GRB 140110A
GCN Circular 15714
Subject
GRB 140110A: Fermi-LAT detection of a burst
Date
2014-01-10T13:16:18Z (11 years ago)
From
Elisabetta Bissaldi at U.Innsbruk/IAPP <Elisabetta.Bissaldi@uibk.ac.at>
E. Bissaldi (University & INFN Trieste), E. Sonbas (Adiyaman University),
F. Longo (University & INFN Trieste), and J. Racusin (NASA/GSFC),
report on behalf of the Fermi-LAT team:
Starting at 06:18:37.94 on January 10th, 2014, Fermi LAT detected
high energy emission from GRB 140110A, which was also detected
by Fermi-GBM (trigger 411027520).
The best LAT on-ground location is found to be RA, Dec 28.90, -36.26 (J2000)
with an error radius of 0.50 deg (90% containment, statistical error only).
This was 30 deg from the LAT boresight at the time of the trigger.
Only the first 1300 s of LAT data have been processed.
They show a significant increase in the event rate within 5 degrees
of the GBM location after the GBM trigger that is spatially and temporally
correlated with the GBM emission with high significance.
Around 20 photons above 100 MeV are observed within 200 seconds.
The highest energy photon is a 735 MeV event which is observed
160 seconds after the GBM trigger.
A Swift ToO has been requested for this burst.
The Fermi LAT point of contact for this burst is
Elisabetta Bissaldi (Elisabetta.Bissaldi@ts.infn.it).
The Fermi LAT is a pair conversion telescope designed to cover the
energy band
from 20 MeV to greater than 300 GeV. It is the product of an international
collaboration between NASA and DOE in the U.S. and many scientific
institutions
across France, Italy, Japan and Sweden.
GCN Circular 15715
Subject
GRB 140110A Tiled Swift observations
Date
2014-01-10T14:14:10Z (11 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 140110A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00023
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
GCN Circular 15716
Subject
GRB 140110A: Fermi GBM observation
Date
2014-01-10T16:10:42Z (11 years ago)
From
Andreas von Kienlin at MPE <azk@mpe.mpg.de>
A. von Kienlin (MPE) and V. Connaughton (UAH)
report on behalf of the Fermi GBM Team:
"At 06:18:37.94 UT on 10 January 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140110A (trigger 411027520 / 140110263), which was
also detected by Fermi/LAT (Bissaldi et al. 2014, GCN 15714).
The GBM on-ground location is consistent with the LAT position. The angle
from the Fermi LAT boresight at the time of the trigger is 34 degrees.
The GBM light curve shows a single pulse with a duration (T90)
of about 9 s (50-300 keV). The time-averaged spectrum from T0-0.524 s to
T0+5.764 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.61 (+0.07/-0.06) and
the cutoff energy, parameterized as Epeak, is 1550 (+300/-250) keV.
The event fluence (10-1000 keV) in this time interval is
(7.1 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+2.69 s in the 10-1000 keV band
is 3.6 +/- 0.2 ph/s/cm^2.
A Band function fits the spectrum equally well with Epeak= 1400(+290/-260)
keV,
alpha = -0.59 (+0.08/-0.07) and beta = -2.7 (+0.4/-1.1) .
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 15719
Subject
GRB 140110A: OT detection in Swift/UVOT imaging
Date
2014-01-10T21:31:17Z (11 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI) reports
Inspection of the UVOT u-band image of the field1 of the tiled Swift
observations (Evans, GCN 15715) reveals a very bright optical source,
no present at DSS, at coordinates
R.A. = 01:54:57.50
Dec. = -36:16:38.71
Error Circ. ~ 1.5 arcsec
No known minor planet, near-Earth object, and comet would appear at
this position at the UVOT observational time.
Thus this object could be the optical afterglow of GRB 140110A, and
may worth some photometric follow-ups to check its variation.
GCN Circular 15720
Subject
GRB 140110A: Reported UVOT OT not GRB afterglow
Date
2014-01-10T22:11:38Z (11 years ago)
From
Jamie A. Kennea at PSU/Swift-XRT <kennea@swift.psu.edu>
J. A. Kennea and M. M. Chester (PSU) report on behalf of the Swift team:
The UVOT detected optical transient reported by Xu (GCN 15719) is not
related to GRB 140110A (Bissaldi et al., GCN 15714). The transient appears
at different locations in two observations taken by UVOT as part of the
Swift target-of-opportunity observations of GRB 140110A (Evans, GCN
15715). We believe that this transient is most likely an optical artifact.
