# GCN_circulars

GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11234
SUBJECT: GRB 100901A: ISON-NM optical observations
DATE:    10/09/06 17:30:05 GMT
FROM:    Leonid Elenin at ISON  <l.elenin@gmail.com>

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

We continue observation of the Swift GRB 100814A (Immler et al. GCN Circ.
11159)
with 0.45-m telescope of ISON-NM observatory on Sep. 04 (UT) 09:04:35 -
10:06:19,
Sep. 05 (UT) 08:45:52 - 09:50:20 and Sep. 06 (UT) 09:36:57 - 11:14:22.

The afterglow (Immler et al., GCN 11159; Guidorzi et al., GCN 11160; Ivanov
et al.,
GCN 11161; Klunko et al., GCN 11162) is well detected on stacked images
for three epochs.

Preliminary photometry of unfiltered image against USNO-B1.0 1127-0027229,
assuming R=16.16  is following:

T-T0      filter   exposure   mag.  mag. error
--------------------------------------------------------------

2.8336    W      12x300   19.78    +/- 0.25

3.8206    W      12x300   20.38    +/- 0.20

4.8700    W      20x300   20.97    +/- 0.22

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

The images of GRB100901A is available at:

http://www.spaceobs.org/images/GRB1000901A-3epochs.jpg


GRB_name: GRB100906A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11235
SUBJECT: GRB 100906A: MASTER preliminary prompt+afterglow lc
DATE:    10/09/06 18:13:03 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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


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

Observations on  MASTER robotic telescope at Tunka (MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010,  Advances in Astronomy, 
vol. 2010, pp. 1-7) are continued (Ivanov et al., GCN CIRCULAR 11228, 
Gorbovskoy et al., GCN CIRCULAR 11231).
We have very smoth light curve up to 4 hours after trigger time. 
The power low index afterglow decay (F~T_alpha) apha is equal  -0.83+-0.02 
. 
The preliminary 20 min automatical light curve is available at
http://observ.pereplet.ru/images/GRB100906A/lc_GRB100906A_30min.png
(unfiltered).

This automatical pohtometry calibrated by   USNOB1  stars.


The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB100901A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11236
SUBJECT: GRB 100901A: TLS observations, SDSS calibration, decay slope
DATE:    10/09/06 18:56:47 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, U. Laux and B. Stecklum (TLS Tautenburg) report:

We obtained further observations at multiple epochs of the afterglow of
GRB 100901A (Immler et al., GCN 11159) with the TLS 1.34m Schmidt
telescope. After another completely overcast night, we obtained data under
good to excellent conditions in the third and fourth nights.

For our first epoch (Kann et al., GCN 11187) we had used 5 USNO B1.0 R2
stars. Now, we compare their magnitudes with those derived from the SDSS
catalog. We find that two of the stars we used, at

RA = 01:49:05.595, Dec. = +22:44:51.96;
RA = 01:48:59.497, Dec. = +22:46:18.56

must be variable, they yield strongly divergent zero points compared to
the SDSS values for the other three stars.

For the other three stars, which yield a stable zero point, we find:

RA = 01:48:49.484, Dec. = +22:47:42.14; USNO R2 = 18.44; SDSS = 18.46
RA = 01:48:53.990, Dec. = +22:48:30.07; USNO R2 = 17.73; SDSS = 17.91
RA = 01:49:06.790, Dec. = +22:47:02.97; USNO R2 = 15.37; SDSS = 15.64

Note that the last star has been used by many observers to calibrate the
afterglow, we find that it is 0.27 mag fainter, this is in agreement with
what was reported by Andreev et al., GCN 11191. Recalibrating all reported
magnitudes based on this calibration with this value strongly reduces the
scatter in the light curve. Note the recently reported magnitudes by
Elenin et al. (GCN 11234) are about 0.4 magnitudes too bright.

Using these three stars, we re-calibrate our earlier data and add
additional observations as follows:

Mid-Time Rc dRc Exptime
1.384629 19.16 0.03 1 x 300
1.388656 19.24 0.04 1 x 300
1.424663 19.28 0.03 1 x 300
1.428691 19.36 0.03 1 x 300
1.432719 19.25 0.04 1 x 300
1.436747 19.18 0.04 1 x 300
3.309522 20.53 0.07 4 x 300
3.549130 20.70 0.04 1 x 600 + 2 x 450 + 4 x 300
4.398521 21.30 0.05 4 x 600
4.424271 21.31 0.26 1 x 120
4.430357 21.37 0.13 1 x 600
4.559408 21.27 0.10 1 x 600

Midtime is in days after the trigger, exposure time in seconds.

We find that all observations after one day can be fit with a single power
law with slope alpha = 1.46. This is steeper than the slope reported by
Pandey & Zheng (GCN 11179), in agreement with the break proposed by Kann
et al. (GCN 11187), though we caution the Delta alpha is shallow (and in
agreement with the theoretical value for a cooling break) and there may
still be calibration issues.

This message may be cited.


GRB_name: GRB100905A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11237
SUBJECT: GRB 100905A: Swift/UVOT Upper Limits
DATE:    10/09/06 19:08:45 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU) and F. E. Marshall (NASA/GSFC) report on behalf
of the Swift/UVOT team.

The Swift/UVOT began settled observations of the field of
GRB 100905A 77s after the BAT trigger (Marshall et al.,
GCN Circ. 11214).  Data summed from the first and second orbits
do not reveal a source at the enhanced position of the X-ray
afterglow (Evans et al., GCN Circ. 11219).

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

FILTER     T_start(s)  T_stop    Exposure     Mag/3UL
========================================================
white fc      78        228        147        >20.77
white         78       2055        450        >21.29
V            619       1933        155        >19.01
B            545       2031        155        >19.81
u fc         290        540        245        >20.08
u            290       2006        381        >20.17
uvw1         668       1982        155        >19.53
uvm2        5654       7290        393        >20.19
uvw2        5245      12865       1278        >21.26
=======================================================

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 0.06 (Schlegel et al.,
1998, ApJS, 500, 525). The photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB100906A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11238
SUBJECT: GRB 100906A: TLS Multicolor Observations
DATE:    10/09/06 20:39:03 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, A. Nicuesa Guelbenzu, F. Ludwig and B. Stecklum (TLS 
Tautenburg) report:

We observed the afterglow of the bright Swift GRB 100906A (Markwardt et 
al., GCN 11227) with the 1.34m TLS Schmidt telescope as soon as dusk set 
in. We obtained 3 x 300 sec images in Z, Ic, Rc, V and B each. The 
afterglow is clearly detected in all images.

Assuming the star at RA = 01:54:46.82, Dec. = +55:37:55.3 to have 
USNOB1.0 R2 = 15.70, we find the following magnitude for the afterglow:

Rc = 18.84 +/- 0.03 at 0.247478 days after the GRB.

Further observations are planned if weather permits.

This message may be cited.


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11239
SUBJECT: GRB 100906A: Ondrejov 65cm observations
DATE:    10/09/06 21:41:29 GMT
FROM:    Petr Kubanek at AIO  <pkubanek@gmail.com>

Kamil Hornoch, Peter Kusnirak, Barbora Mikulecka, Petra Hornochova,
Petr Scheirich, Tomas Kusnirak and Jan Strobl (Astronomical Institute,
Czech Republic) and Petr Kubanek (IPL UV Valencia, IAA CSIC Granada)
reports on behalf of larger collaboration:

We observed position of GRB100906A with Ondrejov 65cm telescope. Its
optical counterpart (Markwardt et al., GCN 11227) is well detected on
stacked 6x180 second R band exposure with mid-point at 2010-09-06
19:51:14 UT, with preliminary magnitude 19.5 +- 0.5 mag.

Further observations and calibrations with this as well as other
instruments are ongoing.


GRB_name: GRB100906A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11240
SUBJECT: GRB100906A: MITSuME  Okayama Optical Observation
DATE:    10/09/07 00:06:52 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 100906A (Markwardt et al., GCN 11227)
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 2010-09-06 13:53:54 UT (~4.4 min after
the burst).  We detected the previously reported afterglow
(Markwardt et al., GCN 11227; Ivanov et al., GCN 11228; Melandri
et al., GCN 12229) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.00662    13:58:60     540.0   15.58  0.04  14.42  0.02  14.00  0.02
0.01784    14:15:09     540.0   16.52  0.05  15.35  0.03  14.98  0.04
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB100906A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11242
SUBJECT: GRB 100906A: Swift/UVOT Observations
DATE:    10/09/07 02:33:56 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU) and C. B. Markwardt (NASA/GSGC) report on behalf
of the Swift/UVOT team.

The Swift/UVOT began settled observations of the field of
GRB 100906A 89s after the BAT trigger (Markwardt et al.,
GCN Circ. 11227).  Data summed from the first orbit confirms
a fading optical transient at the position report by Markwardt
et al.  The non-detection in the UVW2 and UVM2 filters is consistent
with the Gemini redshift of 1.727 reported by Tanvir et al.
(GCN Circ. 11230).  Observations of the GRB are continuing.

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

FILTER     T_start(s)  T_stop    Exposure     Mag/3UL
========================================================
u (fc)       146        396        245     14.93+-0.02
u            146       1305        490     15.40+-0.01
v            453       1381        116     15.97+-0.05
b            403       1330        116     16.49+-0.04
uvw1         503       1280         97     17.13+-0.11
uvm2         478       1404        115       >18.97
uvw2         429       1356        116       >19.19
=======================================================

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 0.36 (Schlegel et al.,
1998, ApJS, 500, 525). The photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB100906A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11243
SUBJECT: GRB 100906A: Enhanced Swift-XRT position
DATE:    10/09/07 03:20:48 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 5488 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 100906A, 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 = 28.68397, +55.63068 which is equivalent
to:

RA (J2000): 01h 54m 44.15s
Dec (J2000): +55d 37' 50.5"

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

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

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


GRB_name: GRB100906A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11244
SUBJECT: GRB 100906A: Swift-XRT refined analysis
DATE:    10/09/07 03:58:18 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A. P. Beardmore (U. Leicester) and C. B. Markwardt (NASA/GSFC) report
on behalf of the Swift-XRT team:

We have analysed 16.6 ks of XRT data for GRB 100906A (Markwardt et
al. GCN Circ. 11227), from 70 s to 40.2 ks after the BAT trigger. The
data comprise 228 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 11243).

The X-ray light curve initially shows a large flare, peaking at a
count rate of ~2000 count s^-1 at T+120s, contemporary with the late
time BAT activity (Barthelmy et al., GCN Circ. 11233). It then
declines rapidly before breaking to a shallower decay slope of alpha =
0.74 +/- 0.04 after T+270s. This is followed by a further break at
T+10854 s to an slope of 1.96 +0.17 -0.13.

A spectrum formed from the PC mode data can be fit by an absorbed
power-law with a photon index of 2.15 +/-0.08. The best-fitting
absorption column is (8.1 +/- 2.5) x 10^21 cm^-2, at a redshift of
1.727 (Tanvir et al. GCN Circ. 11230), in addition to the Galactic
value of 2.2 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to
observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from
this spectrum is 4.1 x 10^-11 (7.1 x 10^-11) erg cm^-2 count^-1.  We
do not report a WT time averaged spectral fit here as this would be
affected by the spectral evolution during the flaring activity,
evident in the hardness ratio.

If the light curve continues to decay at the same rate, the count rate
at T+24 hours will be 5.9 x 10^-3 count s^-1, corresponding to an
observed (unabsorbed) 0.3-10 keV flux of 2.4 x 10^-13 (4.2 x 10^-13)
erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00433509.

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


GRB_name: GRB100906A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11245
SUBJECT: GRB 100906A: Observations at the Virtual Telescope
DATE:    10/09/07 04:25:33 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi (Bellatrix Astronomical Observatory, Italy) reports:

The Virtual Telescope main instrument (0.36m-f/8.7) observed
this GRB afterglow on Sept. 7, 2010 at 03:35 Universal Time.

Unfiltered photometry, using R mags from USN0 B1.0 for the
reference stars, provided a magnitude of 19.5, while the
astrometry provided the following end figures:

RA: 44.10s
Decl.: 49.5"
(J2000)

in excellent agreement with UVOT finding (GCN 11227)


This message can be cited.


GRB_name: GRB100901A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11246
SUBJECT: GRB 100901A: TLS Detection at 5.5 days
DATE:    10/09/07 05:13:41 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, F. Ludwig and B. Stecklum (TLS Tautenburg) report:

We observed the afterglow of the Swift GRB 100901A (Immler et al., GCN
11159) with the TLS 1.34m Schmidt telescope under excellent conditions in
the fifth night. We obtained 3 x 600 sec images in Rc, the afterglow is
faintly visible in each single image and well-detected in the stack.
Calibration against the SDSS (Kann et al., GCN 11236) yields Rc = 21.91
+/- 0.11 at 5.550556 days after the GRB. This is somewhat subluminous
compared to the extrapolation of the earlier decay (Kann et al., GCN
11236) but only further deep observations can confirm if another break has
occured.

Further observations are improbably due to upcoming inclement weather.

This message may be cited.


GRB_name: GRB100906A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11247
SUBJECT: GRB 100906A: TLS Monitoring
DATE:    10/09/07 05:33:46 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, A. Nicuesa Guelbenzu, F. Ludwig and B. Stecklum (TLS
Tautenburg) report:

Further to Kann et al. (GCN 11238), we continued monitoring the afterglow
of GRB 100906A (Markwardt et al., GCN 11227) with the 1.34m TLS Schmidt
telescope under excellent conditions in intermittent intervals all night.
Beyond the 15 detections reported in Kann et al. (GCN 11238), we obtained
further nine Rc images (300 sec each) spread over the night, as well as
one further Ic (300 sec) and one further Z (600 sec) image at the end of
the night, during morning twilight. The afterglow is clearly detected in
all our images.

Due to crowding, we use SExtractor under GAIA to subtract background mesh
maps, then perform aperature photometry without needing to measure the
surrounding sky background (which is around 0). Errors are estimates based
on how clear the detection is, the last Rc frame was taken in strong
twilight already. We assume R2 = 15.9 for the USNOB1.0 star at RA =
01:54:55.247, Dec. = +55:38:31.40, and measure:

Midtime  Rc dRc
0.247478 18.97 0.05
0.251517 19.06 0.05
0.255556 19.04 0.05
0.390570 19.08 0.05
0.430154 19.27 0.05
0.451022 19.18 0.05
0.498974 19.64 0.05
0.521231 19.62 0.05
0.525421 19.67 0.05
0.554113 19.80 0.05
0.570108 19.97 0.15

The afterglow seems to transition from a plateau phase (0.25 - 0.4 days)
to a much steeper decay.

Further observations are improbable due to upcoming inclement weather.

This message may be cited.


GRB_name: GRB100906A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11248
SUBJECT: GRB 100906A: Fermi GBM observation
DATE:    10/09/07 07:13:10 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team: 

"At 13:49:27.63 UT on 06 September 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100906A (trigger 305473769 / 100906576)
which was also detected by the Swift-BAT (Markwardt et al. 2010, GCN 11227)
The GBM on-ground location is consistent with the Swift position. 
The angle from the Fermi LAT boresight is 95 degrees.

The GBM light curve shows several bright peaks
with a duration (T90) of about 105 s (50-300 keV). 
The time-averaged spectrum from T0 to T0+122 s is 
best fit by a Band function with Epeak = 106.0 +17.5/-20.2 keV, 
alpha = -1.34 +0.08/-0.06, and beta = -1.98 +0.06/-0.07. 
(Castor C-stat 1044 for 479 d.o.f.)

The event fluence (10-1000 keV) in this time interval is 
(2.64E-05 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+10.1 s in the 10-1000 keV band 
is 14.45 +/- 0.29 ph/s/cm^2.


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


GRB_name: GRB100906A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11249
SUBJECT: GRB100906A: Optical observations at IAO
DATE:    10/09/07 08:42:23 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), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 100906A (Markwardt et al., GCN 11227)
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 2010-09-06 17:20:53 UT (~3.5 h after
the burst).  We detected the previously reported afterglow
(Markwardt et al., GCN 11227; Ivanov et al., GCN 11228; Melandri
et al., GCN 12229) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.15249    17:29:02     840.0    19.3   0.1   18.3   0.1   17.6   0.1
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB100906A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11250
SUBJECT: GRB100906A: non-detection at 15GHz
DATE:    10/09/07 10:08:45 GMT
FROM:    Guy Pooley at MRAO, Cambridge, UK  <ggp1@cam.ac.uk>

The AMI Large Array (Cambridge, UK) was used to observe the field
of GRB 100906A (Markwardt et al, GCN11227) in the band 13.5 to 17.2 GHz
from 2010 Sep 06 23h31m to Sept 07 03h35m (starting 9h42m after the
trigger). The weather conditions were very poor and the noise levels
consequently high; no detection of GRB 100906A was made, with a formal
flux density at the UVOT position from GCN11227 of 380 microJy 
and an rms noise of 136 microJy.

This message is quotable in publications.

Guy Pooley, on behalf of the AMI collaboration


GRB_name: GRB100906A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11251
SUBJECT: Konus-Wind observation of GRB 100906A
DATE:    10/09/07 10:27:34 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 100906A, (Swift/BAT trigger=433509:
Markwardt et.al, GCN 11227; Barthelmy et.al, GCN 11233)
triggered Konus-Wind at T0=49770.732s UT (13:49:30.732)

The burst light curve started with a complex ~20s-long structure,
followed by a weaker softer emission episode starting at ~T0+100 s.
The total duration of the burst is ~150 s.
The emission is seen up to 2 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB100906_T49770/

As observed by Konus-Wind the burst
had a fluence of (2.6  0.4)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+9.728s,
of (2.7  0.3)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+139.264 s) is best fit
in the 20 keV - 2 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -1.5 (-0.2, +0.4),
the high energy photon index beta = -2.3 (<-2.0),
the peak energy Ep = 142(-60, +119) keV (chi2 = 84/60 dof).

The spectrum of the most intense part of the burst
(measured from T0+0.256 to T0+16.384 s) is best fit
in the 20 keV - 2 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -1.1 (-0.1, +0.1),
the high energy photon index beta = -2.2 (-0.3, +0.2),
the peak energy Ep = 180(-40, +45) keV (chi2 = 68/60 dof).

The spectrum of the second bursting episode
(measured from T0+98.304 to T0+122.880 s) is best fit
in the 20 keV - 2 MeV range by the simple power law model with
the photon index = 2.55 (-0.2, +0.25), chi2 = 63/62 dof.

Assuming z=1.727 (Tanvir, Wiersema, and Levan et al., GCN 11230)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, Omega_Lambda = 0.73,
the isotropic energy release E_iso = (2.2  0.4)x1053 erg,
the peak luminosity (L_iso)_max = (5.7  0.6)x1052 erg/s.

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


GRB_name: GRB100906A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11252
SUBJECT: GRB100906A: R band observations
DATE:    10/09/07 15:55:11 GMT
FROM:    Janos Kelemen at Konkoly Obs/Hungary  <kelemen@konkoly.hu>

J. Kelemen and K. Sarneczky (Konkoly Observatory)
Z. Kuli and B. Ujhelyi (Hungarian Astronomical Association)

on behalf of the GRB OT observing program at the Konkoly Observatory.

On 09 september 2010 02:25:57 UT (45390 s after the burst) we observed the
field of GRB 100906A detected by Swift (trigger=433509; Markwardt et al., 
GCN 11227) with a 60/90 cm  Schmidt telescope located at the Mountain Station
of the Konkoly Observatory using R filter. The exposure time of the CCD images
were 300 s. We clearly detected the fading afterglow at RA(J2000) = 01h 54m
44.12s Dec(J2000) = +55d 37' 49.3" (astrometry with ASTROMETRICA using UCAC3
catalogue.) with an uncertainty of 0.2 arcseconds. 

Time      Mag     Error.      Flag.
[s]       [R]    [1-sigma]  
-------------------------------------
45390    20.6      0.1          -
45709    20.7      0.1          -
46028    21.3      0.1          -
-------------------------------------

The above magnitudes have not been corrected for the Galactic extinction.


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11253
SUBJECT: GRB 100906A: GRAS-007 optical observations
DATE:    10/09/07 17:19:18 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:

GRAS-007 PlaneWave CDK 17" F6.8 telescope and STL-11000M CCD camera
(Global-Rent-a-Scope, Nerpio, Spain) were used to detect GRB 100906A optical
afterglow. The observations were started at 2010-09-07 02:13:24 (UT) and
stopped at 2010-09-07 03:40:53 (UT). A number of unfiltered images with 120
sec and 600 sec exposure time were made. The afterglow was detected at
following position RA 01 54 44.12 and DEC +55 37 49.4 consistent those given
by Melandri A. et al. (GCN 11229) to within positional errors.

The following magnitude was obtained from the observations using USNO-B1.0
1456-0062169 (R = 15.70) as the comparison:

+T0 (hour)  Filter Exp (sec) Mag Mag err Limit
   
13:00:24 (midpoint) unfiltered 3x600s 19.8 0.4 21.0

   

A JPG image of the 3x600 sec observations is available at the following URL:
http://cutenews.kassiopeia.net/data/upimages/GRB100906A.jpg


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11254
SUBJECT: GRB 100906A: RTT150 optical observations
DATE:    10/09/07 18:30:39 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

A. Tkachenko (IKI), I. Khamitov (TUG), 
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Bikmaev, N. Sakhibullin (KSU/AST),
Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)


The optical counterpart of GRB 100906A (GCN 11227) was observed with
Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National
Observatory, Turkey), starting at Sep 06, 19:28 UT, i.e. ~5.64 hours after
the burst, using TFOSC.

Three series of BRI frames were made under moderate weather conditions. The
afterglow is clearly detected in all images.

Assuming the star at RA = 01:54:46.82, Dec. = +55:37:55.3 to have USNOB1.0
R2MAG = 15.70, we estimated the following magnitudes for the OT on combined
images of every set:

 t-t0     band   mag   err 
 6.048 h    R   18.80  0.02
 9.610 h    R   19.08  0.02
13.554 h    R   19.69  0.04

The color of the afterglow changes from (B-R)=1.21 to (B-R)=1.31 at the
beniginning and at the end of our observations.


GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11255
SUBJECT: GRB 100901A: CrAO optical observations
DATE:    10/09/07 18:32:18 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed  the afterglow (Immler et al., GCN 11159) of the Swift GRB 
100901A (Immler  et al., GCN 11159) with AZT-11 telescope of CrAO 
observatory on September 3 (UT) 20:24 - 21:18 and 5 (UT) 22:39 - 23:51.  The 
afterglow photometry is based on the same reference stars of SDSS DR7 used 
in  our previous reports (GCNs 11191, 11200):

T0+      Filter,   Exposure, mag.
(mid, d)              (s)

2.3045 R  19x180 20.07 +/- 0.08
4.4045 R  18x180 21.10 +/- 0.20

The photometry is compatible with photometry  at the same period (4.39 - 
4.55 days) reported by Kann et al (GCN 11236). 


GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11256
SUBJECT: GRB 100901A: Confirmation of WSRT Radio Detection
DATE:    10/09/07 19:33:23 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

  A.J. van der Horst (NASA/MSFC/ORAU), K. Wiersema (U of Leicester),
A.P. Kamble, R.A.M.J. Wijers, E. Rol (U of Amsterdam) and
C. Kouveliotou (NASA/MSFC) report on behalf of a large collaboration:

"We observed the position of the GRB 100901A afterglow at 4.9 GHz
with the Westerbork Synthesis Radio Telescope at September 6 20.33 UT
to September 7 08.30 UT, i.e. 5.28 - 5.78 days after the burst (GCN 11159).
We confirm our earlier detection (GCN 11221) and measure a brightening
of the radio counterpart at the position of the X-ray and UV/optical
afterglow (GCN 11195), with a flux density of 193 +/- 30 microJy.

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


GRB_name: GRB100901A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11257
SUBJECT: EVLA detection of radio afterglow of GRB100901A
DATE:    10/09/07 21:09:26 GMT
FROM:    Poonam Chandra at Royal Mil. College Canada  <Poonam.Chandra@rmc.ca>

Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on behalf of a larger 
collaboration:

"We observed GRB 100901A (Immler et al. GCN 11159) with the Expanded Very Large 
Array (EVLA) on September 06.47 UT at a C band wide receiver (receiver 
frequency range 4-8 GHz). We detect the radio afterglow of the GRB at the 
Swift-XRT position (Osborne et al. GCN 11167) at 4.5 and 7.9 GHz frequencies. 
The flux densities at 4.5 and 7.9 GHz bands are 331+/-30 uJy and 
440+/-27 uJy, respectively.

The EVLA is still undergoing active commissioning and we caution that
these results should be considered preliminary. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc."


GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11258
SUBJECT: GRB100901A: IAO optical upper limits at 4 days after the burst
DATE:    10/09/08 18:36:26 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), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 100901A (Immler et al., GCN 11159)
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 2010-09-05 19:53:16 UT (~4.3 day after the
burst). We did not detect the previously reported afterglow (Immler
et al., GCN 11159 and many follow-up observations) 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
------------------------------------------------------
4.26159    19:50:52  1080.0     >21.6  >21.3  >19.8
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB100906A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11259
SUBJECT: GRB100906A: detection at 15GHz
DATE:    10/09/09 10:16:04 GMT
FROM:    Guy Pooley at MRAO, Cambridge, UK  <ggp1@cam.ac.uk>

The AMI Large Array (Cambridge, UK) was used to make two further
observations of the field of GRB 100906A (Markwardt et al, GCN11227)
in the band 13.5 to 17.2 GHz (GCN11250 reports the first observation).

date/time                              flux   sigma / microJy
2010 Sep 08 06h51m to Sep 08 07h51m     137     140
2010 Sep 08 22h03m to Sep 09 00h18m     465      70

The GRB is clearly detected in the second of these observations, 
mean time 57h17m after the trigger.

(A radio source catalogued in NVSS, 87GB, 7C is also visible in the 
field near 01 55 11 +55 35 20 (J2000), about 4.5 arcmin from the GRB.)


This message is quotable in publications.

Guy Pooley, on behalf of the AMI collaboration


GRB_name: GRB100909A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11260
SUBJECT: GRB 100909A: a long GRB detected by INTEGRAL
DATE:    10/09/09 10:22:05 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 60 s has been detected by IBAS in the 
IBIS/ISGRI data at 09:04 U.T. on September 9th.  The detection 
significance was slightly below the threshold for automatic alert 
delivery.

Its refined coordinates (J2000) are:
 RA:  73.9506 [degrees]
 DEC: 54.6544 [degrees]

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

A preliminary analysis gives a 20-200 keV fluence of about 10e-6 erg/cmsq.

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB100909A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11261
SUBJECT: GRB 100909A: Swift target of opportunity observation
DATE:    10/09/09 13:04:56 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU), S. D. Barthelmy (GSFC), M. M. Chester (PSU),
P. A. Evans (U Leicester), J. M. Gelbord (PSU), J. A. Kennea (PSU),
K. L. Page (U Leicester) and R. L. C. Starling (U Leicester) report on
behalf of the Swift Team:

Swift began a target of opportunity observation of GRB 100909A
on September  9, 2010 at 12:18 UT, approximately 3.2 hours
after the burst was detected by INTEGRAL. Swift data for these
observations utilize Target ID 20147. 

The XRT began observing the field at 12:19:37.4 UT, 11.7 ks after the
INTEGRAL trigger. In 1.8 ks of promptly downlinked data there is a faint source,
detected at the 3.2-sigma level at: RA, Dec= 73.94797, +54.65798 which is 
equivalent to:

RA (J2000) : 04h 55m 47.51s
Dec (J2000): +54d 39' 28.7''

with an estimated uncertainty of 6 arcsec (radius, 90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 11687 seconds after the INTEGRAL trigger. No credible
afterglow  candidate has been found in the initial data products. The
2.7'x2.7' sub-image  covers 44% of the INTEGRAL error circle and 100%
of the XRT error circle. The typical 3-sigma upper limit has  been
about 19.6 mag. The coverage of the INTEGRAL and XRT error circles by
the 8'x8'  region for the list of sources generated on-board is
uncertain because the  large number of sources filled the available
telemetry. No correction has been  made for the expected extinction
corresponding to E(B-V) of 0.51. 

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


GRB_name: GRB100902A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11262
SUBJECT: GRB 100902A :  Confirmation of afterglow and re-brightening with C=?UTF-8?Q?FHT_r=E2=80=99?=-band imaging
DATE:    10/09/09 14:08:41 GMT
FROM:    Kuiyun Huang at ASIAA  <ljhuang@asiaa.sinica.edu.tw>

GRB 100902A :  Confirmation of afterglow and re-brightening with CFHT rÃ¢\200\231-band imaging

K.Y. Huang (ASIAA), Y. Urata (NCU), M. Im (CEOU/SNU) and T. Sakamoto (NASA/GSFC)

We made rÃ¢\200\231-band observation using CFHT for the GRB 100902A field. The observation started at 5.8 days after the
Swift/BAT trigger (Sakamoto et al. GCN 11181).  The stacked image show a point source at the position of the optical
afterglow candidate reported by Updike et al. (GCN 11209). The brightness against with several USNO-B stars is 23.2
+/-0.1, which is about 1 magnitude brighter than the report of GROND. This  result implies the source could be the
optical afterglow and show the re-brightening.
Combined with reports of GROND (Updike et al. GCN 11209) and UKIRT (Im et al GCN 11210), the GRB 1000902A
afterglow shows the extremely red color (r-K~ 5 mag).

Further photometric and spectroscopic observations are encouraged.

We thank Dr. Thomas Kruehler and Dr. Sylvio Klose for providing the reference image taken by GROND. We also
thank Dr. Nadine Manset and QSO team for arranging the CFHT observations.


GRB_name: GRB100909A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11263
SUBJECT: GRB 100909A: Planned XMM-Newton observation
DATE:    10/09/09 14:08:46 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.esac.esa.int>

XMM-Newton will observe GRB 100909A at location
(RA=4h 55m 48s, DEC=+54d 39' 15", J2000),
starting at 04:30 UT, on September 10, 2010,
for an exposure of 31000 seconds.




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GRB_name: GRB100909A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11264
SUBJECT: GRB 100909A: ROTSE-III Optical Limits
DATE:    10/09/09 14:29:13 GMT
FROM:    Brad Schaefer at LSU  <schaefer@grb.phys.lsu.edu>

B. E. Schaefer (Louisiana State) reports on behalf of the ROTSE 
collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
100909A (INTEGRAL trigger 6060; Mereghetti et al., GCN 11260), producing
images beginning 6.4 s after the GCN notice time. An automated response
took the first image at 10:41:45.5 UT, 5811.6 s after the burst.  For the
first 20 minutes the conditions were partly cloudy with occassional holes,
but after 11:02 UT the sky became clear and excellent. We took 10 5-sec,
10 20-sec and 116 60-sec exposures. These unfiltered images are calibrated
relative to USNO A2.0 (R).

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma INTEGRAL/IBIS error circle, for both single images and coadding
into sets of 10.  The Swift XRT team reports that a faint X-ray source is
visible at 12:19 UT (Siegel et al. 2010, GCN 11261), and we have also
closely examined this error circle, again finding no variable star or
object of interest.  The Swift XRT position is not crowded, although there
is one fairly faint star in it. Individual images have limiting magnitudes
ranging from 12.8-17.6; we set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
10:44:07.5   10:45:25.7        78     15.7         5953.6       Y
11:02:58.7   11:07:40.0       281     18.5         7084.8       Y


GRB_name: GRB100909A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11265
SUBJECT: GRB 100909A: Faulkes Telescope North afterglow candidate
DATE:    10/09/09 14:58:36 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), Z. Cano, D. Bersier (LJMU),
P. O'Brien (U. Leicester) report on behalf of a large collaboration:

The Faulkes Telescope North automatically began observing INTEGRAL
GRB 100909A (Mereghetti et al. GCN Circ. 11260) on September 09,
10:42:34 UT, 1.6 hours from the GRB trigger time.
Within the Swift-XRT error circle (Siegel et al. GCN Circ. 11261)
we identify an uncatalogued, possibly fading object at the following
position:

RA(J2000):  04:55:47.86
Dec(J2000): +54:39:32.1

with the following magnitudes:

Mid Time from      Exposure      Filter     Magnitude
GRB (hours)          (s)
-------------------------------------------------------
2.07                540            R        21.6 +- 0.2
2.16                520            i        20.6 +- 0.1
5.05               1200            R        22.1 +- 0.2
-------------------------------------------------------

Calibration was done against the nearby USNOB-1 star
RA,DEC=04:55:49.14, +54:39:42.66, assuming R2=16.82, I=16.06.
We note that the uncatalogued source lies 3" from a
USNOB-1 object with R2=18.54.


GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11266
SUBJECT: GRB 100901A: optical observation in Maidanak, break confirmation
DATE:    10/09/10 01:48:03 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (SAI MSU),  A. Pozanenko (IKI),  M. Ibrahimov (MAO), B. Hafizov 
(MAO), B. Satovski (Astrotel)  report on behalf of  larger GRB  follow-up 
collaboration:

We observed  the field of the Swift GRB 100901A (Immler  et al., GCN 11159) 
with AZT-22 telescope of Maidanak observatory starting  Sep. 7 (UT) 
20:32:06. We clearly detect the afterglow (Immler  et al., GCN 11159 and 
other follow-up ground based observations) in R-filter. The photometry of a 
stacked image is based on the same reference SDSS-DR7 stars used by our 
collaboration previously (GCNs 11191, 11200, 11255):

T0+      Filter,   Exposure, mag.
(mid, d)              (s)

6.2977  R        4*300    22.05+/-0.09

The photometry above confirms suggested break (Kann et al, GCN 11246) in a 
light curve of the afterglow. 


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11267
SUBJECT: GRB 100906A: optical observations at Mt.Terskol
DATE:    10/09/10 02:44:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

M. Andreev, A. Sergeev (Terskol Branch of Institute of Astronomy), 
A.Pozanenko (IKI), N. Parakhin, S. Velichko, N. Borachok (IC AMER)
V. Petkov (Baksan Neutrino Observatory INR RAS) on behalf of larger GRB 
follow up collaboration report:

We observed the field of Swift GRB 100906A (Markwardt  et al., GCN 11227) 
with Zeiss-2000 telescope of Mt.Terskol observatory starting Sep. 06 (UT) 
23:56. We obtained images in g,V, r filters. The afterglow (Markwardt et al. 
GCN 11227, Ivanov et al. GCN 11228, Melandri et al. GCN 11229)  is clealy 
detected in all filters. The preliminary photometry is based on GSC2.3 
catalog and Jordi et al. (2006) UBVRcIc -> ugriz transformations:

T0+      Filter,     Exp.       OT
(d)

0.4213   r            6x120   19.43 +/-0.03
0.4626   g         10x120    20.11 +/-0.02
0.4785   V          7x120    19.77 +/-0.03


GRB_name: GRB100909A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11268
SUBJECT: GRB 100909A: Swift-XRT refined analysis
DATE:    10/09/10 03:35:20 GMT
FROM:    Jonathan Gelbord at PSU/Swift  <jgelbord@astro.psu.edu>

J. M. Gelbord (PSU) and M. H. Siegel (PSU) report on behalf of the
Swift-XRT team:

We have analysed 7.7 ks of XRT data for GRB 100909A (Mereghetti et al.,
GCN Circ. 11260; Siegel et al., GCN Circ. 11261), from 11.8 ks to
25.8 ks after the Integral trigger. The data are entirely in Photon
Counting (PC) mode. Using 1953 s of PC mode data and 1 UVOT images,
we find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
73.94760, +54.65970 which is equivalent to:

RA (J2000): 04 55 47.42
Dec(J2000): +54 39 34.8

with an uncertainty of 5.4 arcsec (radius, 90% confidence).

The X-ray light curve appears to be fading, although we note that the
evidence is limited by the small number of counts in the XRT data
(approximately 60 counts spread over three orbits).  When modelled with
a power-law decay, the best-fitting decay index is alpha=1.2 (+1.1,
-1.0).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+0.8, -0.7). The best-
fitting absorption column is 4.8 (+3.4, -2.6) x 10^21 cm^-2, consistent
with the Galactic value of 2.8 x 10^21 cm^-2 (Kalberla et al. 2005).
The time-averaged 0.3-10 keV flux observed (unabsorbed) is 2.8 x 10^-13
(7.1 x 10^-13) erg cm^-2 s^-1. The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum is
4.4 x 10^-11 (1.1 x 10^-10) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of
1.2, the count rate at T+24 hours will be 1.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of
4.2 x 10^-14 (1.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020147.

