GRB140110A

This page lists all entries on GRB140110A in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 15714 GCN 15715 GCN 15716 GCN 15719 GCN 15720 GCN 15721 GCN 15724 GCN 15725 GCN 15726 GCN 15747 GCN 15757

Summary table
Variable Value Source
GRB_name_Fermi GRB140110263
T0 6:18:37.680 UTC Fermi_GBM
ra 28.9000° Fermi_LAT
decl -36.2600° Fermi_LAT
pos_error 5.00e-01° Fermi_LAT
T90 9.472 s Fermi_GBM
T90_error 1.619 s Fermi_GBM
T90_start 6:18:37.680 UTC Fermi_GBM
fluence 5.43e-06 erg/cm² Fermi_GBM
fluence_error 4.53e-08 erg/cm² Fermi_GBM
T100 9.472 s
GBM_located False
mjd 56667.26293611111 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB140110263
trigger_name bn140110263
ra 28.9000°
decl -36.2600°
pos_error 3.41e+00°
datum 2014-01-10
t_trigger 6:18:37.936 UTC
T90 9.472 s
T90_error 1.619 s
T90_start 6:18:37.680 UTC
fluence 5.43e-06 erg/cm²
fluence_error 4.53e-08 erg/cm²
flux_1024 3.58e+00 erg/cm²/s
flux_1024_error 1.79e-01 erg/cm²/s
flux_1024_time 2.69e+00 erg/cm²/s
flux_64 4.84e+00 erg/cm²/s
flux_64_error 9.46e-01 erg/cm²/s
IPN table
GRB_name GRB140110A
ra 28.9000°
decl -36.2667°
pos_error 5.00e-01°
Fermi LAT table
GRB_name_Fermi GRB140110263
GRB_name GRB140110A
MET 411027520.94
datum 2014-01-10
t_trigger 6:18:37.940 UTC
ra 28.9000°
decl -36.2600°
pos_error 5.00e-01°
GCN 15714 table
GRB_name GRB140110A
GCN_number 15714
Detection_method Fermi LAT Det
t_trigger 6:18:37.940 UTC
ra 28.9000°
decl -36.2600°
Circular_text TITLE: GCN CIRCULAR NUMBER: 15714 SUBJECT: GRB 140110A: Fermi-LAT detection of a burst DATE: 14/01/10 13:16:18 GMT FROM: Elisabetta Bissaldi at U.Innsbruk/IAPP 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 15715 table
GRB_name GRB140110A
GCN_number 15715
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 15715 SUBJECT: GRB 140110A Tiled Swift observations DATE: 14/01/10 14:14:10 GMT FROM: Phil Evans at U of Leicester 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 15716 table
GRB_name GRB140110A
GCN_number 15716
Detection_method Fermi GBM Det
t_trigger 6:18:37.940 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 15716 SUBJECT: GRB 140110A: Fermi GBM observation DATE: 14/01/10 16:10:42 GMT FROM: Andreas von Kienlin at MPE 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 15719 table
GRB_name GRB140110A
GCN_number 15719
Detection_method Swift-UVOT Other
ra 28.7396°
decl -36.2774°
Circular_text TITLE: GCN CIRCULAR NUMBER: 15719 SUBJECT: GRB 140110A: OT detection in Swift/UVOT imaging DATE: 14/01/10 21:31:17 GMT FROM: Dong Xu at DARK/NBI 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 15720 table
GRB_name GRB140110A
GCN_number 15720
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 15720 SUBJECT: GRB 140110A: Reported UVOT OT not GRB afterglow DATE: 14/01/10 22:11:38 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT 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 15721 table
GRB_name GRB140110A
GCN_number 15721
Detection_method Swift Other
ra 28.5843°
decl -36.4934°
Circular_text TITLE: GCN CIRCULAR NUMBER: 15721 SUBJECT: GRB 140110A: Swift XRT observations DATE: 14/01/11 12:03:01 GMT FROM: Alessandro Maselli at INAF/IASF Palermo 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 15724 table
GRB_name GRB140110A
GCN_number 15724
Detection_method Swift-UVOT Det
ra 29.2999°
decl -36.2967°
Circular_text TITLE: GCN CIRCULAR NUMBER: 15724 SUBJECT: GRB 140110A: Swift/UVOT Observations DATE: 14/01/11 18:28:39 GMT FROM: Samantha Oates at MSSL 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 15725 table
GRB_name GRB140110A
GCN_number 15725
Detection_method IPN Triangulation
t_trigger 6:18:38 UTC
ra 299.5700°
decl -22.8280°
Circular_text TITLE: GCN CIRCULAR NUMBER: 15725 SUBJECT: IPN Triangulation of GRB 140110A DATE: 14/01/11 21:02:15 GMT FROM: Valentin Pal'shin at Ioffe Inst 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 15726 table
GRB_name GRB140110A
GCN_number 15726
Detection_method retraction
Circular_text TITLE: GCN CIRCULAR NUMBER: 15726 SUBJECT: GRB 140110A: Swift/UVOT retraction of UVOT candidates DATE: 14/01/12 13:45:30 GMT FROM: Samantha Oates at MSSL 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 15747 table
GRB_name GRB140110A
GCN_number 15747
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 15747 SUBJECT: GRB 140110A: Further Swift-XRT Observation DATE: 14/01/16 16:36:12 GMT FROM: Alessandro Maselli at INAF/IASF Palermo 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 15757 table
GRB_name GRB140110A
GCN_number 15757
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 15757 SUBJECT: GRB 140110A: Second Follow-up Swift-XRT Observation DATE: 14/01/22 14:29:04 GMT FROM: Alessandro Maselli at INAF/IASF Palermo 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.