated by the close 
bright star.
The message may be cited


GRB_name: GRB130327B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14398
SUBJECT: GRB 130327B: Swift/XRT source is not the afterglow
DATE:    13/04/19 20:11:29 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA) and E. Troja (NASA/GSFC/CRESST) for the Swift team:

Swift carried out an additional 4.6 ksec observation of the field containing GRB 
130327B (e.g. Longo et al, GCN 14344; Ohno et al, GCN 14347), starting at 
2013-04-18 12:43:13 UT, approximately 22 days after the burst.  The source 
reported in Krimm & Mangano (GCN 14353) as a possible afterglow to GRB 130327B 
is still detected at a rate of 0.002  0.001 cts/s (0.3-10 keV), which is 
statistically consistent with the rate reported in GCN 14353.  Since we would 
expect a GRB afterglow to have faded over this time period, we conclude that the 
XRT source is not associated with GRB 130327B, and is instead a background 
source, possibly an AGN.
 No further Swift observations are planned.


GRB_name: GRB130419A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14399
SUBJECT: GRB 130419A, Swift-BAT refined analysis
DATE:    13/04/19 20:22:04 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA),S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC),J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC),N. P. M. Kuin (UCL-MSSL),A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC),D. M. Palmer (LANL),T. Sakamoto (AGU),
M. Stamatikos (OSU),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 130419A (trigger #553918)
(Kuin, et al., GCN Circ. 14391). The BAT ground-calculated position is
RA, Dec = 355.278, 9.900 deg which is
    RA(J2000)  =  23h 41m 06.7s
    Dec(J2000) = +09d 54' 00.6"
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.

The mask-weighted light curve shows a single long period of emission starting
about T+30 sec, peaking at T+60 sec and declining until T+140 sec.  There is
weak secondary peak at T+120 sec superimposed on the main declining emission.
A slew took the source out of the BAT field of view around T+280 sec.
T90 (15-350 keV) is 75.7 +- 49.6 sec (estimated error including systematics).

The time-averaged spectrum from T+40.09 to T+169.51 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.43 +- 0.28.  The fluence in the 15-150 keV band is 7.8 +- 1.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+55.43 sec in the 15-150 keV band
is 0.3 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/553918/BA/


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14400
SUBJECT: GRB 130418A: Submm observations from SMA
DATE:    13/04/19 22:04:32 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

S. Martin (ESO/ALMA), A. de Ugarte Postigo (IAA-CSIC) and G. Petitpas (SMA)
report on behalf of a larger collaboration:

We have observed the field of GRB 130418A (De Pasquale et al., GCN 14377) with 
the Submillimeter Array (SMA) at Mauna Kea (Hawai, USA) in submm wavelengths.
Observations consisted of 1.25 hr on target with an average time 6.5 UT on 19
April 2013 (11.5 hr after the burst). We used 6 antennas on compact configuration, 
under average weather conditions, with a precipitable water vapour of 2.5 mm or
an optical depth at 225 GHz of ~0.1. The central observing wavelength was 
340 GHZ.

On a preliminary reduction we do not detect any source consistent with the 
position of the GRB down to a 3-sigma limit of 14.5 mJy (r.m.s. 4.8mJy). This limit
is consistent with the 3 mm detection by CARMA (Perley, GCN 14387)

We acknowledge excellent support from the SMA staff.


GRB_name: GRB130418A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14401
SUBJECT: GRB 130418A: SMARTS optical/IR afterglow observations
DATE:    13/04/19 22:41:06 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU), reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained
optical/IR imaging of the error region of GRB 130418A (GCN 14377,
De Pasquale et al.) at two epochs (with mid-exposure times of
2013-04-19 00:03 UT & 01:24 UT). For each epoch, several dithered
images were obtained with total summed exposure times of
15 min in V and I and 12 min in J and K.

The fading afterglow of GRB 130418A (e.g. GCN 14377, De Pasquale
et al.; GCN 14378, Gorosabel et al.; GCN 14379, Quadri et al.)
was detected with the following magnitudes:

mid-exposure
time
(hours)               V mag              I mag               J
mag              K mag
5.03944 hours   18.41 +/- 0.03  17.57 +/- 0.03  16.46 +/- 0.10  14.82 +/-
0.10
6.38972 hours   18.59 +/- 0.03  17.69 +/- 0.03  16.70 +/- 0.10  15.05 +/-
0.10

(Optical photometry is calibrated against Landolt standard stars
and IR photometry is calibrated against a 2MASS star in the field.)

Between about 5 hrs and 6.4 hrs post-burst, the GRB afterglow fades with
a decay rate of approximately alpha = 0.6 +/- 0.2 in the optical
(where afterglow flux is proportional to t^-alpha).