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


GRB_name: GRB100909A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11269
SUBJECT: GRB100909A: NOT optical afterglow confirmation
DATE:    10/09/10 05:38:48 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek, Javier Gorosabel (IAA-CSIC) and Sergio Simon 
(IAC-ULL) report on behalf of a larger colaboration:

"We observed the optical afterglow of GRB100909A (Mereghetti
et al. GCNC11260; Siegel et al. GCNC11261; Guidorzi et al.
GCNC 11265) with the 2.56m Nordic Optical Telescope equipped
with ALFOSC, starting on September 10 at 4:30 UT (i.e. 19.4h
after the burst).

A preliminary analysis of the 600-s R-band exposure shows the
proposed afterglow with magnitude R~23.2 in respect to the
R2=18.54 object mentioned by Guidorzi et al. (GCNC11265).
This implies a decay rate alpha~1.6, and confirms the fading
nature of the object.

This message may be cited."


GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11270
SUBJECT: GRB 100901A: optical observations in Mondy and R-light curve
DATE:    10/09/10 09:59:02 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the  Swift GRB 100901A (Immler  et al., GCN 11159)  with 
AZT-33IK telescope of Sayan observatory (Mondy) starting Sep. 01 (UT) 
13:44:30 and continued observations within 2 nights after burst onset. 
Preliminary light curve of Mondy observation in R as well as  R, r and 
nonfiltered observations inreported on  behalf of our follow up 
collaboration (Klunko et al,  GCN 11162; Andreev  et al,  GCN 11166; Andreev 
et al,  GCN 11168; Elenin et al,  GCN 11184;  Andreev  et al,  GCN 11191; 
Andreev  et al,  GCN 11200; Andreev  et al,  GCN 11201; Elenin et al,  GCN 
11234; Rumyantsev et al,  GCN 11255; Volnova et al,  GCN 11266) can be found 
at
http://grb.rssi.ru/GRB100901A/GRB100901A_lc.png

The photometry calibration was performed against the same SDSS DR7 stars.
There are some distinct features of the light curve. The tail of the flare 
reported earlier (Ivanov et al, GCN 11178), the rapid increase brightness 
after power law decay until 0.1d since trigger, the deep gap at ~0.13d, and 
the bump at ~0.3d corresponding to the bump in XRT light curve (Page et al, 
GCN 11171). We also confirm the late break between 5 and 6 days of the 
afterglow (Kann et al,  GCN 11246; Volnova et al,  GCN 11266). 

[GCN OPS NOTE(10sep10):  Per author's request, the Subject line
was changed from 100906A to 100901A.]


GRB_name: GRB100901A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11271
SUBJECT: GRB 100901A: errata of GRB name in GCN 11270
DATE:    10/09/10 10:43:36 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration  report:

In Subject field of GCN 11270 we erroneously reported the GRB name.
It should be "GRB 100901A: optical observations in Mondy and R-light curve"
The light curve of GRB 100906A will be reported later.
We apologize for possible inconvenience.


GRB_name: GRB100909A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11272
SUBJECT: GRB 100909A: Swift/UVOT observations
DATE:    10/09/10 21:19:23 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and M. H. Siegel (PSU) report, on behalf
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of
GRB 100909A 11747 s after the INTEGRAL trigger (Mereghetti et
'al.,GCN Circ. 11260). Data summed from the first and second orbits
do not reveal a source at the enhanced position of the X-ray
afterglow (Gelbold et al., GCN Circ. 11268).

The 3-sigma upper limits f are reported below:

FILTER T_start(s) T_stop    Exposure   Mag/3UL
========================================================
wh      11747     25861     1809       >21.9
v       14755     18362      894       >20.21
b       11906     44659     1770       >21.48
u       33619     34527      885       >20.84
w1      19275     20040      752       >20.39
w2      13732     14301      561       >20.33
=======================================================

  The above magnitudes are not corrected for the strong Galactic
extinction corresponding to a reddening of E_{B-V} = 0.51 (Schlegel
et al., 1998, ApJS, 500, 525). The photometry is on the UVOT
photometric system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB100909A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11273
SUBJECT: GRB100909A: MITSuME  Ishigakijima Optical upper limits
DATE:    10/09/12 01:13:44 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), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 100909A (Mereghetti et al., GCN 11260)
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 10 16:05:58 UT (~1.3 days after the INTEGRAL
trigger). We could not detect the previously reported afterglow
(Siegel et al., GCNC 11261; Guidorzi et al., GCN 11265;
Gelbord and Siegel, GCN 11268; Jelinek et al., GCN 11269) 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
------------------------------------------------------
1.31686    16:41:10   960.0     >21.3  >20.9  >20.0
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB100910A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11276
SUBJECT: GRB 100910A: Fermi GBM detection
DATE:    10/09/13 15:22:24 GMT
FROM:    Narayana Bhat at U Alabama/Huntsville/GBM  <Narayana.Bhat@nasa.gov>

P. N. Bhat(UAHuntsville)
reports on behalf of the Fermi GBM Team:

"At 19:37:43.96UT on 10 September 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100910A (trigger 305840265 / 100910818).

The on-ground calculated location, using the GBM trigger
data, is RA = 238.1, DEC = -34.62 (J2000 degrees,
equivalent to 15 h 52.4 m, -34 d 37'), with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
 
The angle from the Fermi LAT boresight is 51 degrees.

The GBM light curve consists of 4 pulses
with a duration (T90) of about 14.6 s (50-300 keV).
The time-averaged spectrum from T0-3.2 s to T0+18.3 s is
best fit by a Band function with Epeak = 143 +/- 7.0 keV,
alpha = -0.92 +/- 0.04, and beta = -2.26 +/- 0.08

(C-stat 1038 for 733 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(1.48 +/- 0.02)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+8.576 s in the 10-1000 keV band
is 23.35 +/- 0.24 ph/s/cm^2.

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


GRB_name: GRB100915A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11277
SUBJECT: GRB 100915A: Swift detection of a likely burst
DATE:    10/09/15 01:51:42 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@astro.psu.edu>

O. M. Littlejohns (U Leicester), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), A. Rowlinson (U Leicester),
M. H. Siegel (PSU) and M. Stamatikos (OSU/NASA/GSFC) report on behalf
of the Swift Team:

At 01:31:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100915A (trigger=434178).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 315.648, +65.667 which is 
   RA(J2000) = 21h 02m 36s
   Dec(J2000) = +65d 39' 60"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This is a BAT image-only trigger with significance
reported on-board of 8.67 sigma.  Ground processing of the BAT scaled map
image indicates a slightly weaker, 6.4 sigma excess.  As is typical for 
such triggers, there is nothing obvious in the raw light curve.  We will 
need to wait for event-by-event data on the ground to clarify the nature 
of the light curve. 

The XRT began observing the field at 01:33:17.7 UT, 131.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
315.6937, 65.6731 which is equivalent to:
   RA(J2000)  = 21h 02m 46.50s
   Dec(J2000) = +65d 40' 23.0"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 71 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 2.27
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 5.89e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 140 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
0.51. 

Burst Advocate for this burst is O. M. Littlejohns (oml2 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB100915B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11278
SUBJECT: GRB 100915B: a long GRB detected by INTEGRAL
DATE:    10/09/15 07:19:49 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 4 s has been detected by IBAS in the 
IBIS/ISGRI data at 05:49:39 U.T. on September 15th.

Its refined coordinates (J2000) are:
RA=  85.3944 (deg) 
DEC=+25.0949 (deg)

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

A preliminary analysis gives a   20-200 keV fluence of about  3e-7 
erg/cm2 and a peak flux of about 1 ph/cm2 s  (1 s integration time)

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB100915A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11279
SUBJECT: GRB 100915A: Enhanced Swift-XRT position
DATE:    10/09/15 10:24:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 5278 s of XRT Photon Counting mode data and 9 UVOT
images for GRB 100915A, 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 = 315.69440, +65.67303 which is equivalent
to:

RA (J2000): 21h 02m 46.66s
Dec (J2000): +65d 40' 22.9"

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: GRB100915A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11280
SUBJECT: GRB 100915A: Swift-XRT refined analysis
DATE:    10/09/15 11:37:28 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@star.le.ac.uk>

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

We have analysed 8.5 ks of XRT data for GRB 100915A (Littlejohns et al.
GCN Circ. 11277), from 138 s to 18.8 ks after the BAT trigger. The data
comprise 95 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Osborne et al. (GCN. Circ 11279).

The light curve can be modelled with a series of
power-law decays. The initial decay index is alpha=0.9 (+0.6, -1.8). At
T+320 s the decay steepens to an alpha of 2.4 (+0.6, -0.3). The light
curve breaks again at T+1058 s to a decay with alpha=0.66 (+0.16,
-5.16), before a final break at T+6126 s after which the decay index is
1.6 (+0.8, -0.3).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.37 (+0.21, -0.20). The
best-fitting absorption column is 3.8 (+1.3, -1.1) 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 1.74 (+/-0.18) and a
best-fitting absorption column of 4.6 (+1.0, -0.9) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 5.5 x 10^-11 (8.2 x 10^-11) erg cm^-2
count^-1.

If the light curve continues to decay with a power-law decay index of
1.6, the count rate at T+24 hours will be 1.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.7 x
10^-14 (8.4 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/00434178.

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


GRB_name: GRB100915A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11281
SUBJECT: GRB 100915A: Swift-BAT refined analysis
DATE:    10/09/15 13:06:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), O. M. Littlejohns (U Leicester),
C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
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 100915A (trigger #434178)
(Littlejohns, et al., GCN Circ. 11277).  The BAT ground-calculated position is
RA, Dec = 315.664, 65.676 deg, which is 
   RA(J2000)  =  21h 02m 39.4s 
   Dec(J2000) = +65d 40' 32.3" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 54%.
 
The mask-weighted light curves shows two broad peaks, the first starting
at ~T-90sec, peaking at ~T+5 sec, and ending at ~T+90 sec.  The second,
weaker peak starts at ~T+110, peaks at ~T+170 sec and ends at ~T+190 sec.
T90 (15-350 keV) is 200 +- 31 sec (estimated error including systematics).
 
The time-averaged spectrum from T-36.3 to T+72.2 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 2.88 +- 0.00, 
and Epeak of 265.2 +- 0.0 keV (chi squared 66.1 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+8.76 sec in the 15-150 keV band is
0.5 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.50 +- 0.23 (chi squared 73.1 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/434178/BA/


GRB_name: GRB100915A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11282
SUBJECT: GRB 100915A:  Swift/UVOT Upper Limits
DATE:    10/09/15 14:10:44 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and O. M. Littlejohns (U Leicester) report on behalf
of the Swift/UVOT team.

The Swift/UVOT began settled observations of the field of
GRB 100915A 123s after the BAT trigger (Littlejohns et al.,
GCN Circ. 11277).  No new source is found at the enhanced
XRT position (Osborne et al., GCN Circ. 11279).

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

FILTER      T_start(s)    T_stop     Exposure      Mag/3UL
===========================================================
white fc        140          290        147        >21.46
white           142        11637       1619        >22.83
v               123        13122       1057        >20.98
b               557         7343        467        >21.43
u fc            300          550        246        >20.68
u               300         7161        963        >21.52
uvw1            680         6956        491        >20.87
uvm2           1256        18902       2787        >21.79
uvw2            606        12544       1152        >21.50

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 0.51 (Schlegel et al.,
1998, ApJS, 500, 525).  The photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB100915A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11283
SUBJECT: GRB 100915A: Correction to Swift-BAT refined analysis
DATE:    10/09/15 14:56:36 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC) 
(i.e. the Swift-BAT team):

We would like to make corrections to the BAT refined analysis of GRB 100915A 
(GCN Circ. 11281).  The BAT time-averaged spectrum is best fit by a simple 
power-law (PL) model rather than a power-law with an exponential cutoff (CPL) 
model.  We believe a low signal to noise in the observed spectrum of this burst 
causes a significant improvement in chi2 by a CPL model over a PL model.  We 
would like to correct the 3rd paragraph of GCN Circ. 11281 to:

"The time-averaged spectrum from T-36.3 to T+72.2 sec is best fit by a simple 
power-law model.  The power law index of the time-averaged spectrum is
1.50 +- 0.24.  The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+8.76 sec in the 15-150 keV band
is 0.5 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. "

We apologize for possible inconvenience.  We would like to thank Eleonora Troja 
for pointing this issue.  


GRB_name: GRB100915B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11284
SUBJECT: GRB 100915B: Fermi GBM observation
DATE:    10/09/15 20:52:50 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

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

"At 05:49:39.62 UT on 15 Sept 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100915B (trigger 306222581 / 100915243)
which was also detected by INTEGRAL/IBIS (Mereghetti et al. 2010, GCN
11278). The GBM on-ground location is consistent with the INTEGRAL
position.
The angle from the Fermi LAT boresight is 125 degrees.

The GBM light curve consists of one pulse
with a duration (T90) of 7.8 (+/- 0.7) s (50-300 keV).
The time-averaged spectrum from T0-5.6 s to T0+3.6 s is
adequately fit by a power law function with an exponential
high energy cutoff.  The power law index is 1.35 (+1.63/- 1.10) and
the cutoff energy, parameterized as Epeak, is 83.49 (+ 14.50/-9.81) keV
(CSTAT 273 for 243 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(4.82 +/- 0.06)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-2.56 s in the 10-1000 keV band
is 1.85 +/- 0.19 ph/s/cm^2.

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


GRB_name: GRB100915A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11285
SUBJECT: GRB 100915A: GRT Optical Observation
DATE:    10/09/16 00:11:56 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (UMCP/GSFC), N. Gehrels (GSFC),
T. Okajima (JHU/GSFC), Y. Urata (NCU), C.A. Wallace (FGCU)

We observed the field of GRB 100915A detected by Swift
(trigger #434178; Littlejohns et al., GCN Circ. 11277) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

A total 423 images of 5 sec (200 images), 30 sec (80 images), 
60 sec (120 images) and 100 sec (23 images) exposures were taken in 
the R filter starting from September 15 01:33:32 (UT) about 146 
seconds after the trigger (70 seconds after the BAT position notice) 
and stopped on September 15 05:49:30 (UT).  We do not detect 
the optical afterglow both in the individual images and the stacked 
image, which only combined good quality 418 images, inside the XRT 
position (Osborne et al., GCN #11279).  The estimated five sigma 
upper limit of the combined image (total exposure of 12500 sec) is 
~19.8 mag using the USNO-B1 catalog. 


GRB_name: GRB100915B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11286
SUBJECT: GRB 100915B: GRT Optical Observation
DATE:    10/09/16 00:15:23 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (UMBC/GSFC), D. Donato (UMCP/GSFC), N. Gehrels (GSFC),
T. Okajima (JHU/GSFC), Y. Urata (NCU), C.A. Wallace (FGCU)

We observed the field of GRB 100915B detected by INTEGRAL 
(trigger #6061; Mereghetti et al., GCN Circ. 11278) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).

A total 226 images (excluding the bad quality images) of 5 sec (200 images) 
and 30 sec (26 images) exposures were taken in the R filter starting from 
September 15 05:50:55 (UT) about 76 seconds after the trigger (62 seconds 
after the initial INTEGRAL position notice) and stopped on 
September 15 06:37:44 (UT).  The weather condition was relatively poor 
during the observation.  We do not detect the optical afterglow both in 
the individual images and the stacked image inside the INTEGRAL position 
(Mereghetti et al., GCN #11278).  The estimated five sigma upper limit 
of the combined image (total exposure of 1740 sec) is ~17.7 mag using 
the USNO-B1 catalog. 


GRB_name: GRB100915A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11287
SUBJECT: GRB100915A: MITSuME  Ishigakijima Optical upper limits
DATE:    10/09/16 15:22:45 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), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 100915A (Littlejohns et al., GCN 11277)
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 10 10:46:01 UT (~9.2 h after the trigger).
We did not find any new point source within the enhanced XRT error
circle (Osborne et al., GCNC 11279) 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
------------------------------------------------------
0.40450    11:13:34   2760.0    >22.0  >21.5  >21.0
0.56696    15:07:30   4560.0    >22.5  >21.8  >21.1
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB100917A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11288
SUBJECT: GRB 100917A: Swift detection of a burst
DATE:    10/09/17 05:23:07 GMT
FROM:    Owen Littlejohns at U of Leicester  <oml2@star.le.ac.uk>

O. M. Littlejohns (U Leicester), A. P. Beardmore (U Leicester),
P. A. Evans (U Leicester), J. M. Gelbord (PSU), E. A. Hoversten (PSU),
C. B. Markwardt (NASA/GSFC), C. Pagani (U Leicester),
K. L. Page (U Leicester), A. Rowlinson (U Leicester),
M. H. Siegel (PSU) and C. A. Swenson (PSU) report on behalf of the
Swift Team:

At 05:03:25 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100917A (trigger=434360).  Swift did not slew to the burst
location due to a moon observing constraint. The BAT on-board calculated 
location is RA, Dec 289.265, -17.104 which is 
   RA(J2000) = 19h 17m 04s
   Dec(J2000) = -17d 06' 15"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a weak peak 
with a duration of about 4 sec.  The peak count rate
was ~400 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift cannot slew to the BAT position. 
There will thus be no XRT or UVOT data for this trigger. 

This trigger will be in moon constraint until approximately 06:30 UT
 on the 19th of September. 

Burst Advocate for this burst is O. M. Littlejohns (oml2 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB100917A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11289
SUBJECT: GRB 100917A: Swift-BAT refined analysis
DATE:    10/09/17 18:46:15 GMT
FROM:    Craig Markwardt at NASA/GSFC/UMD  <craigm@milkyway.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
O. M. Littlejohns (U Leicester), C. B. Markwardt (GSFC/UMD),
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-240 to T+960 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 100917A (trigger
#434360) (Littlejohns, et al., GCN Circ. 11288).  The BAT ground-
calculated position is RA, Dec = 289.250, -17.120 deg which is
    RA(J2000)  =  19h 17m 00.1s
    Dec(J2000) = -17d 07' 12.1"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 62%.

The mask-weighted light curve shows a FRED-like profile with rise time
of ~5 sec and decay time of ~30 sec.  T90 (15-350 keV) is 66 +- 22 sec
(estimated error including systematics).

The time-averaged spectrum from T-2.1 to T+76 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.67 +- 0.23.  The fluence in the 15-150 keV band is 8.6 +-
1.2 x 10^-7 erg/cm2.  The 1-sec peak photon flux measured from T+3.22
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.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/434360/BA/


GRB_name: GRB100916A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11290
SUBJECT: GRB 100916A: Fermi GBM detection
DATE:    10/09/18 04:35:26 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

  A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM 
Team:

"The Fermi Gamma-Ray Burst Monitor (GBM) trigger 306355274 at 
18:41:12.49 UT
on 16 September 2010, tentatively classified as Distant Particles, is in 
fact
a GRB. The source location is close to the Earth's limb, which gave rise to
the original classification. The GBM light curve consists of a ~0.5 s short
spike on top of lower level emission extending for ~20 s.

The on-ground location of GRB 100916A, using the GBM trigger data, is
RA = 152.0, Dec = -59.4 (J2000 degrees, equivalent to 10h 08m, -59d 23'),
with an uncertainty of 3.5 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 142 
degrees."


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11291
SUBJECT: GRB100906A: Ashra-1 observation of early optical emission
DATE:    10/09/19 07:17:24 GMT
FROM:    Makoto Sasaki at ICRR/U.Tokyo  <sasakim@icrr.u-tokyo.ac.jp>

Y.Asaoka, S.Hirai, T.Itoh, M.Masuda, Y.Morimoto, K.Ota, M.Sasaki
(ICRR,Univ.Tokyo), D.Kogure, S.Ogawa, H.Tsujikawa (Toho Univ.),
P.Binder (Univ.Hawaii Hilo), J.Learned (Univ.Hawaii Manoa)
report on behalf of the Ashra-1 collaboration:

We have searched for optical emission in the field of GRB100906A
(Markwardt, et al., GCN Circ. 11227) around the BAT-triggered GRB time
(T0) with one of the light collector units in the Ashra-1 detector
(http://www.icrr.u-tokyo.ac.jp/~ashra) on Mauna Loa on Hawaii Island
(latitude = 19.5412 deg. N, longitude =155.5676 deg. W, altitude =3330m).

The Ashra-1 light collector unit has the achieved resolution of a few
arcmin, viewing 42 degree circle region of which center is located at
Alt = 60 deg, Azi = 0 deg. The sensitive region of wavelength is
similar to the B-band.

We quickly analyzed 200 images covering the field of GRB100906A every
6s with 4s exposure time respectively during the observation between
T0-600s and T0+600s. We detected no new optical object within the PSF
resolution around the GRB100906A determined by Swift-UVOT (Markwardt,
et al., GCN Circ. 11227)

As a result of our preliminary analysis, the following 3-sigma limiting
magnitudes are derived:

----------------------------------------------------------------------
Starting&Ending Exp.Time,  3-sigma Limit. Mag.
----------------------------------------------------------------------
-593.2   -589.2      12.1
-587.3   -583.3      12.2
    .        .                       .
    .        .                       .
  -1.4      2.6      12.0
   4.5      8.5      12.1
    .        .                       .
    .        .                       .
 590.5    594.5      12.2
 596.4    600.4      12.1
----------------------------------------------------------------------
The limiting magnitudes were estimated in comparison with stars in
Tycho-2 Catalog to be distributed between 12.0 and 12.2 as above
partly listed.

Figures of limiting optical magnitudes vs time comparing with other
measurements and can be found at: http://www.icrr.u-tokyo.ac.jp/~ashra/GRB100906A.

This message may be cited.

====================================
SASAKI Makoto
ICRR, University of Tokyo
5-1-5 Kashiwa-no-ha Kashiwa 277-8582
tel/fax +81-4-7136-3143
====================================


GRB_name: GRB100915A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11292
SUBJECT: GRB 100915A: TAROT Calern observatory optical observations
DATE:    10/09/19 07:42:30 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (CESR-OMP), Gendre B. (IASF),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 100915A detected by SWIFT
(trigger 434178) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 97s after the GRB trigger
(20s after the notice). The elevation of the field decreased from
47 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).
Time sampling is 10 seconds / pixel.
We do not detect any OT with a limiting magnitude of:
t0+97s to t0+157s : R > 17.2

We co-added a series of exposures:
t0+174s to t0+394s : R > 19.0

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

This message may be cited.


GRB_name: GRB100917A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11293
SUBJECT: GRB 100917A: TAROT La Silla observatory optical observations
DATE:    10/09/19 08:51:19 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz A. (CESR-OMP), Gendre B. (IASF),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 100917A detected by SWIFT
(trigger 434360) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 261s after the GRB trigger
(15s after the notice). The elevation of the field decreased from
22 degrees above horizon and weather conditions
were fair.

We co-added a series of exposures.
We do not detect any OT in the BAT refined position provided
by Cummings et al. 2010 (GCNC 11289) with a limiting
magnitude of:

t0+261s to t0+531s : R > 14.1

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

N.B. Galactic coordinates are lon= 20.2843 lat=-13.2388
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: GRB100924A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11294
SUBJECT: GRB 100924A: Swift detection of a burst
DATE:    10/09/24 04:16:37 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF-IASFPA), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
E. A. Hoversten (PSU), C. B. Markwardt (NASA/GSFC) and
B. Sbarufatti (INAF-OAB/IASFPA) report on behalf of the Swift Team:

At 03:58:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100924A (trigger=434843).  Swift did not slew to the burst. 
The BAT on-board calculated location is 
RA, Dec 0.671, +7.015 which is 
   RA(J2000) = 00h 02m 41s
   Dec(J2000) = +07d 00' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 90 sec.  The peak count rate
was ~5457 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an Moon observing constraint, Swift cannot slew to the BAT
position until 13:21 UT on 2010 September 25. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB100924A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11295
SUBJECT: GRB 100924A: Swift-BAT refined analysis
DATE:    10/09/25 03:03:08 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
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 100924A (trigger #434843)
(Mangano, et al., GCN Circ. 11294).  The BAT ground-calculated position is
RA, Dec = 0.672, 7.004 deg which is 
   RA(J2000)  =  00h 02m 41.3s 
   Dec(J2000) = +07d 00' 15.0" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 25%.
 
The mask-weighted light curve shows an initial cluster of two peaks starting
at ~T-4 sec, peaking at ~T_zero, and returning to essentially background at ~T+20 sec.
The second cluster has approximately 8 peakis starting at ~T+20 sec, with
main peaks at ~T+35, +45, +52, +60, amd +68, and returning to background
around T+120 sec.  T90 (15-350 keV) is 96.0 +- 16.0 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-15.1 to T+128.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.53 +- 0.06.  The fluence in the 15-150 keV band is 8.3 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+56.40 sec in the 15-150 keV band
is 1.5 +- 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/434843/BA/


GRB_name: GRB100925A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11296
SUBJECT: GRB 100925A: Swift detection of a burst
DATE:    10/09/25 08:45:18 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF-IASFPA), E. A. Hoversten (PSU),
C. B. Markwardt (NASA/GSFC), B. Sbarufatti (INAF-OAB/IASFPA),
R. L. C. Starling (U Leicester) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:

At 08:05:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100925A (trigger=434928).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 254.736, -15.236 which is 
   RA(J2000) = 16h 58m 57s
   Dec(J2000) = -15d 14' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This is an image trigger with on-board significance
of 8.1 sigma.  As is typical for image triggers, there is no obvious structure
in the raw light curve. 

The XRT began observing the field at 08:36:18.0 UT, 1872.2 seconds
after the BAT trigger. XRT found a bright, uncatalogued X-ray source
located at RA, Dec 254.7603, -15.2576 which is equivalent to:
   RA(J2000)  = 16h 59m 02.47s
   Dec(J2000) = -15d 15' 27.3"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 115 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 1882 seconds after the BAT trigger. No credible afterglow candidate
has been found in the initial data products. Data from the 2.7'x2.7' sub-image
are not available at this time. 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 0.61. 




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


GRB_name: GRB100924A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11297
SUBJECT: GRB 100924A: GROND detection of an optical/NIR afterglow
DATE:    10/09/25 09:50:24 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady, T. Kruehler, and J. Greiner (all MPE Garching) report on
behalf of the GROND team:

We observed the field of GRB 100924A (Mangano et al., GCN 11294)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile).

Observations started at 04:32 UT on September 24, 0.57 hours after the
GRB and were performed under very challenging observing conditions, in
particular a full moon at close distance. A second epoch of imaging was
performed starting at 00:36 UT on September 25.

In the first epoch we detect a bright point source in all channels at:

RA = 00:02:42.26
Dec = 07:00:02.8

inside the refined BAT error circle (Barthelmy et al., GCN 11295) and
with a preliminary magnitude of r' = 17.19. Both, photometry and
astrometry have been tied to the SDSS catalog. The object faded below r'
 > 20 in the second epoch and is not present in the much deeper archival
SDSS frames. We hence conclude that this is the optical/NIR afterglow of
GRB 100924A.


GRB_name: GRB100925A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11298
SUBJECT: GRB100925A UVOT afterglow
DATE:    10/09/25 12:23:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

F. E. Marshall (NASA/GSFC) reports on behalf of the Swift team:

In response to GRB100925 (Swift/BAT trigger 434928), UVOT took a finding chart 
exposure of 150 seconds with the White filter starting 1882 seconds after the 
BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' 
sub-image at
RA(J2000) =   16:59:01.68 = 254.75702
DEC(J2000) = -15:15:28.4 = -15.25789
with a 90%-confidence error radius of about 0.61 arc sec.
This position is 11" from the center of the XRT error circle (Mangano et al. GCN 
Circ. 11296). The estimated magnitude is 16.83 with a 1-sigma error of about 
0.14. No correction has been made for the expected extinction corresponding to 
E(B-V) of 0.61.


GRB_name: GRB100925A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11299
SUBJECT: GRB 100925A: Nearby DSS Source - SN-GRB or new Galactic transient?
DATE:    10/09/25 13:55:24 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (TLS Tautenburg) speculates:

GRB 100925A (Mangano et al., GCN 11296) is a very peculiar event. It was
an extremely long image trigger (1592 seconds), yet, after slewing to it,
Swift discovered that the X-ray afterglow is still bright. Furthermore,
looking at the Swift XRT repository page (Evans et al. 2007, 2009)
(http://www.swift.ac.uk/xrt_curves/00434928/) the source remains
constantly bright over almost 9000 seconds (two orbits).

Inspection of the DSS images of this field, using the position of the
bright UVOT transient (Marshall, GCN 11298), shows that there is what
seems to be an extended source a few arcseconds to the west (R.A.:
16:59:01.501; Dec.: -15:15:28.76 according to the native DSS WCS system).
It is clearly detected in the red frame, and more marginally in the IR
frame (DSS blue or SDSS are not available for this field). There are also
some stars nearby, but at much larger separation (> 10 arcsec). There is
no source directly beneath the UVOT position.

While the initial properties are reminiscent of two local XRFs associated
with broadlined Type Ic SNe, namely XRF 060218 (Campana et al. 2006) and
XRF 100316D (Starling et al. 2010) (the nearby DSS source being the host
galaxy), the continuing strong X-ray emission as well as the position near
the Galactic bulge (Galactic longitude 5.52, Galactic latitude 16.56) may
also point to a new Galactic source.

Spectroscopic follow-up is encouraged.

This message may be cited.


GRB_name: GRB100925A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11300
SUBJECT: MAXI J1659-152: Swift-BAT refined analysis (triggers 434928 and 434931)
DATE:    10/09/25 18:55:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using only a partial data set from T+247 to T+303, T+706 to T+723 and
T+728 to T+963 sec (T=08:05:06 UT) from recent downlinks, we report further analysis
of MAXI J1659-152 (Swift-BAT trigger #434928) (Negoro, ATEL 2873 and
initially reported as GRB 100925A in Mangano, et al., GCN Circ. 11296).
The BAT ground-calculated position is RA, Dec = 254.750, -15.206 deg, which is 
   RA(J2000)  =  16h 59m 00.0s 
   Dec(J2000) = -15d 12' 20.1" 
with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 38%.
 
No statement can be given about the BAT lightcurve because of the fragmented
coverage of the transient.  This fragmentation is caused by (a) a second
Swift-BAT trigger on the same source (a 64-sec image trigger, #434931,
at 09:47:13 UT) and (b) the very long integration time of the first trigger (26.5 min).
The normal set of event-by-event data used to do this "refined" analysis
is not fully available (the on-board event ring buffer has been nearly
completely wrapped).
 
The time-averaged spectrum in the 3 time intervals listed above
is best fit by a simple power-law model.  The power law index
of the time-averaged spectrum is 1.79 +- 0.43.  We caution even this
limited analysis because of the partial coverage of the time interval
of the event. 

Further, the time-averaged spectrum from T+0.0 to T+64.0 sec (T=09:47:13 UT,
the second trigger) is best fit by a simple power-law model.  The power law
index of the time-averaged spectrum is 2.36 +- 0.61.  All the quoted errors
are at the 90% confidence level.

The GCN Notices for the first trigger were distributed with a GRB label,
because the location did not match any known source in the on-board and
ground catalogs.  However, the GCN Notices for the second trigger were
labeled as a transient because the location matched the location of the
first trigger (AT trigger locations are maintained in the on-board catalog
up to the 4th trigger in a 3-deep ring buffer).


GRB_name: GRB100925A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11301
SUBJECT: GRB 100925A / MAXI J1659-152: BOOTES-2/TELMA and IAC80 optical observations
DATE:    10/09/25 22:09:39 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

M. Jelnek (IAA-CSIC Granada), C. Zurita, M. Viss (IAC Tenerife),
P. Papics (Katholieke Universiteit Leuven), P. Kubnek (IPL, Univ.
de Valencia), L. Sabau-Graziati (INTA), A, de Ugarte Postigo (DARK/NBI),
R. Cunniffe, J. Gorosabel and A. J. Castro-Tirado (IAA-CSIC), report on
behalf of a larger collaboration:

"Following the detection of MAXI J1659-152 (Negoro et al. ATEL
2873) by Swift (GRB 100925A, Magano et al. GCNC 11296), we
have obtained further observations at the position of the
optical counterpart reported by Marshall et al. (GCNC 11298)
with the 0.6m TELMA robotic telescope at the BOOTES-2 station
in Mlaga and the 0.8m IAC telescope at Observatorio del Teide
in Tenerife (Spain). TELMA observations started on 25 Sep 20.1
UT in the R-band filter. IAC80 observations were carried out
in BVRI with dense monitoring in the R-band.  For a combined
image (120 x 20s) Preliminary analysis yields R = 16.6 +/- 0.1
(based on USNO B-1.0 magnitude for a 15.5 star 1 arcmin north
of the target), thus supporting a Galactic transient (Kann, GCNC 11299),
either a hard outburst of a new compact binary, or a magnetar candidate
similarly to GRB 070610/SWIFT J195509+261406 (Castro-Tirado et
al. 2008, Nat 405, 556; Stefanescu et al. 2008, Nat 405, 503).
Spectroscopic observations are most essential to discern its
nature."

This message can be quoted.

[GCN OPS NOTE(26sep10): Per author's request, the Kann citation
was added and 071006 was changed to 070610.]


GRB_name: GRB100925A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11303
SUBJECT: GRB100925A/MAXI J1659-152: Galactic origin from SED analysis
DATE:    10/09/26 00:44:23 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

Dong Xu (Weizmann Institute) reported on a larger collaboration:

GRB100925A happened in the error circle of MAXI J1659-152 (Negoro et
al., ATel 2873; Magano et al., GCN 11296). Spectroscopy or a broadband
SED is critical to pin down its origin. The Swift UVOT and XRT data
were analyzed, covering 2000-1x10^4 s since the BAT trigger.
Generally, UVOT light curves are rather flat as the X-ray does.

The flux densities in the six UVOT filters without Galactic extinction
correction are rather low compared with the X-ray flux density. The
UVW2 flux density is almost comparable to that of the X-ray.  Assuming
the source being extragalactic and correction of E(B-V)~0.61 (Magano
et al., GCN 11296) applied, then UVOT flux densities are too high
compared with the downward extrapolation of the X-ray, if interpreted
with synchrotron radiation mechanism. Additionally, the UVOT spectral
index has \beta~2 (F_\nu \propto \nu^\beta) in this case, which is
unusual for GRB afterglows. To make UVOT-XRT SED explained by one
single mechanism, a moderate extinction is required. We found
E(B-V)~0.35 would naturally give rise to a good SED modeling: the
synchrotron radiation lies in the slow cooling phase with the minimum
frequency ~3x10^15 Hz, above which X-ray has \beta_X~-(p-1)/2~0.7
(i.e., p~2.4) and below which UVOT has \beta_opt~1/3. Therefore, we
suggest this source is of Galactic origin.

If the above synchrotron mechanism governs the broadband SED from
radio to X-ray, then MAXI J1659-152 is likely not detectable at radio,
especially when the synchrotron-self absorption frequency is above the
radio band. Therefore, radio follow-up is encouraged.

[GCN OPS NOTE(28sep10): Per auther's request, "100525A" was changed
to "100925A" in both the Subject line and text.]


GRB_name: GRB100925A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11305
SUBJECT: GRB 100925A / MAXI J1659-152: SARA-S Observations
DATE:    10/09/26 04:03:03 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike and Dieter H. Hartmann (Clemson University) report:

We observed the field of GRB 100925A / MAXI J1659-152 (Mangano et
al., GCN 11296) using the SARA-South 0.6m telescope located at CTIO
beginning 15 hours after the trigger and continuing for 3 hours in the
BVRI Bessel filters under good conditions.  We clearly detect the
source (Marshall, GCN 11298) in each image.

Filter    Exp Time   Magnitude
---------------------------------
B         120s       16.8 +/- 0.1
V         120s       16.3 +/- 0.1
R         120s       16.3 +/- 0.1
I         120s       16.1 +/- 0.1

Magnitudes are given relative to field stars in the USNO B1.0 and
NOMAD catalogs.  This message may be cited.


