GRB190103B

This page lists all entries on GRB190103B in GRBweb

Summary IPN Swift GCN 23602 GCN 23603 GCN 23604 GCN 23606 GCN 23607 GCN 23612 GCN 23631 GCN 23684

Summary table
Variable Value Source
T0 21:03:51 UTC GCN_circulars,Swift Det
ra 212.5690° Swift
decl 35.2610° Swift
pos_error 1.81e-04° Swift
T90 19.5 s Swift
T90_start 21:03:51 UTC Swift
fluence 1.20e-05 erg/cm² Swift
T100 19.5 s
GBM_located False
mjd 58486.87767361111 GCN_circulars,Swift Det
IPN table
GRB_name GRB190103B
ra 212.5750°
decl 35.2667°
pos_error 5.00e-02°
Swift table
GRB_name GRB190103B
t_trigger 21:03:51 UTC
ra 212.5690°
decl 35.2610°
pos_error 1.81e-04°
T90 19.5 s
fluence 1.20e-05 erg/cm²
GCN 23602 table
GRB_name GRB190103B
GCN_number 23602
Detection_method Swift Det
t_trigger 21:03:51 UTC
ra 212.5740°
decl 35.2610°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23602 SUBJECT: GRB 190103B: Swift detection of a burst DATE: 19/01/03 21:14:34 GMT FROM: Scott Barthelmy at NASA/GSFC A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. A. Kennea (PSU), H. A. Krimm (NSF/USRA), M. J. Moss (George Washington University), K. L. Page (U Leicester), D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 21:03:51 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190103B (trigger=881709). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 212.574, +35.261, which is RA(J2000) = 14h 10m 18s Dec(J2000) = +35d 15' 40" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows several overlapping peaks with a duration of about 40 sec. The peak count rate was ~5800 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 21:05:24.5 UT, 93.3 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 212.5695, 35.2617 which is equivalent to: RA(J2000) = 14h 10m 16.68s Dec(J2000) = +35d 15' 42.1" with an uncertainty of 4.8 arcseconds (radius, 90% containment). This location is 13 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. The initial flux in the 2.5 s image was 7.42e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 102 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 0.01. Burst Advocate for this burst is A. Y. Lien (amy.y.lien 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.)
GCN 23603 table
GRB_name GRB190103B
GCN_number 23603
Detection_method Swift-XRT Det
ra 212.5693°
decl 35.2610°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23603 SUBJECT: GRB 190103B: Enhanced Swift-XRT position DATE: 19/01/04 01:34:44 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 2781 s of XRT Photon Counting mode data and 5 UVOT images for GRB 190103B, 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 = 212.56927, +35.26100 which is equivalent to: RA (J2000): 14h 10m 16.63s Dec (J2000): +35d 15' 39.6" 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.
GCN 23604 table
GRB_name GRB190103B
GCN_number 23604
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 23604 SUBJECT: GRB 190103B: Swift-XRT refined Analysis DATE: 19/01/04 04:24:42 GMT FROM: Phil Evans at U of Leicester B. Sbarufatti (INAF-OAB/PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), A. Tohuvavohu (PSU) and A.Y. Lien report on behalf of the Swift-XRT team: We have analysed 7.8 ks of XRT data for GRB 190103B (Lien et al. GCN Circ. 23602), from 99 s to 18.1 ks after the BAT trigger. The data comprise 437 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. 23603). The late-time light curve (from T0+4.2 ks) can be modelled with a power-law decay with a decay index of alpha=1.03 (+/-0.10). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.38 (+/-0.06). The best-fitting absorption column is 4.27 (+0.28, -0.27) x 10^21 cm^-2, in excess of the Galactic value of 1.4 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.89 (+/-0.11) and a best-fitting absorption column of 3.9 (+0.6, -0.5) 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 (6.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.9 (+0.6, -0.5) x 10^21 cm^-2 Galactic foreground: 1.4 x 10^20 cm^-2 Excess significance: 11.8 sigma Photon index: 1.89 (+/-0.11) If the light curve continues to decay with a power-law decay index of 1.03, the count rate at T+24 hours will be 0.027 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-12 (1.6 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/00881709. This circular is an official product of the Swift-XRT team.
GCN 23606 table
GRB_name GRB190103B
GCN_number 23606
Detection_method Swift-BAT Det
ra 212.5610°
decl 35.2540°
Circular_text TITLE: GCN CIRCULAR NUMBER: 23606 SUBJECT: GRB 190103B: Swift-BAT refined analysis DATE: 19/01/04 16:24:28 GMT FROM: Amy Lien at GSFC C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (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 190103B (trigger #881709) (Lien, et al., GCN Circ. 23602). The BAT ground-calculated position is RA, Dec = 212.561, 35.254 deg which is RA(J2000) = 14h 10m 14.6s Dec(J2000) = +35d 15' 13.4" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 6%. The mask-weighted light curve shows several overlapping pulses that starts at ~T-10 s and ends at ~T+16 s. The main peak occurs at ~T0. T90 (15-350 keV) is 19.5 +- 2.7 sec (estimated error including systematics). The time-averaged spectrum from T-10.43 to T+16.18 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.99 +- 0.29, and Epeak of 85.0 +- 18.6 keV (chi squared 58.41 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-5 erg/cm2 and the 1-sec peak flux measured from T+0.60 sec in the 15-150 keV band is 16.3 +- 1.5 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.63 +- 0.06 (chi squared 74.91 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/881709/BA/
