GRB 100103A
GCN Circular 10307
Subject
GRB 100103A: a long GRB detected with INTEGRAL
Date
2010-01-03T18:45:15Z (15 years ago)
From
Diego Gotz at CEA <diego.gotz@cea.fr>
D.Gotz (CEA-Saclay), S.Mereghetti, A. Paizis, (IASF- Milano), E.
Bozzo, L. Gibaud, M. Beck (ISDC, Versoix), and J. Borkowski (CAMK,
Torun) on behalf of the IBAS Localization Team report:
a long gamma ray burst has been detected by IBAS in the IBIS/ISGRI
data at 17:42:32 U.T. on January 3rd. It lasts about 40 s and its
refined coordinates (J2000) are:
R.A.: 112.366 [degrees]
DEC.: -34.482 [degrees]
with an uncertainty of 1.6 arcmin (90% c.l.).
A preliminary analysis gives a peak flux in the 20-200 keV range of
about 3.5 ph/cmsq/s (1 s integration time) and a fluence over the same
energy range of about 3e-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.
GCN Circular 10308
Subject
GRB 100103A: Swift/XRT position
Date
2010-01-03T21:58:26Z (15 years ago)
From
Jamie A. Kennea at PSU/Swift-XRT <kennea@astro.psu.edu>
J. A. Kennea (PSU) and W. H. Baumgartner (GSFC/UMBC) report on behalf of
the Swift Team:
Swift began a target of opportunity observation of the INTEGRAL detected
GRB 100103A (GCN #10307), at 18:36UT on January 3rd, 2010, approximately
54 mins after the INTEGRAL detection. In approximately 2.5 ks of Photon
Counting mode data, we find an uncatalogued source in the XRT field of
view with a preliminary position of RA, Dec (J2000) = 112.37327,
-34.487811, which is equivalent to:
RA(J2000) = 07h 29m 29.5s
Dec(J2000) = -34d 29' 16.1"
with an estimated uncertainty of 6 arcmins radius (90% confidence). This
position lies 0.5 arcmins from the INTEGRAL reported position. We
currently cannot confirm if this source is fading.
GCN Circular 10309
Subject
GRB 100103A: Correction to Swift position error
Date
2010-01-03T22:04:21Z (15 years ago)
From
Jamie A. Kennea at PSU/Swift-XRT <kennea@astro.psu.edu>
J. A. Kennea (PSU) and W. H. Baumgartner (GSFC/UMBC) report on behalf of
the Swift Team:
The position error in GCN #10308 should be "6 arcseconds radius (90%
confidence)". We apologize for the error.
GCN Circular 10310
Subject
GRB 100103A: Swift/UVOT Upper Limits
Date
2010-01-03T23:57:10Z (15 years ago)
From
Margaret Chester at PSU <chester@astro.psu.edu>
M. M. Chester (PSU), M. H. Siegel (PSU), S. Immler (NASA/CRESST/GSFC),
and W. H. Baumgartner (GSFC/UMBC) report on behalf of the Swift/UVOT
team:
The Swift/UVOT began observing the INTEGRAL-detected GRB 100103A
(D.Gotz, et al., GCN Circ. 10307) at 18:36UT on January 3rd, 2010,
approximately 54 mins after the INTEGRAL detection. No optical
afterglow consistent with the Swift/XRT candidate (J. Kennea, et al.,
GCN Circ. 10308) is detected in the UVOT exposures. Preliminary 3-
sigma upper limits using the UVOT photometric system (Poole et al.
2008, MNRAS, 383, 627) are:
Filter T_start(s) T_stop(s) Exp(s) Mag
----------------------------------------------------------------
v 3244 4409 1165 >20.44
u 4418 5554 1136 >20.70
The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.29 in the direction of the XRT
candidate (Schlegel et al. 1998).
GCN Circular 10311
Subject
Konus-Wind observation of GRB 100103A
Date
2010-01-04T20:02:23Z (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 100103A (Gotz et al., GCN 10307)
triggered Konus-Wind at T0=63766.807s UT (17:42:46.807).