GRB_name: GRB100925A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11306
SUBJECT: GRB100925A/MAXI J1659-152  MITSuME Ishigakijima and Okayama Optical Observation
DATE:    10/09/26 08:20:38 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama (IAO, NAOJ), K. Yanagisawa, Y. Shimizu,
H. Toda (OAO, NAOJ), S. Nagayama, T. Miyaji, J. Watanabe (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 100925A / MAXI J1659-152 (Mangano et al.,
GCN 11296; Barthelmy et al., GCN 11300) with the optical three color
(g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of
Okayama Astrophysical Observatory and the Murikabushi 1m telescope of
Ishigakijima Astronomical Observatory.

We detected the previously reported source at the UVOT position
(Marshall, GCN 11298) in all the three bands.

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

Okayama Astrophysical Observatory:
The observation started on 2010-09-25 09:58:43 UT (~ 1.9 h after the
trigger).
#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.08949    10:13:57    1560.0   17.13  0.06  16.46  0.03  16.45  0.16
0.11081    10:44:39    1500.0   17.08  0.08  16.61  0.04  16.32  0.19
0.13201    11:15:11    1560.0   17.15  0.09  16.46  0.05  15.98  0.15

Ishigakijima Astronomical Observatory:
The observation started on 2010-09-25 10:53:50 UT (~ 2.8 h after the
trigger).
#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.12082    10:59:03     480.0   16.97  0.04  16.48  0.02  16.24  0.03
0.12818    11:09:40     540.0   17.05  0.03  16.52  0.02  16.32  0.03
0.13556    11:20:17     540.0   17.02  0.04  16.52  0.02  16.30  0.02
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB100925A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11308
SUBJECT: GRB 100925A / MAXI J1659-152: Optical observation with the Kottamia 188cm telescope
DATE:    10/09/26 19:37:50 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

M. Yoshida, K. S. Kawabata (HASC, Hiroshima U.), Gamal B. Ali,
A. Haroon, A. Essam, I. Zead, A. Nakhlawy, and M. Ismail (NRIAG,
Egypt) report:

We observed GRB 100925A / MAXI J1659-152 (Mangano et al., GCN
11296;Barthelmy et al., GCN 11300; Marshall et al. GCN 11298;
Negoro et al.ATEL 2873) with the Newtonian CCD camera attached to
the 188 cm telescope of Kottamia Astronomical Observatory in Egypt
on September 26 2010. We measured the brightness of this possible
X-ray binary (Ugarte Postigo et al. GCN 11307) in B, V, R and I
bands. Results of the photometry are listed below. We used a
nearby USNO B1.0 star (USNO 0747-0361593) for photometric
calibration.

band        START-UT        T-EXP[sec]   mag.(Vega)  error(*)
-------------------------------------------------------------
B     2010-09-26 18:11:24   300.0        16.64       0.08
V($)  2010-09-26 18:17:05   180.0        16.33       0.06
R     2010-09-26 17:59:24   120.0        16.11       0.05
I     2010-09-26 18:01:59   120.0        15.87       0.04
-------------------------------------------------------------

(*) Poisson noise error only.
($) We interpolated the B2 and the R2 magnitudes of the
comparison star to estimate the V band magnitude of the star.


GRB_name: GRB100925A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11309
SUBJECT: GRB 100925A / MAXI J1659-152: WSRT Radio and Polarization Detection
DATE:    10/09/27 01:15:56 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

  A.J. van der Horst (NASA/MSFC/ORAU), J. Granot (U of Hertfordshire),
Z. Paragi (JIVE), C. Kouveliotou (NASA/MSFC), R.A.M.J. Wijers (U of
Amsterdam) and E. Ramirez-Ruiz (UC Santa Cruz) report:

"We observed the position of the hard X-ray transient GRB 100925A /
MAXI J1659-152 (GCN 11296, ATel #2873, GCN 11307) with the Westerbork
Synthesis Radio Telescope at 4.8 GHz, at September 26 14.27 to 19.75 UT,
i.e. 1.37 days after the Swift/BAT trigger (GCN 11296) and 1.60 days
after the start of the source brightening in MAXI/GSC (ATel #2873).
We detect a radio source at the Swift/UVOT position of the transient
(GCN 11298), with a flux density of 4.92 +/- 0.04 mJy. The source is
linearly polarized at a level of 23 +/- 2 %, but there is no circular
polarization detected, with a 3-sigma upper limit of 2 %.

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


GRB_name: GRB100928A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11310
SUBJECT: GRB 100928A: Swift detection of a burst
DATE:    10/09/28 02:34:10 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (NASA/GSFC), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), G. Stratta (ASDC) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 02:19:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100928A (trigger=435160).  
The BAT on-board calculated location is RA, Dec 223.036, -28.561 which is 
   RA(J2000) = 14h 52m 09s
   Dec(J2000) = -28d 33' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 6 sec.  The peak count rate
was ~700 counts/sec (15-350 keV), at ~1 sec after the trigger.  There 
may be additional emission at T+180 sec. 

Due to an Sun observing constraint, Swift cannot slew to the BAT
position until 20:05 UT on 2010 December 26. There will thus be no XRT
or UVOT data for this trigger. 

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: GRB100924A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11311
SUBJECT: GRB 100924A: Fermi GBM observation
DATE:    10/09/28 07:11:07 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team: 

"At 03:58:08.32 UT on 24 September 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100924A (trigger 306993490 / 100924165).
which was also detected by the Swift-BAT (Mangano et al. 2010, GCN 11294).
The GBM on-ground location is consistent with the Swift position.
 
The angle from the Fermi LAT boresight is 57 degrees.

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

The GBM light curve shows a bright initial peak
with a duration (T90) of about 9.0 +/- 0.4 s (50-300 keV). 
Fermi entered the SAA ~ 35 s after the trigger.
Thus, the observation of additional emission episodes,
as reported in Mangano et al. 2010, GCN 11294, was not possible.

The time-averaged spectrum from T0+0.003 s to T0+9.088 s is 
best fit by a simple power law function with index -1.59 +0.02/-0.02
(Castor C-STAT 1767 for 725 d.o.f.).

The event fluence (10-1000 keV) in this time interval is 
(3.33 +/- 0.04)E-06 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+0.384 s in the 10-1000 keV band 
is 7.3 +/- 0.2 ph/s/cm^2.


GRB_name: GRB100928A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11312
SUBJECT: GRB 100928A, Swift-BAT refined analysis
DATE:    10/09/28 12:40:44 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), V. D'Elia (ASDC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC),G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 100928A (trigger #435160)
(D'Elia, et al., GCN Circ. 11310).  The BAT ground-calculated position is
RA, Dec = 223.037, -28.542 deg which is
    RA(J2000)  =  14h 52m 09.0s
    Dec(J2000) = -28d 32' 32.5"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 15%.

The mask-weighted light curve showed a single peak starting at T-1 with a total
duration of ~6 seconds. T90 (15-350 keV) is 3.3 +- 0.6 sec (estimated error 
including systematics).

The time-averaged spectrum from T+0.9 to T+4.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.79 +- 0.29.  The fluence in the 15-150 keV band is 3.5 +- 0.6 x 10-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.31 sec in the 15-150 keV band
is 2.5 +- 0.5 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/435160/BA/


GRB_name: GRB100924A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11313
SUBJECT: GRB 100924A: Suzaku WAM observation of the prompt emission
DATE:    10/09/28 12:51:41 GMT
FROM:    Satoshi Sugita at Aoyama Gakuin U.  <sugita@phys.aoyama.ac.jp>

S. Sugita (Nagoya U.), T. Uehara, Y. Hanabata,
T. Takahashi, Y. Fukazawa (Hiroshima U.),
N. Vasquez (Tokyo Tech.) K. Yamaoka (Aoyama Gakuin U.),
Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo),
S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report:


The multi-spiked long GRB 100924A (Swift/BAT trigger #434843, GCN
11294; Mangano et al.,)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 03:58:09.027 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0-1s,
ending at T0+65s with a duration (T90) of about 60 seconds.
The fluence in 100 - 1000 keV was 5.90 (+0.86/-0.84) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0s was 1.44 (+-0.23) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1s to
T0+65s is well fitted by a single power-law with a photon index
of 2.55 (+0.38/-0.29) (chi^2/d.o.f = 25.1/15).
All the quoted errors are at statistical 90% confidence level.

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


GRB_name: GRB100925A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11314
SUBJECT: GRB 100925A / MAXI J1659-152: MASTER optical observations
DATE:    10/09/29 16:00:26 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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


We observed GRB 100925A / MAXI J1659-152 (Mangano et al., GCN
11296; Barthelmy et al., GCN 11300; Marshall et al. GCN 11298;
Negoro et al.ATEL 2873) in automatic regime after sunset
  at Tunka and Kislovodsk (MASTER-Net: http://observ.pereplet.ru, Lipunov 
et al., 2010,  Advances in Astronomy, vol. 2010, pp. 1-7).
The elevation of the source was about 15 degrees at Tunka and about  22 
degrees at Kislovodsk.

The results of the R photometry  are:

   Date                JD            T-T_trigger [day] R[mag]  [+-]   Site

2010-09-25 12:09:27  2455465.00657     0.098          16.08   0.25   Tunka
2010-09-26 02:54:12  2455465.62098     0.274          16.14   0.20   Tunka
2010-09-26 16:25:36  2455466.18445     1.276          16.20   0.10   Kislo


This  photometry calibrated by   USNOB1  stars.


The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB100728B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11317
SUBJECT: GRB 100728B: X-shooter redshift
DATE:    10/10/07 12:41:13 GMT
FROM:    Hector Flores at Obs.de Paris,Meudon  <hector.flores@obspm.fr>

H. Flores (GEPI/Obs. de Paris), J. P. U. Fynbo, A. de Ugarte
Postigo, B. Milvang-Jensen, D. Malesani (DARK/NBI), P. Goldoni
(APC/Univ. Paris 7 and SAp/CEA), C. C.  Thoene (IAA-CSIC Granada), S.
Piranomonte (INAF/Roma), S. D. Vergani (GEPI/Obs. de Paris),
F. Onori (Univ. Roma 3)
report on behalf of the X-Shooter GRB collaboration:

We have observed the afterglow of the GRB 100728B (Morris et al., GCN
11009; Perley et al., GCN 11010) with the ESO VLT equipped with the
X-shooter spectrograph. The observation started on  2010-07-29 at 08:15
UT (22 hr after the GRB). A total exposure of 4x600 s was obtained,
covering the spectral range from 300 to 2500 nm. Due to technical
problems with the atmospheric dispersion corrector, the sensitivity of
the instrument was below the nominal value during this observation so
the signal-to-noise ratio of the spectrum is very low.

In the spectra we detect a broad absorption line consistent with a
damped Lyman-alpha line and absorption features consistent with the MgII
doublet at a common redshift of z=2.106. Given the low S/N of the
spectrum, this redshift measurement should be considered tentative.

We acknowledge the Paranal staff, in particular Alain Smette, for
valuable support with the observations, and Daniel Perley (Berkeley) for
providing us a finding chart with the afterglow.

[GCN OPS NOTE(07oct10): Per author's request, Onori was added to the
author list.]


GRB_name: GRB101008A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11318
SUBJECT: GRB 101008A: Swift detection of a burst
DATE:    10/10/08 16:52:27 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), S. Immler (CRESST/GSFC/UMD),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), C. Pagani (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
A. Rowlinson (U Leicester), B. Sbarufatti (INAF-OAB/IASFPA),
M. H. Siegel (PSU), M. C. Stroh (PSU) and E. Troja (NASA/GSFC/ORAU)
report on behalf of the Swift Team:

At 16:43:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101008A (trigger=435903).  Swift could not slew to the
burst location due to an Earth limb constraint. 
The BAT on-board calculated location is 
RA, Dec 328.891, +37.062 which is 
   RA(J2000) = 21h 55m 34s
   Dec(J2000) = +37d 03' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows many peaks
in an overall FRED envelope structure with a duration of about 15 sec. 
The peak count rate was ~2500 counts/sec (15-350 keV), at ~1 sec 
after the trigger. 

Due to an observing constraint, Swift will not slew until 
T0+50.8 minutes. There will be no XRT or UVOT data until
this time. 

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


GRB_name: GRB101008A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11319
SUBJECT: GRB 101008A: Swift/XRT Detection of an Afterglow with no UVOT Counterpart
DATE:    10/10/08 18:34:31 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

W. H. Baumgartner (GSFC/UMBC),
P. A. Evans (U Leicester),
S. T. Holland (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL),
C. Pagani (U Leicester),
K. L. Page (U Leicester), and
M. H. Siegel (PSU)
report on the behalf of the Swift UVOT team:

    The XRT began observing the field of GRB 101008A (Baumgartner et al. 2010,
GCNC 11318) at 17:35:56.9 UT, 3161.7 seconds after the BAT trigger.  Using promptly
downlinked data we find an uncatalogued X-ray source located at RA, Dec 328.87463,
37.06580 which is equivalent to:

    RA(J2000) =  21h 55m 29.91s
   Dec(J2000) = +37d 03' 56.9"

with an uncertainty of 3.9 arcseconds (radius, 90% containment).  This
location is 48 arcseconds from the BAT onboard position, within the BAT
error circle.  This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time.

    A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.44 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 3
(+4.38/-2.94) x 10^21 cm^-2 (90% confidence).

    UVOT took a finding chart exposure of 150 seconds with the white filter
starting 3167 seconds after the BAT trigger.  No credible afterglow candidate
has been found in the initial data products.  The 2.7' x 2.7' sub-image covers
100% of the XRT error circle.  The preliminary 3-sigma upper limit in the white
filter is 20.3 mag.  No correction has been made for the expected Galactic
extinction corresponding to a reddening of E_{B-V} =  0.19 mag.  Photometry is
on the UVOT photometry system of Poole et al. (2008).


GRB_name: GRB101008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11320
SUBJECT: GRB 101008A: 1.23m CAHA optical observations
DATE:    10/10/08 20:59:00 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC,  Granada),  U. Carsenty  (DLR,  Berlin), P.  
Kubanek  (IAA-CSIC, Granada  &  U. of Valencia), G. Hahn  (DLR,  
Berlin), report on behalf of a larger collaboration:

"We have carried out R-band observations of the Swift GRB 101008A  
(Baumgartner et al., GCNC 11318, GCNC 11319) with the 1.23m Calar Alto  
telescope. The observations were carried out in R-band on October  
8.7957-8.8118 UT (2.38 -  2.76 hours post  trigger) under poor  
atmospheric conditions. We do not detect any optical source consistent  
with the XRT error circle (Baumgartner et al., GCNC 11319) down to a  
limiting magnitude of R=19.7 (3 sigma, calibrated against USNO-B1.0)".


GRB_name: GRB101008A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11321
SUBJECT: GRB 101008A: Enhanced Swift-XRT position
DATE:    10/10/08 21:32:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1745 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 101008A, 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 = 328.87505, +37.06713 which is equivalent
to:

RA (J2000): 21h 55m 30.01s
Dec (J2000): +37d 04' 01.7"

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

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

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


GRB_name: GRB101008A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11322
SUBJECT: Subject: GRB 101008: Swift/UVOT Upper Limits
DATE:    10/10/08 23:55:17 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P.M. Kuin (MSSL/UCL) and W. H. Baumgartner (GSFC/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 101008
3167 s after the BAT trigger (Baumgartner et al., GCN Circ. 11318).
No optical afterglow consistent with the XRT position (Beardmore
et al., GCN Circ 11321) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

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

white_FC          3167         3316          147         >20.6
white             3167         5372          541         >21.3
v                 4147         5752          363         >19.6
b                 3531         5167          393         >20.6
u                 3326         4962          393         >20.1
w1                4557         4757          197         >20.1
m2                4352         4552          197         >20.3
w2                3943         5577          393         >20.6

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.19 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB100915A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11323
SUBJECT: GRB 100915 optical upper limit
DATE:    10/10/09 01:08:30 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We observed the field of the Swift GRB 100915A (Littlejohns et al.,
GCN 11277) with AZT-33IK telescope of Sayan observatory (Mondy) on
Sep. 15 between (UT) 14:02 - 16:54 under variable weather conditions
and mean seeing of about ~1.9". In the two stacked images of two
epochs we do not detect any source in enhanced XRT error circle
(Osborne et al. GCN 11279). The upper limits (3 sigma) of the two
stacked images based on USNO-B1.0 field stars are the following:

t-t0,d   filter  exp.,s uplim
0.53437 R    15*60  23.2
0.60644 R    15*60  23.4


GRB_name: GRB101008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11324
SUBJECT: GRB 101008A: SAO RAS optical observations
DATE:    10/10/09 01:56:35 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. S. Moskvitin, T. A. Fatkhullin, A. V. Zyazeva
report on behalf of a larger collaboration:

We have observed the field of the GRB 101008A (Baumgartner et al.,
GCN#11318, GCN#11319; Beardmore et al., GCN#11321) with the 1m
telescope Zeiss-1000 of SAO RAS, Russia. The observations were carried
out in Rc band on October, 8.763 -- 8.800 UT (1.581 -- 2.484 hours
after the trigger).

We have detected three possible candidates of the OT near the enhanced
XRT error box, which are absent in the DSS R-band image.
A comparison of the DSS and our images is demonstrated at
ftp://ftp.sao.ru/pub/grb/GRB101008A/GRB101008A.jpeg

We have measured the R magnitudes of these three objects according
to R2 = 16.33 of the USNO-B1.0 star 1270-0570798:

S1 R = 20.84 +/- 0.04
S2 R = 21.03 +/- 0.06
S3 R = 21.01 +/- 0.05

All the errors are formal and they do not include the errors of
the USNO-B1.0 to Johnson-Cousins photometric system transformation.

This message may be cited.


GRB_name: GRB101008A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11325
SUBJECT: GRB 101008A: Swift-XRT refined analysis
DATE:    10/10/09 08:36:00 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) and W. H. Baumgartner (GSFC/UMBC) report on
behalf of the Swift-XRT team:

We have analysed 5.5 ks of XRT data for GRB 101008A (Baumgartner et al.
GCN Circ. 11318), from 3169 s to 26.9 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Beardmore et al. (GCN. Circ 11321).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.2 (+0.5, -0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.0 (+/-0.5). The best-fitting
absorption column is 2.8 (+2.0, -1.4) x 10^21 cm^-2, in excess of the
Galactic value of 1.4 x 10^21 cm^-2 (Kalberla et al. 2005). The counts
to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from
this spectrum is 4.5 x 10^-11 (6.8 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of
1.2, 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 5.9 x
10^-14 (8.9 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/00435903.

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


GRB_name: GRB101008A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11326
SUBJECT: GRB101008A, GROND detection of a fading afterglow
DATE:    10/10/09 10:58:06 GMT
FROM:    Marco Nardini at MPE  <nardini@mpe.mpg.de>

M. Nardini, P. Schady, J. Greiner (MPE Garching) report on behalf of the
GROND team:

We observed the field of GRB 101008A (Swift trigger 435903; Baumgartner et
al., GCN#11318) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla
Observatory (Chile).

Observations started at 00:26 UT 2010 October 9th, 7.8h time after the GRB
trigger, and lasted 2 hours. They were performed at an average seeing of
1.2  and at an average airmass of 2.5.

In all our g'r'i'z'JHK images we detect the 3 objects reported by
Moskvitin et al., GCN#11324.

While sources S1 and S3 do not show any clear fading with respect to that
reported by  Moskvitin et al., GCN#11324, our  preliminary  photometry
shows  that S2 has faded with respect to the value reported by Moskvitin
et al. (GCN#11324). Calibrating our images against the same USNO star as
Moskvitin et al., we calculate a fading of ~0.7mag between the GROND
preliminary photometry centred at 8.7h after the trigger and that reported
in Moskvitin et al.

We therefore conclude that this is the optical/NIR afterglow of GRB101008A.

Our photometry is not corrected for foreground extinction of E(B-V)=0.19.
The detection in g' band implies a redshift constraint z<3.5.


GRB_name: GRB101008A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11327
SUBJECT: GRB 101008A: Swift-BAT refined analysis
DATE:    10/10/10 02:30:51 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-248 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 101008A (trigger #435903)
(Baumgartner, et al., GCN Circ. 11318).  The BAT ground-calculated position is
RA, Dec = 328.882, 37.060 deg which is 
   RA(J2000)  =  21h 55m 31.8s 
   Dec(J2000) = +37d 03' 36.4" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 58%.
 
The mask-weighted light curve shows a single FRED-like peak starting ~T-30 sec,
peaking at ~T+0 sec, and returning to background at ~T+100 sec.
T90 (15-350 keV) is 104 +- 35 sec (estimated error including systematics).
 
The time-averaged spectrum from T-4.0 to T+106.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.59 +- 0.24.  The fluence in the 15-150 keV band is 1.1 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.42 sec in the 15-150 keV band
is 1.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/435903/BA/


GRB_name: GRB101008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11328
SUBJECT: GRB 101008A: MASTER prompt optical observations 
DATE:    10/10/10 18:46:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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


E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
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, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk



MASTER-Net robotic telescopes (MASTER-Net: http://observ.pereplet.ru)
located  near Ekaterinburg (Kourovka)  and Tunka (Baykal Lake) was pointed 
to the Swift GRB 101008A (Baumgartner et al., GCN#11318, GCN#11319; 
Beardmore et al., GCN#11321) 53 s after trigger time (immediately after 
roof opening and with last night focus) and 8309s after trigger time (the 
Tunka delay was due to weather conditions).

Time duration of the  GRB 101008A is 104 +- 35 sec (Barthelmy et al., 
GCN#11327). So we have prompt optical limit at Kourovka site.
We see marginaly possible OT (S2,  Moskvitin et al.,GCN#11324; Nardini et 
al., GCN#11326) at Tunka observations.

We have next unfiltered estimation:

t_start-t_trig(s)   mean time     exp_time(s)     m             Coadd? 
Site
--------------------------------------------------------------------------
       53            58    10         >14.5        N             Kourovka
       53           141   410         >16.0        Y             Kourovka
     8309         10260   540       19.5+-1.0      Y             Tunka
--------------------------------------------------------------------------
MASTER II have 2 images per exposition time.
The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101008A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11329
SUBJECT: GRB 101008A: MASTER prompt optical observations (correction to  GCN#11328)
DATE:    10/10/10 18:59:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

I am sorry, the table in GCN#11328
  is :

t_start-t_trig(s)   mean time     exp_time(s)     m      Coadd?    Site
--------------------------------------------------------------------------
       53              58            10          >14.5     N      Kourovka
       53             141           410          >16.0     Y      Kourovka
     8309           10260           540        19.5+-1.0   Y      Tunka
--------------------------------------------------------------------------

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101008A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11330
SUBJECT: GRB 101008A: Fermi GBM observation
DATE:    10/10/11 16:29:13 GMT
FROM:    Lin Lin at UAH/NAOC  <ll0005@uah.edu>

Lin Lin (UAH)
report on behalf of the Fermi GBM Team: 

"At 16:43:15.61 UT on 08 Oct. 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101008A (trigger 308248997 / 101008697).

The burst was also detected by the SWIFT-BAT
(W. H. Baumgartner et al. 2010, GCN 11318)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 79 degrees.

The GBM light curve shows a fast rise - slow decay peak
with a duration (T90) of about 7 s (50-300 keV). 
The time-averaged spectrum from T0-1.536 s to T0+5.376 s is 
best fit by a simple power law function with index -1.42 +/- 0.03
(C-stat 1249.1 for 612 d.o.f.).

The event fluence (10-1000 keV) over the above time interval is 
(2.016 +/- 0.083)E-6 erg/cm^2. The 0.064-sec peak photon flux measured 
starting from T0+1.344 s in the 10-1000 keV band 
is 4.90 +/- 0.84 ph/s/cm^2.

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


GRB_name: GRB101011A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11331
SUBJECT: GRB 101011A: Swift detection of a burst
DATE:    10/10/11 17:11:43 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), M. M. Chester (PSU), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
V. Mangano (INAF-IASFPA), K. L. Page (U Leicester),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC),
A. Rowlinson (U Leicester), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and E. Troja (NASA/GSFC/ORAU) report on
behalf of the Swift Team:

At 16:58:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101011A (trigger=436094).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 48.298, -65.986, which is 
   RA(J2000)  =  03h 13m 12s
   Dec(J2000) = -65d 59' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows about 5 peaks
with a duration of about 50 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 16:59:53.5 UT, 78.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 48.29427,
-65.98212 which is equivalent to:
   RA(J2000)  = 03h 13m 10.62s
   Dec(J2000) = -65d 58' 55.6"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 14 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.27 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.4
(+3.08/-2.53) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 6.35e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 84 seconds after the BAT trigger. No credible
afterglow candidate has  been found in the initial data products. The
2.7'x2.7' sub-image covers 100% of  the XRT error circle. The typical
3-sigma upper limit has been about 19.6 mag.   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 J. K. Cannizzo (cannizzo AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB101011A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11332
SUBJECT: GRB 101011A: Swift-BAT refined analysis
DATE:    10/10/11 20:22:32 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. K. Cannizzo (NASA/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
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+302 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 101011A (trigger #436094)
(Cannizzo, et al., GCN Circ. 11331).  The BAT ground-calculated position is
RA, Dec = 48.274, -65.990 deg, which is 
   RA(J2000)  =  03h 13m 05.7s 
   Dec(J2000) = -65d 59' 23.2" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 87%.
 
The mask-weighted light curve shows an initial FRED-like pulse starting
at ~T-0.3 sec, peaking at ~T+0.6 sec, then followed by several other weaker 
peaks lasting out to ~T+90 sec.  T90 (15-350 keV) is 71.5 +- 18.3 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.4 to T+84.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.24 +- 0.14.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.22 sec in the 15-150 keV band
is 1.3 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/436094/BA/


GRB_name: GRB101011A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11333
SUBJECT: GRB 101011A: Enhanced Swift-XRT position
DATE:    10/10/11 20:46:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1274 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 101011A, 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 = 48.29486, -65.98182 which is equivalent
to:

RA (J2000): 03h 13m 10.77s
Dec (J2000): -65d 58' 54.5"

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: GRB101011A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11334
SUBJECT: GRB 101011A: Swift/UVOT Observations of a Possible Optical Afterglow
DATE:    10/10/11 23:16:27 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

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

      The Swift/UVOT observed the field of GRB 101011A starting 66 s
after the BAT trigger (Cannizzo, et al., 2010, GCN Circ. 11331).
Settled observations started at 85 s.  We detect an optical source
that may be fading and is not present in the USNO-B1.0 catalogue,
2MASS point source catalogue, or the DSS.  The preliminary UVOT
position is:

     RA (J2000) =  03:13:10.47  =  48.29363 (deg)
    Dec (J2000) = -65:58:54.7   = -65.98186 (deg)

with an estimated uncertainty of 1.14 arcsec (radius, 90% confidence,
statistical + systematic).  This is 1.84 arcsec west of the
UVOT-enhanced XRT position (Evans, et al., 2010, GCN Circ. 11333).

     Preliminary white magnitudes and 3-sigma upper limits for
the source are:

Filter      T_start   T_stop    Exp(s)      Mag  Err
-----------------------------------------------------------
white (fc)       85      235       147    21.38 0.34
white           876     1025       147   >21.7
-----------------------------------------------------------

     The quoted magnitudes and upper limits have not been corrected
for the expected Galactic extinction along the line of sight
corresponding to a reddening of E_{B-V} = 0.03 mag (Schlegel, et al.,
1998, ApJS, 500, 525).  All photometry is on the UVOT photometry
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB101011A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11335
SUBJECT: GRB 101011A: XRT Refined Analysis
DATE:    10/10/11 23:26:10 GMT
FROM:    Antonia Rowlinson at U.of Leicester  <bar7@star.le.ac.uk>

A. Rowlinson (U. Leicester) and J. K. Cannizzo (NASA/UMBC) report on
behalf of the Swift-XRT team:

We have analysed 3.9 ks of XRT data for GRB 101011A (Cannizzo et al. GCN
Circ. 11331), from 66 s to 7.2 ks after the BAT trigger. The data
comprise 86 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et al.
(GCN. Circ 11333).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.8 (+0.5, -1.7). At T+116 s the decay
steepens to an alpha of 2.49 (+0.18, -0.19) before breaking again at
T+656 s to a final decay with index alpha=1.13 (+0.28, -0.25).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.41 (+0.20, -0.19). The
best-fitting absorption column is 7.6 (+6.0, -4.3) x 10^20 cm^-2,
consistent with the Galactic value of 3.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.94 (+0.26, -0.30)
and a best-fitting absorption column of 1.5 (+/-0.8) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.2 x 10^-11 (5.7 x 10^-11) erg cm^-2
count^-1.

If the light curve continues to decay with a power-law decay index of
1.13, the count rate at T+24 hours will be 4.2 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-14 (2.4 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/00436094.

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


GRB_name: GRB101011A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11336
SUBJECT: GRB 101011A: Zadko observatory - Gingin optical observations
DATE:    10/10/12 09:07:35 GMT
FROM:    Bruce Gendre at ASDC  <bruce.gendre@asdc.asi.it>

M. Laas-Bourez(UWA/ICRAR), D. Coward(UWA), D. Blair (UWA),
B. Gendre (ASDC/OAR), M. Boer (OHP-CNRS), A. Klotz (CESR-UPS-CNRS),  P.
Thierry (CESR-UPS-CNRS) report:

We imaged the field of GRB 101011A detected by SWIFT
(trigger 436094) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 3932.8s after the GRB trigger
(3910s after the notice). The elevation of the field increased from
55 degrees above horizon and weather conditions
were good with a high level of humidity.

30 images have been maded with a duration of 180.0s each
(see the description in Klotz et al., 2006, A&A 451, L39).
At the position of the XRT afterglow (Evans et al., GCN 11333), we do
not detect any source with a limiting magnitude of g>   19.5
on the single images.

We co-added a series of exposures between t0+3932.8s to t0+9869.4s
We do not detect any afterglow, with a limiting magnitude of  g>   21.5


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

N.B. Galactic coordinates are lon=283.3069 lat=-45.3657

This message may be cited.


GRB_name: GRB101011A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11337
SUBJECT: GRB 101011A, GROND upper limits
DATE:    10/10/12 13:43:38 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

M. Nardini, T. Kruehler (both MPE Garching), S. Klose, A. Rossi (both TLS 
Tautenburg), and J. Greiner (MPE Garching) report on behalf of the GROND 
team:

We observed the field of GRB 101011A (Swift trigger #436094; Cannizzo et 
al. 2010, GCN #11331; Markwardt et al. 2010, GCN #11332) simultaneously in 
g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 
2.2 m MPI/ESO telescope on LaSilla. Observations started at 00:10 UT, 
October 12, i.e. seven hours after the burst once the field became visible 
over La Silla.

In stacked images with a mid-time of 1:06 UT (seeing 2.2 arcsec; mean 
airmass 1.8) we do not detect any source at the position of the faint 
optical transient seen by UVOT (Holland et al. 2010, GCN #11334) down to 
the following limits (3 sigma, AB system):

g' > 24.4,
r' > 23.7,
i' > 22.7,
z' > 22.5,
J  > 22.1,
H  > 21.5.

These upper limits have been calibrated based on USNO and 2MASS stars.


GRB_name: GRB101011A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11338
SUBJECT: GRB 101011A: Swift/UVOT observations
DATE:    10/10/12 14:08:49 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 101011A
85s after the BAT trigger (Cannizzo et al., GCN Circ. 11331).
Summing up white band exposures up to 1374s after the trigger, including
the finding chart, we find a strong indication (2.9 sigma level) of an
uncatalogued source at

 RA = 03h 13m 10.77s, Dec = -65d 58m 54.0s (J2000)
 RA = 48.29487, Dec = -65.98167 (J2000)

with an error of 1.1 arcseconds. This refined position is within 0.5
arcseconds from the XRT refined position (Evans et al., GCN Circ. 11333)
and supersedes the previous onegiven in Holland et al. (GCN Circ. 11334).
In the individual and summed UVOT exposures in other filters, no optical 
afterglow is detected. Preliminary 3-sigma upper limits using the UVOT 
photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first 
finding chart (FC) exposure and subsequent exposures are:

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

white(FC) 85 235147      >21.3
white85  137437321.7  0 0.4
white4311   6627393      >22
v627   187251375      >20.8
b533   419181055      >21.4
u297   417372865      >22.0
uw1 577  476962595      >21.7
um2 652   460172996      >21.7
uw2 603  17812 376      >21.5


The values quoted above 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: GRB100902A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11339
SUBJECT: GRB 100902A: D50 optical limit
DATE:    10/10/13 15:54:24 GMT
FROM:    Jan Strobl at AI AS CR,Ondrejov  <jan@strobl.cz>

Jan Strobl (1,2), Martin Nekola (1), Martin Blazek (1,2), Martin Jelinek
(3), Cyril Polasek (1), Petr Kubanek (3,4), Matus Kocka (1) and
Rene Hudec (1,2)
(1. ASU AVCR Ondrejov, 2. FEL CVUT Praha, 3. IAA Granada, 4. IPL UV
Valencia)

We report on the observation of the field of the Swift GRB 100902A 
(Sakamoto et al., GCN 11181) with the 0.5m telescope D50 in Ondrejov 
(Czech Republic), starting at 22:03:08 UT, i.e. ~2.5h after the trigger.
A sequence of 20s unfiltered images was obtained. We coadded 225x20s 
exposure, obtaining an image with a limitting magnitude Rc~19.1, with an 
effective exposure time 3.68h after the trigger (23:13 UT). We do not 
detect any new source within the XRT error circle (Beardmore et al., GCN 
11188).

This message can be cited.

[GCN OPS NOTE(13oct10):  Per author's request, the affilation footnotes
were fixed.]


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11340
SUBJECT: GRB 100906A: D50 optical detection
DATE:    10/10/13 16:00:35 GMT
FROM:    Jan Strobl at AI AS CR,Ondrejov  <jan@strobl.cz>

Jan Strobl (1,2), Martin Blazek (1,2), Martin Jelinek (3), Cyril Polasek
(1), Petr Kubanek (3,4), Martin Nekola (1), Matus Kocka (1) and
Rene Hudec (1,2)
(1. ASU AVCR Ondrejov, 2. FEL CVUT Praha, 3. IAA Granada, 4. IPL UV 
Valencia)

We report on the observation of the Swift GRB 100906A (Markwardt et al.,
GCN 11227) with the 0.5m telescope D50 in Ondrejov (Czech Republic),
starting at 21:17:37 UT, i.e. ~7.5h after the trigger. Eventually, six
hours of observational data were obtained, with the last image taken at
3:23:20 UT.

We clearly detect the afterglow reported by Ivanov et al. (GCN 11228),
and at the the beginning of our sequence (coadded first 7x 20s, exp.
mean time = 21:19 UT) we measure a magnitude 18.7 +- 0.2.

This message can be cited.


GRB_name: GRB101014A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11341
SUBJECT: GRB 101014A: Fermi GBM detection
DATE:    10/10/14 19:12:34 GMT
FROM:    David Tierney at UCD  <david.tierney@ucd.ie>

Dave Tierney (UCD) and Adam Goldstein (UAH) 
report on behalf of the Fermi GBM Team: 

"At 04:11:52.62 UT on 14 October 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101014A (trigger 308722314 / 101014175 ).

The on-ground calculated location, using the GBM trigger 
data, is RA = 26.94, DEC = -51.07 (J2000 degrees, 
equivalent to 01 h 47 m, -51 d 04 '), with an uncertainty 
of 1.0 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 54 degrees.
This burst resulted in a Fermi spacecraft repointing maneuver.

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

The GBM light curve consists of multiple pulses
with a T90 of about 450 s (50-300 keV). 
The time-averaged spectrum from T0+1.5 s to T0+473.6 s is 
best fit by a Band function with Epeak = 181.40 (+5.66/-5.44) keV, 
alpha = -1.27 (+0.01/-0.01), and beta = -2.07 (+0.02/-0.02)
(C-stat of 2499.1 for 591 d.o.f.).

The event fluence (10-1000 keV) in this time interval is 
(2.072 +/- 0.009)E-04 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+208.77 s in the 8-1000 keV band 
is 58.96 +/- 0.42 ph/s/cm^2.



