GRB180210A

This page lists all entries on GRB180210A in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 22407 GCN 22408 GCN 22409 GCN 22412 GCN 22413 GCN 22415 GCN 22450

Summary table
Variable Value Source
GRB_name_Fermi GRB180210517
T0 12:24:38 UTC Fermi_LAT
ra 1.8000° Fermi_LAT
decl 18.3500° Fermi_LAT
pos_error 1.80e-01° Fermi_LAT
T90 38.913 s Fermi_GBM
T90_error 0.724 s Fermi_GBM
T90_start 12:24:42.644 UTC Fermi_GBM
fluence 4.42e-05 erg/cm² Fermi_GBM
fluence_error 4.83e-08 erg/cm² Fermi_GBM
T100 43.557 s
GBM_located False
mjd 58159.51710648148 Fermi_LAT
Fermi GBM table
GRB_name_Fermi GRB180210517
trigger_name bn180210517
ra 1.8417°
decl 18.5528°
pos_error 2.57e+00°
datum 2018-02-10
t_trigger 12:24:38.548 UTC
T90 38.913 s
T90_error 0.724 s
T90_start 12:24:42.644 UTC
fluence 4.42e-05 erg/cm²
fluence_error 4.83e-08 erg/cm²
flux_1024 1.67e+01 erg/cm²/s
flux_1024_error 3.38e-01 erg/cm²/s
flux_1024_time 2.39e+01 erg/cm²/s
flux_64 2.36e+01 erg/cm²/s
flux_64_error 1.54e+00 erg/cm²/s
IPN table
GRB_name GRB180210A
ra 1.8000°
decl 18.3500°
pos_error 1.83e-01°
Fermi LAT table
GRB_name_Fermi GRB180210517
GRB_name GRB180210A
MET 539958283.0
datum 2018-02-10
t_trigger 12:24:38 UTC
ra 1.8000°
decl 18.3500°
pos_error 1.80e-01°
GCN 22407 table
GRB_name GRB180210A
GCN_number 22407
Detection_method Fermi GBM Det
t_trigger 12:24:38.550 UTC
ra 3.3300°
decl 21.0100°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22407 SUBJECT: GRB 180210A: Fermi GBM detection DATE: 18/02/10 17:28:41 GMT FROM: Elisabetta Bissaldi at INFN,Bari E. Bissaldi (Politecnico & INFN Bari) reports on behalf of the Fermi GBM Team: "At 12:24:38.55 UT on 10 February 2018, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 180210A (trigger 539958283 / 180210517). The on-ground calculated location, using the GBM trigger data, is RA = 3.33, DEC = 21.01 (J2000 degrees), with an uncertainty of 1.5 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg systematic error [Connaughton et al. 2015, ApJS, 216, 32]). The trigger resulted in an Autonomous Repoint Request (ARR) by the GBM Flight Software owing to the high peak flux of the GRB. This ARR was accepted and the spacecraft slewed to the GBM in-flight location. The initial angle from the Fermi LAT boresight to the GBM ground location is 31 degrees. The GBM light curve consists of a multi-peaked emission episode with a duration (T90) of about 40 s (50-300 keV). The time-averaged spectrum from T0 to T0+31 s is best fit by a Band function with Epeak = 145 +/- 3 keV, alpha = -0.45 +/- 0.02, and beta = -2.60 +/- 0.06. The event fluence (10-1000 keV) in this time interval is (4.21 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+24 s in the 10-1000 keV band is 16.7 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 22408 table
GRB_name GRB180210A
GCN_number 22408
Detection_method Fermi LAT Det
t_trigger 12:24:38.550 UTC
ra 1.8000°
decl 18.3500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22408 SUBJECT: GRB 180210A: Fermi-LAT detection DATE: 18/02/10 20:00:21 GMT FROM: Elisabetta Bissaldi at INFN,Bari F. Dirirsa (U. Johannesburg) and E. Bissaldi (Politecnico & INFN Bari) report on behalf of the Fermi-LAT team: "At 12:24:38.55 UT on February 10, 2018 Fermi-LAT detected high-energy emission from GRB 180210A, which was also detected by Fermi-GBM (trigger 539958283/180210517) (E. Bissaldi, GCN 22407). The best LAT on-ground location is found to be RA, Dec = 1.80, 18.35 (J2000 deg) with an error radius of 0.18 deg (90 % containment, statistical error only). This was 30 deg from the LAT boresight at the time of the trigger and triggered an autonomous repoint of the spacecraft. The data from the Fermi-LAT show a significant increase in the event rate that is spatially correlated with the trigger with high significance. The highest-energy photon is a 4 GeV event which is observed 363 seconds after the GBM trigger. A Swift ToO has been approved for this burst. The Fermi-LAT point of contact for this burst is Feraol F. Dirirsa (fdirirsa@uj.ac.za). 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 22409 table
GRB_name GRB180210A
GCN_number 22409
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22409 SUBJECT: GRB 180210A: Swift ToO observations DATE: 18/02/10 21:10:45 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/LAT GRB 180210A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/ToO_GRBs/00020787 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the Fermi/LAT event. 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; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team.