GCN Circular 15721
Subject
GRB 140110A: Swift XRT observations
Date
2014-01-11T12:03:01Z (11 years ago)
From
Alessandro Maselli at INAF/IASF Palermo <maselli@ifc.inaf.it>
A. Maselli (INAF-IASFPA), S. Campana (INAF-OAB), D. Malesani (DARK/NBI)
and P. A. Evans (U. Leicester) report on behalf of the Swift team:
Swift-XRT has observed the error circle of the Fermi/LAT GRB 140110A
(Bissaldi et al., GCN 15714), also detected by Fermi/GBM (von Kienlin &
Connaughton, GCN 15716), in a series of observations tiled on the sky.
The total exposure time is 12.8 ks spread over 7 fields; the maximum
exposure within the sky observed was 3.9 ks. The observations started
28.4 ks after the Fermi/LAT trigger. Within these data there are two
objects (source #1 and source #3) which are in the 1RXS catalogue and
five sources which are not catalogued in X-rays. At the present time we
cannot be sure which of these, if any, is the afterglow. However, we
note that the light curve of source #2, with a mean count rate of (1.23
� 0.27) x 10^-2 ct s^-1, suggests evidence of decay.
Source details:
Source 1
RA: 28.58425 = 01h 54m 20.22s (J2000)
Dec: -36.49342 = -36d 29' 36.3" (J2000)
Err: 4.4" (radius, 90% confidence)
Exposure time: 1.7 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_1.php
Source 2
RA: 28.53253 = 01h 54m 7.81s (J2000)
Dec: -36.12000 = -36d 07' 12.0" (J2000)
Err: 5.4" (radius, 90% confidence)
Exposure time: 2.6 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_2.php
Source 3
RA: 28.63188 = 01h 54m 31.65s (J2000)
Dec: -36.70189 = -36d 42' 06.8" (J2000)
Err: 5.4" (radius, 90% confidence)
Exposure time: 1.5 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_3.php
Source 4
RA: 29.24134 = 01h 56m 57.92s (J2000)
Dec: -36.06453 = -36d 03' 52.3" (J2000)
Err: 6.2" (radius, 90% confidence)
Exposure time: 1.6 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_4.php
Source 5
RA: 28.36418 = 01h 53m 27.40s (J2000)
Dec: -36.32146 = -36d 19' 17.3" (J2000)
Err: 5.7" (radius, 90% confidence)
Exposure time: 1.7 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_5.php
Source 6
RA: 28.46195 = 01h 53m 50.87s (J2000)
Dec: -36.04399 = -36d 02' 38.4" (J2000)
Err: 6.2" (radius, 90% confidence)
Exposure time: 1.0 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_6.php
Source 7
RA: 28.94482 = 01h 55m 46.76s (J2000)
Dec: -36.43079 = -36d 25' 50.8" (J2000)
Err: 6.2" (radius, 90% confidence)
Exposure time: 2.7 ks
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/index_7.php
This circular is an official product of the Swift-XRT team.
GCN Circular 15724
Subject
GRB 140110A: Swift/UVOT Observations
Date
2014-01-11T18:28:39Z (11 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (UCL-MSSL) and M. Stamatikos (OSU) report on behalf of the Swift/UVOT team:
The Swift/UVOT observed the error circle of the Fermi/LAT GRB 140110A
(Bissaldi et al., GCN Circ. 15714) in a series of u band observations
tiled on the sky. The total exposure time is 12.7 ks spread over 7
fields; each field was observed typically for 1.8 ks. Observations
started 28.4 ks after the Fermi/LAT trigger. At the locations of the
XRT candidates (Maselli et al., GCN Circ. 15721), we find sources
2 and 6 lie outside of the UVOT field of view, while the rest are
consistent with known objects within the USNO-B1 catalogue.
However, within the UVOT fields we find two uncatalogued sources:
The refined UVOT position for UVOT source 1 is:
RA (J2000) 1:57:11.98
Dec (J2000) -36:17:48.2
The refined UVOT position for UVOT source 2 is:
RA (J2000) 1:55:13.95
Dec (J2000) -35:54:14.0
both positions have an estimated uncertainty of 0.6 arcsec (radius, 90% confidence).
At this time we are unable to determine if either of these sources are fading.
Preliminary magnitudes for the two UVOT uncatalogued sources using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:
Source Filter T_start(s) T_stop(s) Exp(s) Mag
UVOT1 u 28798 30607 1734 19.63 +/- 0.10
UVOT2 u 30251 63599 1793 19.56 +/- 0.10
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 15725
Subject
IPN Triangulation of GRB 140110A
Date
2014-01-11T21:02:15Z (11 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,
V. Pal'shin on behalf of the IPN,
V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein,
on behalf of the Fermi GBM team, and
S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on
behalf of the Swift-BAT team, report:
The long-duration GRB 140110A (Bissaldi et al., GCN Circ. 15714; von
Kienlin & Connaughton, GCN Circ. 15716) has been also observed by Swift
(BAT), and MESSENGER (GRNS), so far, at about 22718 s UT (06:18:38). The
burst was outside the coded field of view of the BAT.