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


GRB_name: GRB101014A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11342
SUBJECT: Konus-Wind observation of GRB 101014A
DATE:    10/10/15 11:45:11 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 very long bright GRB 101014A (Fermi/GBM
trigger 308722314 / 101014175: Tierney & Goldstein, GCN 11341)
triggered Konus-Wind at T0=15115.250s UT (04:11:55.250)

The burst light curve shows a complex multi-peaked
structure with a total duration of ~480 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/GRB101014_T15115/

As observed by Konus-Wind the burst
had a fluence of (2.5  0.7)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+208.896s,
of (2.6  0.2)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+445.184 s) is best fit
in the 20 keV - 10 MeV range by the GRB (Band) model,
for which:
the low-energy photon index alpha = -1.26 (-0.13, +0.15),
the high energy photon index beta = -2.2 (-1.4, +0.2),
the peak energy Ep = 220(-47, +76)keV (chi2 = 64/84 dof).

The spectrum at the maximum count rate
(measured from T0+208.128 to T0+210.176 s) is best fit
in the 20 keV - 10 MeV range by the GRB (Band) model,
for which:
the low-energy photon index alpha = -1.12 (-0.05, +0.06),
the high energy photon index beta = -2.45 (-0.65, +0.30),
the peak energy Ep = 920(-170, +180)keV (chi2 = 79/69 dof).

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


GRB_name: GRB101011A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11343
SUBJECT: GRB 101011A: BOOTES-3 Upper Limit
DATE:    10/10/16 10:14:45 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C. Tello, M. Jelinek, A.J. Castro-Tirado,  J. Gorosabel (IAA-CSIC,
Granada), A, de Ugarte Postigo (DARK/NBI), W. Allen (Vintage Lane Obs.),
Ph. Yock and Kuan-Yu Lin (Auckland Univ.), report on behalf of a larger
collaboration:

"We have carried out  observations of the  Swift GRB 101011A (Cannizzo et
al. GCNC 11331) on Oct 12.4751 - 12.6972 UT (~23.76 hr after the onset of
the burst, mean observing time) with the 0.6m Yock-Allen robotic telescope
(BOOTES-3) located in Blenheim, New Zealand.


We do not detect any optical source within the Swift-XRT refined error
circle (Evans et al. GCNC 11333).
The 3 sigma limiting magnitude of the co-added unfiltered image
(Texp=165x60s) is R ~ 19.0, using USNO-B1.0 as photometric reference.


GRB_name: GRB101011A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11344
SUBJECT: GRB 101011A: Fermi GBM detection
DATE:    10/10/16 23:51:41 GMT
FROM:    Michael Burgess at UAH  <james.burgess@uah.edu>

Michael Burgess (UAH)
reports on behalf of the Fermi GBM Team:

"At 16:58:36.53 UT on 11 October 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101011A (trigger 308509118 /101011707) which  
was
also detected by the SWIFT-BAT (Cannizzo et al. 2010, GCN 11331)
The GBM on-ground location is consistent with the Swift position.
This burst was also independently detected by INTEGRAL SPI-ACS.
The angle from the Fermi LAT boresight is 144 degrees.

The GBM light curve consists of a several moderately bright
peaks with a duration (T90) of about 35.01 s (8-1000 keV).
The time-averaged spectrum from T0-0.768 s to T0+35.78 s is
best fit by a power law function with an exponential
high energy cutoff.  The power law index is -.49 +/- .25 and
the cutoff energy, parameterized as Epeak, is 296.6 +/- 49.4 keV

The event fluence (8-1000 keV) in this time interval is
(5.24 +/- .39)E-6 erg/cm^2. The .256-sec peak photon flux measured
starting from T0+25.15 s in the 8-1000 keV band
is 5.16 +/- 1.6 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
________________________________
J. Michael Burgess
University of Alabama - Huntsville
National Space Science and Technology Center
james.m.burgess@nasa.gov
256.792.8423
ICQ: 573311449

________________________________
J. Michael Burgess
jmichaelburgess@gmail.com
256.792.8423


GRB_name: GRB101017A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11345
SUBJECT: GRB 101017A: Swift detection of a burst with optical counterpart
DATE:    10/10/17 10:45:42 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), J. M. Gelbord (PSU), D. Grupe (PSU),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
C. B. Markwardt (NASA/GSFC), P. T. O'Brien (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 10:32:47 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101017A (trigger=436429).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 291.378, -35.141 which is 
   RA(J2000) = 19h 25m 31s
   Dec(J2000) = -35d 08' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a complex series
of peaks in a FRED envelope about 40 seconds long, with possible
further emission out to T+100 seconds.  The peak count rate
was ~12000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 10:34:08.4 UT, 81.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 291.38546,
-35.14513 which is equivalent to:
   RA(J2000)  = 19h 25m 32.51s
   Dec(J2000) = -35d 08' 42.5"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 26 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 (7.69 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.8
(+3.15/-2.65) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 8.79e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 88 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 19:25:32.56 = 291.38565
  DEC(J2000) = -35:08:41.4  = -35.14482
with a 90%-confidence error radius of about 0.72 arc sec. This position is 2.7
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.98 with a 1-sigma error of about  0.19. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.17. 

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


GRB_name: GRB101017A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11346
SUBJECT: GRB 101017A: ROTSE-III Optical Limits
DATE:    10/10/17 11:41:31 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey (U Mich), report on behalf of the ROTSE collaboration:

ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded to
GRB 101017A (Swift trigger 436429; M. H. Siegel et al. GCN 11345),
producing images soon after the GCN notice time. We took 10 5-sec, 10
20-sec and 20 60-sec exposures. These unfiltered images are calibrated
relative to USNO A2.0 (R).

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle or at the UVOT position, for both single
images and coadding into sets of 10. Individual images have limiting
magnitudes ranging from 15.6-16.4; we set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
10:34:55.2   10:35:15.2        20     16.4          127.8       N
10:37:49.3   10:42:31.6       282     17.5          301.9       Y


GRB_name: GRB101017A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11347
SUBJECT: GRB 101017A: Swift-BAT refined analysis
DATE:    10/10/17 16:32:05 GMT
FROM:    Craig Markwardt at NASA/GSFC/UMD  <craigm@milkyway.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
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-60 to T+240 sec from the recent telemetry 
downlink, we report further analysis of BAT GRB 101017A (trigger 
#436429) (Siegel, et al., GCN Circ. 11345).  The BAT ground-calculated 
position is RA, Dec = 291.377, -35.141 deg which is
    RA(J2000)  =  19h 25m 30.5s
    Dec(J2000) = -35d 08' 25.9"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). 
The partial coding was 43%.

The mask-weighted light curve resembles an overall FRED-like profile, 
starting at T-5 sec, peaking at T+2 sec, but with multiple shorter 
spikes superimposed.  An extended tail is detectable out to at least 
T+160 sec.  T90 (15-350 keV) is 70.0 +- 3.0 sec (estimated error 
including systematics).

The time-averaged spectrum from T-5.5 to T+111 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 1.45 +- 0.03.  The fluence in the 15-150 keV band is 1.8 +- 
0.1 x 10^-5 erg/cm2.  The 1-sec peak photon flux measured from T+2.58 
sec in the 15-150 keV band is 9.4 +- 0.4 ph/cm2/sec.  All the quoted 
errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/436429/BA/


GRB_name: GRB101017A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11348
SUBJECT: GRB 101017A: Enhanced Swift-XRT position
DATE:    10/10/17 17:59:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1922 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 101017A, 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 = 291.38586, -35.14514 which is equivalent
to:

RA (J2000): 19h 25m 32.61s
Dec (J2000): -35d 08' 42.5"

with an uncertainty of 2.6 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: GRB101014A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11349
SUBJECT: GRB 101014A: Fermi LAT detection
DATE:    10/10/17 20:11:44 GMT
FROM:    James Chiang at SLAC  <jchiang@slac.stanford.edu>

Yasuyuki Tanaka, Masanori Ohno (ISAS/JAXA), Johan Bregeon (INFN,
Pisa), Elena Moretti (KTH), Giacomo Vianello (CIFS, SLAC) and
Nicola Omodei (Stanford) report on behalf of the Fermi LAT collaboration.

The Fermi Large Area Telescope (LAT) detected emission from GRB
101014A, which was also detected by GBM at 04:11:52.62 UT, 14 October
2010 (GBM trigger 308722314, GCN 11341).

This burst was initially at an angle of ~54 degrees to the LAT
boresight and triggered an autonomous repoint of the spacecraft.
Because of the burst's proximity to the orbital pole, there was
substantial contamination in the surrounding region owing to gamma-ray
emission from the Earth's limb. A significant excess above background
was not seen using standard analysis procedures.

Using a non-standard data selection that increases the low energy
acceptance at the cost of a greater background (~13 Hz), the LAT
light curve consists of a single, narrow pulse with ~3 s width,
containing over 200 counts above background. This pulse was detected
approximately 210 s after the GBM trigger time. A spectral fit of the
LAT data in the 3 s pulse window yields a photon index of -2.6 +/-
0.1 (stat) and a flux of 0.020 +/- 0.014 ph/s-cm^2 in the 10-100 MeV
band. These data have insufficient spatial resolution to provide a
reliable LAT localization.

Further analysis is ongoing.

The Fermi LAT point of contact for this burst is Yasuyuki Tanaka
(tanaka@astro.isas.jaxa.jp).

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: GRB101017A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11350
SUBJECT: Konus-Wind observation of GRB 101017A
DATE:    10/10/18 07:50:50 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 101017A, (Swift/BAT trigger=436429:
Siegel et.al, GCN 11345; Palmer et.al, GCN 11347)
triggered Konus-Wind at T0=37961.692s UT (10:32:41.692)

The burst light curve shows a jagged FRED-like
structure with a total duration of ~45 s.
The emission is seen up to 2 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101017_T37961/

As observed by Konus-Wind the burst
had a fluence of (6.7  0.4)x10-5 erg/cm2,
and a 256-ms peak flux measured from T0+5.632s
of (7.0  0.9)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+40.448 s) is best fit
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = -1.18  0.06,
and Ep = 600(-45, +52) keV (chi2 = 66/58 dof).

The spectrum at the maximum count rate
(measured from T0+0.256 to T0+7.680 s) is best fit
in the 20 keV - 2 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.9  0.1,
and Ep = 742(-90, +113) keV (chi2 = 62/58 dof).

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


GRB_name: GRB101017A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11351
SUBJECT: GRB101017A: MITSuME Okayama optical upper limits
DATE:    10/10/18 09:27:41 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 101017A (Siegel et al., GCN 11345)
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 2010-10-17 10:33:28 UT (~41 sec after
the burst). We did not find any new point source within the
enhanced XRT error circle (Goad et al., GCNC 11348) 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
------------------------------------------------------
0.01517    10:54:37  1800.0     >17.6  >17.9  >17.6
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB101008A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11352
SUBJECT: GRB 101008A: optical observations
DATE:    10/10/18 10:06:08 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We observed  the field  of the Swift GRB 101008A (Baumgartner et al., GCN
11318) with ZTE telescope of SAI MSU observatory on Oct. 12 (UT) 18:57 -
20:42. We clearly detect objects S1 and S3 (Moskvitin  et al., GCN 11324) in
coordinates (J2000) RA=21 55 29.91, Dec=+37 03 56.6 and RA=21 55 29.85,
Dec=+37 04 05.0, correspondingly. We do not detect the object  S2
(Moskvitin  et al., GCN 11324; Nardini et al., GCN 11326). The photometry is
based on the same USNO star as Moskvitin et al.

Source,  T0+,     Filter,   Exposure,    mag.,        Upper Limit (3 sigma)
             (mid, d)              (s)

S1        4.1297    R       97x60           21.0 +/- 0.1      22.4
S2        4.1297    R       97x60           21.6 +/- 0.2      22.4

Since we do not detect the afterglow candidate S2 up to R=22.4 we can
confirm the GRB 101008A afterglow detection.
The finding chart can be found at
http://grb.rssi.ru/GRB101008A/GRB101008a_101012_ZTE.gif


GRB_name: GRB101008A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11353
SUBJECT: GRB 101008A: correction to the GCN 11352
DATE:    10/10/18 12:31:09 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

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

We do not detect the object S2 (Moskvitin et al., GCN 11324;
Nardini et al., GCN 11326). And the table should be read as

Source, T0+,   Filter,  Exposure,  mag.,    Upper Limit (3 sigma)
      (mid, d)       (s)

S1    4.1297  R    97x60      21.0 +/- 0.1   22.4
S3    4.1297  R    97x60      21.6 +/- 0.2

We apologize for possible inconvenience


GRB_name: GRB101017A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11354
SUBJECT: GRB 101017A: Swift/UVOT Observations
DATE:    10/10/18 14:20:49 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.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 101017A 88s after the BAT trigger (Siegel et al.,
GCN Circ. 11345).  The source reported by Siegel et al.
is confirmed in the u and white filters but has not been detected
since the first orbit.

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

FILTER     T_start(s)  T_stop    Exposure     Mag/3uL
========================================================
white (fc)     88        238      147       19.85+-0.22
white          88       1724      409       20.09+-0.17
white        5660       7296      393         >21.03
v             630       1773      136         >18.81
v            6071      11723     1158         >19.93
b             556       1699      116         >19.66
b            5456       7091      393         >20.30
u             301        550      245       19.15+-0.23
u             301       1675      343       19.22+-0.20
u            5250       6886      393         >19.94
uvw1          679       1648      116         >19.22
uvw1         5046      13365     1112         >20.60
uvm2          654       1797      116         >19.08
uvm2         6276      12628     1082         >20.63
uvw2          605       1749      136         >19.52
uvw2         5866       7502      393         >20.22
=======================================================

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 0.17 (Schlegel et al.,
1998, ApJS, 500, 525). The photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB101017A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11355
SUBJECT: GRB 101017A: Swift XRT refined analysis
DATE:    10/10/19 01:44:43 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

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

We have analyzed 21.8 ks of XRT data for GRB 101017A (Siegel  et al.
GCN Circ. 11345), from 87 s to 82800 s after the  BAT trigger. The
data comprise 210 s in Windowed Timing (WT) mode with the remainder
in Photon Counting (PC) mode. The light curve can be modeled
with  a multiple broken power-law model. After an initial decay
slope of 2.22+/-0.08 the light curve steepens at T_break=260+40-20 s
with a slope of 3.85+1.13-0.34 and flattens again at T+527+52-69 s
with a decay slope of 1.35+/-0.08.

A spectrum formed from the WT mode data can be fitted with an
absorbed power-law with a photon spectral index of 1.38+/-0.06 and
an absorption column density of 20.85+2.48-2.31 x 10^20 cm^-2 which
is in excess of the Galactic column density of 7.69 x 10^20 cm^-2
(Kalberla et al. 2005). A fit to the pc mode data shows that the
spectrum has steepened with a photon spectral index of 2.08+/-0.20.
The absorption column density of this fit is consistent with the
result from the WT data. The counts to 0.3-10 keV flux conversion
factor deduced from the WT spectrum  is 6.63 x 10^-11 and
7.70 x 10^-11 erg cm^-2 count^-1 for the observed and the absorption
corrected count rates. For the pc mode we found conversion factors
are 5.00 x 10^-11 and 7.57 x 10^-11 ergs cm^-2 counts^-1,
respectively.

If the light curve continues to decay with a power-law decay index
of 1.35, the count rate at T+48 hours will be in the order of
3 x 10^-4 count s^-1, corresponding to an observed (unabsorbed)
0.3-10 keV flux of 1.5 x 10^-14 (2.3 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00436429.

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


GRB_name: GRB101017A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11356
SUBJECT: GRB 101017A: miniTAO/ANIR NIR upper limits
DATE:    10/10/19 05:34:13 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

K. Motohara, T. Tanabe, S. Koshida, T. Morokuma,
T. Minezaki, and Y. Yoshii (University of Tokyo)
report on behalf of the TAO project team:

We observed GRB 101017A (Siegel et al., GCN 11345) with
the near-infrared camera ANIR mounted on the miniTAO 1.0m
telescope at the University of Tokyo Atacama Observatory
on the summit of Co. Chajnantor (5640 m altitude) in
the northern Chile.

The J- and Ks-band observations started from 2010-10-18
00:37 UT (14hours after the burst), and total exposure time
was 300sec for each band. No object was detected within
the enhanced XRT error circle (Goad et al., GCNC 11348).

Three sigma upper limits are listed below, where the flux
calibrations were carried out using 2MASS stars within
the FoV.

Band    Mid-UT    AB-Mag
----------------------------
Ks      00:40:25  >19.3
J       00:46:51  >19.9
----------------------------


GRB_name: GRB101020A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11357
SUBJECT: GRB 101020A: Swift detection of a burst
DATE:    10/10/20 23:54:11 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. J. Saxton (UCL-MSSL), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC),
M. De Pasquale (UCL-MSSL), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), O. M. Littlejohns (U Leicester),
C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and E. Troja (NASA/GSFC/ORAU)
report on behalf of the Swift Team:

At 23:40:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101020A (trigger=436737).  Due to a Sun constraint, Swift 
was unable to slew to the burst. The BAT on-board calculated location 
is RA, Dec 189.566, +23.161 which is 
   RA(J2000) = 12h 38m 16s
   Dec(J2000) = +23d 09' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual with image triggers, the BAT 
light curve does not show any clear structure.  Ground processing
of the flight scaled map shows a strong 14 sigma source.  The peak 
count rate was ~200 counts/sec (15-350 keV), at ~0 sec after the 
trigger.  There are no known X-ray transient sources near this position. 

Due to an Sun observing constraint, Swift cannot slew to the BAT
position until 17:41 UT on 2010 November 02. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is C. J. Saxton (cjs2 AT mssl.ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB101020A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11358
SUBJECT: GRB 101020A, Swift-BAT refined analysis 
DATE:    10/10/21 13:36:55 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
G. Sato (ISAS), C. J. Saxton (UCL-MSSL), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (GWU) (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 Swift/BAT GRB 101020A (trigger #436737)
(Saxton, et al., GCN Circ. 11357).  The BAT ground-calculated position is
RA, Dec = 189.607, 23.129 deg which is
    RA(J2000)  =  12h 38m 25.8s
    Dec(J2000) = +23d 07' 44.1"
with an uncertainty of 3.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 42%.

The mask-weighted light curve shows a very broad peak with no obvious features,
extending roughly from T-50 sec to T+150 sec.  Most of the emission is below 50 
keV.  A pre-planned slew took the burst out of the field of view at about T+230 
sec.  T90 (15-350 keV) is 175.0 +- 28. sec (estimated error including systematics).

The time-averaged spectrum from T-50.0 to T+159.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.04 +- 0.17.  The fluence in the 15-150 keV band is 2.6 +- 0.3 x 10^-06 
erg/cm^2. The 1-sec peak photon flux measured from T+19.00 sec in the 15-150 keV 
band is 0.5 +- 0.2 ph/cm^2/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/436737/BA/


GRB_name: GRB101020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11359
SUBJECT: GRB 101020A: MASTER polarization optical observations
DATE:    10/10/21 14:16:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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


E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
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, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk



MASTER-Net robotic telescopes (MASTER-Net: http://observ.pereplet.ru)
located  near Ekaterinburg (Kourovka)   was pointed to 
the Swift GRB 101008A (Saxton et al., GCN#11357) 22 s after Notice Time 
and 106 s after trigger time  at large zenit distance (80 degrees).

We have number  images in two perpendicular polarizations (along apha & 
dec) in V-band.

We have no found any OT.


t_start-t_trig(s)   mean time     exp_time(s)   m_lim     Coadd?   Filter
--------------------------------------------------------------------------
      106            116              20          14.0      N      V+P1
      106            116              20          14.0      N      V+P2
      106            116             20+20        14.5      Y     V+P1+P2
--------------------------------------------------------------------------
MASTER II have 2 images per exposition time.
The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101020A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11360
SUBJECT: GRB 101020A: BOOTES2 follow-up and limit
DATE:    10/10/21 14:23:38 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek (IAA-CSIC) and Antonio de Ugarte Postigo
(DARK/NBI) on behalf of a larger collaboration report: 

"The 0.6m Telma telescope at BOOTES-2 (Malaga, Spain) observed
the errorbox of GRB101020a (Saxton et al., GCNC11357) in the
early morning of 21. October 2010, starting 04:48 UT. 40x 60s
r' band images were taken. The combined exposure has a 3-sigma
magnitude limit r'>18.0 calibrated against USNO-A2.0. The
effective exposure time is 05:08:14UT, i.e.  5.46h after the
GRB trigger."


GRB_name: GRB101020A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11361
SUBJECT: GRB 101020A: MASTER prompt and afterglow limit 
DATE:    10/10/22 15:41:40 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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


E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
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, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk



MASTER-Net robotic telescopes (MASTER-Net: http://observ.pereplet.ru)
located  near Ekaterinburg (Kourovka)   was pointed to the Swift GRB 101008A 
(Saxton et al., GCN#11357) 22 s after Notice Time and 106 s after trigger time 
at large zenit distance (80 degrees) (Krushinski et al., GCN Circ 11359).


We have no found any OT.


t_start-t_trig(s)   mean time     exp_time(s)   m_lim     Coadd?   Filter
--------------------------------------------------------------------------
      106            116             20+20        14.9       Y        V
      472           2836             4300         18.5       Y        V
--------------------------------------------------------------------------

MASTER II have 2 images per exposition time.
The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11362
SUBJECT: GRB 101011A: miniTAO/ANIR NIR upper limits
DATE:    10/10/23 01:17:30 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

M. Konishi, T. Morokuma, S. Koshida, N. Matsunaga,
T. Minezaki, and Y. Yoshii (University of Tokyo)
report on behalf of the TAO project team:

We observerd GRB 101011A (Cannizzo et al., GCN 11331) with
the near-infrared camera ANIR mounted on the miniTAO 1.0m
telescope at the University of Tokyo Atacama Observatory
on the summit of Co. Chajnantor (5640m altitude) in
the northern Chile.

The Ks-band observation started from 2010-10-13 06:20 UT
(38hours after the burst), and total exposure time was
1620sec. No object was detected within the enhanced XRT
error circle (Evans et al., GCNC 11333).

The three sigma upper limit is listed below, where the flux
calibration was carried out using 2MASS stars within the FoV.

Band Mid-UT AB-Mag
----------------------------
Ks 06:35:02 >19.7
----------------------------


GRB_name: GRB101023A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11363
SUBJECT: GRB 101023A: Swift detection of a burst
DATE:    10/10/23 23:32:06 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@astro.psu.edu>

C. J. Saxton (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
M. De Pasquale (UCL-MSSL), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), O. M. Littlejohns (U Leicester),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
S. R. Oates (UCL-MSSL), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. Stamatikos (OSU/NASA/GSFC), R. L. C. Starling (U Leicester) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 22:50:12 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101023A (trigger=436981).  Swift slewed immediately to the 
burst.
The BAT on-board calculated location is
RA, Dec 317.954, -65.394 which is
    RA(J2000) = 21h 11m 49s
    Dec(J2000) = -65d 23' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The lightcurve shows a small initial pulse at 
T+0
seconds with a large FRED pulse at about T+55 sec. The peak flux was
32000 counts/sec at T+55 sec.

The XRT began observing the field at 22:51:36.9 UT, 84.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 317.9704, -65.3859 which is equivalent to:
    RA(J2000)  = 21h 11m 52.89s
    Dec(J2000) = -65d 23' 09.2"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 37 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 100 seconds with the White
filter  starting 92 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. The XRT position lies 10.6" from a catalogued USNO
object, photometry is difficult due to the bright halo of the 13th
magnitude USNO star. More data is required to determine if a new
source is present.

Burst Advocate for this burst is C. J. Saxton (cjs2@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: GRB101023A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11364
SUBJECT: GRB 101023A: REM NIR observations
DATE:    10/10/24 01:01:45 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza (INAF/Brera), E. Palazzi (INAF-IASFBo) on behalf
of the REM team report:

The robotic 60-cm REM telescope located at La Silla (Chile) observed
automatically the field of GRB 101023A (Saxton et al. GCN 11363) with the
REMIR near-infrared camera in imaging mode.

Inspection of two set of H-band images, carried out 37 and 63 minutes post
burst, respectively, does not reveal any afterglow candidate within the
XRT error circle down to a 3sigma limiting magnitude of H~14.8 and H~15.5,
respectively (calibrated against the 2MASS catalogue).


GRB_name: GRB101023A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11365
SUBJECT: GRB 101023A: Enhanced Swift-XRT position
DATE:    10/10/24 02:41:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 934 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 101023A, 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 = 317.96358, -65.38852 which is equivalent
to:

RA (J2000): 21h 11m 51.26s
Dec (J2000): -65d 23' 18.7"

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

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

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


GRB_name: GRB101023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11366
SUBJECT: GRB 101023A: Gemini discovery of optical afterglow
DATE:    10/10/24 03:00:08 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J.Levan (U. Warwick), D. Perley (U. Berkeley) and P. D'Avanzo
(INAF-OAB)  report for a larger collaboration:

"We observed the field of GRB 101023A (Saxton et al. GCN 11363)
with GMOS on Gemini-South. We obtained a first epoch of observations
in the r-band beginning at 24 October 00:38, approximately 1.8 hours
post-burst. A second epoch was obtained at 01:26. In these two
observations we identify a fading point source at a location of

RA(J2000) 21:11:51.24 
DEC(J2000) -65:23:15.84

We identify this as the afterglow of GRB 101023A. The afterglow
fades by approximately 0.35 magnitudes between the two epochs of
observation, and has r~20.5 in our first epoch (based on archival
zeropoints). The afterglow position is ~2.8" from the refined XRT 
position of Osborne et al. (GCN 11365).

We thank the staff of Gemini, in particular Henry Lee, for their
help with these observations."


GRB_name: GRB101023A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11367
SUBJECT: GRB 101023A: Swift-BAT refined analysis
DATE:    10/10/24 03:20:47 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
C. J. Saxton (UCL-MSSL), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+542 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 101023A (trigger #436981)
(Saxton, et al., GCN Circ. 11363).  The BAT ground-calculated position is
RA, Dec = 317.949, -65.389 deg, which is 
   RA(J2000)  =  21h 11m 47.8s 
   Dec(J2000) = -65d 23' 20.1" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11%.
 
The mask-weighted light curve shows a small peak starting at ~T-10 sec, peaking
at T_zero.  The main emission starts with about 3 overaping peaks peaking at
~T+54 and ~T+58 sec and ending at ~T+140 sec.  T90 (15-350 keV) is 80.8 +- 2.2 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-11.0 to T+137.3 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.26 +- 0.15, 
and Epeak of 101.1 +- 18.9 keV (chi squared 45.1 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.7 +- 0.1 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+57.34 sec in the 15-150 keV band is
0.0 +- 0.0 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.67 +- 0.03 (chi squared 69.3 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/436981/BA/


GRB_name: GRB101023A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11368
SUBJECT: GRB 101023A: Swift-XRT Team Refined Analysis
DATE:    10/10/24 05:51:00 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

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

We have analysed 961 s of XRT data for GRB 101023A (Saxton et al. GCN Circ. 
11363), from 88 s to 6.0 ks after the BAT trigger. The data comprise 109 s in 
Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The 
enhanced XRT position for this burst was given by Osborne et al. (GCN. Circ 
11365).

The light curve can be modelled with an initial power-law decay with an index 
of alpha=4.30 (+0.11, -0.13), followed by a break at T+174 s to an alpha of 
1.22 (+0.03, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed 
power-law with a photon spectral index of 1.99 (+/-0.06). The best-fitting 
absorption column is 1.93 (+/-0.16) x 10^21 cm^-2, in excess of the 
Galactic value of 2.6 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode 
spectrum has a photon index of 2.15 (+0.22, -0.21) and a best-fitting 
absorption column of 2.1 (+/-0.6) x 10^21 cm^-2. The counts to observed 
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum 
is 3.8 x 10^-11 (6.1 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of 
1.22, 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 7.6 x 10^-13 (1.2 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/00436981.

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


GRB_name: GRB101023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11369
SUBJECT: GGRB 101023A: GROND detection of the optical-NIR afterglow
DATE:    10/10/24 06:55:06 GMT
FROM:    Marco Nardini at MPE  <nardini@mpe.mpg.de>

M. Nardini, F. Olivares E., and J. Greiner (all MPE Garching) report
on behalf of the GROND team:

We observed the field of GRB 101023A (Swift trigger 436981; Saxton et
al., GCN #11363) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP, 120, 405) mounted at the 2.2 m ESO/MPI telescope at La
Silla Observatory (Chile). Observations started on October 23 at 23:59
UT, 1.2 hours after the GRB trigger, and were performed at an average
seeing of 1.4" and at an average airmass of 1.3.

We detect the afterglow reported by Levan et al. (GCN #11366) in all
GROND bands. Co-added images of 24 min of integration time in g'r'i'z'
and 20 min in JHK with midtime at 01:47 UT yield the following
magnitudes in the AB system:

g' = 21.16 +/- 0.04,
r' = 20.50 +/- 0.02,
i' = 20.00 +/- 0.02,
z' = 19.59 +/- 0.02,
J = 19.08 +/- 0.04,
H = 18.76 +/- 0.06, and
K = 17.64 +/- 0.06,

calibrated against GROND zeropoints and 2MASS field stars. We notice
that the K-band magnitude might be contaminated by the near bright
star. Between Oct 24 at 00:03 UT and Oct 24 at 1:47 UT the afterglow
faded of ~0.75 mag in 1.75h.

No corrections for the expected Galactic foreground extinction were
made, which corresponds to a reddening of E(B-V)=0.033 mag in the
direction of the burst (Schlegel et al. 1998). Observations are
continuing.


GRB_name: GRB101024A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11370
SUBJECT: GRB 101024A: Swift detection of a burst with an optical afterglow
DATE:    10/10/24 12:03:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M. De Pasquale (UCL-MSSL), A. P. Beardmore (U Leicester),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), P. T. O'Brien (U Leicester),
C. Pagani (U Leicester), C. J. Saxton (UCL-MSSL),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC) and R. L. C. Starling (U Leicester)
report on behalf of the Swift Team:

At 11:39:29.82 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101024A (trigger=437016).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 66.475, -77.248 which is
    RA(J2000) = 04h 25m 54s
    Dec(J2000) = -77d 14' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The lightcurve shows 4 distinct peaks, with the
brightest peaking at T0+10s. Duration was about 23s.

The XRT began observing the field at 11:40:46.8 UT, 77.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 66.5064, -77.2648 which
is equivalent to:
    RA(J2000)  = 04h 26m 1.54s
    Dec(J2000) = -77d 15' 53.2"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 66 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.52 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.2
(+1.39/-1.27) x 10^21 cm^-2 (90% confidence).

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 81 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
   RA(J2000)  = 04:26:01.73 =  66.50719
   DEC(J2000) = -77:15:55.9  = -77.26552
with a 90%-confidence error radius of about 0.64 arc sec. This position is 2.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.38 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.09.

Burst Advocate for this burst is M. De Pasquale (mdp@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: GRB101023A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11371
SUBJECT: Swift/UVOT observations of GRB101023A
DATE:    10/10/24 13:44:00 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB
101023A 93 s after the BAT trigger (Saxton et al, GCN Circ. 11363)
with a 100s finding chart in the white filter.
UVOT detected a fading optical source, with a position consistent
with the enhanced XRT position (Osborne et al, GCN Circ. 11365), in
the white filter exposures and, very marginally, in the first u
band exposure. We identify this object as the optical afterglow
of GRB101023A.
There is no detection of this source in other filters, either in
single or summed up exposures.

The position of this optical afterglow is

RA =21h 11m 51.26s (317.96360)
Dec = -65d 23m 15.7s (-65.38769) (J2000)

with an estimated uncertainty of 0.6 arcsec. This position is
consistent with the source identified by Gemini (Levan et al,
GCN Circ. 11366) and GROND Nardini et al., GCN 11369). We caution
that the photometry of this object is rather complicated by the
presence of a bright star 13rd magnitude star, which is located
about 15 arcseconds from the optical afterglow.

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

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

white (fc)      93        193        100     19.4 +/- 0.2
white         5895      10094        960     21.7 +/- 0.4 (2.8 sigma)
v             3524      15873       1082         >20.2
b             4344       4483        137         >20.2
u             4139       4339        200     20.5 +/- 0.6 (2 sigma)
u            21640      22548        882         >21.1
w1            3934      21633       1126         >21.1
m2            3728      16778       1082         >21.2
w2           10101      10653        544         >21.0


The values quoted above 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: GRB101024A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11372
SUBJECT: GRB 101024A: Enhanced Swift-XRT position
DATE:    10/10/24 14:20:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 614 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 101024A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 66.50630, -77.26539 which is equivalent
to:

RA (J2000): 04h 26m 1.51s
Dec (J2000): -77d 15' 55.4"

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: GRB101024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11373
SUBJECT: GRB 101024A: GRAS06 optical observations
DATE:    10/10/24 14:59:45 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:

GRAS06 (Global-Rent-a-Scope, Moorook, Australia) RCOS-16 telescope 
and SBIG STL-1001E CCD camera were used to detect GRB 101024A 
optical afterglow. The observations were started at 2010-10-24 11:58:06 (UT) 
and stopped at 2010-10-24 12:30:00 (UT). Three unfiltered observations
with 600s exposure times were made. The afterglow was detected at
following position RA 04 26 01.43 and DEC -77 15 55.9 consistent those
given by Evans P.A. et al. (GCN 11370) to within positional errors.

The following magnitudes were obtained from the observations using 
NOMAD1 0127-0023968 (V = 16.94) as the comparison:

Tmid(s) + T0    Filter            Exp (sec)    Mag      Mag err   Limit
1416                unfiltered       600            19.2      0.4          21.0
2074                unfiltered       600            20.8      0.8          21.0
2730                unfiltered       600          >21.0                     21.0

A jpg image of the 600sec observations is available at the following
URL: http://cutenews.kassiopeia.net/data/upimages/GRB101024A.png


GRB_name: GRB101024A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11374
SUBJECT: GRB 101024A: Swift-BAT refined analysis
DATE:    10/10/24 17:55:08 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (GWU), 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), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU), J. Tueller (GSFC)
(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 101024A (trigger #437016)
(De Pasquale, et al., GCN Circ. 11370).  The BAT ground-calculated position is
RA, Dec = 66.465, -77.261 deg, which is 
   RA(J2000)  =  04h 25m 51.6s 
   Dec(J2000) = -77d 15' 39.7" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 76%.
 
The mask-weighted light curve consists of 4 peats, the first starting at
~T-2 sec, peaking at ~T_zero, then the 3 remaining peaks at T+3 sec,
~T+10, and ~T+18 sec, and returning to background at ~T+30 sec.
T90 (15-350 keV) is 18.7 +- 0.5 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.3 to T+20.1 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.15 +- 0.31, 
and Epeak of 60.0 +- 9.3 keV (chi squared 49.9 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.5 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+9.39 sec in the 15-150 keV band is
5.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.84 +- 0.07 (chi squared 66.9 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/437016/BA/


GRB_name: GRB101024A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11375
SUBJECT: GRB101024A: Swift/UVOT
DATE:    10/10/24 19:21:47 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 101024A
82 s after the BAT trigger (De Pasquale et al., GCN Circ. 11370).
An optical afterglow is detected within the refined XRT error circle
(Beardmore et al., GCN Circ. 11372) in the white filter finding chart.
The same source is detected very marginally in the sum of the following 
white filter exposures. It is not found in any other filter, either
in single and in summed exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

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

white_FC         82          232          147      19.4 +/- 0.2
u_FC            294          543          246         >20.3
white           573         6068          413   22.3 +/- 0.6 (2.1 sigma)
v               624         6479          413         >20.0
b               549         5864          413         >20.6
u               294         5659          459         >20.6
w1              673         5454          216         >20.1
m2              648         5249          221         >19.7
w2              599         6274          413         >20.5

The values quoted above are not corrected for the non-negligible Galactic 
extinction due to the reddening of E(B-V) = 0.09 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB101023A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11376
SUBJECT: GRB 101023A: Fermi GBM observation
DATE:    10/10/24 20:40:56 GMT
FROM:    Michael S. Briggs at UAH and MSFC  <michael.briggs@nasa.gov>

Michael S. Briggs (UAHuntsville) reports on behalf of the Fermi GBM Team:

"At 22:50:04.73 UT on 23 October 2010, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 101023A (trigger 309567006 / 101023.951).

The burst was also detected by the SWIFT-BAT (C. J. Saxton et al. 2010,
GCN 11363).  The GBM on-ground location is consistent with the Swift
position.