GCN 22412 table
GRB_name GRB180210A
GCN_number 22412
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22412 SUBJECT: GRB 180210A: Tiled Swift observations DATE: 18/02/11 19:31:45 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 180210A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00069 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; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team.
GCN 22413 table
GRB_name GRB180210A
GCN_number 22413
Detection_method Swift-XRT Other
ra 1.8418°
decl 18.5527°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22413 SUBJECT: GRB 180210A: Swift-XRT afterglow detection DATE: 18/02/12 14:45:50 GMT FROM: Valerio D'Elia at ASDC A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), S. J. LaPorte (PSU), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), S.L. Gibson (U. Leicester) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 180210A (Dirirsa et al. GCN Circ. 22408), collecting 7.5 ks of Photon Counting (PC) mode data between T0+31.0 ks and T0+117.4 ks. Four uncatalogued X-ray sources are detected, of which one ("Source 1", the brightest) is fading with 3-sigma significance, and is therefore likely the GRB afterglow. Using 4922 s of PC mode data and 4 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 1.84177, +18.55274 which is equivalent to: RA (J2000): 00h 07m 22.02s Dec(J2000): +18d 33' 09.9" with an uncertainty of 1.7 arcsec (radius, 90% confidence). This position is 12.4 arcmin from the Fermi/LAT position. The light curve can be modelled with a power-law decay with a decay index of alpha=1.57 (+0.36, -0.28). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.3 (+/-0.4). The best-fitting absorption column is 3.6 (+1.7, -1.4) x 10^21 cm^-2, in excess of the Galactic value of 3.7 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 2.7 x 10^-11 (5.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.6 (+1.7, -1.4) x 10^21 cm^-2 Galactic foreground: 3.7 x 10^20 cm^-2 Excess significance: 3.7 sigma Photon index: 2.3 (+/-0.4) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020787. The results of the full analysis of the XRT observations are available at http://www.swift.ac.uk/ToO_GRBs/00020787. This circular is an official product of the Swift-XRT team.
GCN 22415 table
GRB_name GRB180210A
GCN_number 22415
Detection_method Konus-Wind Det
t_trigger 12:24:38.454 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22415 SUBJECT: Konus-Wind observation of GRB 180210A DATE: 18/02/14 13:27:42 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, A. Tsvetkova, A. Lysenko, A.Kozlova, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 180210A (Fermi-GBM detection: Bissaldi, GCN Circ. 22407; Fermi-LAT detection: Dirirsa and Bissaldi, GCN Circ. 22407) triggered Konus-Wind at T0=44678.454 s UT (12:24:38.454). The burst light curve shows a multipeaked structure which starts at ~T0-6 s and has a total duration of ~65 s. The emission is seen up to ~5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB180210_T44678/ As observed by Konus-Wind, the burst had a fluence of 4.81(-0.30,+0.36)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+20.224 s, of 5.35(-1.07,+1.10)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+47.360 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.49(-0.13,+0.15), the high energy photon index beta = -3.12(-0.54,+0.30), the peak energy Ep = 153(-8,+8) keV (chi2 = 84/97 dof). The spectrum near the maximum count rate (measured from T0+16.128 to T0+22.784 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) model with the following parameters: the low-energy photon index alpha = -0.08(-0.24,+0.27), the high energy photon index beta = -3.25(-1.02,+0.37), the peak energy Ep = 152(-11,+12) keV (chi2 = 106/91 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 22450 table
GRB_name GRB180210A
GCN_number 22450
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22450 SUBJECT: GRB 180210A: Insight-HXMT/HE observation DATE: 18/02/26 02:59:43 GMT FROM: Xuefeng Lu at IHEP X. F. Lu, J. Y. Liao, C. K. Li, Y. Huang, Y. Zhu, S. L. Xiong, X. B. Li, C. Z. Liu, Z. W. Li, J. L. Zhao, Y. F. Zhang, X.F. Li, Z. Chang, Y. J. Jin, C. L. Zou (IHEP), A. M. Zhang, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, H. Y. Wang, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: At 2018-02-10T12:24:38.55 UT, the Insight-HXMT/HE detected GRB 180210A(trigger ID: HEB180210517) in a routine search of the data, which was also triggered by Fermi/GBM(GCN Circ. 22407),Fermi/LAT(GCN Circ. 22408), Swift/XRT(GCN Circ. 22413) and KONUS-Wind(GCN Circ. 22415). The Insight-HXMT/HE light curve consists of a multi-peaked pulse with a duration (T90) of 26.7 s measured from T0+3.9 s. The 1-s peak rate, measured from T0+23.9 s, is 3173.8 cnts/sec. The total counts from this burst is 40447.9 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB180210517_lc.jpg All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (record energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. The time-averaged spectrum from T0-8 to T0+30 s is adequately fit by a Power Law model with spectral index = -1.86 +/- 0.03. The energy fluence is (4.5 +/- 0.2) E-05 erg/cm^2 in 200 - 5000 keV in this time interval. The analysis results presented above are preliminary, final results will be published elsewhere. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org/index.php/enhome. [GCN OPS NOTE(26feb18): "2018-02-10T17:29:06.000" was changed to "2018-02-10T12:24:38.55" and "HEB180210728" was changed to "HEB180210517".]