We have triangulated this GRB to a GBM-MESSENGER annulus centered at
RA(2000)=299.570 deg (19h 58m 17s) Dec(2000)=-22.828 deg (-22d 49'
41"), whose radius is 76.183 �� 0.140 deg (3 sigma).
This annulus intersects the Fermi-LAT 90% CL error circle (Bissaldi et
al., GCN Circ. 15714) to form an error box whose area is about 3 times
smaller than that of the LAT error circle, and whose
corners are:
-----------------------------------------------
RA(2000), deg Dec(2000), deg
-----------------------------------------------
Corners:
29.211 (01h 56m 51s) -36.693 (-36d 41' 35")
28.826 (01h 55m 18s) -35.764 (-35d 45' 49")
28.614 (01h 54m 27s) -35.817 (-35d 49' 00")
28.999 (01h 56m 00s) -36.754 (-36d 45' 13")
-----------------------------------------------
This box may be improved.
Only one of the reported XRT sources (Maselli et al., GCN Circ. 15721),
the source 7, is consistent with the IPN annulus and, hence, can be the
afterglow.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140110_T22717/IPN/
GCN Circular 15726
Subject
GRB 140110A: Swift/UVOT retraction of UVOT candidates
Date
2014-01-12T13:45:30Z (11 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (UCL-MSSL) and M. Stamatikos (OSU) report on behalf of the Swift/UVOT team:
We have further investigated source 2 from Oates et al. (GCN 15724). While this source
is not present in the USNO-B1 catalogue, it is present in the DSS and GSC-2.3 catalogue.
We therefore retract this source as a potential afterglow candidate for GRB 140110A.
We also note that source 1 is not within the IPN annulus (Hurley et al., GCN 15725) and
is therefore also unlikely to be the optical afterglow for this GRB.
GCN Circular 15747
Subject
GRB 140110A: Further Swift-XRT Observation
Date
2014-01-16T16:36:12Z (11 years ago)
From
Alessandro Maselli at INAF/IASF Palermo <maselli@ifc.inaf.it>
A. Maselli (INAF-IASFPA), D. Malesani (DARK/NBI) and P. A. Evans (U.
Leicester) report on behalf of the Swift team:
On 2014 January 15, Swift has returned to observe the field of the Fermi
GRB 140110A (Bissaldi et al., GCN 15714; von Kienlin & Connaughton, GCN
15716). Five uncatalogued X-ray sources were listed by Maselli et al.
(GCN 15721) as a result of the analysis of seven tiled XRT observations
(Evans, GCN 15715) carried out on January 10. According to Pal'shin et
al. (GCN 15725), the position of just one of these sources (#7) is
consistent with the IPN annulus.
During the XRT observation carried out on January 15, which started 455
ks after the LAT trigger, the source #7 was detected at a mean count
rate of 2.64 (+1.06, -0.84) x 10^-3 ct s^-1 which is consistent with the
one [2.61 (+1.25, -0.95) x 10^-3 ct s^-1] corresponding to five days
earlier. Consequently, this source is unlikely to be the afterglow of
GRB 140110A. Further details of the XRT analysis carried out on the
field of GRB 140110A are available at the following link:
http://www.swift.ac.uk/xrt_products/TILED_GRB00023/.
This circular is an official product of the Swift-XRT team.
GCN Circular 15757
Subject
GRB 140110A: Second Follow-up Swift-XRT Observation
Date
2014-01-22T14:29:04Z (11 years ago)
From
Alessandro Maselli at INAF/IASF Palermo <maselli@ifc.inaf.it>
A. Maselli (INAF-IASFPA) and P. A. Evans (U. Leicester) report on behalf
of the Swift team:
Swift carried out a second follow-up observation to investigate the
behaviour of the X-ray source #2 reported by Maselli et al. (GCN 15721)
as a result of the analysis of tiled observations covering the LAT error
circle. This source, although outside the error box formed by the
intersection between the LAT error circle and the IPN annulus reported
by Pal'shin et al.(GCN 15725), suggested initially a possible fading
behaviour (Maselli et al., GCN 15721).
The new observation started on January 21, 928 ks after the LAT trigger,
and had an exposure of 6.3 ks. The source #2 has been detected with a
mean count rate of (1.24 � 0.16) x 10^-2 ct s^-1 which is consistent
with the one (1.23 � 0.27) x 10^-2 ct s^-1 corresponding to eleven days
earlier. Therefore, we exclude that it may be the afterglow of GRB 140110A.
The Swift-XRT tiled observations have covered the whole error box
reported by Pal'shin et al. (GCN 15725) and no credible counterpart for
the X-ray afterglow has been detected (see also Maselli et al., GCN 15747).
This circular is an official product of the Swift-XRT team.