GRB 101112A
GCN Circular 11396
Subject
GRB 101112A: a long GRB detected by INTEGRAL
Date
2010-11-12T23:03:08Z (15 years ago)
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.
GCN Circular 11397
Subject
GRB101112A: Liverpool Telescope Afterglow Candidate
Date
2010-11-12T23:11:23Z (15 years ago)
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.
GCN Circular 11398
Subject
GRB 101112A: BOOTES-2/TELMA optical afterglow candidate
Date
2010-11-12T23:13:09Z (15 years ago)
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. Jeli�nek, R. Cunniffe
O. Lara-Gil, C. Thoene, S. Guziy, J. Gorosabel (IAA-CSIC Granada),
R. Fernandez-Mu�oz (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.]
GCN Circular 11399
Subject
GRB 101112A - XRT source detection/analysis
Date
2010-11-13T09:28:33Z (15 years ago)
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(J2000.0): 19h 28m 55.08s
Dec (J2000.0): +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.
GCN Circular 11400
Subject
Konus-Wind observation of GRB 101112A
Date
2010-11-13T12:26:47Z (15 years ago)
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.
GCN Circular 11402
Subject
GRB 101112A: optical observations
Date
2010-11-13T18:23:26Z (15 years ago)
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.
GCN Circular 11403
Subject
GRB 101112A: Fermi GBM detection
Date
2010-11-14T00:58:46Z (15 years ago)
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."
GCN Circular 11404
Subject
Possible detection of INTEGRAL burst GRB 101112A by the EVLA
Date
2010-11-14T01:52:45Z (15 years ago)
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."
GCN Circular 11419
Subject
GRB 101112A: OSN and BTA observations
Date
2010-11-19T09:00:43Z (15 years ago)
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.
GCN Circular 11616
Subject
GRB 101112A: Maidanak and CrAO optical observations
Date
2011-01-28T22:36:09Z (14 years ago)
From
Alina Volnova at SAI MSU <alinusss@gmail.com>
GRB 101112A: Maidanak and CrAO optical observations
A. Volnova (SAI MSU), A. Pozanenko (IKI), �. Ezhkova (SAI MSU), �M.
Ibrahimov (MAO), V. Rumyantsev (CrAO), K. Antoniuk (CrAO), B. Satovski
(Astrotel) report on behalf of �larger GRB �follow-up collaboration:
We observed the field of the INTEGRAL GRB 101112A (Gotz et al., GCN
11396) with AZT-22 telescope of �MAO observatory in R-band on Nov.13
between (UT) 13:37:57 - 14:10:56 (Pozanenko et al, GCN 11402) and
Nov.14 between (UT) 14:42:43 - 15:15:49 under
good weather conditions and seeing ~0.9". �Both observational
sequences consist of 6 images with exposure of 300 seconds.
Additionally �we �observed the field �with �AZT-11 telescope of CrAO
in R-band on Nov.13 between (UT) 16:07:10 - 16:52:23.
Near the position of the optical afterglow (Guidorzi et al.GCN 11397,
A. de Ugarte Postigo et al. GCN 11398) there are two bright stars.
They are not separated on DSS and are included in USNO-B1.0 like a
single source USNO-B1.0 1293-0343482 (R = 18.77). In our images the
stars is well separated at the distance 2.7" between them.
The afterglow is in the wing of the southern star. �The star has the
magnitude R = 19.2 +/- 0.08 and coordinates (J2000) RA = 19:28:54.947,
Dec
= +39:21:12.29 �with position uncertainty of 0.15 arcsec. �After
subtraction of a PSF-like profile of the star from stacked image of
Nov.13 in the XRT error circle (Evans et al., GCN 11399) we found a
faint source in coordinates (J2000) RA = 19:28:54.856, Dec =
+39:21:10.67 �with position uncertainty of 0.2 arcsec. This position
is in agreement with afterglow coordinates reported by Guidorzi et al.
(GCN 11397). The distance between southern star and optical afterglow
is ~ 1.9". Using the same procedure we do not detect the afterglow on
Nov.14 �up to 22.5m.
The photometry of the sources based on several field stars from USNO-B1.0:
t-t0 (d), filter tstart �exp.,s ,d OT � �uplim(3 sigma) telescope
0.65558 R �13:37:57 �6*300 �22.2+/-0.20 �22.5 � � �AZT-22
0.76346 R �16:07:10 15*180 �n/d � � � � � � 21.1 � � �AZT-11
1.70060 R �14:42:43 �6*300 � n/d � � � � � � 22.5 � � �AZT-22
Taken together all published photometry of the afterglow (Guidorzi et
al.GCN 11397, Fatkhullin et al. GCN 11419) �we obtained light curve
which can be fairly well described by single power law with
alpha=-1.08.
The finding chart as well as light curve of the GRB 101112A can be
found at http://grb.rssi.ru/GRB101112A/