GCN 23607 table
GRB_name GRB190103B
GCN_number 23607
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 23607 SUBJECT: GRB 190103B: Bassano Bresciano observatory upper limit DATE: 19/01/04 17:41:11 GMT FROM: Ulisse Quadri at Bassano Bresciano Obs U.Quadri, L.Strabla and A.Quadri report: We imaged the field of GRB 190103B detected by SWIFT(trigger 881709) with the robotic telescope of (IAU station 565) Bassano Bresciano Observatory, Italy. Member of: AAVSO - American Association of Variable Star Observers. ISSP - Italian Supernovae Search Project. UAI/SSV - Unione Astrofili Italiani/sezione stelle variabili. The observations started 194.16 min after the GRB trigger, with our Schmidt telescope D=320/400 mm F/D=3.1. Weather conditions were good. We co-added 64 exposures of 240 sec each. Start T0+ End T0+ Vlim 194.16 min 459.27 min 19.5 We did not found any optical counterpart in the error box of the XRTcandidate. A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. A. Kennea (PSU), et al. Magnitudes were estimated with the UCAC4 cat. and are not corrected for galactic dust extinction. Reference: http://www.osservatoriobassano.org/GRB.asp The message may be cited.
GCN 23612 table
GRB_name GRB190103B
GCN_number 23612
Detection_method Konus-Wind Det
t_trigger 21:03:52.010 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 23612 SUBJECT: Konus-Wind observation of GRB 190103B DATE: 19/01/05 19:47:56 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report: The GRB 190103B (Swift detection: Lien et al., GCN 23602; Markwardt et al., GCN 23606) triggered Konus-Wind at T0=75832.010 s UT (21:03:52.010). The burst light curve shows a double-peaked structure which starts at ~T0-10 s and has a total duration of ~27 s. The emission is seen up to ~2 MeV. As observed by Konus-Wind, the burst had a fluence of 1.96(-0.08,+0.08)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+1.408 s, of 3.87(-0.79,+0.79)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+22.528 s) is best fit in the 20 keV - 16 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.17(-0.09,+0.09), and Ep = 142(-9,+11) keV (chi2 = 97/98 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.88 (chi2 = 97/97 dof). The spectrum near the peak count rate (measured from T0+0.256 to T0+6.144 s) is best fit in the 20 keV - 16 MeV range by the power law with exponential cutoff model with alpha = -0.96(-0.10,+0.10), and Ep = 157(-10,+11) keV (chi2 = 90/92 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.92 (chi2 = 90/91 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB190103_T75832/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 23631 table
GRB_name GRB190103B
GCN_number 23631
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 23631 SUBJECT: GRB 190103B: CALET Gamma-Ray Burst Monitor detection DATE: 19/01/07 11:40:49 GMT FROM: Valentin Pal'shin at AGU A. Tezuka, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), S. Matsukawa, H. Onozawa, T. Ito, H. Morita, Y. Sone (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), A. V. Penacchioni, P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 190103B (Swift-BAT trigger #881709: Lien et al., GCN Circ. 23602, Markwardt et al., GCN Circ. 23606; Konus-Wind observation: Tsvetkova et al., GCN Circ. 23612) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 21:03:46.478 UTC on 3 January 2019. The burst signal was seen by all CGBM detectors. The burst light curve shows two multi-peaked pulses which start at T-6.9 sec, peak at T+5.4 sec, and end at T+22.3 sec. The T90 and the T50 durations measured by the SGM data are 19.6 +- 2.5 sec and 9.1 +- 1.0 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1230584543/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.
GCN 23684 table
GRB_name GRB190103B
GCN_number 23684
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 23684 SUBJECT: GRB 190103B: Swift/UVOT Upper Limits DATE: 19/01/14 15:53:58 GMT FROM: Paul Kuin at MSSL A. A. Breeveld (UCL-MSSL) and A. Y. Lien (GSFC/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190103B 103 s after the BAT trigger (Lien et al., GCN Circ. 23602). No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 23603) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 103 253 147 >20.5 u_FC 316 565 246 >19.5 white 103 23827 1860 >21.8 v 646 40393 2202 >20.6 b 571 46547 2987 >21.5 u 316 46101 3922 >21.3 w1 4776 45188 3715 >21.2 m2 4570 41036 2792 >21.1 w2 4161 39480 1904 >21.0 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).