The burst light curve shows a single-pulse structure
with a duration of ~50 s. There is a hint of the soft
extended emission which lasts to ~250 s after T0.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB100103_T63766/
As observed by Konus-Wind the burst
had a fluence of 1.2(+/-0.2)x10-5 erg/cm2,
and a 256-ms peak flux measured from T0+7.168s
of 0.9(+/-0.1)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+41.216 s)
is well fitted in the 20 keV - 2 MeV range by GRB (Band) model for which:
the low-energy photon index alpha = -0.91 (-0.38,+0.63),
the high energy photon index beta = -2.2(<-1.9),
the peak energy Ep = 157(-51, +83)keV (chi2 = 45/57 dof).
The spectrum of the most intense part of the burst (from T0 to T0+8.448 s)
is well fitted in the 20 keV - 2 MeV range by GRB (Band) model for which:
the low-energy photon index alpha = -0.82 (-0.25,+0.28),
the high energy photon index beta = -2.7(<-2.2),
the peak energy Ep = 204(-38, +56)keV (chi2 = 54.8/57 dof).
All the quoted values are preliminary.
All the quoted errors are at the 90% confidence level.
GCN Circular 10312
Subject
GRB 100103A - UVOT-enhanced XRT position
Date
2010-01-05T07:35:56Z (15 years ago)
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:
Using 3971 s of XRT Photon Counting mode data and 2 UVOT images for the
INTEGRAL burst GRB 100103A, 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 = 112.37270, -34.49020 which is equivalent
to:
RA (J2000): 07 29 29.46
Dec (J2000): -34 29 24.9
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
GCN Circular 10313
Subject
GRB 100103A: Swift-XRT team refined analysis
Date
2010-01-06T13:49:35Z (15 years ago)
From
Kim Page at U.of Leicester <kpa@star.le.ac.uk>
K.L. Page (U. Leicester) and W.H. Baumgartner (GSFC/UMBC) report on behalf
of the Swift-XRT team:
We have analysed 8 ks of XRT data for the INTEGRAL GRB 100103A (Gotz et
al. GCN Circ. 10307) obtained during two observations, from 3.3-10.3 ks
and 196-224 ks after the trigger. The source found by Kennea & Baumgartner
(GCN Circ. 10308; improved position given by Page et al. in GCN Circ.
10312) is now clearly fading, with a decay slope of alpha = 0.87 (+0.14,
-0.10). We therefore confirm that this is, indeed, the X-ray afterglow.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.86 (+0.32, -0.30). The
best-fitting absorption column is 6.5 (+1.3, -0.7) x 10^21 cm^-2, in
excess of the Galactic value of 2.4 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 3.9 x 10^-11 (1.7 x 10^-10) erg cm^-2
count^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020125.
This circular is an official product of the Swift-XRT team.
GCN Circular 10314
Subject
GRB 100103A: GROND Upper Limits
Date
2010-01-07T13:08:48Z (15 years ago)
From
Jochen Greiner at MPI <jcg@mpe.mpg.de>
R. Filgas, F. Olivares, J. Greiner, T. Kruehler (all MPE Garching)
and S. Klose (Tautenburg Observatory) report on behalf of the GROND team:
We observed the field of GRB 100103A (INTEGRAL trigger #5970; Gotz et al.,
GCN #10307) 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 January 4, 2010 at
00:48 UT, 7.1 hours after the GRB trigger. They were performed at
variable seeing of 2-3" and at an average airmass of 1.4.
No source is found within the 1.7" XRT error circle (Page et al., GCN #10312).
Comparison to the Digital Sky Survey and 2MASS also reveals no new sources
within a 10 arcsec surrounding. Co-added images of 24.6 min of integration time
in g'r'i'z' and 20 min in JHK, centered at 01:29 UT yield the following
specific upper limits (AB system):
g' > 24.9
r' > 24.2
i' > 23.6
z' > 23.8
J > 21.2
H > 20.6
K > 19.2
calibrated against USNO and 2MASS field stars. No correction for the Galactic
foreground extinction was made, which correspond to a reddening of
E(B-V)=0.29 mag in the direction of the burst (Schlegel et al. 1998).