The GBM light curve shows two major pulses, the first from 0 to 25 s
relative to the trigger time, the second from 45 to 100 seconds, with
the GRB having a T90 duration of 77 +/- 8 s (50-300 keV).
The spectrum from 0 to 95 s is well fit with a cutoff power law with
an index of -1.64 +/- 0.01 and an Epeak of 277 +/- 14 keV.   The fluence
(10-1000 keV) for the t90 time interval is (6.4 +/- 0.1) E-05 erg/cm^2.

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








 


GRB_name: GRB101023A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11377
SUBJECT: GRB 101023A: Swift detection of a burst
DATE:    10/10/24 20:42:42 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

C. J. Saxton (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
M. De Pasquale (UCL-MSSL), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), O. M. Littlejohns (U Leicester),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
S. R. Oates (UCL-MSSL), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. Stamatikos (OSU/NASA/GSFC), R. L. C. Starling (U Leicester) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 22:50:12 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101023A (trigger=436981).  Swift slewed immediately to the burst.
The BAT on-board calculated location is 
RA, Dec 317.954, -65.394 which is 
   RA(J2000) = 21h 11m 49s
   Dec(J2000) = -65d 23' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The lightcurve shows a small initial pulse at T+0
seconds with a large FRED pulse at about T+55 sec. The peak flux was 
32000 counts/sec at T+55 sec.

The XRT began observing the field at 22:51:36.9 UT, 84.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 317.9704, -65.3859 which is equivalent to:
   RA(J2000)  = 21h 11m 52.89s
   Dec(J2000) = -65d 23' 09.2"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 37 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 100 seconds with the White
filter  starting 92 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. The XRT position lies 10.6" from a catalogued USNO
object, photometry is difficult due to the bright halo of the 13th
magnitude USNO star. More data is required to determine if a new
source is present.

Burst Advocate for this burst is C. J. Saxton (cjs2@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: GRB101024A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11378
SUBJECT: GRB 101024A: Fermi GBM observation
DATE:    10/10/24 22:06:01 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

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

"At 11:39:33.60 UT on 24 October 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101024A (trigger 309613175/101024486)
which was also detected by the Swift-BAT
(De Pasquale et al. 2010, GCN 11370).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 142 degrees.

The GBM light curve consists of three pulses with the first
pulse starting about 5 seconds before the trigger.
The event has a duration (T90) of about 24 (+/-2) s (50-300 keV).
The time-averaged spectrum from T0-0.003 s to T0+19.456 s is
adequately fit by a power law function with an exponential
high energy cutoff.  The power law index is 1.4 (+1.6/-0.8)  and
the cutoff energy, parameterized as Epeak, is 56.25 (+5.96/-5.54) keV
(CSTAT 447 for 359 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(1.2 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.5 s in the 8-1000 keV band
is 8.2 +/- 0.5 ph/s/cm^2.

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


GRB_name: GRB101023A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11379
SUBJECT: GRB 101023A: miniTAO/ANIR NIR detection
DATE:    10/10/25 05:08:56 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

K. Motohara, T. Tanabe, S. Koshida, T. Morokuma,
T. Minezaki, and Y. Yoshii (University of Tokyo),
report on behalf of the TAO project team:

We observed GRB 101023A (Saxton et al., GCN 11363) with
the near-infrared camera ANIR mounted on the miniTAO 1.0m
telescope at the University of Tokyo Atacama Observatory
on the summit of Co. Chajnantor (5640m altitude) in
the northern Chile.

The J-, H-, and Ks-band observations started from
2010-10-24 02:48 UT (3hours after the burst), and total
exposure time was 540sec for each band. The afterglow was
detected in all the three bands at the position reported
by Levan et al. (GCN 11366). The seeing was 0.9-1.0arcsec
throughout the observations, and the image of the afterglow
was clearly separated from the nearby bright star.

AB magnitudes are are listed below, where the flux calibrations
were carried out using 2MASS stars within the FoV.

Band   Mid-UT    AB-Mag
----------------------------
Ks      02:53:05  19.40 +/- 0.10
H       03:07:41  20.28 +/- 0.27
J       03:24:36  19.92 +/- 0.14
----------------------------


GRB_name: GRB101024A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11380
SUBJECT: GRB 101024A: Zadko observatory - Gingin. Optical observations
DATE:    10/10/25 09:57:20 GMT
FROM:    Myrtille LAAS-BOUREZ at U.Western Australia  <myrtille.laas@oamp.fr>

GRB 101024A: Zadko observatory - Gingin. Optical observations
-------------------------------------------------------------
M. Laas-Bourez (UWA/ICRAR), A. Klotz (CESR-UPS-CNRS), D. Coward (UWA), D. Blair (UWA),
M. Boer (OHP-CNRS), P. Thierry (CESR-UPS-CNRS) report:

We imaged the field of GRB 101024A detected by SWIFT
(trigger 437016) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 215s after the GRB trigger
(199s after the notice). The elevation of the field increased from
27 degrees above horizon and weather conditions
were good with humidity (77%).

We detect a new fading source in the error box given by SWIFT
We detected the candidate couterpart mentioned by De Pasquale et al. (GCNC 11370)
at the following position (+/- 0.5 arcsec):

RA(J2000) = 04h26m01s76
DEC(J2000) = -77d15m55s64

The first image is trailed with a duration of 30.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
IT was taken between 214.7s - 244.7s after GRB.
It will be analyzed later.

Next images show the decay of the OT:

OT was R=16.75 between 259s and 289s after GRB, filter C
OT was R=17.07 between 305s and 335s after GRB, filter C
OT was R=17.15 between 349s and 379s after GRB, filter C
OT was R=17.19 between 394s and 424s after GRB, filter C


Magnitudes were estimated with the star : NOMAD1 0127-0023961
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=290.5330 lat=-34.1439

This message may be cited.



<http://www.zt.science.uwa.edu.au/>


GRB_name: GRB101024A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11381
SUBJECT: GRB 101024A: Swift XRT refined analysis 
DATE:    10/10/25 11:32:55 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

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

We have analysed 11 ks of Swift XRT data for GRB 101024A (De Pasquale et 
al. GCN Circ. 11370), from 62 s to 57.2 ks after the BAT trigger. The data 
comprise 8 s in Windowed Timing (WT) mode (taken while Swift was slewing), 
with the remainder in Photon Counting (PC) mode. The enhanced XRT position 
for this burst was given by Beardmore et al. (GCN. Circ 11372).

The light curve can be modelled with a series of power-law decays. The 
initial decay index is alpha=5.0 (+5.0, -3.9). At T+77 s the decay 
flattens to an alpha of -0.03 (+0.16, -0.18) before breaking again at 
T+870 s to a final decay with index alpha=1.30 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed 
power-law with a photon spectral index of 1.95 (+0.13, -0.10). The 
best-fitting absorption column is 1.06 (+0.29, -0.13) x 10^21 cm^-2, in 
excess of the Galactic value of 6.5 x 10^20 cm^-2 (Kalberla et al. 2005). 
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor 
deduced from this spectrum is 4.0 x 10^-11 (5.1 x 10^-11) erg cm^-2 
count^-1.

If the light curve continues to decay with a power-law decay index of 
1.30, the count rate at T+24 hours will be 6.0 x 10^-3 count s^-1, 
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.4 x 10^-13 
(3.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at 
http://www.swift.ac.uk/xrt_products/00437016.

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


GRB_name: GRB101024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11382
SUBJECT: GRB 101024A: Zadko observatory - Gingin. Optical observations refined analysis
DATE:    10/10/26 08:46:02 GMT
FROM:    Myrtille LAAS-BOUREZ at U.Western Australia  <myrtille.laas@oamp.fr>

GRB 101024A: Zadko observatory - Gingin. Optical observations refined
analysis
-------------------------------------------------------------------------------
M. Laas-Bourez (UWA/ICRAR), A. Klotz (CESR-UPS-CNRS), D. Coward (UWA),
D. Blair (UWA),
M. Boer (OHP-CNRS), P. Thierry (CESR-UPS-CNRS) report:

We analyzed carefully early images of GRB101024A
taken with the Zadko telescope, Gingin, Australia
(see Laas-Bourez et al. 2010 GCNC 11380). Images
are unfiltered. Magnitudes are converted into R
band using the star NOMAD1 0127-0023961 R=13.61
supposing (V-R)=0.6 for the optical counterpart
of the GRB. Magnitudes are not corrected for galactic
dust extinction.

-------------------------------
start end   Rmag
(s)   (s)
-------------------------------
215   222  16.55 +/-0.15
222   245  16.72 +/-0.15
259   289  16.86 +/-0.12
305   335  17.06 +/-0.12
349   379  17.24 +/-0.12
394   424  17.23 +/-0.12
-------------------------------

Considering a law decay in flux proportional to
t^-alpha, there is a consistent decrease with
alpha ~ 1.1 between 215 and ~ 360 seconds.
After 360 seconds, a plateau seems to be reached
lasting at least 60 seconds.

Compared to the UVOT data taken in the same range
of time (De Pasquale et al. 2010 GCNC 11375) the
optical afterglow is very red, consistent with a
redshift z>2.

This message may be cited.

<http://www.zt.science.uwa.edu.au/>


GRB_name: GRB101024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11383
SUBJECT: GRB 101024A: GROND optical/NIR observations
DATE:    10/10/26 17:45:31 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

T. Kruehler, F. Olivares, M. Nardini and J. Greiner (all MPE Garching)
report on behalf of the GROND team:

GROND (Greiner et al. 2008, PASP 120, 405), mounted at the 2.2m MPG/ESO
telescope at La Silla Observatory (Chile), started observations of the
field of GRB 101024A (de Pasquale et al., GCN #11370) in g'r'i'z'JHK at
07:42 UT on 2010-10-26, 43.7 h after the burst. We detect the optical
afterglow (de Pasquale et al., GCNs #11370, 11375, Hentunen et al., GCN
#11373, Laas-Bourez et al., GCNs #11380, 11382) marginally in the r' and
i' bands.

Preliminary AB magnitudes and upper limits at a midtime of 08:14 UT on
2010-10-26 in stacked images with 50 min of total integration time in each
g'r'i'z' and 40 min in JHK are:

g' > 24.1
r' = 24.5 +- 0.3
i' = 23.8 +- 0.2
z' > 23.7
J > 21.8
H > 21.3
K > 20.5

These magnitudes have been derived by calibrating the images against the
GROND zeropoints and 2MASS field stars and are not corrected for the
expected foreground reddening of E(B-V)=0.088 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB101023A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11384
SUBJECT: Konus-Wind observation of GRB 101023A
DATE:    10/10/27 14:51:43 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 GRB 101023A, (Swift/BAT trigger=436981:
Saxton, et al., GCN 11363; Stamatikos et.al, GCN 11367)
triggered Konus-Wind at T0=82264.703s UT (22:51:04.703)

The burst light curve started, at ~T0-65s, with a weak
initial pulse, followed by a much brighter and harder
emission episode, peaked at ~T0+5s.
The total duration of the burst is ~100 s.
The emission is seen up to 2 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101023_T82264/

As observed by Konus-Wind the burst
had a fluence of (6.6  0.5)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+4.096s,
of (7.1  0.5)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of major part of the burst
(from T0 to T0+29.952 s) is best fit
in the 20 keV - 2 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -1.07 (-0.07, +0.08),
the high energy photon index beta = -2.5 (-0.3, +0.7),
the peak energy Ep = 200(-16, +17) keV (chi2 = 73/57 dof).

The spectrum at the maximum count rate
(measured from T0+0.256 to T0+6.400 s) is best fit
in the 20 keV - 2 MeV range by the GRB (Band)
model, for which:
the low-energy photon index alpha = -0.84 (-0.07, +0.08),
the high energy photon index beta = -2.8 (-0.4, +0.2),
the peak energy Ep = 239(-17, +18) keV (chi2 = 56/57 dof).

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


GRB_name: GRB090111A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11385
SUBJECT: GRB 090111, the review of the sky area in plate archives (1976-1996)
DATE:    10/10/28 11:47:27 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

GRB 090111, the review of the sky area in plate archives (1976-1996)
   V.V. Golovnya, L.N. Kizyun (Main Astronomical Observatory, Kyiv)
   report:

   We have undertaken the review of the sky area of GRB 090111
   (Evans et al., GCN 8796) on astronegatives, collected in Ukrainian NAS
   Main
   astronomical observatory plate archive (1976-1996)[1,2,3].  All the
   plates
   with the possible object appearance are digitized using Microtek
   ScanMaker
   9800XL TMA flatbed scanner and have been placed into Golosiiv Plate
   Archive
   database DBGPA with open access to them.

   The list of plates is given in the table:
   YYYYMMDD UT       GUA_ID          Exp. LimMag  Star
   19790419 22:37:48 GUA040C001160B   5   14.4    USNO A2 0900-08951386
   19790503 23:54:51 GUA040C001168B   6   14.4    USNO A2 0900-08951386
   19790503 23:54:51 GUA040D001169    6   14.65   USNO A2 0900-08945162
   19800515 23:06:42 GUA040D001747   20   14.4    USNO A2 0900-08951386
   19800515 23:06:34 GUA040C001746B  20   14.65   USNO A2 0900-08945162
   19810521 22:48:36 GUA040D001952    3   11.63   TYC 384-480-1
   19820515 22:46:59 GUA040C000082A  27   16.35   USNO A2 0900-08949620
   19910613 21:25:17 GUA040C001800A  22.5 17.3    USNO A2 0900-08949717

   GUA ID - Double Wide-angle Astrograph (D/F=40/2000, M=103"/mm)
   of the Ukrainian NAS Main astronomical observatory in Kyiv
   (Marsden's number - 83) the plate number[4].
   Exp.   - Duration of the maximum exposures (minutes).
   LimMag - Limited mag, derived in the 15 minutes area around the
   location
   given in Evans et al., GCN 8796
   Star   - Comparison star.

   The preview images can be found
   http://gua.db.ukr-vo.org/img/grb/090111/index.html.
   The images with full resolution are available via e-mail on demand.
   References:
   1. L.Pakulyak , N.Kharchenko, E.Izhakevich, V.Golovnya, V.Kisljuk,
   V.Andruk. Data base of photographic observations of celestial bodies
   of
   Golosiiv observatory. Baltic Astron. 6, 1997.
   2. L.Pakulyak, N.Kharchenko, E.Izhakevich, V.Golovnya, V.Andruk,
   V.Kisljuk. Data base of photographic observations of celestial bodies
   of Golosiiv observatory in Kiev. Newsletters of IAU WG "Wide-field
   imaging" No 9, 1997
   3. V.Kislyuk, A.Yatsenko, G.Ivanov, L.Pakuliak, T.Sergeeva. The
   FON Astrographic catalogue (FONAC): version1.0. Proc. of Journees
   1999 and IX Lohrmann-Kolloquium "Motion of celestial bodies,
   astromerty and astronomical reference frames", Drezden, September
   13-15,1999
   4.L.Pakulyak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
   http://gua.db.ukr-vo.org/


GRB_name: GRB101030A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11386
SUBJECT: GRB 101030A: Swift detection of a burst
DATE:    10/10/30 16:13:55 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC), M. M. Chester (PSU),
V. D'Elia (ASDC), J. M. Gelbord (PSU), C. Guidorzi (U Ferrara),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
R. Margutti (INAF-OAB), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and
E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 15:56:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101030A (trigger=437408).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 166.390, -16.387 which is 
   RA(J2000)  =  11h 05m 34s
   Dec(J2000) = -16d 23' 11"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows that the burst began
with a bright peak starting at around -70 sec from the trigger, 
followed by a second episode starting at T-10 sec and consisting of two
overlapping peaks with a duration of about 80 sec.  We note that the 
first peak occurred during a pre-planned slew, so the BAT could not 
trigger on it; it is also possible that BAT missed emission from the 
burst before T-100 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 15:57:35.6 UT, 65.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
166.3825, -16.3782 which is equivalent to:
   RA(J2000)  = 11h 05m 31.80s
   Dec(J2000) = -16d 22' 41.5"
with an uncertainty of 2.5 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.24
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 2.81e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 73 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.04. 

Burst Advocate for this burst is 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: GRB101030A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11387
SUBJECT: GRB 101030A: Enhanced Swift-XRT position
DATE:    10/10/30 18:30:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 807 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 101030A, 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 = 166.38198, -16.37812 which is equivalent
to:

RA (J2000): 11h 05m 31.68s
Dec (J2000): -16d 22' 41.2"

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: GRB101030A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11388
SUBJECT: GRB 101030A: Swift-BAT refined analysis
DATE:    10/10/30 19:16:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(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 101030A (trigger #437408)
(Melandri, et al., GCN Circ. 11386).  The BAT ground-calculated position is
RA, Dec = 166.390, -16.389 deg, which is 
   RA(J2000)  =  11h 05m 33.6s 
   Dec(J2000) = -16d 23' 22.0" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.
 
The mask-weighted light curve shows the burst already in progress as it came
into the BAT FoV at ~T-60 sec during a pre-planned slew.  The lightcurve decreases
from that time and nearly returns to background levels at ~T-18 sec.
Then it begins to rise again, peaking at T+1 sec and ~T+9 sec and returning
to background at ~T+70 sec.  There is possible emission at the 2-sigma level
from T+130 sec to T+170 sec.  T90 (15-350 keV) is 92.0 +- 50 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-55.2 to T+47.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.82 +- 0.10.  The fluence in the 15-150 keV band is 2.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+8.78 sec in the 15-150 keV band
is 0.9 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/437408/BA/


GRB_name: GRB101030A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11389
SUBJECT: GRB 101030A: Swift/UVOT Upper Limits
DATE:    10/10/31 04:17:28 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and A. Melandri (INAF-OAB) report
on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB
101030A 73s after the BAT trigger (Melandi et al., GCN 11386).
We do not detect any source at the enhanced Swift XRT position
(Evans et al., GCN 11387).  UVOT magnitude 3-sigma upper limits
are reported in the following table:

Filter  T_start  T_stop  Exp(s)  Mag (3-sigma upper limit)
-------------------------------------------------------------
white(fc)  73      223    146      > 20.32
white      73     1008    327      > 20.75
v         617      808     38      > 17.89
b         542      735     38      > 18.83
u         285      710    260      > 19.68
uvw1      666      857     38      > 18.39
uvm2      641      833     38      > 18.18
uvw2      592      784     38      > 18.61

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight of E_(B-V) = 0.04
(Schlegel et al. 1998). All photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB101030A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11390
SUBJECT: GRB 101030A : Swift XRT refined analysis
DATE:    10/10/31 13:47:52 GMT
FROM:    Andrea Melandri at Liverpool John Moores U  <axm@astro.livjm.ac.uk>

A. Melandri, R. Margutti and B. Sbarufatti (INAF-OAB) report on  
behalf of the Swift-XRT team:

We have analysed 7.4 ks of XRT data for GRB 101030A (Melandri et al.  
GCN Circ. 11386), from 71 s to 19.2 ks after the BAT trigger. The  
data comprise 118 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 11387).

The light curve can be modelled with a series of power-law decays.  
The initial decay index is alpha=2.32 (+0.26, -0.33). At T+112 s the  
decay steepens to an alpha of 3.97 (+0.24, -0.22). The light curve  
breaks again at T+478 s to a decay with alpha=-0.08 (+0.18, -1.43),  
before a final break at T+5105 s after which the decay index is 1.12  
(+0.22, -0.21).

A spectrum formed from the WT mode data can be fitted with an  
absorbed power-law with a photon spectral index of 2.87 (+0.15,  
-0.13). The best-fitting absorption column is 1.83 (+0.26, -0.24) x  
10^21 cm^-2, in excess of the Galactic value of 4.2 x 10^20 cm^-2  
(Kalberla et al. 2005). The PC mode spectrum has a photon index of  
2.11 (+0.12, -0.20) and a best-fitting absorption column of 8.1  
(+2.7, -3.9) x 10^20 cm^-2. The counts to observed (unabsorbed)  
0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x  
10^-11 (4.6 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of  
1.12, the count rate at T+24 hours will be 4.7 x 10^-3 count s^-1,  
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x  
10^-13 (2.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at  
http://www.swift.ac.uk/xrt_products/00437408.

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


GRB_name: GRB101030A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11391
SUBJECT: GRB 101030A: GROND optical/NIR afterglow candidate
DATE:    10/10/31 19:43:07 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

T. Kruehler, P. Schady, and J. Greiner (all MPE Garching)  report on
behalf of the GROND team:

GROND (Greiner et al. 2008, PASP 120, 405), mounted at the 2.2m MPG/ESO
telescope at LaSilla Observatory (Chile), performed automated follow-up
observations of GRB 101030A (Melandri et al., GCN #11386) as soon as the
field rose above the pointing constraints of the telescope. Imaging was
performed simultaneously in g'r'i'z'JHK starting at 08:12 UT on
2010-10-31, which is 16.3 h after the burst. Inside the enhanced XRT error
circle (Evans et al., GCN# 11387), GROND detects a single object at:

RA (J2000)= 11:05:31.68
Dec (J2000)= -16:22:41.1

with uncertainties of 0.3" in each coordinate.

Preliminary AB magnitudes and upper limits in stacked images of 15 min
integration time in each g'r'i'z' and 20 min in JHK at a midtime of 08:46
UT are:

g' = 22.9 +- 0.3
r' = 22.4 +- 0.1
i' = 22.0 +- 0.1
z' = 22.1 +- 0.2
J = 21.7 +- 0.4
H > 21.2
K > 20.5

which have been tied to SDSS and 2MASS field stars. No statement about
variability can be made at this point. No source is reported at this
location in the SDSS, which is somewhat deeper than the object's
magnitudes, and hence we suggest this source is the optical/NIR afterglow
of GRB101030A.

We thank the ESO staff at LaSilla observatory, and in particular P. Arias,
for their excellent support and assistance with the observations.


GRB_name: GRB101030A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11392
SUBJECT: GRB 101030A : MOA optical observation
DATE:    10/11/06 18:06:59 GMT
FROM:    Suzuki Daisuke at MOA-II  <dsuke@stelab.nagoya-u.ac.jp>

D. Suzuki, K. Omori, S. Kobara, H. Naito and T. Sako (STE Lab, Nagoya Univ.)
on behalf of the MOA Collaboration report:

We searched for an optical afterglow of GRB101030A (GCN 11386, Melandri et
al.)
starting from 15:59:39 UT on 2010 Oct. 30th with the MOA-II 1.8m telescope
at Mt.John observatory in New Zealand. The images were taken with a wideband
Red filter
(center wavelength ~ 750nm and FWHM ~ 250nm), and we found a new source
within
the error circle of the Swift XRT source position (GCN 11387).
The estimated magnitudes are the followings.

t-t0(sec) Imag err exp.
-------------------------
190  20.0  2.3  300
610  19.5  4.0  100
-------------------------

Large errors in the magnitude estimation are due to the observations
during dawn and under the moon light. Consequently, relatively small
number of field stars affects in the large errors.
These magnitudes were calibrated against the USNO-B1.0 catalog stars,
and not corrected for the Galactic extinction.


GRB_name: GRB090113A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11393
SUBJECT: GRB 090113, the review of the sky area in plate archives
DATE:    10/11/09 20:31:53 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

GRB 090113, the review of the sky area in plate archives
V.V. Golovnya, L.N. Kizyun, L.K. Pakuliak (Main Astro Obs, Kyiv)
report:

We have undertaken the review of the sky area of GRB 090113 (Evans et
al., GCN 8809) on astronegatives, collected in Ukrainian NAS Main
astronomical observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek ScanMaker
9800XL TMA flatbed scanner and have been placed into Golosiiv Plate 
Archive database DBGPA with open access to them.

The list of plates is given in the table:
YYYYMMDD UT       GUA_ID          Exp.  LimMag  
19881004 23:10:05 GUA040C001340   16.0  16.2    
19891025 20:42:19 GUA040C001518A  22.5  16.0    
19891025 21:38:29 GUA040C001520A  16.0  15.0  
19891026 19:55:50 GUA040C001521B  19.0  15.0    
19891026 21:50:31 GUA040C001525   18.0  15.3   
19930924 23:42:35 GUA040C002246   20.2  15.3   
 
GUA ID - Double Wide-angle Astrograph (D/F=40/2000, S=103"/mm)
         of the Ukrainian NAS Main astronomical observatory in Kyiv
         (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposures (minutes).
LimMag - Limited mag, derived in the 8 minutes area around the location
         given in Evans et al., GCN 8809:
         RA (J2000): 02h 08m 13.63s, Dec (J2000): +33d 25' 42.9".

The preview images can be found
http://gua.db.ukr-vo.org/img/grb/090113/index.html.
The images with full resolution are available via e-mail on demand.
References:
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org/


GRB_name: GRB090113A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11394
SUBJECT: GRB 090113, the review of the sky area in plate archives
DATE:    10/11/09 20:33:35 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

GRB 090113, the review of the sky area in plate archives
V.V. Golovnya, L.N. Kizyun, L.K. Pakuliak (Main Astro Obs, Kyiv)
report:

We have undertaken the review of the sky area of GRB 090113 (Evans et
al., GCN 8809) on astronegatives, collected in Ukrainian NAS Main
astronomical observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek ScanMaker
9800XL TMA flatbed scanner and have been placed into Golosiiv Plate 
Archive database DBGPA with open access to them.

The list of plates is given in the table:
YYYYMMDD UT       GUA_ID          Exp.  LimMag  
19881004 23:10:05 GUA040C001340   16.0  16.2    
19891025 20:42:19 GUA040C001518A  22.5  16.0    
19891025 21:38:29 GUA040C001520A  16.0  15.0  
19891026 19:55:50 GUA040C001521B  19.0  15.0    
19891026 21:50:31 GUA040C001525   18.0  15.3   
19930924 23:42:35 GUA040C002246   20.2  15.3   
 
GUA ID - Double Wide-angle Astrograph (D/F=40/2000, S=103"/mm)
         of the Ukrainian NAS Main astronomical observatory in Kyiv
         (Marsden's number - 83) the plate number [1].
Exp.   - Duration of the maximum exposures (minutes).
LimMag - Limited mag, derived in the 8 minutes area around the location
         given in Evans et al., GCN 8809:
         RA (J2000): 02h 08m 13.63s, Dec (J2000): +33d 25' 42.9".

The preview images can be found
http://gua.db.ukr-vo.org/img/grb/090113/index.html.
The images with full resolution are available via e-mail on demand.
References:
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org/


GRB_name: GRB100906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11395
SUBJECT: GRB 100906A: optical observations
DATE:    10/11/11 17:56:47 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (SAI MSU),  A. Pozanenko (IKI), M. Andreev, A. Sergeev
(Terskol Branch
of Institute of Astronomy),   V. Rumyantsev, K. Grankin (CrAO), A.
Erofeeva, G. Kornienko (UAFO), I. Molotov (ISON), E. Klunko (ISTPM),
Ibrahimov (MAO), B. Satovski (Astrotel) on behalf of GRB follow up
collaboration report:

We observed the optical afterglow (Markwardt et al. GCN 11227, Ivanov
et al. GCN 1128) of GRB 100906A (Markwardt et al. GCN 11227) with the
following telescopes: GAS-250 (Ussuriysk Astrophysical Observatory),
AZT-14 (Mondy observatory), Zeiss-2000 and Zeiss-600 (Mt.Terskol
observatory),  Shajn telescope (CrAO) and AZT-22 (Maidanak
observatory). Observations started at 14:02 UT, i.e. approximately 13
minutes after the burst trigger. Observations in different optical
bands (B, V, R, I, g, r) cover the period of t-t_0 from 0.12 up to
2.46 days. The photometry calibration was made against several stars
of GSC2.3 catalog. The light curve of GRB 100906A afterglow can be
found at
http://grb.rssi.ru/GRB100906A/GRB100906A_lc.png .

From the R band of light curve one can see a clear break around ~0.5
days after the burst with alpha_1 = -0.7 +/- 0.1 before and alpha_2 =
-2.0 +/- 0.3 after break.
Color index B-R measured between 0.22 and 0.24 days after the burst
does not change within the error bars and is equal to 1.33 +/- 0.12,
while the B-R index measured at 1.26 days after the burst trigger is
equal to 1.61+/- 0.19.


GRB_name: GRB101112A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11396
SUBJECT: GRB 101112A: a long GRB detected by INTEGRAL
DATE:    10/11/12 23:03:08 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D. Gotz (CEA-Saclay), S.Mereghetti, A.Paizis (IASF- Milano), E. Bozzo,  
V. Savchenko, C. Ferrigno, M. Beck (ISDC, Versoix), and J. Borkowski  
(CAMK, Torun) on behalf of the IBAS Localization Team report:
a long gamma ray burst lasting about 10 s has been detected by IBAS in  
the IBIS/ISGRI data at 22:10:24 U.T. on November 12th.
Its refined coordinates (J2000) are:
R.A. =  292.218347 (deg)
Dec. = +39.359032 (deg)

with an uncertainty of 1.3 arcmin (90% c.l.).

A preliminary analysis gives a 20-200 keV fluence of about  6e-7 erg/ 
cm2 and a peak flux of about 1.6 ph/cm2 s  (1 s integration time).

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB101112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11397
SUBJECT: GRB101112A: Liverpool Telescope Afterglow Candidate
DATE:    10/11/12 23:11:23 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), R.J. Smith, C.G. Mundell, I.A. Steele,
S Kobayashi (Liverpool JMU), A. Gomboc (U. Ljubljana),
report on behalf of a larger collaboration:

The 2-m Liverpool Telescope robotically followed up INTEGRAL
GRB 101112A (Gotz et al. GCN Circ. 11396). The automatic analysis
pipeline LT-TRAP identified a fading afterglow candidate at:

RA 19:28:54.87  Dec +39:21:11.1 (J2000)

with position uncertainty 0.4 arcsec and
with

R=15.99 +- 0.02 mag @ 7.7 min
R=17.05 +- 0.03 mag @ 19.2 min

Photometric calibration is wrt USNOB-1 star at 19:28:54.733,
+39:21:00.87 with R2=16.15.


GRB_name: GRB101112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11398
SUBJECT: GRB 101112A: BOOTES-2/TELMA optical afterglow candidate
DATE:    10/11/12 23:13:09 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

GRB 101112A: BOOTES-2/TELMA optical afterglow candidate

A. de Ugarte Postigo (DARK/NBI Copenhagen), P. Kubanek (IPL Univ. of 
Valencia), J. C. Tello, R. Sanchez-Ramirez, M. Jelinek, R.  Cunniffe
O. Lara-Gil, C. Thoene, S. Guziy, J. Gorosabel (IAA-CSIC Granada),
R. Fernandez-Muoz (EELM-CSIC), S. Castillo-Carrion, C. Perez del Pulgar
(Univ. of Malaga), D. Perez-Ramirez (Univ. de Jaen), L. Sabau-Graziati (INTA)
and A. J. Castro-Tirado (IAA-CSIC) report:

"Following the detection of GRB 101112A by INTEGRAL (Gotz et al. GCNC 
11396), the 0.6m TELMA  robotic telescope at the BOOTES-2 station in 
Malaga (Southern Spain) responded 31 s after reception of the GCN alert 
(i.e. 109 s after the onset of the event).  Within the IBIS/INTEGRAL 
error box, we find a source not present at the DSS-2 red at coordinates 
(J2000) R.A.:19:28:54.88,  Dec: +39:21:11.6 (error  0".5).  We measure 
R about 18  for the co-added 31 first images (3-s each, using an r' band 
filter, at mid exposure time 22:12 UT, i.e. 156-s after the onset of the 
burst).  The source has gone in the images taken at later times so we 
propose this to be the optical afterglow  to GRB 101112A. Further 
observations are in progress. Multiwavelength observations (including 
optical spectroscopy) are requested."

This message can be quoted.

[GCN OPS NOTE(12nov10): Per author's request, OL-G, CT, DP-R were added
and a duplicate of PK was removed.]


GRB_name: GRB101112A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11399
SUBJECT: GRB 101112A - XRT source detection/analysis
DATE:    10/11/13 09:28:33 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and H. A. Krimm (CRESST/GSFC/USRA),
report on behalf of the Swift-XRT team:

We have analysed 5.6 ks of XRT data for GRB 101112A (Gotz et al. GCN Circ.
11396), from 6215 s to 18.4 ks after the INTEGRAL trigger. The data are entirely 
in Photon Counting (PC) mode. We find an uncatalogued, fading point source at 
RA, Dec=292.2295, 39.3531 which is equivalent to:

RA(J2000):   19h 28m 55.08s
Dec (J2000): +39d 21' 11.0"

with an estimated uncertainty of 4 arcsec (radius, 90% confidence). This 
position is 38 arcsec from the INTEGRAL position, and 2.4 arcsec from the 
optical afterglow of Guidorzi et al (GCN Circ 11397), in agreement with both of 
these positions.

The X-ray light curve can be modelled with a power-law decay with a decay index
of alpha=0.9 (+/-0.6). A spectrum formed from the PC mode data can be fitted
with an absorbed power-law with a photon spectral index of 2.2 (+/-0.4). The
best-fitting absorption column is 2.0 (+1.2, -0.7) x 10^21 cm^-2, consistent
with the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al. 2005). The counts
to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum is 3.7 x 10^-11 (5.9 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of 0.9, the
count rate at T+24 hours will be 3.7 x 10^-3 count s^-1, corresponding to an
observed (unabsorbed) 0.3-10 keV flux of 1.4 x 10^-13 (2.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020149.

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


GRB_name: GRB101112A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11400
SUBJECT: Konus-Wind observation of GRB 101112A
DATE:    10/11/13 12:26:47 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 101112A, (localized by INTEGRAL: Gotz et.al, GCN 11396)
triggered Konus-Wind at T0=79831.681s UT (22:10:31.681)

The burst light curve shows a single pulse
with a total duration of ~15 s.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101112_T79831/

As observed by Konus-Wind the burst
had a fluence of (1.95  0.45)x10-6 erg/cm2,
and a 256-ms peak flux, measured from T0,
of (0.85  0.25)x10-6 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+8.448 s) is best fit
in the 20 keV - 1 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.4(-0.7, +1.0),
and Ep = 107(-22, +39) keV (chi2 = 28/50 dof).

The spectrum at the maximum count rate
(measured from T0 to T0+0.256 s) is best fit
in the 20 keV - 1 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.75(-0.6, +0.9),
and Ep = 132(-38, +72) keV (chi2 = 6/14 dof).

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


GRB_name: GRB101112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11401
SUBJECT: GRB 10112A: MASTER optical observations
DATE:    10/11/13 16:18:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located at Kislovodsk was pointed to the  GRB101112A 21 sec s after
notice time and 36 sec after GRB time at 2010-11-12 22:11:11.00 UT at
very high zenit distance (~88 degrees).
On our first (10s exposure) set we haven't found optical transient  within
UNDEF error-box (ra=19 29 16 dec=+39 23 22 r=0.047500).

The 5-sigma upper limit has been about 15.7 mag

We have no found any OT at Liverpool OT position (Guidorzi et al., GCN
Circ 11397).

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11402
SUBJECT: GRB 101112A: optical observations
DATE:    10/11/13 18:23:26 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed  the field of INTEGRAL GRB 101112A (Gotz  et al., GCN 11396) 
with AZT-22 telescope of Maidanak observatory between Nov. 13 (UT) 
13:37:57 -- 14:05:56.Totally we obtained 6 images of 300 s exposure in R 
filter. The afterglow (Guidorzi et al. GCN 11397; A. de Ugarte Postigo et 
al. GCN 11398) is not visible on single images, and upper limit of the 
single image is R~20m at Nov.13 (UT) 13:40.
The result above is preliminary.

We thank Olga Ezhkova  for performing the observations and for support.


GRB_name: GRB101112A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11403
SUBJECT: GRB 101112A: Fermi GBM detection
DATE:    10/11/14 00:58:46 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 22:10:32.45 UT on 12 November 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101112A (trigger 311292634 / 101112924)
which was also detected by INTEGRAL (Gotz et al. 2010, GCN 11396)
The GBM on-ground location is consistent with the INTEGRAL position.

The GBM lightcurve consists of a single bright pulse at trigger time
preceded by a smaller pulse ~6 s before trigger time with a total duration
(T90) of about 9.2 s (50-300 keV). The time-averaged spectrum from T0-6.1 s
to T0+4.1 s is best fit by a Band function with Epeak = 105.8 +/- 26.0 keV, 
alpha = -0.79 +/- 0.24, and beta = -2.02 +/- 0.15 (Castor C-Stat 420.5 for 
359 d.o.f.).

The event fluence (8-1000 keV) in this time interval is 
(2.96 +/- 0.21)E-6 erg/cm^2. The 1-sec peak photon flux 
measured starting from T0+0.13 s in the 8-1000 keV band 
is 8.08 +/- 0.41 ph/s/cm^2.

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


GRB_name: GRB101112A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11404
SUBJECT: Possible detection of INTEGRAL burst GRB 101112A by the EVLA
DATE:    10/11/14 01:52:45 GMT
FROM:    Poonam Chandra at Royal Mil. College Canada  <Poonam.Chandra@rmc.ca>

"Poonam Chandra (RMC), Dale A. Frail (NRAO) and S. Bradley Cenko (Berkeley) report on behalf of a larger collaboration:

We
 observed the INTEGRAL long burst GRB 101112A (Gotz et al. GCN 11396) 
with the Expanded Very Large Array (EVLA) in 33.56 GHz frequency on 2010
 November 13 starting at 01:11:17 UT, around 3 hours after the detection of the 
GRB. We have a
 possible detection of the radio afterglow within the Liverpool 
telescope optical error circle (Guidorzi et al. GCN 11397) with a flux 
density of 149+/54 uJy. The peak flux position of the radio afterglow is
 J2000: RA 19:28:54.88, Dec 39:21:10.81. 

Note that this is the fastest response of a GRB alert by the EVLA which is currently in the commissioning phase. We thank the EVLA staff for scheduling our observations so promptly. The 
National Radio Astronomy Observatory is a facility of the National Science
 Foundation operated under cooperative agreement by Associated Universities,
 Inc."


GRB_name: GRB101114A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11405
SUBJECT: GRB 101114A, Swift-BAT GRB detected by ground processing
DATE:    10/11/15 00:08:33 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Based on the ground data processing, we found the GRB 101114A (trigger=438392) 
at T0=00:32:50 UT.  The BAT onboard analysis of the trigger was prematurely 
terminated by a slew to a different target.  We have only limited event-by-event 
data on the ground for this trigger.

Using the data set from T0 to T0+4.1 sec,  the BAT ground-calculated position 
in the 15-200 keV band is RA, Dec = 303.193, 14.029 deg which is 
   RA(J2000)  =  20h 12m 46.3s 
   Dec(J2000) = +14d 01' 44.4" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The image significance is 13.6 sigma.  The partial coding was 30%.  
 
The mask-weighted light curve shows a sigle FRED-like spike starting before 
T0, peaking at T0+2 sec and ending after T0+10sec.  Because of the incomplete data 
(the event data are only available from T0 to T0+10 sec), we can only state 
that the duration of the burst is >10 sec.  

The time-averaged spectrum from T0 to T0+10 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.29 +- 0.17.  The fluence in the 15-150 keV band is 8.0 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+2.00 sec in the 15-150 keV band
is 1.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
A Swift TOO is being done to get an XRT position.


GRB_name: GRB101114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11406
SUBJECT: GRB 101114A: Swift-XRT candidate afterglow detection and analysis
DATE:    10/11/15 09:30:57 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have analysed 7.9 ks of XRT data for GRB 101114A (Sakamoto et al. et
al. GCN Circ. 11405), from 73.3 ks to 91.1 ks after the BAT trigger.
The data are entirely in Photon Counting (PC) mode. An uncatalogued
X-ray source is detected inside the BAT error circle; the source shows
weak (~1-sigma) evidence of fading in this observation. Using 1631 s of
PC mode data and 1 UVOT image, we find an enhanced XRT position (using
the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 303.21110, +14.03270 which is equivalent to:

RA (J2000): 20h 12m 50.67s
Dec(J2000): +14d 01' 57.6"

with an uncertainty of 2.8 arcsec (radius, 90% confidence). This is 64
arcsec from the BAT position of Sakamoto et al. (GCN Circ. 11405)

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+1.1, -0.6). The
best-fitting absorption column is 1.6 (+2.5, -0.3) x 10^21 cm^-2,
consistent with the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.7 x 10^-11 (5.5 x 10^-11) erg
cm^-2 count^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020150.

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


GRB_name: GRB101114A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11408
SUBJECT: Konus-Wind observation of GRB 101114A
DATE:    10/11/16 10:49:16 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long GRB 101114A discovered in BAT ground analysis (Sakamoto et al., 
GCN 11405) was detected by Konus-Wind in the waiting mode.

The burst light curve shows a rather bright pulse at ~T0(BAT) preceded 
by two weak pulses at ~T0(BAT)-100 s and ~T0(BAT)-50 s. The total burst 
duration is ~110 s.

As observed by Konus-Wind, the burst had a fluence of (4.7 +/- 
2.4)x10^-6 erg/cm2 (in the 20 - 1200 keV energy range).

Modeling the K-W 3-channel spectrum of the main pulse (accumulated from 
T0-2.2 s to T0+6.6 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.15 +/- 0.29, Ep = 296 +/- 129 keV.

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB101114A/


GRB_name: GRB101114A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11409
SUBJECT: GRB 101114A: GROND Upper limits
DATE:    10/11/16 20:25:59 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

GRB 101114A: GROND Upper limits

J. Elliott, R. Filgas and J. Greiner (all MPE Garching) report on behalf
of the GROND team:

We observed the field of GRB 101114A (Swift trigger 438392; Sakamoto et
al., GCN #11405) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla
Observatory (Chile).

Observations started at 00:42 UT in twilight and just before reaching the
20 deg above horizon telescope limit, on November 16, 48 hours after the
GRB trigger, and have total exposure of 425 s in g'r'i'z' and 720 s in JHK.
They were performed at an average seeing of 2.5" and at an average airmass
of 2.7.

We do not detect a source within the Swift-XRT error circle reported by
Evans (GCN #11406) down to the following 3 sigma upper limits (all in AB):

g' > 21.8,

r' > 22.1,

i' > 21.7,

z' > 21.5,

J > 20.3,

H > 19.8 and

K > 19.2

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)= 0.19 in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB101117B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11411
SUBJECT: GRB 101117B: Swift detection of a burst
DATE:    10/11/17 19:27:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. W. Wolf (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. Campana (INAF-OAB), N. Gehrels (NASA/GSFC), D. Grupe (PSU),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), W.B Landsman (GSFC),
V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC) and
P. T. O'Brien (U Leicester) report on behalf of the Swift Team:

At 19:13:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101117B (trigger=438675).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 172.909, -72.662 which is 
   RA(J2000) = 11h 31m 38s
   Dec(J2000) = -72d 39' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a two-spike
structure with a duration of about 6 sec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 19:14:40.9 UT, 77.0 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 173.00251, -72.66317 which
is equivalent to:
   RA(J2000)  = 11h 32m 0.60s
   Dec(J2000) = -72d 39' 47.4"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 100 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.33 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.2
(+2.09/-1.81) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the white
filter  starting  82 seconds after the BAT trigger.  No credible
afterglow candidate  has been found in the initial data products.  The
2.7' x 2.7' sub-image covers 100%  of the XRT error circle.  The
estimated 3-sigma upper limit is white > 20.4 mag.  No correction has
been made for the expected Galactic extinction corresponding to a 
reddening of E_{B-V} =  0.38 mag.  Photometry is on the UVOT
photometry system of Poole et al. (2008). 

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


GRB_name: GRB101117B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11412
SUBJECT: GRB 101117B: Swift/UVOT Discovery of an Optical Afterglow 
DATE:    10/11/17 19:42:13 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

Stephen Holland (CRESST/USRA/GSFC) reports,
on behalf of the UVOT Team

     The Swift/UVOT source list has an uncatalogued source at the location of
the XRT afterglow (Wolf et al. 2010, GCNC 1141).  Preliminary photometry
indicates an approximate white magnitude of 18.2.


GRB_name: GRB101117B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11413
SUBJECT: GRB 101117B: Enhanced Swift-XRT position
DATE:    10/11/17 23:59:36 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 1061 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 101117B, 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 = 173.00136, -72.66293 which is equivalent
to:

RA (J2000): 11h 32m 0.33s
Dec (J2000): -72d 39' 46.5"

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

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

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


GRB_name: GRB101117B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11414
SUBJECT: GRB 101117B: Swift-BAT refined analysis
DATE:    10/11/18 00:14:30 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), J. Tueller (GSFC),
T. N. Ukwatta (GWU), C. W. Wolf (PSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 101117B (trigger #438675)
(Wolf, et al., GCN Circ. 11411).  The BAT ground-calculated position is
RA, Dec = 172.991, -72.651 deg which is 
   RA(J2000)  =  11h 31m 57.8s 
   Dec(J2000) = -72d 39' 04.7" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.
 
The mask-weighted light curve shows two overlapping peaks starting
at ~T-0.2 sec, peaking at ~T+1.0 sec, and roughly exponentially decaying
out to ~T+40 sec.  There is possible emission (at the 2-sigma c.l.)
from around T+150 to T+220 sec.  T90 (15-350 keV) is 5.2 +- 1.8 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.1 to T+8.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.50 +- 0.09.  The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.74 sec in the 15-150 keV band
is 4.5 +- 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/438675/BA/

This burst was called the "B" burst to avoid possible confusion with the
earlier published XRF 101117A event by the MAXI team (GCN Circ 11410).


GRB_name: GRB101114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11415
SUBJECT: GRB 101114A: Confirmation of the X-ray afterglow
DATE:    10/11/18 14:46:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

We have performed a second epoch observation with Swift-XRT of GRB
101114A (Sakamoto et al., GCN Circ. 11405). This observation was 5.5 ks
in length, beginning 3.5 days after the GRB trigger. The source reported
by Evans et al. (GCN Circ. 11406) is still detected, but has faded
significantly to a level of 1.6 (+/- 0.9) x 10^-3 ct/sec. We thus
confirm that this is the afterglow of GRB 101114A.

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


GRB_name: GRB101114A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11416
SUBJECT: GRB101114A: Swift/UVOT Upper Limits
DATE:    10/11/18 21:46:25 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W. Landsman (GSFC/Adnet) and T. Sakamoto (GSFC/UMBC) report on behalf of 
the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 101114A  
20.3 hrs after the BAT trigger (Sakamoto et al., GCN 11405). We do not 
detect any source at the enhanced Swift XRT position (Evans  GCN 11406, 
11415).  UVOT magnitude 3-sigma upper limits are reported in the 
following table:

Filter  T_start  T_stop  Exp(s)  Mag (3-sigma upper limit)
-------------------------------------------------------------
white     74084    86413   2325 > 21.9
v         74901    87330   2567 > 20.5
u         73267    91074   2822 > 21.0

The quoted upper limits have not been corrected for the expected 
Galactic extinction along the line of sight of E_(B-V) = 0.19 (Schlegel
et al. 1998).    All photometry is on the UVOT photometric system 
described  in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB101117B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11417
SUBJECT: GRB 101117B: Swift-XRT refined analysis
DATE:    10/11/18 23:02:04 GMT
FROM:    Chris Wolf at PSU  <cwolf@astro.psu.edu>

C. A. Wolf (PSU) and D. Grupe (PSU) report on behalf of the Swift-XRT team:

We have analyzed 15.7 ks of XRT data for GRB 101117B (Wolf et al. GCN Circ.
11411), from 86 s to 63.0 ks after the BAT trigger. The data are entirely
in Photon Counting (PC) mode.

The light curve can be modeled with an initial power-law decay with an
index of alpha=0.76 (+0.08, -0.09), followed by a break at T+1239 s to an
alpha of 1.26 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.23 (+/-0.11). The best-fitting
absorption column is 3.18 (+/-0.43) x 10^21 cm^-2, in excess of the
Galactic value of 1.33 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 5.7 x 10^-11 (10.5 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of 1.26,
the count rate at T+24 hours will be 2.19 x 10^-3 count s^-1, corresponding
to an observed (unabsorbed) 0.3-10 keV flux of 1.25 x 10^-13 (2.30 x
10^-13) erg cm^-2 s^-1. The count rate at T+48 hours will be 0.89 x 10^-3
count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of
5.07 x 10^-14 (9.35 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/00438675.

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


GRB_name: GRB101112A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11419
SUBJECT: GRB 101112A: OSN and BTA observations
DATE:    10/11/19 09:00:43 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

T. A. Fatkhullin, V. N. Komarova, V.V. Sokolov, A.S. Moskvitin 
(SAO-RAS), J. Gorosabel, A. Sota and A.J. Castro-Tirado (IAA-CSIC),  A. 
de Ugarte Postigo (DARK/NBI), on behalf of a larger collaboration, report:

"Following the detection of the optical afterglow to the INTEGRAL GRB 
101112A (Gotz et al., GCNC 11396), we have undertaken observations of
the region with the 1.5-m telescope at Sierra Nevada Obs. (Spain) on Nov 
13 and with the 6.0-m BTA at SAO-RAS in Zelenchukskaia (Russia) on Nov 
14 and Nov 15. At the location of the optical afterglow (Guidorzi et 
 al., GCNC 11397, de Ugarte Postigo et al., GCNC 11398) a faint source 
with R-band magnitude about 23 was detected on Nov 14.766 UT, which was 
below the detection limit on Nov 15.838 UT. This value should be 
compared with R = 15.6, as derived from the BOOTES-2/TELMA early time 
images on Nov 12.9260 UT (a value that supersedes the one given on GCNC 
11398 which was based on a wrong photometric calibration). The fact that 
the optical counterpart is blended (1."2) with a brighter star (with R 
about 18) has made useless the attempted spectroscopy on Nov 14.8 UT."

This message can be quoted.


GRB_name: GRB101117B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11420
SUBJECT: GRB 101117B: Swift/UVOT Observations of the Optical Afterglow
DATE:    10/11/22 15:25:34 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <Stephen.T.Holland@nasa.gov>

S. T. Holland (CRESST/GSFC/USRA) and
C. W. Wolf (PSU)
report on the behalf of the Swift UVOT team:

      The Swift/UVOT observed the field of GRB 101117B starting 63 s
after the BAT trigger (Wolf, et al., 2010, GCN Circ. 11411).  Settled
observations started at 82 s.  We detect the optical afterglow
(Holland, 2010, GCN Circ. 11412) in the U, B, and white filters.  The
refined UVOT position is


     RA (J2000)  11:32:00.54  =  173.00225 (deg)
    Dec (J2000) -72:39:45.9   =  -72.66275 (deg)

with an estimated uncertainty of 0.43 arcsec (radius, 90% confidence,
statistical + systematic).  This is 1.16 arcsec northwest of the
UVOT-enhanced XRT position (Goad, et al., 2010, GCN Circ. 11413).

     Preliminary magnitudes, and 3-sigma upper limits for detecting a
source in the finding charts and in the co-added images, are

Filter      T_start   T_stop    Exp(s)      Mag   Err
-----------------------------------------------------------
white (fc)       82      232       147     17.81 0.08 
    u (fc)      295      545       246     18.68 0.15

    v           626      646        20    >17.9
    b           551      571        20     18.22 0.27
    u           700     1325        59    >19.1
 uvw1           675     1300        78    >19.3
 uvm2           825     1275        58    >18.7   
 uvw2           601     1051        58    >19.0
white           575      595        20     19.20 0.34
-----------------------------------------------------------

     The quoted magnitudes and upper limits have not been corrected
for the expected Galactic extinction along the line of sight
corresponding to a reddening of E_{B-V} = 0.38 mag (Schlegel, et al.,
1998, ApJS, 500, 525).  All photometry is on the UVOT photometry
system described in Poole et al. (2008, MNRAS, 383, 627).

     The non-detection in the UVOT uvw1 filter, and the observed UVOT
spectral energy distribution at 600 s, is consistent with GRB 101117B
having a redshift of approximately z <= 3, although we can not rule
out the non-detection in the ultraviolet being due to extinction in
the host galaxy.  The white light curve exhibits a power-law decay
with an index of alpha = -0.8 +/- 0.1 between 82 and 6005 s after the
BAT trigger.


GRB_name: GRB101117B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11421
SUBJECT: GRB 101117B: GROND Upper limits
DATE:    10/11/22 19:05:49 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

J. Elliott, R. Filgas, J. Greiner, P. Schady and T. Kruehler (all MPE
Garching) report
on behalf of the GROND team:

We observed the field of GRB 101117B (Swift trigger 438675; Wolf et al.,
GCN #11411) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla
Observatory (Chile).

Observations started at 05:15 UT on November 19, 34 hours after the GRB
trigger, and have total exposure of 6003 s in g'r'i'z' and  4800 s in JHK.
They were performed at an average seeing of 2.0" and at an average airmass
of 1.8.

We do not detect a source within the UVOT error circle reported by Holland
& Wolf (GCN #11420) down to the following 3 sigma upper limits (all in
AB):

g' > 23.7

r' > 23.8

i' > 23.5

z' > 23.3

J > 21.7,

H > 21.2 and

K > 20.4

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)= 0.38 in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB101024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11422
SUBJECT: Optical observation of GRB 101024A
DATE:    10/11/23 01:47:10 GMT
FROM:    AAVSO GRB Network at AAVSO  <matthewt@aavso.org>

Chris Stockdale (Churchill, Victoria, Australia) reports to the AAVSO
International High Energy Network the following optical observation of
GRB 101024 (GCN #11370, De Pasquale et al.):

Chris Stockdale reports a detection of the optical afterglow of GRB 
101024 (GCN #11370, De Pasquale et al.; #11371, De Pasquale et al.;
#11373, Hentunen et al.; #11382, Laas-Bourez et al.; #11383 Kruehler et 
al.), detecting the afterglow at the same position as the Swift UVOT 
position. The afterglow was observed unfiltered for 24 minutes beginning 
at 12:42:07 UT on 2010 October 24.  Thirteen exposures of 24 minutes 
were taken for the detection; a median combination of images 2 through 
13 having a midpoint time of 12:54:25 UT on 2010 October 24 yields a CR 
magnitude of 19.3 with calculated S/N of 5.5; the magnitude was measured 
relative to the R-band catalog magnitude of USNO-B1.0 0127-0023867 
(R=15.7).  Observations were made using an SBIG ST-7XME CCD camera 
attached to a 280 mm Schmidt-Cassegrain.  The position of the afterglow 
was imaged for an additional 60 minutes subsequent to these frames, but 
the source was not detected.

The AAVSO High Energy Network was made possible through grants from the
Charles Curry Foundation and NASA.


GRB_name: GRB101123A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11423
SUBJECT: GRB 101123A: Fermi GBM detection
DATE:    10/11/25 01:16:48 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

Sylvain Guiriec (UAH)
reports on behalf of the Fermi GBM Team:

At 22:51:34.97  UT on 23 November 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101123A (trigger 312245496 / 101123952).

The on-ground calculated location, using the GBM trigger
data, is RA = 131.24, DEC = 6.51 (J2000 degrees,
equivalent to 08 h 54 m 27 s,  06 d 30 ' 36 ''), 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 is 86 degrees.

GBM triggered on a weak pulse followed by three separate emission periods
with a total duration (T90) of about 105 s (50-300 keV).
The time-averaged spectrum of the brightest part of the burst from T0+42 s
 to T+57 s is adequately fit by a Band function with Epeak = 476 +/- 11 keV,
alpha = -0.75 +/- 0.01, and beta = -2.14 +/- 0.03.

The event fluence (10-1000 keV) over the T90 duration is
(1.283 +/- 0.006)E-4 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+51.7 s in the 8-1000 keV band is 49 +/- 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: GRB101123A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11424
SUBJECT: IPN triangulation of bright GRB 101123A
DATE:    10/11/26 20:06:14 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

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

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team,

E. Del Monte, E. Costa, I. Donnarumma, Y. Evangelista, M. Feroci,
I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta,
on behalf the SuperAGILE team,

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

and

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

Fermi (GBM), INTEGRAL (SPI-ACS), AGILE (MiniCalorimeter and
SuperAGILE), Swift (BAT), Konus-Wind, MESSENGER (GRNS), and Mars Odyssey 
(HEND) observed the bright GRB 101123A at about 22:52:14 UT (the 
Fermi/GBM trigger 312245496: Guiriec, GCN 11423). The burst was outside 
the coded fields of view of the BAT and SuperAGILE.

We have triangulated this burst to the following 3 sigma error box:
-----------------------------------------------
     RA(2000), deg              Dec(2000), deg
-----------------------------------------------
Center:
  131.381 (08h 45m 32s)   + 5.563 (+05d 33' 47")
Corners:
  130.942 (08h 43m 46s)   + 4.586 (+04d 35' 11")
  131.755 (08h 47m 01s)   + 6.277 (+06d 16' 35")
  131.827 (08h 47m 18s)   + 6.584 (+06d 35' 02")
  131.011 (08h 44m 03s)   + 4.873 (+04d 52' 23")
-----------------------------------------------

The error box area is 433 sq. arcmin.
The maximum distance between the box corners is 2.2 deg.
This error box may be improved.

A map is posted at http://ssl.berkeley.edu/ipn3/101123A
showing the GBM best-fit position (blue star), and the IPN annuli (solid
lines with centers dot-dashed).


GRB_name: GRB101123A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11425
SUBJECT: Konus-Wind observation of GRB 101123A
DATE:    10/11/27 11:10:20 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 bright GRB 101123A (Fermi/GBM
trigger 312245496 / 101123952: Guiriec, GCN 11423;
localized by IPN: Hurley et al., GCN 11424)
triggered Konus-Wind at T0=82338.387s UT (22:52:18.387)

The burst light curve contains three main bursting
episodes with a total duration of ~120 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/GRB101123_T82338/

As observed by Konus-Wind the burst
had a fluence of (2.5  0.3)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+9.984s,
of (1.9  0.3)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+118.272 s) is best fit
in the 20 keV - 10 MeV range by the GRB (Band) model,
for which:
the low-energy photon index alpha = -0.9 (+/-0.1),
the high energy photon index beta = -2.1 (-0.2, +0.1),
the peak energy Ep = 449(-66, +83)keV (chi2 = 100/84 dof).

The spectrum at the maximum count rate
(measured from T0+9.984 to T0+11.776 s) is best fit
in the 20 keV - 10 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.81(+/-0.08),
and Ep = 574(-52, +60) keV (chi2 = 69/62 dof).
Fitting this spectrum by the GRB (Band) model
yields to the same values of alpha and Ep, with
only an upper limit for beta (< -3.3)

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


GRB_name: GRB101123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11426
SUBJECT: GRB 101123A: MASTER prompt optical observations 
DATE:    10/11/27 15:55:17 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru, 2x400 
mm, 2x4 square degrees)  located at 
Kislovodsk and 6 very wide field cameras (420 square degrees)was pointed 
to the long bright  GRB101123A (Fermi/GBM trigger 312245496 / 101123952: 
Guiriec, GCN 11423; localized by IPN: Hurley et al., GCN 11424) 23 
sec after  notice time and 39 sec  after trigger under Moon light 
with some haze.

After some repointing and imaging due to  continuously
  updating GRB socket position 
robotic telescope was made several frames at IPN error box (Hurley et 
al., GCN 11424).

The first 2 telescope images (20 sec exp. time) covered 90%  IPN error 
box was maded 111 sec after GRB.

The 3-sigma upper limit has been about 15.0 (telescopes) and 10.0 (wide 
field cameras).
There is no OT brighter 10 mag on Very Wide Field Cameras.
Robot find two merginally OT candidates on telescope images:

OT   Date        Time       Ra             Dec           Mag(R)
1. 2010-11-23 22:53:25 08h 45m 06.61s , +05d 14m 47s.1   14.3
2. 2010-11-23 22:55:28 08h 45m 52.58s , +05d 48m 00s.4   13.2

However both transients are visible only on single image.
The images, OT candidates and map of the error boxes position  are 
available at 
http://observ.pereplet.ru/images/GRB101123A/grb.html  .

The message may be cited.

mailto: lipunov@sai.msu.ru


GRB_name: GRB101123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11427
SUBJECT: GRB 101123A: ROTSE optical observations
DATE:    10/11/29 23:41:57 GMT
FROM:    W.K. Zheng at NAOC  <zwk@bao.ac.cn>

W. Zheng, S. B. Pandey and C. Akerlof (U Mich), report on behalf of
the ROTSE collaboration:

ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia,
responded to GRB 101123A (Fermi/GBM trigger 312245496 / 101123952: 
Guiriec, GCN 11423; localized by IPN: Hurley et al., GCN 11424)
107s after the burst. Observation was performed in 2x2 tiling mode,
covered totally ~3.6x3.6 square degrees around the center of GBM
trigger. Observation lasted for ~1.3 hours with 20s exposure time
for each image.

The location of the two OT candidates reported by Gorbovskoy et al.
(GCN 11426) were both covered by ROTSE images.
For candidate 1, the first ROTSE image was started at
2010-11-23 22:54:50.91, 196s after the burst.
For candidate 2, the first ROTSE image was started at
2010-11-23 22:53:51.31, 136s after the burst.

We do not detected any point source at either of the two candidate
locations in the single or the co-added images. The limiting
magnitude is ~16.0 mag for single image and ~16.7 mag for co-added
images.


GRB_name: GRB101201A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11429
SUBJECT: GRB 101201A detected in ground analysis of BAT data
DATE:    10/12/02 00:05:45 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

GRB 101201A detected in ground analysis of BAT data

J. R. Cummings (GSFC/UMBC/CRESST), H. A. Krimm (GSFC/USRA/CRESST),
D. M. Palmer (LANL), S. D. Barthelmy (GSFC)
on behalf of the Swift-BAT team

At 10:01:48, Swift-BAT detected GRB 101201A (BAT triggers 439595-6, Fermi GBM
312890511). There was no source found onboard. A strong source was found in
ground analysis at RA, Dec 1.955, -16.196, which is:

RA (J2000)    00h 07m 49s
Dec (J2000)  -16d 11m 46s

with an estimated uncertainty radius of 2 arcmin (90% containment). This point
is 1.8 degrees from the GBM position, within the GBM error circle. It was
about 3% coded.

The burst was about 50 seconds long, with 3 overlapping peaks.  The available
BAT event-by-event data covers most of the second peak.

A Swift TOO for XRT follow-up is in progress.


GRB_name: GRB101201A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11430
SUBJECT: GRB 101201A: GROND Detection of the Optical/NIR Afterglow
DATE:    10/12/02 02:49:33 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

A. Nicuesa Guelbenzu, (Tautenburg Obs.), P.Schady and J.Greiner (MPE  
Garching) report on behalf of the GROND team:

We observed the field of GRB 101201A (Swift trigger 439595-6, Fermi  
GBM 312890511; Cummings et al., GCN #11429) simultaneously in  
g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at  
the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile).

Observations started during twilight, at 00:36 UT on 2010-12-02, 14.6  
hours after the GRB trigger, and are continuing. They were performed  
at an average seeing of better than 0.8" and at an average airmass of 1.

We found a bright, uncatalogued point source within the 2 arcmin Swift- 
BAT error circle at

RA (J2000) = 00:07:52.19 s

DEC (J2000) = -16:11: 05.42

with an uncertainty of 0.5" in each coordinate.

The source is detected in all optical and NIR GROND filters and had a  
preliminary AB magnitude or r' = 19.67+/-0.01 10 mins after the start  
of our observations. The source faded by ~0.3 magnitudes within the  
first 1.5 hours of GROND observations, leading us to conclude that  
this is the afterglow of GRB101201A.

The detection of the source in the reddest GROND filter puts an upper  
limit on the redshift of this GRB of z < ~3. Given magnitudes are  
calibrated against USNO zeropoints and are not corrected for the  
expected Galactic foreground extinction corresponding to a reddening  
of E_(B-V)=0.02 mag in the direction of the burst (Schlegel et al.  
1998).


GRB_name: GRB101201A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11431
SUBJECT: GRB 101201A: Swift/UVOT Detection
DATE:    10/12/02 05:00:45 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU) and V. Magnano (INAF-IASFPA) report on behalf of
the Swift/UVOT team:

The Swift/UVOT began observations of the field of GRB101201A
approximately 14 hours after the BAT detection (GCN Circ. 11429).
We confirm the uncataloged source reported Guelbenzu et al.
(GCN Circ. 11430).  We also find evidence of fading between
the two orbits.  Magnitudes for the first and second orbit exposures
are listed below.

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

white            52065        52087           21         19.90+-0.49
white            57847        58387          531         20.01+-0.11
u                51218        52058          827         19.50+-0.17
u                57000        57840          826         20.01+-0.26

The above magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E_{B-V} = 0.02 (Schlegel et al.,
1998, ApJS, 500, 525). The photometry is on the UVOT photometric
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB101201A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11433
SUBJECT: GRB 101201A: Swift-XRT refined Analysis
DATE:    10/12/02 15:51:21 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

V. Mangano (INAF/IASF Pa), B. Sbarufatti (INAF/OAB - IASF Pa) report on
behalf of the Swift-XRT team:

We have analysed 4.9 ks of XRT data for GRB 101201A (Cummings  et al.
GCN Circ. 11429), from 51.2 ks to 69.7 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. Using 3879 s of PC mode
data and 3 UVOT images, we find an enhanced XRT position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 1.96750, -16.18540 which is equivalent to:

RA (J2000): 00h 07m 52.21s
Dec(J2000): -16d 11' 07.4"

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=3.80 (+0.03, -1.25).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.4 (+0.7, -0.6). The
best-fitting absorption column is  8 (+14, -6) x 10^20 cm^-2,
consistent with the Galactic value of 2.2 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.2 x 10^-11 (4.6 x
10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:        8 (+14, -6) x 10^20 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:        2.4 (+0.7, -0.6)

If the light curve continues to decay with a power-law decay index of
3.80, the count rate at T+24 hours will be 4.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x
10^-13 (2.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020152.

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


GRB_name: GRB101201A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11434
SUBJECT: GRB 101201A: Fermi GBM observation
DATE:    10/12/02 16:38:38 GMT
FROM:    Suzanne Foley at MPE  <sfoley@mpe.mpg.de>

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

"At 10:01:49.74 UT on 01 Dec 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101201A (trigger 312890511 / 101201418)
which was also detected by the SWIFT-BAT
(Cummings et al. 2010, GCN 11429).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 74 degrees.

The GBM light curve consists of 3 main pulses
with a duration (T90) of about 79 (+/-11) s (50-300 keV).
The time-averaged spectrum from T0+2.048 s to T0+81.922 s is
well fit by a power law function with an exponential
high energy cutoff.  The power law index is -1.50 (+/-0.03) and
the cutoff energy, parameterized as Epeak, is 275.70 (+37.20/-27.80) keV
(CSTAT 1263.1 for 480 d.o.f.).

The event fluence (10-1000 keV) over the T90 duration is
(2.41 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+31.74 s in the 10-1000 keV band
is 6.7 +/- 0.2 ph/s/cm^2.


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


GRB_name: GRB101030A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11435
SUBJECT: GRB101030A
DATE:    10/12/02 21:20:39 GMT
FROM:    Valentyna Golovnya at Main Astro Obs,Kyiv  <golov_v@ukr.ne>

GRB 101030A, the review of the sky area in plate archives
V.V. Golovnya, L.K. Pakuliak (Main Astro Obs, Kyiv)
report:

We have undertaken the review of the sky area of GRB 101030A (Evans et
al., GCN 11387) on astronegatives, collected in Ukrainian NAS Main
astronomical observatory plate archive (1976-1996). All the plates with 
the possible object appearance are digitized using Microtek ScanMaker
9800XL TMA flatbed scanner and have been placed into Golosiiv Plate 
Archive database DBGPA with open access to them.

The list of plates is given in the table:
YYYYMMDD   UT       Plates/Films  Exp.  LimMag            
19860501  19:23:22  GUA040C002903 30.0  12.25
19860501  19:23:27  GUA040D002904 11.9  13.15
19860503  00:29:45  QUI021B000206 10.1  12.15
19860503  00:48:10  QUI021B000208 10.1  12.15

Plates/Films:  
GUA040C the plates archive identifier of DWA (D/F=400/2000,M=103"/mm)
GUA040D   of the Ukrainian NAS Main astronomical observatory in Kyiv
          (Marsden's number - 83) the plate number [1].
QUI021B -the films archive identifier of AFU-75 (D/F=210/740,M=280"/mm) 
          of the Quito Astro. Obs. in Ecuador
         (Marsden's number - 781) the plate number [1].
Exp.  -   Duration of the maximum exposures (minutes).
LimMag -  Limited mag, derived in the 50 minutes area around the 
          location given in Evans et al., GCN 11387:
          RA (J2000): 11h 05m 31.68s, Dec (J2000): -16d 22' 41.2".

The preview images of 4 areas together with the 8 min.of arc area from 
SkyMap can be found in http://gua.db.ukr-vo.org/img/grb/101030A/index.
The images with full resolution are available via e-mail on demand.

References:
1.L.Pakuliak DATABASE of GOLOSIIV PLATE ARCHIVE (DBGPA V2.0),
http://gua.db.ukr-vo.org/


GRB_name: GRB101129A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11436
SUBJECT: GRB 101129A SHB found by IPN and in ground analysis of BAT data
DATE:    10/12/03 02:36:37 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC/CRESST), D. M. Palmer (LANL),
S. D. Barthelmy (GSFC), and T. Sakamoto (GSFC/UMBC/CRESST) on
behalf of the BAT team,

Valentin Pal'shin (Ioffe Inst) and K. Hurley (UCB) on behalf of
the IPN,

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

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team,

A. P. Beardmore (U Leicester) and J. A. Kennea (PSU) on behalf of
the Swift-XRT 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,

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


At 15:39:31 UTC, Swift-BAT detected a rate increase due to GRB 101129A
(BAT trigger #439471. Only a sub-threshold image source was found
onboard.  This event corresponds to Fermi GBM trigger #312737973. The
IPN was alerted.  In ground analysis, the source was detected with
slightly greater confidence at RA, Dec 155.921, -17.645 which is:

RA (J2000)       10h 23m 41s
Dec (J2000)    -17d 38m 42s

with an estimated uncertainty radius of 3 arcmin (90% containment).
Correlation of Swift-BAT counting rates and SPI-ACS counting rates,
and SPI-ACS with Messenger yielded intersecting annuli consistent with
this position. The burst was also detected by Suzaku-WAM.

As seen in BAT, the burst consisted of a single pulse with a T90 of about
0.35 +- 0.05 sec.

The burst was faint and short. The low-number statistics in BAT make a
fit to the spectrum very uncertain. The photon index was approximately
0.8 +- 0.5.  The fluence was approximately (9 +- 5) x 10^-08 ergs/cm^2.

A Swift TOO observation was executed at 11 hours after the burst.  The
location of the burst was observed by the Swift-XRT and Swift-UVOT for
a total of about 1400 seconds.  No afterglow was detected.  No further
observations are planned.


GRB_name: GRB101130A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11437
SUBJECT: IPN Localization of GRB101130 (possible short duration burst)
DATE:    10/12/03 21:32:42 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

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

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

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

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

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

Konus-Wind, MESSENGER GRNS, and Mars Odyssey HEND observed this
burst at 34766 s on November 30, 2010.  As seen by Konus-Wind, the 
time history displayed a short (~1.5 s long) pulse, and a weak 
pulse at ~T0+50 s (with a duration of ~6 s). There is evidence
for this second pulse in the MESSENGER data at the same time after 
the main pulse, confirming their common origin.

We have localized it to a preliminary, 3 sigma error box whose 
coordinates are

          RA(2000)     Dec(2000)
CENTER:     61.803o=04 h 07 m 12.73 s    -16.759o=-16 o 45 '  33.09 "
CORNERS:    62.468o=04 h 09 m 52.39 s    -17.210o=-17 o 12 '  34.62 "   
            62.953o=04 h 11 m 48.62 s    -17.213o=-17 o 12 '  45.80 "      
            60.654o=04 h 02 m 37.06 s    -16.270o=-16 o 16 '  11.27 "    
            61.144o=04 h 04 m 34.57 s    -16.297o=-16 o 17 '  48.56 "

The error box area is ~1500 sq. arcmin.  This error box may be improved.
Time history and spectral information will be reported in a forthcoming
GCN Circular.


GRB_name: GRB101029A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11438
SUBJECT: Konus-Wind observation of GRB 101029A
DATE:    10/12/05 16:51:55 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 GRB 101129A
(localized by BAT and IPN: Cummings  et al. GCN 11436)
triggered Konus-Wind at T0=56370.759s UT (15:39:30.759)

The burst light curve consists of a single pulse
with a total duration of ~0.4 s.
The emission is seen up to 5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101129_T56370/

As observed by Konus-Wind the burst
had a fluence of 3.5(+1.4/-1.1)x10-6 erg/cm2,
and a 16-ms peak flux measured from T0-0.096s
of 1.7(+0.7/-0.5)x10-5 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+0.128 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.4 (-0.4, +0.5),
and Ep = 1210(-400, +680) keV (chi2 = 8.1/12 dof).

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


GRB_name: GRB101129A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11439
SUBJECT: Konus-Wind observation of GRB 101129A
DATE:    10/12/05 16:58:13 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short hard GRB 101129A
(localized by BAT and IPN: Cummings  et al. GCN 11436)
triggered Konus-Wind at T0=56370.759s UT (15:39:30.759)

The burst light curve consists of a single pulse
with a total duration of ~0.4 s.
The emission is seen up to 5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101129_T56370/

As observed by Konus-Wind the burst
had a fluence of 3.5(+1.4/-1.1)x10-6 erg/cm2,
and a 16-ms peak flux measured from T0-0.096s
of 1.7(+0.7/-0.5)x10-5 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+0.128 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.4 (-0.4, +0.5),
and Ep = 1210(-400, +680) keV (chi2 = 8.1/12 dof).

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

[GCN OPS NOTE(06dec10): Per authors's request, the author list was added.]


GRB_name: GRB101204A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11440
SUBJECT: GRB  101204A detected in ground analysis of BAT data
DATE:    10/12/06 02:55:20 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

At 23:53:29 UTC on December 4, 2010 Swift-BAT detected GRB 101204A (BAT
trigger # 439806).  No source was detected onboard. An automated script
on the ground detected a source at RA, Dec 167.548, -20.434, which is

RA (J2000)    11h 10m 11.6s
Dec (J2000)  -20d 26m 04s

The source was 3.5% coded.

As seen by BAT, the burst was a single gradual pulse about 10 seconds
long. In the 10-second interval for which we have detailed event data,
which covers almost all of the burst, the spectrum is best fitted by
a simple power law with a photon index of 1.3 +- 0.2.  The fluence from
15 to 150 keV was 1.2 +- 0.4 x 10^-6 erg/cm^2.  The spectrum may be
slightly distorted by edge of FOV effects, tending to reduce the number
of lower-energy photons detected relative to higher-energy photons.

A Swift TOO has been requested.


GRB_name: GRB101130A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11441
SUBJECT: Konus-Wind observation of GRB 101130A
DATE:    10/12/06 14:04:58 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:

GRB 101130A (localized by IPN: Hurley et al., GCN 11437)
triggered Konus-Wind at T0=34766.178s UT (09:39:26.178)

The burst light curve starts with a short (~1.5 s) pulse,
followed by a weaker pulse at ~T0+55 s (with a duration of ~6 s).
The emission is seen up to ~1 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101130_T34766/

As observed by Konus-Wind the burst
had a fluence of 3.1(+1.1/-1.0)x10-6 erg/cm2,
and a 16-ms peak flux measured from T0-0.048s
of 2.8(+0.8/-0.7)x10-6 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+65.792 s) is best fit
in the 20 keV - 1 MeV range by a simple power law model
with the index = -1.85 (-0.3, +0.35), chi2 = 44/48 dof.

The spectrum of the initial short pulse
(measured from T0 to T0+0.256 s) is best fit
in the 20 keV - 1 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.6 (-0.6, +0.9),
and Ep = 190(-55, +135) keV, chi2 = 26/18 dof.

The spectrum of the second pulse
(measured from T0+57.600 to T0+65.792 s) is best fit
in the 20 keV - 1 MeV range by a simple power law model
with the index = -2.1 (-0.5, +0.7), chi2 = 49/48 dof.


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


GRB_name: GRB101204A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11442
SUBJECT: GRB 101204A Swift-XRT/UVOT afterglow candidate
DATE:    10/12/06 19:22:04 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF-OAB/IASFPA), S. Oates (MSSL) report
on behalf of the Swift-XRT and Swift-UVOT teams

We have analysed 4.9 ks of XRT data for GRB 101204A (Cummings  et al. GCN
Circ. 11440), from 126.2 ks to 134.4 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. Using 4956 s of PC mode data
and 2 UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 167.53712, -20.41924 which is equivalent to:

RA (J2000): 11h 10m 08.91s
Dec(J2000): -20d 25' 09.2"

with an uncertainty of 2.3 arcsec (radius, 90% confidence). The source is
detected at a level of 2.0+/-0.2E-3 counts/s, corresponding to a  0.3-10
keV flux of 1.4E-12 erg cm-2 s-1. At this time we are not able to tell if
the source is fading.

The Swift/UVOT began settled observations of the field of GRB 101204A
126199 s after the BAT trigger (Cummings et al., GCN Circ. 11440). An
uncatalogued source is found at the UVOT position RA(J2000)=
167.53683 deg, DEC(J2000) = -20.42014, which is:

    RA (J2000) =   11:10:08.84
   Dec (J2000) = -20:25:12.5

with an estimated uncertainty of 0.6 arcsec (radius, 90% confidence). This
position is consistent with the XRT candidate position.

At this time we are not able to tell if this source is fading. Preliminary
magnitudes using the UVOT photometric system(Poole et al. 2008,
MNRAS, 383, 627) for the initial exposures are:

Filter  T_start(s)  T_stop(s)   Exp(s)       Mag
#####################################################
v       126194       127496     1281   20.28 +/- 0.24
v       131976       133278     1281   20.71 +/- 0.34
u       127505       128780     1255   19.79 +/- 0.13
u       133286       134378     1074   19.91 +/- 0.15
#####################################################

The values quoted above 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: GRB101129A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11443
SUBJECT: GRB 101129A : Suzaku WAM observation of the prompt emission
DATE:    10/12/07 01:13:09 GMT
FROM:    Norisuke Ohmori at Miyazaki U  <ohmori@astro.miyazaki-u.ac.jp>

N. Ohmori, A. Daikyuji, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka (Aoyama Gakuin U.), 
S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, 
T. Yasuda (Saitama U.),P. Tsai, Y. Urata, H.M. Lin (NCU), 
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), 
N. Vasquez (Tokyo Tech.), Y. E. Nakagawa, M. Serino, T. Tamagawa (RIKEN), 
K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.), 
on behalf of the Suzaku WAM team, report:


The short GRB 101129A (localized by Swift/BAT and IPN; Cummings et al., 
GCN11436) triggered the Suzaku Wide-band  All-sky Monitor (WAM) which 
covers an energy range of 50 keV - 5 MeV at 2010-11-29 15:39:31.92 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0+0.2s,
ending at T0+0.6s, with a duration (T90) of about 0.31 seconds. The fluence
in 100 - 1000 keV was 1.54 (-0.47, +0.12) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0s was 2.50 (-0.89, +0.30) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+1s is well fitted by a power-law with exponential cutoff model:
dN/dE =  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.43 (-0.62, +0.46), and
Epeak       1027 (-215, +292)  keV (chi^2/d.o.f. = 40.2/54).

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: GRB101204A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11444
SUBJECT: GRB 101204A Afterglow Candidate, VATT Observations
DATE:    10/12/07 03:48:56 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

P. Garnavich and J. Pagnini (Notre Dame) report:

We observed field of GRB 101204A beginning on Dec. 6.51 (UT) with
the Vatican Advanced Technology Telescope (VATT) and VATT4K CCD
camera. The imaging was centered on the original BAT position
(Cummings, GCN 11440) and were obtained 1.52 days after the burst.
Six R-band images were taken in poor conditions. The optical
afterglow candidate identified by Swift-UVOT (Sbarufatti et al., GCN
11442) is detected in the VATT images.

The deepest images centered on Dec. 6.521 give R=20.0+/-0.1 mag calibrated
from the USNO B1.0 star at 11:10:13.908 -20:26:07.8 with R2=17.74 mag.
The observations span less than 20 minutes so it is not possible to
determine if the source is fading.


GRB_name: GRB101204A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11445
SUBJECT: GRB101204A  GROND Detection of the Optical/NIR Afterglow
DATE:    10/12/07 21:22:30 GMT
FROM:    Robert Filgas at MPI  <filgas@mpe.mpg.de>

A. Nicuesa Guelbenzu (Tautenburg Obs.), R. Filgas, J. Greiner and P.
Schady (all MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 101204A (Swift trigger 439806; Cummings,
GCN #11440) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla
Observatory (Chile).

Observations started at 05:55 UT on December 7, 2.2 days after the GRB
trigger,and ended at 08:36 UT. They were performed at an average seeing of
1.2" and at an average airmass of 1.5.

We confirm the afterglow candidate reported by Sbarufatti et al.(GCN
#11442). After calibrating against the comparison star from Garnavich et
al.(GCN #11444), we find the afterglow candidate to have faded by at least
0.6 mag in the time between the VATT (Garnavich et al.) and GROND
observations. We also find the SED of this source to be well-fit by a
power-law, providing further evidence of this being the afterglow of
GRB101204A.

Based on the best 7.7 min of total exposures in g'r'i'z' and 8 min in
JHK taken at 08:18 UT, we estimate preliminary magnitudes (all in AB) of

g' = 21.3 +- 0.1 mag,

r' = 21.0 +- 0.1 mag,

i' = 20.8 +- 0.1 mag,

z' = 20.5 +- 0.1 mag,

J = 20.3 +- 0.1 mag and

H = 19.6 +- 0.1 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)=0.033 mag in the
direction of the burst (Schlegel et al. 1998).

We thank the ESO staff at LaSilla observatory, and in particular A. Sanchez,
for their excellent support and assistance with the observations.


GRB_name: GRB101204A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11446
SUBJECT: GRB 101204A: Swift-XRT refined Analysis
DATE:    10/12/09 16:38:18 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

B. Sbarufatti (INAF/OAB-IASF Pa) reports on behalf of the Swift-XRT
team:

We have analysed 24 ks of XRT data for GRB 101204A (Cummings  et al.
GCN Circ. 11440), from 126.2 ks to 383.1 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. Using 9912 s of PC mode
data and 4 UVOT images, we find an enhanced XRT position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 167.53700, -20.41980 which is equivalent to:

RA (J2000): 11h 10m 8.88s
Dec(J2000): -20d 25' 11.5"

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.33 (+0.24, -0.23).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.14 (+0.34, -0.18). The
best-fitting absorption column is  consistent with the Galactic value
of 3.3 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.4 x 10^-11 (3.9 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.3 (+4.4, -0.0) x 10^20 cm^-2
Galactic foreground: 3.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.14 (+0.34, -0.18)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020153.

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


GRB_name: GRB101204A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11447
SUBJECT: GRB101204A: Swift/UVOT observations
DATE:    10/12/09 19:11:39 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) & B. Sbarufatti (INAF-OAB/IASFPA) report
on behalf of the Swift-XRT and Swift-UVOT teams

The Swift/UVOT began settled observations of the field of GRB 101204A
126195 s after the BAT trigger (Cummings et al., GCN Circ. 11440).

In agreement with report from Nicuesa Guelbenzu et al., (GCN Circ.  
11445), we
find the afterglow candidate in (Sbarufatti et al. GCN Circ. 11442)
to have faded. Preliminary magnitudes using the UVOT photometric
system (Poole et al. 2008, MNRAS, 383, 627) for summed exposures are:

Filter  T_start(s)  T_stop(s)   Exp(s)       Mag
#####################################################
v       126195       133279     2563    20.51 +/- 0.19
v       271960       336155     3553    > 21.62
u       127505       134378     2329    20.03 +/- 0.12
u       272471       336626     3273    21.27 +/- 0.26
#####################################################

The values quoted above 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: GRB101213A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11448
SUBJECT: GRB 101213A: Swift detection of a burst
DATE:    10/12/13 11:18:16 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (NASA/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), S. Campana (INAF-OAB), V. D'Elia (ASDC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. Rowlinson (U Leicester),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester), G. Stratta (ASDC) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 10:49:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101213A (trigger=440285).  Swift slewed immediately to the burst.
The BAT on-board calculated location is RA, Dec 241.286,+21.915 which is 
   RA(J2000) = 16h 05m09s
   Dec(J2000) = +21d54'53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED-like
structure with a duration of about 100 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~0 sec after the trigger.

The XRT began observing the field at 10:51:08.6 UT, 105.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 241.3139, +21.8984 which is equivalent to:
   RA(J2000)  = 16h 05m 15.33s
   Dec(J2000) = +21d 53' 54.2"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 110 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 114 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.06.

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


GRB_name: GRB101213A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11449
SUBJECT: GRB 101213: object within the X-ray error circle
DATE:    10/12/13 12:06:44 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani and A. de Ugarte Postigo (DARK/NBI), report:

We notice the presence of an object within the error circle of the X-ray 
afterglow of GRB 101213 (Sakamoto et al., GCN 11448; see also 
http://www.swift.ac.uk/sper/). The object is visible in the DSS as well 
in gri images of the SDSS. It is classified as a galaxy in the SDSS 
catalog. The coordinates are:

RA(J2000) = 16:05:15.20
Dec(J2000) = 21:53:49.2

Magnitudes from the SDSS are (AB):

g = 22.07 +- 0.09
r = 21.22 +- 0.07
i = 21.12 +- 0.12

Despite the bad visibility of this GRB right now, the field will be 
observable from the Northern hemisphere in a couple of weeks. Given the 
brightness of the potential host galaxy, and hence the likely low 
redshift, a search for an associated SN may be attempted (also to 
confirm the object as the GRB host).


GRB_name: GRB101213A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11450
SUBJECT: GRB 101213A: Enhanced Swift-XRT position
DATE:    10/12/13 14:46:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 2148 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 101213A, 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 = 241.31370, +21.89715 which is equivalent
to:

RA (J2000): 16h 05m 15.29s
Dec (J2000): +21d 53' 49.7"

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

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

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


GRB_name: GRB101213A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11451
SUBJECT: GRB 101213A: Swift/UVOT Upper Limits
DATE:    10/12/13 16:52:37 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W. Landsman (NASA/Adnet) and T. Sakamoto (NASA/UMBC) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 101213A 114 s after the BAT trigger (Sakamoto et al., GCN Circ. 11448).   No optical afterglow consistent with the XRT position (Osborne et al., GCN Circ. 11450) is detected in the initial UVOT exposures.   Preliminary 3-sigma upper limits using the UVOT photometric system  (Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC) exposure and subsequent exposures are:

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

white_FC           114          264          147>21.0
u_FC               327          577          246>19.8
white              114         5066          286>21.4
v                 3919         4119          197>19.2
b                  583         4940          216>20.5
u                  327         4733          442>20.4
w1                4329         4529          197>20.3
m2                4124         4323          197>20.4

The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.06 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB101213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11452
SUBJECT: GRB 101213A: Swift-XRT refined Analysis
DATE:    10/12/13 18:29:00 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and T. Sakamoto (NASA/UMBC) report on behalf
of the Swift-XRT team:

We have analysed 4.9 ks of XRT data for GRB 101213A (Sakamoto  et al.
GCN Circ. 11448), from 95 s to 16.9 ks after the  BAT trigger. The data
comprise 270 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 11450).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.33 (+/-0.14). At T+196 s the decay
steepens to an alpha of 3.14 (+0.27, -0.18) before breaking again at
T+407 s to a final decay with index alpha=0.90 (+0.04, -0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.62 (+0.08, -0.07). The
best-fitting absorption column is  5.73 (+0.30, -0.29) x 10^21 cm^-2,
in excess of the Galactic value of 4.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.44 (+0.18, -0.17)
and a best-fitting absorption column of 6.5 (+0.9, -0.8) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.4 x 10^-11 (1.2 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.5 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 4.6 x 10^20 cm^-2
Excess significance: 13.5 sigma
Photon index:      2.44 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
0.90, the count rate at T+24 hours will be 0.021 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.4 x
10^-13 (2.6 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/00440285.

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


GRB_name: GRB101213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11453
SUBJECT: GRB 101213A, Swift-BAT refined analysis
DATE:    10/12/13 21:59:32 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori@milkyway.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), 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-240 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 101213A (trigger #440285)
(Sakamoto, et al., GCN Circ. 11448).  The BAT ground-calculated position is
RA, Dec = 241.297, 21.905 deg which is 
   RA(J2000)  =  16h 05m 11.3s 
   Dec(J2000) = +21d 54' 17.6" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 31%.
 
The mask-weighted light curve shows two overlapping peaks.  The first peak is starting 
at ~T-5 sec and peaking at ~T+0.  The second peak is peaking at ~T+15 sec, and roughly 
exponential decaying out to ~T+100 sec.  T90 (15-350 keV) is 135 +- 38 sec 
(estimated error including systematics).  
 
The time-averaged spectrum from T-3.1 to T+197.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.53 +- 0.09.  The fluence in the 15-150 keV band is 5.0 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T-0.26 sec in the 15-150 keV band
is 2.2 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/440285/BA/


GRB_name: GRB101213A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11454
SUBJECT: GRB 101213A: Fermi GBM observation
DATE:    10/12/14 10:01:12 GMT
FROM:    David Gruber at MPE  <dgruber@mpe.mpg.de>

David Gruber (MPE) reports on behalf of the Fermi GBM Team: 

"At 10:49:20.80 UT on 13 December 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101213A (trigger 313930162 / 101213451)
which was also detected by the Swift/BAT
(Sakamoto et al. 2010, GCN 11448).
The GBM on-ground location is consistent with the Swift position.
 
The angle from the Fermi LAT boresight is 129 degrees.

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

The GBM light curve conists of two overlapping FRED like pulses
with a duration (T90) of about 45 (+/-4) s (50-300 keV). 
The time-averaged spectrum from T0-1.536 s to T0+44.545 s is 
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.09 (+/-0.07) and
the cutoff energy, parameterized as Epeak, is 315.0 (+46.7/-35.9) keV
(CSTAT 740 for 365 d.o.f.).

The event fluence (10-1000 keV) in this time interval is 
(1.40 +/- 0.01)E-05 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+2.944 s in the 10-1000 keV band 
is 4.67 (+/-0.32) ph/s/cm^2.

A Band function fits the spectrum equally well (CSTAT 739 for 365 d.o.f.) 
with Epeak= 309.7 (+48.9/-40.0) keV, alpha = -1.1 (+/-0.07) 
and beta = -2.35 (+0.29/-0.72). 

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


GRB_name: GRB101213A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11456
SUBJECT: Konus-Wind observation of GRB 101213A
DATE:    10/12/14 14:03:15 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 101213A (Swift/BAT trigger #440285:
Sakamoto, et al., GCN 11448; Cummings, et al., GCN 11453)
triggered Konus-Wind at T0=38958.472s UT (10:49:18.472)

The burst light curve consists of two overlapping pulses
with a total duration of ~50 s.
The emission is seen up to ~2 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101213_T38958/

As observed by Konus-Wind, the burst
had a fluence of (1.3  0.3)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0-0.512s,
of (0.60  0.15)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+41.216 s) is best fit
in the 20 keV - 2 MeV range by the GRB (Band) model,
for which:
the low-energy photon index alpha = -0.7 (-0.3, +0.4),
the high energy photon index beta = -2.3 (-1.5, +0.3),
the peak energy Ep = 198(-49, +92)keV, chi2 = 51/59 dof.

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


GRB_name: GRB101213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11457
SUBJECT: Redshift solution(s) for GRB101213A from Swift-XRT data
DATE:    10/12/15 13:55:47 GMT
FROM:    Sergio Campana at INAF-OAB  <sergio.campana@brera.inaf.it>

S. Campana (INAF-OAB), S. Covino (INAF-OAB), A. Cucchiara (UCB/LBNL/UCSC),
P. A. Evans  (U Leicester), D. Grupe (PSU), D. Malesani (DARK/NBI),
T. Sakamoto (NASA/UMBC) and R. L. C. Starling (U Leicester):

Swift BAT triggered on the early activity of GRB 101213A (Sakamoto et
al. 2010, GCN 11448). Swift XRT started observing 106 s after the
trigger observing the main event. We selected the time interval between
112-154 s during which the hardness ratio (as judged from the Swift/XRT
spectrum repository at http://www.swift.ac.uk/xrt_spectra/00440285/ )
and the power law photon index (as judged from the Swift/XRT burst analyser
http://www.swift.ac.uk/burst_analyser/00440285/ ) are consistent
with a constant. We bin the spectrum to 30 counts per energy bin and
used the latest response matrices v012. The spectrum is in Windowed Timing
mode (WT) and contains about 6,000 counts. We fit the WT spectrum with 
XSPEC
using the model tbabs*ztbabs*(cutoff), (the cutoff power-law model provides
much better results in terms of column density evaluation with respect to a
simple power-law model when small spectral variations are present).
We assume a Galactic column density of 4.6x10^20 cm^-2 (Kalberla et al.
2005, A&A 440 775). In the intrinsic column density vs.
redshift plane there is just one deep minimum hinting for a redshift
z=2.9^+0.2_-0.8 (90% confidence level) and an intrinsic column density
N_H(z)=(1.5^+0.7_-0.3)x10^23 cm^-2. The X-ray spectrum is soft with
Gamma~2.5 at the end of the prompt phase and no signs of spectral curvature
(cut-off energy > 30 keV).

The absorption pattern towards GRB 101213A is complicated by the galaxy
reported by Malesani & de Ugarte Postigo (2010, GCN 11449). We tried to fit
an extra absorption component fixed either to z=0.1 or z=0.5 (i.e. the two
possible photometric redshifts of the putative host galaxy observed in the
SDSS, z=0.10+/-0.07 and z=0.47+/-0.22, respectively), with basically no
effects on the overall results. This low-redshift component is not able
alone to account for the observed absorption pattern.

Looking at the burst analyser page (see above), we also note that there is
a mismatch in the BAT and XRT power law photon indices during the short
interval during which there are contemporanous data. Motivated by this we
fit the XRT spectrum with a broken power law.
The fit is as good as the power law fit. In this case we obtain a very soft
low-energy photon index of Gamma1=3.1+/-0.2 and a high-energy photon index
Gamma2=2.0+/-0.2 (consistent with the BAT extrapolation). The transition
energy is around 3 keV. In this case, the redshift is z=0.3^+0.4_-0.1 
and the
intrinsic column density is (1.1^+0.3_-0.2)x10^22 cm^-2. In this case the
redshift determination is consistent with the putative host galaxy but the
resulting X-ray spectrum is peculiar, with a spectral variation Delta 
Gamma~1
and a spectrum that remains (almost) constant for ~150 s, becoming even
softer later on.
Alternatively, the X-ray spectrum could be fit (equally well) with a black
body plus a power law component. In this case the redshift is 
z=0.3^+0.1_-0.2
and the intrinsic column density NH=(1.1^+0.3_-0.2)x10^22 cm^-2. The power
law is very soft with Gamma~3.3 and the black body (rest-frame) temperature
is high kT=2.3^+1.3_-0.5 keV. The black body radius is ~2x10^11 cm.
We note that the black body temperature is much higher than what is observed
in, e.g., GRB 060218 (kT~0.2 keV, Campana et al. 2006, Nat 442 1008) or
GRB 100316D (kT~0.1 keV, Starling et al. 2010, MNRAS in press).

We can conclude that in all cases, the X-ray afterglow flux is heavily
absorbed and this is in line with the non-detection with UVOT.
Given the presence of a candidate host galaxy within the XRT refined error
circle (Malesani & de Ugarte Postigo 2010), we cannot rule out a low
redshift solution, but in this case a peculiar X-ray spectrum is observed.


GRB_name: GRB101213A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11458
SUBJECT: GRB 101213A : Suzaku WAM observation of the prompt emission
DATE:    10/12/16 10:18:38 GMT
FROM:    Yoshitaka Hanabata at Hiroshima U  <hanabata@hep01.hepl.hiroshima-u.ac.jp>

Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.), 
N. Ohmori, A. Daikyuji, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka (Aoyama Gakuin U.), 
S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, S. Hong, W. Iwakiri,
K. Takahara, T. Yasuda (Saitama U.), P. Tsai, Y. Urata (NCU), 
N. Vasquez (Tokyo Tech.), Y. E. Nakagawa, M. Serino, T. Tamagawa (RIKEN), 
K. Nakazawa, K. Makishima (Univ. of Tokyo), 
on behalf of the Suzaku WAM team, report:


The multi-spiked long GRB 101213A (Swift/BAT trigger #440285, GCN
11448; Sakamoto et al.,) triggered the Suzaku Wide-band All-sky
Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at
10:49:19.352 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0-1s,
ending at T0+50s with a duration (T90) of about 32 seconds.
The fluence in 100 - 1000 keV was 7.47 (+1.14/-1.06) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0+2s was 0.84 (+0.10/-0.09) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1s to
T0+50s is well fitted by a single power-law with a photon index
of 2.08 (+0.24/-0.21) (chi^2/d.o.f = 19.9/14).

Due to the brightness of this burst, a 3% systematic error was added
for low energy channels.
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/trig/grb_table.html


GRB_name: GRB101023A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11459
SUBJECT: Request for Supernova related data for GRB 101023A
DATE:    10/12/18 10:03:22 GMT
FROM:    Sandip K. Chakrabarti at S.N. Bose Nat. Centre for Basic Sci.  <chakraba@bose.res.in>

R. Ruffini, L. Izzo, A. Penacchione, S.K. Chakrabarti on behalf of ICRAnet
reports:

We have tentatively identified the redshift factor z of GRB 101023A (GCN
11363, 11364, 11365, 11366) to be between 0.7 to 1.0 from Amati relation. This
GRB had two major pulses whose E_iso appear to be ~10^52 ergs and ~2x10^53
ergs respectively. Despite being bright and nearby, no Supernovae has been
reported for this source. We encourage anyone having data especially around
1st to 7th of November, 2010, on this object on supernovae association (either
way) to report them to facilitate understanding this object.


GRB_name: GRB101023A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11460
SUBJECT: Request for Supernova related data for GRB 101023A
DATE:    10/12/18 10:03:30 GMT
FROM:    Sandip K. Chakrabarti at S.N. Bose Nat. Centre for Basic Sci.  <chakraba@bose.res.in>

R. Ruffini, L. Izzo, A. Penacchione, S.K. Chakrabarti on behalf of ICRAnet
reports:

We have tentatively identified the redshift factor z of GRB 101023A (GCN
11363, 11364, 11365, 11366) to be between 0.7 to 1.0 from Amati relation. This
GRB had two major pulses whose E_iso appear to be ~1052 ergs and ~2x1053 ergs
respectively. Despite being bright and nearby, no Supernovae has been reported
for this source. We encourage anyone having data especially around 1st to 7th
of November, 2010, on this object on supernovae association (either way) to
report them to facilitate understanding this object.


GRB_name: GRB101219A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11461
SUBJECT: GRB 101219A: Swift detection of a short hard burst
DATE:    10/12/19 02:50:58 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@astro.psu.edu>

J. M. Gelbord (PSU), S. D. Barthelmy (GSFC), M. M. Chester (PSU),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), D. Grupe (PSU),
E. A. Hoversten (PSU), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), C. J. Saxton (UCL-MSSL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 02:31:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101219A (trigger=440606).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 74.616, -2.534 which is 
   RA(J2000)  =  04h 58m 28s
   Dec(J2000) = -02d 32' 01"
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 0.3 sec.  The peak count rate
was ~24000 counts/sec (15-350 keV), at 0.0 sec after the trigger. 

The XRT began observing the field at 02:32:30.0 UT, 60.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 74.5854,
-2.5395 which is equivalent to:
   RA(J2000)  = 04h 58m 20.49s
   Dec(J2000) = -02d 32' 22.4"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 111 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 (4.87 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.8
(+1.83/-1.57) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
278 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 18.0 mag. No correction has been made for the expected extinction
corresponding to E(B-V) of 0.06. 

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


GRB_name: GRB101219A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11462
SUBJECT: GRB 101219A: ROTSE-III Optical Limits
DATE:    10/12/19 03:05:57 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey (U Mich), W. Zheng (U Mich) and W. Rujopakarn (Steward),
report on behalf of the ROTSE collaboration:

ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia,
responded to GRB 101219A (Swift trigger 440606; Gelbord J. M., GCN 11461),
producing images beginning 8.1 s after the GCN notice time. An automated
response took the first image at 02:31:48.0 UT, 12.0 s after the burst,
under fair conditions. We took 10 5-sec, 10 20-sec and 10 60-sec exposures.
These unfiltered images are calibrated relative to USNO A2.0 (R). Imaging
is on going.

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle or the XRT error circle, for both single
images and coadding into sets of 10. Individual images have limiting
magnitudes ranging from 15.7-17.2; we set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
02:31:48.0   02:31:53.0         5     15.7           12.0       N
02:31:48.0   02:33:04.1        76     17.2           90.0       Y


GRB_name: GRB101219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11463
SUBJECT: GRB 101219A: REM optical and NIR observations
DATE:    10/12/19 03:32:53 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino (INAF/Brera) and E. Palazzi (IASF-Bo) on behalf of the REM  
team report:

The robotic 60-cm REM telescope located at La Silla (Chile) observed  
automatically the field of GRB 101219A (Gelbord et al. GCN 11461) with  
the ROSS optical and REMIR near-infrared cameras in imaging mode.

The first observations have been performed within about 30s from the  
GRB time.
No counterpart down to the 2MASS limit could be singled out in the XRT  
error circle in the NIR frames, while the proximity of the bright Moon  
(~30 deg) prevented deep optical observations.

Further observations are in progress.


GRB_name: GRB101219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11464
SUBJECT: GRB 101219A: Gemini-South observations
DATE:    10/12/19 04:13:33 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley (UC Berkeley), E. Berger (Harvard), S.B. Cenko (UC 
Berkeley), R. Chornock (Harvard), A. J. Levan (Warwick), N. Tanvir 
(Leicester) report:

We observed the position of GRB 101219A (Gelbord et al., GCN 11461) with 
GMOS-S on the Gemini South telescope in the i-band starting at 2010 Dec 
19 13:14:04 UT (43 min after the burst).  In a stack of the first five 
180-sec exposures we detect a faint object within the XRT error circle 
(GCN #11461) at coordinates (J2000):

RA = 04:58:20.478
DEC = -02:32:22.17

The object is also weakly detected in a single r-band frame, and appears 
to be mildly extended in the i-band images.  Further observations and 
analysis are underway.


GRB_name: GRB101219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11465
SUBJECT: GRB 101219A: SARA-N Upper Limit
DATE:    10/12/19 04:41:10 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike (CRESST/UMD/NASA GSFC), Dieter H. Hartmann (Clemson
University), and Martha A. Leake (Valdosta State University) report:

We observed the field of GRB 101219A (Gelbord et al., GCN 11461) with the
SARA-North 0.9m telescope at KPNO beginning 38 minutes after the trigger
under good conditions and high airmass.  We do not detect the afterglow
candidate (Perley et al., GCN 11464) down to a limiting magnitude of 19.5
in the R band (420 seconds of exposure beginning 38 minutes after trigger)
and 18.6 in the I band (300 seconds of exposure beginning 45 minutes after
trigger) as compared to the USNO B1.0 catalog.  This message may be cited.


GRB_name: GRB101219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11466
SUBJECT: GRB 101219A - NOT observation - upper limit
DATE:    10/12/19 05:21:51 GMT
FROM:    Steve Schulse at U. of Iceland  <steve@raunvis.hi.is>

S. Schulze (U Iceland), D. Malesani (DARK Cosmology Centre), D. Xu  
(Weizmann Institute)
I. Ilyin (AIP Potsdam), P. Jakobsson (U Iceland) on behalf of a larger  
collaboration report:

We observed the field of GRB 101219A (Gelbord et al., GCN 11461) with   
StanCAM mounted
on the NOT telescope on La Palma, Canary Islands (Spain) starting at  
3:34 UT (~1 hour after
the trigger) and ending 4:01:21 UT.

We took seven images in R band with an exposure time of 150 seconds  
each. The stacked
image does not reveal any new source within the XRT error circle  
(Gelbord et al., GCN 11461),
and in particular at the location of  the optical object identified by  
Perley et al. (GCN 11464).

We derive a limiting magnitude of 21 in R-band calibrated against USNO  
stars with a
mid-exposure time of 1.27 hours after the trigger.


GRB_name: GRB101219A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11467
SUBJECT: GRB 101219A: Swift-BAT refined analysis
DATE:    10/12/19 06:11:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), J. M. Gelbord (PSU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(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 the BAT short hard burst GRB 101219A (trigger #440606)
(Gelbord, et al., GCN Circ. 11461).  The BAT ground-calculated position is
RA, Dec = 74.586, -2.527 deg which is 
   RA(J2000)  =  04h 58m 20.7s 
   Dec(J2000) = -02d 31' 37.1" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 94%.
 
The mask-weighted light curve shows two overlapping peaks starting at ~T-0.1 sec
and ending at ~T+0.6 sec.  At the 2-sigma confidence level, there may be
extended emission out to T+30 sec.  T90 (15-350 keV) is 0.6 +- 0.2 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.0 to T+1.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.63 +- 0.09.  The fluence in the 15-150 keV band is 4.6 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.04 sec in the 15-150 keV band
is 4.1 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/440606/BA/


GRB_name: GRB101219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11468
SUBJECT: GRB 101219A: Further Gemini-South Imaging
DATE:    10/12/19 11:52:37 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley), A. J. Levan (Warwick), R. Chornock, E. Berger
(Harvard),  D. A. Perley, J. S. Bloom (UC Berkeley), and N. Tanvir
(Leicester) report on behalf of a larger collaboration:

We have obtained a second series of i'-band imaging (Perley et al., GCN
11464) of the field of the short-hard GRB101219A (Gelbord et al., GCN
11461) with the Gemini Multi-Object Spectrograph mounted on the 8-m Gemini
South telescope.  Observations consisted of 12 x 180 s exposures beginning
at 6:55 UT (~ 4.2 hours after the burst trigger).

Digital subtraction of the two epochs reveals no transient emission within
or around the XRT error circle.  Using several common SDSS objects for
calibration, we place an upper limit of i' > 24.5 mag.  Similarly,
aperture photometry reveals the source mentioned by Perley et al. (GCN
11464), which is clearly extended in our images, remains approximately
constant over this time period, with an i-band magnitude of ~ 23.5.

We further note that no sources are present in any filter in the SDSS
pre-explosion imaging of the field in the immediate environment of the XRT
error circle.  The limits, however, would not be sufficient to detect the
extended source mentioned above.


GRB_name: GRB101219A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11469
SUBJECT: GRB 101219A: Magellan NIR observations
DATE:    10/12/19 12:04:51 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

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

We observed the field of the short-hard burst GRB 101219A (Gelbord et 
al., GCN 11461) with FourStar on the 6.5-m Magellan Baade telescope. 
Observations in the J band began at 03:43:20 UT, 1.2 hours after the BAT 
trigger time.  The source in the XRT error circle found by Perley et al. 
(GCN 11464) is clearly detected in our images, at a preliminary 
magnitude of J=21.6 in comparison to 2MASS stars in the field.  The 
object is clearly extended in our images (seeing <0.5"), so it is likely 
the host galaxy and is not dominated by an afterglow, consistent with 
the non-detection of fading in the optical (Cenko et al., GCN 11468).


GRB_name: GRB101219A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11470
SUBJECT: Konus-Wind observation of short hard GRB 101219A
DATE:    10/12/19 12:41:07 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short hard GRB 101219A, (Swift/BAT trigger=440606:
Gelbord, et al., GCN 11461; Krimm et.al, GCN 11467)
triggered Konus-Wind at T0=09094.716s UT (02:31:34.716)

The total duration of the burst is ~0.6 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/GRB101219_T09094/

As observed by Konus-Wind, the burst
had a fluence of (3.6  0.5)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.032s,
of (2.8  0.8)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the major part of the burst
(from T0 to T0+0.256 s) is best fit
in the 20 keV - 10 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.22 (-0.25, +0.30),
and Ep = 490(-79, +103) keV, chi2 = 27.6/30 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+0.064 s) is best fit
in the 20 keV - 10 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.05 (-0.45, +0.60),
and Ep = 426(-100, +173) keV, chi2 = 9/10 dof.

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


GRB_name: GRB101219A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11471
SUBJECT: GRB 101219A: GROND Upper limits
DATE:    10/12/19 13:26:42 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

F. Olivares E. (MPE Garching), A. Rossi (TLS Tautenburg), J. Greiner,
J. Elliott (both MPE Garching) and D. A. Kann (TLS Tautenburg)
report on behalf of the GROND team:

We observed the field of GRB 101219A (Swift trigger 440606; Gelbord et
al., GCN #11461) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La
Silla Observatory (Chile).

Observations started at 03:52 UT on December 19, 1.36 hours after the
GRB, and have total exposure of 1501 s in g'r'i'z' and 1200 s in JHK.
They were performed at an average seeing of 0.8" and at an average
airmass of 1.13.

We do not detect a source within the XRT error circle reported by
Gelbord (GCN #11461) down to the following 3 sigma upper limits (all
in AB):

g' > 23.4
r' > 23.6
i' > 23.1
z' > 23.2
J > 22.2
H > 21.8 and
K > 20.2

The given limits are derived based on calibrating the images against
SDSS and 2MASS field stars and are not corrected for the
Galactic foreground extinction corresponding to a reddening of
E(B-V)=0.06 in the direction of the burst (Schlegel et al. 1998).

Our limits are not deep enough to detect the host galaxy candidate
found in the optical (Perley et al., GCN 11464, Cenko et al., GCN
11468) and the NIR (Chornock et al., GCN 11469).


GRB_name: GRB101219A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11472
SUBJECT: GRB 101219A: Swift/UVOT Upper Limits
DATE:    10/12/19 13:49:14 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 101219A
67 s after the BAT trigger (Gelbord et al., GCN Circ. 11461).
No optical afterglow consistent with the XRT position
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:

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

white_FC            67          217          147         >20.8
u_FC               279          528          246         >19.9
white               67         5557          467         >21.4
v                  608         5968          432         >19.7
b                  534         6724          369         >20.3
u                  279         6582          658         >20.5
w1                 658         6377          432         >21.0
m2                 632         6172          432         >20.2
w2                 584         5763          432         >20.9

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.06 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB101219B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11473
SUBJECT: GRB 101219B: Swift detection of a burst with an optical afterglow
DATE:    10/12/19 16:52:57 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. M. Gelbord (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
M. M. Chester (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
P. T. O'Brien (U Leicester), D. M. Palmer (LANL) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 16:27:53 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101219B (trigger=440635).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 12.257, -34.532 which is 
   RA(J2000)  =  00h 49m 02s
   Dec(J2000) = -34d 31' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This is an image trigger so as is typical,
the BAT lightcurve does not show anything. 

The XRT began observing the field at 16:30:19.8 UT, 146.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 12.2306, -34.5662 which is equivalent to:
   RA(J2000)  = 00h 48m 55.34s
   Dec(J2000) = -34d 33' 58.3"
with an uncertainty of 5.6 arcseconds (radius, 90% containment). This
location is 145 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 156 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 00:48:55.35 =  12.23061
  DEC(J2000) = -34:33:59.5  = -34.56652
with a 90%-confidence error radius of about 0.62 arc sec. This position is 1.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.84 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.02. 

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


GRB_name: GRB101219A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11474
SUBJECT: GRB 101219A: Swift-XRT refined Analysis
DATE:    10/12/19 21:10:08 GMT
FROM:    Jonathan Gelbord at PSU/Swift  <jgelbord@astro.psu.edu>

J.M. Gelbord (PSU) and D. Grupe (PSU) report on behalf of the
Swift-XRT team:

We have analysed 5.8 ks of XRT data for GRB 101219A (Gelbord et al.
GCN Circ. 11461), from 70 s to 18.0 ks after the  BAT trigger. The
data comprise 13 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode.

The light curve after 200s can be modelled as a power-law decay. The
decay index is alpha=-1.8 (+/-0.2).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.78 (+0.25, -0.23). The
best-fitting absorption column is 3.1 (+1.1, -0.9) x 10^21 cm^-2,
in excess of the Galactic value of 4.87 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.9 x 10^-11 (6.9 x 10^-11) erg
cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:        3.1 (+1.1, -0.9) x 10^21 cm^-2
Galactic foreground: 4.9 x 10^20 cm^-2
Excess significance: 4.8 sigma
Photon index:        1.78 (+0.25, -0.23)

If the light curve continues to decay with a power-law decay index of
1.8, the count rate at T+24 hours will be 2 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.5 x
10^-16 (1.1 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00440606.

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


GRB_name: GRB101219B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11475
SUBJECT: GRB 101219B: Swift-BAT refined analysis
DATE:    10/12/19 21:59:06 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), J. M. Gelbord (PSU), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+766 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 101219B (trigger #440635)
(Gelbord, et al., GCN Circ. 11473).  The BAT ground-calculated position is
RA, Dec = 12.259, -34.556 deg which is 
   RA(J2000)  =  00h 49m 01.9s 
   Dec(J2000) = -34d 33' 21.6" 
with an uncertainty of 3.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 7%.
 
The mask-weighted light curve shows a broad peak starting at ~T+20 sec
and ending at ~T+60 sec.  However, given that there was a pre-planned slew
ending just before T_zero, we can not rule out that was actvitity before
this source came into the BAT FoV.  T90 (15-350 keV) is 34 +- 5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+10 to T+60 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.16.  The fluence in the 15-150 keV band is 2.1 +- 0.4 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+26.84 sec in the 15-150 keV band
is 0.6 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 


GRB_name: GRB101219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11476
SUBJECT: GRB 101219A: IAC80 optical observations
DATE:    10/12/19 22:10:59 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC, Granada), M. Visus (IAC, Obs Teide, Tenerife), J.
Garcia (IAC, Obs Teide, Tenerife), A. de Ugarte Postigo (DARK/NBI,
Copenhagen), report on behalf of a larger collaboration:

"We have observed the field of GRB 101219A (Gelbord et al., GCN 11461)
with  the IAC80 telescope located at the Observatory of Teide, Tenerife.
The observations were carried out in the R and I bands on Dec
19.11291-19.15778  UT (starting 11.1 minutes after the GRB). No object is
detected within the XRT error circle down to R~21.5 and I~20.5
(calibration based on USNO-A2)."


GRB_name: GRB101219B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11477
SUBJECT: GRB 101219B: Fermi GBM observation
DATE:    10/12/20 03:12:52 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <Alexander.J.VanDerHorst@nasa.gov>

A.J. van der Horst (USRA) reports on behalf of the Fermi GBM Team:

"At 16:28:13.12 UT on 19 December 2010, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 101219B (trigger 314468895 /
101219686), which was also detected by the Swift/BAT (GCN 11473).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 59 degrees.

The GBM light curve consists of one peak with a duration (T90)
of 51 +/- 2 s (50-300 keV). The time-averaged spectrum from
T0-4.1 s to T0+47.1 s is best fit by a Band function with
Epeak = 70 +/- 8 keV, alpha = 0.33 +/- 0.36, and beta = -2.12 +/- 0.12.
The event fluence (10-1000 keV) in this time interval is
(5.5 +/- 0.4)E-6 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+5.6 s in the 10-1000 keV band is
2.0 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB101219B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11478
SUBJECT: GRB 101219B: GROND Detection of the Optical/NIR Afterglow
DATE:    10/12/20 03:48:24 GMT
FROM:    Felipe Olivares Estay at MPE  <felipe@mpe.mpg.de>

F. Olivares E. (MPE Garching), A. Rossi (TLS Tautenburg), and J.
Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 101219B (Swift trigger 440635; Gelbord et
al., GCN #11473) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La
Silla Observatory (Chile).

Observations started during twilight at 00:33 UT on December 20, 8.1
hours after the GRB trigger, and were performed at an average seeing
of 1" and an average airmass of 1.05.

We confirm the optical afterglow candidate reported by Gelbord et
al.(GCN #11473). The afterglow faded, however, it is well detected in
all seven GROND optical/NIR bands.

Based on 141 s of total exposure in g'r'i'z' and 240 s in JHK, taken
at 00:36 UT mid-time, we estimate preliminary magnitudes (all in the
AB system) of:

g' = 20.4 +/- 0.1
r' = 20.0 +/- 0.1
i' = 20.0 +/- 0.2
z' = 19.6 +/- 0.1
J =19.2 +/- 0.1
H =18.8 +/- 0.1 and
K = 18.6 +/- 0.1

A second epoch was obtained at 03:10 UT mid-time, with total exposure
time of 1500 s in in g'r'i'z' and 1200 s seconds in JHK. The afterglow
has faded by ~0.3 mag in the r' and J bands, which yields a temporal
decay index of alpha = 1.0 between our two epochs.

Given magnitudes are calibrated against GROND zero points and 2MASS
field stars. The error in the optical bands is dominated
by the zero-point uncertainty. Magnitudes are not corrected for the
expected Galactic foreground extinction corresponding to a reddening
of E(B-V)=0.02 mag in the direction of the burst (Schlegel et al.
1998).


GRB_name: GRB101219A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11479
SUBJECT: GRB 101219A: MITSuME  Ishigakijima Optical upper limits
DATE:    10/12/20 04:23:45 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), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 101219A (Gelbord et al., GCN 11461)
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 2010-12-19 10:30:50 UT (~8.0 h after
the trigger). We did not find any new point source within the XRT
error circle (Gelbord et al., GCN 11461) 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
------------------------------------------------------
0.33651    10:36:04     480.0    >19.1  >19.1  >18.7
0.46387    13:39:28    1500.0    >20.9  >20.7  >20.0
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB101219B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11480
SUBJECT: GRB 101219B: Enhanced Swift-XRT position
DATE:    10/12/20 11:56:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 2429 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 101219B, 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 = 12.23064, -34.56688 which is equivalent
to:

RA (J2000): 00h 48m 55.35s
Dec (J2000): -34d 34' 00.8"

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

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

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


GRB_name: GRB101219B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11481
SUBJECT: GRB 101219B: Swift-XRT refined Analysis
DATE:    10/12/20 16:57:06 GMT
FROM:    Jonathan Gelbord at PSU/Swift  <jgelbord@astro.psu.edu>

J.M. Gelbord (PSU) reports on behalf of the Swift-XRT team:

We have analysed 17 ks of XRT data for GRB 101219B (Gelbord et al.
GCN Circ. 11473), from 136 s to 65.2 ks after the BAT trigger. The
data comprise 415 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 11480).

The light curve (from T0+425 s) can be modelled with a series of
power-law decays. The decay from T+425 s is steep, with an index of
alpha=4.16 (+2.3, -0.50).  At T+638 s the decay flattens to an
alpha of 2.35 (+0.31, -0.46).  Another break at T+4.7 ks is
followed by a flatter decay of alpha = 0.23 (+/-0.15).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.68 (+/- 0.04). The
best-fitting absorption column is consistent with the Galactic value
of 3.14 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has
a photon index of 1.69 (+0.12, -0.11) and a best-fitting absorption
column consistent with the Galactic value. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.1 x 10^-11 (4.3 x 10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+0.9, -3.1) x 10^20 cm^-2
Galactic foreground: 3.14 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.69 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
0.23, the count rate at T+24 hours will be 0.0060 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-13 (1.3 x 10^-13) erg cm^-2 s^-1.  The count rate at T+48 hours
would be 0.0051 count s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00440635.

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


GRB_name: GRB101219B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11482
SUBJECT: GRB 101219B: Swift/UVOT refined analysis
DATE:    10/12/21 00:09:32 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 101219B
156 s after the BAT trigger (Gelbord et al., GCN Circ. 11473).
The optical afterglow is at 7 arcsec distance of a 16th magnitude star.
Special care has been taken to subtract the estimated contribution
of the neghboring star.  The data suggest that after an initial
brightening, there was a dimming around T+550s followed by a
second brightening.

Preliminary magnitudes of the GRB, using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and some selected subsequent exposures are:

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

white_FC           156          306        147.4       17.87   0.06
white              768          788         19.5       17.59   0.10
white             6686         6886        196.6       18.58   0.06
v                  820          840         19.5       17.55   0.27
v                 7097         7296        196.6       18.39   0.15
b                  570          590         19.5       18.79   0.30
b                  744          764         19.4       18.00   0.19
u                  718          738         19.5       17.25   0.18
u                 1298         1318         19.5       17.26   0.18
uvw1              1446         1465         19.4       17.43   0.28
uvw1             16352        16861        501         18.40   0.11
uvm2              7301         7392         89.6       18.15   0.24
uvm2             51175        52075        856         19.54   0.16
uvw2              6892         7092        197         18.04   0.13
uvw2             56901        57801        886         20.21   0.20

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB101219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11483
SUBJECT: GRB 101219A: Chandra Observations
DATE:    10/12/23 22:13:13 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger (Harvard) reports on behalf of a larger collaboration:

"We observed the field of the short GRB 101219A (GCN 11467) with ACIS-S on
the Chandra X-ray Observatory starting on 2010 December 23.05 UT (3.942
days after the burst) for a total of 19.8 ksec.  We do not detect any
source within the XRT error circle (GCN 11461), or in coincidence with the
proposed host galaxy (GCNs 11464, 11468, 11469).  We place a limit of about
3e-15 erg/cm^2/s (3-sigma) on the flux of the X-ray afterglow at a mean time
of 351.6 ksec after the burst, indicating a decline rate of alpha_X<-1.1.

We thank Harvey Tananbaum and the CXO scheduling staff (in particular Ping
Zhao) for rapidly approving and executing this observation."

[GCN OPS NOTE(23dec10):  Per author's request, the "3.942 hours" was changed
to "3.942 days".]


GRB_name: GRB101224A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11484
SUBJECT: GRB 101224A: Swift detection of a short burst
DATE:    10/12/24 05:56:50 GMT
FROM:    Hans Krimm at NASA-GSFC  <krimm@milkyway.gsfc.nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), M. M. Chester (PSU),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
V. Mangano (INAF-IASFPA), K. L. Page (U Leicester),
J. L. Racusin (NASA/GSFC), A. Rowlinson (U Leicester),
T. Sakamoto (NASA/UMBC) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 05:27:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101224A (trigger=440955).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is RA, Dec 285.926, +45.715 which is 
   RA(J2000) = 19h 03m 42s
   Dec(J2000) = +45d 42' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak with a
duration of about 0.5 sec and some possible later activity.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 05:28:31.4 UT, 77.7 seconds after
the BAT trigger. No source was detected in the promptly available XRT
data. 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 83 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The overlap of the sub-image and the
BAT error circle is uncertain. The overlap of the 8'x8' region for the list of
sources generated on-board and the BAT error circle is uncertain. No correction
has been made for extinction. 

This event is fairly near the galactic plane (galactic lon,lat = 76.11, +17.05 deg) 
so there is a possibility that it is a new galactic transient rather than a GRB. 
Further identification will await analysis of the full data set. 
We also note the presence of the galaxy pair MCG+08-34-033 6.5 arc minutes 
from the center of the BAT field of view.  These galaxies are at a distance
of z = 0.017832 ~75 Mpc

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


GRB_name: GRB101224A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11485
SUBJECT: GRB 101224A - UVOT-enhanced XRT position
DATE:    10/12/24 07:57:45 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

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

Upon analysis of the first downlink of Swift-XRT data for GRB 101224A, a 
faint source was detected within the BAT error circle (Krimm et al., GCN 
Circ. 11484). With the current data, it cannot be confirmed whether this 
source is fading.

Using 1245 s of XRT Photon Counting mode data and 1 UVOT image, 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 = 
285.92460, 45.71350 which is equivalent to:

RA (J2000):  19 03 41.91
Dec (J2000): +45 42 48.5

with an uncertainty of 3.2 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB101224A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11486
SUBJECT: GRB 101224A, Swift-BAT refined analysis
DATE:    10/12/24 14:19:41 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@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), 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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 101224A (trigger #440955)
(Krimm, et al., GCN Circ. 11484).  The BAT ground-calculated position is
RA, Dec = 285.939, 45.706 deg which is
     RA(J2000)  =  19h 03m 45.4s
     Dec(J2000) = +45d 42' 22.3"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 53%.

The light curve consists of a pair of overlapping peaks of total
duration 0.2 sec, T90 (15-350 keV) is 0.2 +- 0.01 sec (estimated error
including systematics).

The time-averaged spectrum from T+0.0 to T+0.3 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index -0.93 +- 1.52,
and Epeak of 95.7 +- 35.2 keV (chi squared 62.87 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.8 +- 1.1 x 10^-8 erg/cm2
and the 1-sec peak flux measured from T-0.34 sec in the 15-150 keV band is
0.7 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.05 +- 0.26 (chi squared 71.61 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level.

The hardness ratio S(50-100 keV)/S(25-50 keV) is 1.94, which when plotted
against burst duration places GRB 101224A among the short-hard bursts in the
distribution.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/440955/BA/


GRB_name: GRB101224A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11487
SUBJECT: GRB101224A: MITSuME Okayama optical upper limits
DATE:    10/12/24 15:02:57 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 101024A (Krimm et al., GCN 11484)
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 2010-12-24 08:59:48 UT (~3.6 hours after
the burst). We did not find any new point source within the
UVOT-enhanced XRT error circle (Page et al., GCNC 11485) 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
------------------------------------------------------
0.18147    09:47:32  4680.0     >19.9  >19.7  >18.9
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB101224A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11488
SUBJECT: GRB 101224A: Swift-XRT refined Analysis
DATE:    10/12/24 16:46:07 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) and H. A. Krimm (CRESST/GSFC/USRA) reports on
behalf of the Swift-XRT team:

We have analysed 7.6 ks of XRT data for GRB 101224A (Krimm  et al. GCN
Circ. 11484), from 86 s to 24.5 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. Using 1245 s of PC mode data and
1 UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 285.92460, +45.71350 which is equivalent to:

RA (J2000): 19h 03m 41.91s
Dec(J2000): +45d 42' 48.5"

with an uncertainty of 3.2 arcsec (radius, 90% confidence).

The afterglow is detected during the first orbit with 12 background
subtracted source counts in 1.3 ks of PC data, at a count rate of 1.0 x
10^-2 counts s^-1, while it's not detected in the following orbits (1
background subtracted source count in 6.3 ks of PC data), for a 3 sigma
upper limit of 1.4 x 10^-3 counts s^-1 

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.1 (+/-1.4). The
best-fitting absorption column is  1.1 (+3.5, -0.6) x 10^21 cm^-2,
consistent with the Galactic value of 4.4 x 10^20 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 2.9 x 10^-11 (5.1 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+3.5, -0.6) x 10^21 cm^-2
Galactic foreground: 4.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      3.1 (+/-1.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00440955.

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


GRB_name: GRB101224A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11489
SUBJECT: GRB 101224A: Fermi GBM observation
DATE:    10/12/24 16:51:15 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

Sheila McBreen reports on behalf of the Fermi GBM Team:

"At 05:27:13.86 UT on 24 December 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101224A (trigger 314861235/101224227),
which was also detected by the Swift/BAT (Krimm et al. 2010, GCN 11484).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 72 degrees.

The GBM light curve consists of one pulse
with a duration of about 0.2 s (50-300 keV).
The time-averaged spectrum from T0-0.064 to T0+0.256 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.83 (+0.38/-0.30) and
the cutoff energy, parameterized as Epeak, is 330 (+402/-150) keV
(CSTAT  509 for 488 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(2.4 +/- 0.5)E-07 erg/cm^2. The 64 ms peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 5.40 +/- 0.82 ph/s/cm^2.

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


GRB_name: GRB101224A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11490
SUBJECT: GRB 101224A: Swift/UVOT Upper Limits
DATE:    10/12/24 17:38:45 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W. Landsman (GSFC/Adnet) and H.A. Krimm (CRESST/NASA/USRA) report on 
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 101224A 83 
s after the BAT trigger (Krimm et al., GCN Circ. 11484).    No optical 
afterglow consistent with the XRT position   (Pagani et al., GCN Circ.  
11488)  is detected in the initial UVOT exposures.   Preliminary 3-sigma 
upper limits using the UVOT photometric system (Poole et al. 2008, 
MNRAS, 383, 627) for the first finding chart (FC) exposure and 
subsequent exposures are:

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

white_FC            83          233          147 > 20.8
u_FC               296          546          246 > 19.6
white               83         7201          659 > 21.9
v                  628        12647         1173 > 20.2
b                  551        24555         1030 > 21.4
u                  296        23977         1583 > 20.8
w1                 677        30339         1644 > 20.8
m2                 652        30016         2569 > 20.8
w2                 601        11734         1179 > 20.7

The values quoted above 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: GRB101224A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11491
SUBJECT: GRB 101224A: Pre-event imaging from DeepSky; Detection of a source in the XRT error circle
DATE:    10/12/24 18:25:20 GMT
FROM:    Josh Bloom at UC Berkeley  <jbloom@astron.berkeley.edu>

P.  E. Nugent (LBNL/UC Berkeley) and J. S. Bloom (UC Berkeley) report:

"We co-added 49 archival images from the DeepSky* project at Palomar
Observatory covering the field of GRB 101224A (Krimm et al., GCN
11484). The images were obtained between 2005-2007 from the
Palomar-Quest Consortium at the Oschin Schmidt telescope.  The 3-sigma
limiting magnitude of the stack is approximately R ~ 23.0 mag.

In the combined image we detect a faint (R = 20.5 +/- 0.2 mag,
preliminary photometry, relative to nearby USNO catalog stars), near
the center of the current XRT error circle (Pagani et al. GCN 11488).
We cannot definitely determine if source is extended or not. An image
of the field may be found at:

   http://lyra.berkeley.edu/~jbloom/grb101224a.pdf

The brightness of the source appears to be just consistent with the
UVOT upper limits (Landsman et al.  GCN 11490), especially given the
relatively red response of DeepSky imaging versus that of the UVOT.
This source may be the (bright) host galaxy or a quiescent counterpart
(if indeed the source is indeed Galactic in origin). However, further
observations are required to establish the connection of this source
to the GRB."

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


GRB_name: GRB101224A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11492
SUBJECT: GRB 101224A: NOT optical observation
DATE:    10/12/24 22:57:24 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

D. Xu (Weizmann Inst.), Ilya Ilyin (AIP), J.P.U. Fynbo (DARK/NBI)
report on a larger collaboration:

We observed the field of GRB 101224A (Krimm et al., GCN 11484; Pagani
& Krimm, GCN 11488) at the Nordic Optical Telescope (NOT) equipped
with StanCam. We obtained 5x300 s R-band images with a median time
20:53:06.8 UT (i.e., 15.4316 hr after the BAT trigger). The lowest
airmass for these five images is 4.0 because the altitude was already
~13 degrees when observations started.

The object shown in the pre-event image (Nugent & Bloom, GCN 11491) is
clearly detected in our stacked image at the same position. The object
is extended along the North-South axis to a considerable extent. We
found R~21.5 mag against nearby two USNO B1 stars. This magnitude is a
bit larger than the measurement from the pre-event image, and we
caution that our images were obtained at high airmass and bias and
flatfield frames are not available yet.


GRB_name: GRB101225A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11493
SUBJECT: Trigger 441015: Swift detection of a possible burst or transient
DATE:    10/12/25 19:19:33 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

J. L. Racusin (NASA/GSFC), A. P. Beardmore (U Leicester),
S. Campana (INAF-OAB), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
O. M. Littlejohns (U Leicester), K. L. Page (U Leicester),
B. Sbarufatti (INAF-OAB/IASFPA) and M. H. Siegel (PSU) report on
behalf of the Swift Team:

At 18:37:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 101225A (trigger=441015).  Swift slewed immediately to the burst. 
However, given that this was a 1088-second image trigger, the time from the
trigger time (at the start of the image interval) to the XRT observation is 
over 23 minutes.  The BAT on-board calculated location is 
RA, Dec 0.234, +44.602 which is 
   RA(J2000) = 00h 00m 56s
   Dec(J2000) = +44d 36' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Since this was an image trigger, the 
currently available BAT light curve does not show significant structure. 

The XRT began observing the field at 19:00:48.5 UT, 1383.0 seconds
after the BAT trigger. XRT found a bright, uncatalogued X-ray source
located at RA, Dec 0.1992, +44.6017 which is equivalent to:
   RA(J2000)  = 00h 00m 47.80s
   Dec(J2000) = +44d 36' 06.1"
with an uncertainty of 5.1 arcseconds (radius, 90% containment). This
location is 89 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 data products have not been received at this time. 

The BAT trigger was an unusually long image trigger.  Due to the 
relative proximity to the Galactic plane (l=113.55,b=-17.35), and lack
of fading  information from XRT at this time, we are unsure if this
trigger is a  GRB or transient.  We will report as more information is
available. 

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


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11494
SUBJECT: GRB 101225A (Swift trigger 441015): optical upper limit
DATE:    10/12/25 21:51:06 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

M. Andreev, A. Sergeev (Terskol Branch of Institute of Astronomy), 
A.Pozanenko (IKI) on behalf of larger GRB follow up collaboration report:

We observed the field of the Swift  trigger 441015 = GRB 101225A? (Racusin 
et al, GCN 11493) with Zeiss-600 telescope of Mt.Terskol observatory.
In the XRT error circle (Racusin et al, GCN 11493) we do not detect any 
sources down to R=21.5 (3 sigma):

UT (mid time), Exposure,  Filter, ULimit
19:46              21 x 120s  R        21.5

The combined image can be found at
http://grb.eam.ru/Swift_441015/Trigger_441015_Zeiss600.jpg 


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11495
SUBJECT: Trigger 441015 / GRB 101225A: NOT optical afterglow candidate
DATE:    10/12/25 22:12:53 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

D. Xu (Weizmann Inst.), I. Ilyin (AIP), J.P.U. Fynbo (DARK/NBI) report
on behalf of a larger collaboration:

We observed the field of GRB 101225A (Racusin et al., GCN 11493) at
the Nordic Optical Telescope (NOT) equipped with StanCam. We obtained
3x300 s exposures in each of the V, R, and I filters, starting at
20:10:33.5 UT, 25/12/2010 (i.e., 1.54681 hrs after the BAT trigger).

Within the XRT error circle only one optical source is detected in our
images in each filter at coordinates

(RA,Dec)(J2000) = (00:00:47.5, +44:36:02.4)
(error-radius:  0.7 arcsec)

This source lies on the southwestern border of the Swift/XRT error
circle and not apparently extended. We found R=22.1+/-0.1 mag
(calibrated with nearby USNO B1 stars) at 20:13:3.5 UT (i.e., 1.58847
hrs after the BAT trigger).

Further NOT observation is undergoing in order to check the brightness
variation of this source.


GRB_name: GRB101225A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11496
SUBJECT: Trigger 441015 / GRB 101225A: Further NOT optical observation
DATE:    10/12/26 01:24:57 GMT
FROM:    Dong Xu at Weizmann Inst  <dong@astro.ku.dk>

D. Xu (Weizmann Inst.), I. Ilyin (AIP), J.P.U. Fynbo (DARK/NBI) report
on behalf of a larger collaboration:

We continued to observe the field of GRB 101225A (Racusin et al., GCN
11493) at the Nordic Optical Telescope (NOT) equipped with StanCam. We
obtained 2x300 s exposures in each of the R and I filters, starting at
23:57:30.9 UT, 25/12/2010 (i.e., 5.32942 hrs after the BAT trigger).

The optical source detected in our previous images (Xu et al., GCN
11495) is still present in the new stacked images for both R and I
filters. We found m(R)=22.6+/-0.2 mag at 00:06:03 UT, 26/12/2010
(i.e., 5.47167 hrs after the BAT trigger), which shows that this
object has decreased 0.5 mag in the R filter between the two epochs
with a mean power-law decay index \alpha~0.4. The magnitude in the I
filter, m(I)=21.6+/-0.2, largely remains unchanged.

We thus conclude that this optical source is likely the afterglow of
GRB 101225A. And further observation is encouraged.


GRB_name: GRB101225A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11497
SUBJECT: GRB 101225A: Enhanced Swift-XRT position
DATE:    10/12/26 04:03:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

Using 6262 s of XRT Photon Counting mode data and 15 UVOT
images for GRB 101225A, 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 = 0.19778, +44.60027 which is equivalent
to:

RA (J2000): 00h 00m 47.47s
Dec (J2000): +44d 36' 01.0"

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

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

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


GRB_name: GRB101225A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11498
SUBJECT: GRB 101225A: Swift-XRT refined Analysis
DATE:    10/12/26 08:03:55 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) and J. L. Racusin (NASA/GSFC) report on behalf
of the Swift-XRT team:

We have analysed 13 ks of XRT data for possible GRB 101225A (Racusin et
al., GCN Circ. 11493), from 1.4 ks to 35.6 ks after the  BAT trigger.
The data comprise 2.7 ks in Windowed Timing (WT) mode with the
remainder in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Evans et al. (GCN. Circ 11497).

The light curve shows substantial structure, but the underlying
continuum can be modelled with a broken power-law decay. The initial
decay index is alpha= 1.108 (+/-0.011). At T+21682 s the decay steepens
to an alpha of 5.93 (+/-0.30). 

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.71 (+/-0.04). The
best-fitting absorption column is  1.78 (+/-0.11) x 10^21 cm^-2, in
excess of the Galactic value of 7.9 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.96 (+/-0.06) and a
best-fitting absorption column of 1.58 (+0.16, -0.15) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.1 x 10^-11 (5.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.58 (+0.16, -0.15) x 10^21 cm^-2
Galactic foreground: 7.9 x 10^20 cm^-2
Excess significance: 17.1 sigma
Photon index:      1.96 (+/-0.06)

If the light curve continues to decay with a power-law decay index of
5.59, the count rate at T+24 hours will be 0.0007 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.7 x
10^-14 (3.7 x 10^-14) erg cm^-2 s^-1. 

We note that this is the brightest afterglow that the XRT has ever
observed at a few thousand seconds after the trigger.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00441015.

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


GRB_name: GRB101225A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11499
SUBJECT: GRB 101225A: Swift/UVOT Detection
DATE:    10/12/26 16:20:36 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@astro.psu.edu>

M. H. Siegel (PSU) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 101225A
1387 s after the BAT trigger (Racusion et al., GCN Circ. 11493).  We  
find
a marginal detection in the later data consistent with the enhanced
XRT position (Evans et al., GCN Circ. 11497).  Preliminary 3-sigma upper
limits and magnitudes using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the  exposures are:

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

V          1387        1705       58    >19.11
V          5572       29944     2601    >21.40
B          1485        1655       38    >19.84
B          5161       28991     3933     21.73+-0.29
U          1460        1630       38    >19.35
U          4955        7534      507    >20.68
UVW1       1435        1754       58    >19.25
UVW1       5982        7413      393     20.58+-0.37
UVM2       1410        1729       58    >18.74
UVM2       5777        7208      393     20.12+-0.34
UVW2       1512        1680       38    >18.82
UVW2       5367        6798      393     19.67+-0.22
UVW2      11650       12550      885     20.35+-0.22
UVW2      17470       18370      885     19.62+-0.15
UVW2      23218       29897     1771     20.10+-0.14

The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB101225A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11500
SUBJECT: GRB 101225A, Swift-BAT refined analysis 
DATE:    10/12/26 17:20:01 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), J. L. Racusin (NASA/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-131 to T+1366 sec from the recent telemetry downlink,
we report further analysis of Swift/BAT GRB 101225A (trigger #441015)
(Racusin, et al., GCN Circ. 11493).  The BAT ground-calculated position is
RA, Dec = 0.2037, +44.5739 deg which is
   RA(J2000)  =  00h 00m 48.9s     Dec(J2000) = +44d 34' 26.0"
with an uncertainty of 3.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-tagged light curve shows that the GRB entered the BAT field of view at
~T-80 sec during a pre-planned slew.  The flux slowly declined after this point
and then increased at about T+600 seconds.  There were less significant
fluctuations until the end of the event data at about T+1300.  T90 (15-350 keV)
is  1088.0 +- 20.0 sec (estimated error including systematics).

The time-averaged spectrum from T+0 to T+963 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.82 +- 0.32.  The fluence in the 15-150 keV band is 1.9 +- 0.4 x 10-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band
is 0.0 +- 0.0 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/441015/BA/


GRB_name: GRB101225A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11501
SUBJECT: Tentative redshift of GRB101225A (Christmas's burst) from Swift-XRT data
DATE:    10/12/27 16:29:52 GMT
FROM:    Sergio Campana at INAF-OAB  <sergio.campana@brera.inaf.it>

S. Campana (INAF-OAB), S. Covino (INAF-OAB),
J.L. Racusin (NASA/GSFC) and K. L. Page (U Leicester)
report on behalf of the Swift Team:

GRB 101225A was detected by Swift BAT as an image trigger (Racusin
al. 2010, GCN 11493). Swift XRT started observing 1383 s after the
trigger observing the main event. The afterglow is very bright and
the XRT remained in the Windowed Timing (WT) mode for two consecutive
orbits. Within each orbit the spectrum remain constant as judged from
the hardness ratio and from the power law photon index.
We extract the XRT spectra for each of the first two orbits, separately.
We then fit the two spectra within XSPEC using the model
tbabs * ztbabs * (cutoff), keeping the same absorption pattern and leaving
free the cutoff power-law model for the two spectra (the cutoff power-law
model provides much better results in terms of column density evaluation
with respect to a simple power-law model when small spectral variations
are present).
We assume a Galactic column density of 7.9x10^20 cm-2 (Kalberla et al.
2005, A&A 440 775) and we allow for a 30% uncertainty in the fit. We
binned the spectra to 50 counts per energy bin and used the latest (v12)
response matrix. The detection in the UVW2 filter by UVOT (Siegel &
Racusin 2010, GCN 11499) constrains the redshift to be <1.4.
The fit with the cutoff power-law is relatively good with a reduced
chi^2 of 1.13 (508 dof).
Motivated by the similarities with GRB 060218 (extremely long duration,
soft prompt-emission spectrum, bright smoothly decaying X-ray afterglow
light curve, UV detection with optical non-detection), we fit the X-ray
spectrum including a blackbody component.
The fit improves considerably (and the cutoff energy goes well above the
XRT energy band, becoming unimportant for both spectra).
The new fit provides a reduced chi^2 of 1.07 (504 dof), based on an F-test
the addition of the blackbody component improves the fit by 4.2 sigma.
In the intrinsic column density vs. redshift plane there is just one
deep minimum hinting for a redshift z=0.07^+0.13_-0.04 (90% confidence
level) and an intrinsic column density N_H(z)=(1.5^+0.5_-0.2)x10^21 cm^-2.
The power law component shows a small softening from the first to the
second orbit, with a photon index around 2.2-2.4.
The blackbody component is hot with a temperature of ~1 keV, consistent
among the two observations. The blackbody radius decreases from the first
observation to the second from ~2x10^10 cm to ~0.6x10^10 cm.

Ground-based optical follow-up observations are strongly encouraged in order
to get spectroscopic confirmation for the redshift estimate and, eventually,
to monitor the coming out of a supernova.


GRB_name: GRB101225A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  11502
SUBJECT: GRB 101225A: WHT observations
DATE:    10/12/27 19:18:03 GMT
FROM:    Klaas Wiersema at U of Leicester  <kw113@star.le.ac.uk>

K. Wiersema, N. Tanvir (Leicester) and A. Levan (Warwick) report:

We observed the afterglow of GRB 101225A (Racusin et al. GCN 11493; Xu et al. 
GCN 11496) with the 4.2m William Herschel Telescope.
We used the ACAM instrument to obtain imaging in r and i filters, and low 
resolution spectroscopy.

The afterglow is clearly detected in individual images of 300 second 
exposure, at R=22.8 +/- 0.2 mag (uncertainties are dominated by scatter in 
USNO-B star magnitudes), at 28.2 hrs after burst. The source appears 
pointlike, in the 1.1 arcsecond seeing conditions. We note that this 
magnitude compared with the Xu et al value (GCN 11496) implies a very 
shallow decay.

We obtained two low resolution spectra immediately following the imaging, 
each with 1200 second exposure time. Continuum emission is detected 
in the 5000 - 9300 A range, but no significant emission or absorption 
lines are detected. Detection of continuum up to 5000 A gives a formal 
constraint on the redshift of z<3.1.

At the redshift estimated by Campana et al. (GCN 11501) we would expect to 
detect emission lines in the ACAM spectra (e.g. Balmer lines, [O III]), 
implying that the spectrum is either strongly dominated by the afterglow 
(the host is faint) or that the emission lines are redshifted into 
wavelength areas dominated by strong skylines.

We thank Ovidiu Vaduvescu for excellent support.


