GRB200219A

This page lists all entries on GRB200219A in GRBweb

Summary Fermi GBM IPN Swift GCN 27123 GCN 27125 GCN 27126 GCN 27137 GCN 27138 GCN 27139 GCN 27142 GCN 27148 GCN 27164 GCN 27165 GCN 27218 GCN 27226 GCN 27245 GCN 27305

Summary table
Variable Value Source
GRB_name_Fermi GRB200219317
T0 7:36:45.513 UTC GCN_circulars,Konus-Wind Det
ra 342.6385° Swift
decl -59.1196° Swift
pos_error 1.81e-04° Swift
T90 1.152 s Fermi_GBM
T90_error 1.032 s Fermi_GBM
T90_start 7:36:49.032 UTC Fermi_GBM
fluence 1.58e-06 erg/cm² Fermi_GBM
fluence_error 4.00e-08 erg/cm² Fermi_GBM
T100 291.487 s
GBM_located False
mjd 58898.3171934375 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB200219317
trigger_name bn200219317
ra 342.6379°
decl -59.1200°
pos_error 6.04e+00°
datum 2020-02-19
t_trigger 7:36:49.096 UTC
T90 1.152 s
T90_error 1.032 s
T90_start 7:36:49.032 UTC
fluence 1.58e-06 erg/cm²
fluence_error 4.00e-08 erg/cm²
flux_1024 5.88e+00 erg/cm²/s
flux_1024_error 2.20e-01 erg/cm²/s
flux_1024_time -1.92e-01 erg/cm²/s
flux_64 1.61e+01 erg/cm²/s
flux_64_error 1.10e+00 erg/cm²/s
IPN table
GRB_name GRB200219A
ra 342.6458°
decl -59.1000°
pos_error 5.00e-02°
Swift table
GRB_name GRB200219A
t_trigger 7:36:49 UTC
ra 342.6385°
decl -59.1196°
pos_error 1.81e-04°
T90 288.0 s
fluence 7.40e-07 erg/cm²
GCN 27123 table
GRB_name GRB200219A
GCN_number 27123
Detection_method Fermi GBM final loc
t_trigger 7:36:49 UTC
ra 344.1000°
decl -60.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27123 SUBJECT: GRB 200219A: Fermi GBM Final Real-time Localization DATE: 20/02/19 07:47:13 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely SHORT GRB At 07:36:49 UT on 19 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200219A (trigger 603790614.095852 / 200219317). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 344.1, Dec = -60.0 (J2000 degrees, equivalent to J2000 22h 56m, -60d 00'), with a statistical uncertainty of 13.9 degrees. The angle from the Fermi LAT boresight is 48.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200219317/quicklook/glg_skymap_all_bn200219317.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200219317/quicklook/glg_healpix_all_bn200219317.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200219317/quicklook/glg_lc_medres34_bn200219317.gif
GCN 27125 table
GRB_name GRB200219A
GCN_number 27125
Detection_method Swift Det
t_trigger 7:36:49 UTC
ra 342.6440°
decl -59.1080°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27125 SUBJECT: GRB 200219A: Swift detection of a short burst DATE: 20/02/19 07:55:10 GMT FROM: David Palmer at LANL A. Y. Lien (GSFC/UMBC), E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), J. A. Kennea (PSU), N. J. Klingler (PSU), K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift Observatory Team: At 07:36:49 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 200219A (trigger=957271). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 342.644, -59.108 which is RA(J2000) = 22h 50m 35s Dec(J2000) = -59d 06' 29" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single peak with a duration of about 1 sec. The peak count rate was ~15000 counts/sec (15-350 keV), at ~0.3 sec after the trigger. The XRT began observing the field at 07:37:56.6 UT, 67.5 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 342.6376, -59.1200 which is equivalent to: RA(J2000) = 22h 50m 33.02s Dec(J2000) = -59d 07' 11.8" with an uncertainty of 2.5 arcseconds (radius, 90% containment). This location is 44 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (1.93 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 6.1 (+3.05/-2.63) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 4.22e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 74 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 0.02. 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/)
GCN 27126 table
GRB_name GRB200219A
GCN_number 27126
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27126 SUBJECT: GRB 200219A: MASTER catalog automatic possible Host Galaxy candidate DATE: 20/02/19 09:29:17 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs N.Tiurina, V. Lipunov, E. Gorbovskoy, V.Kornilov, P.Balanutsa,A.Kuznetsov, V. Vladimirov, O.Gress, D. Vlasenko, F.Balakin, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, D. Kuvshinov, V.Shumkov (Lomonosov Moscow State University, SAI, Physics Department), R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias), R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix Aguilar OAFA), H. Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE), O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API), V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University) MASTER Global Robotic Net Catalog System (http://observ.pereplet.ru, Lipunov et al., 2010,Advances in Astronomy,v. 2010, 30L) reducted GRB 200219A (Lien et al. GCN 27125, Lipunov et al GCN 27124) XRT error box. It found possible Host Galaxy in 1 sec from XRT center error box: The Guide Star Catalog, WISE All-Sky Data Release (Cutri+ 2012) AllWISE Data Release (Cutri+ 2013), The VISTA Hemisphere Survey (VHS) catalog DR4.1 (McMahon+, 2013) RA,DEC (AllWISE) coordinates 22 50 33.023904 -59 07 10.83396 This message can be used.
GCN 27137 table
GRB_name GRB200219A
GCN_number 27137
Detection_method Fermi GBM Det
t_trigger 7:36:49.100 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 27137 SUBJECT: GRB 200219A: Fermi GBM observation DATE: 20/02/19 16:35:50 GMT FROM: Elisabetta Bissaldi at INFN,Bari E. Bissaldi (Politecnico and INFN Bari) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 07:36:49.10 UT on 19 February 2020, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 200219A (trigger 603790614/200219317), which was also detected by the Swift/BAT (Lien et al. 2020, GCN 27125). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 49 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 1.1 s (50-300 keV). The time-averaged spectrum from T0-0.064 s to T0+0.448 s is adequately fit by a power law function with an exponential high-energy cutoff. The power law index is -0.60 +/- 0.06 and the cutoff energy, parameterized as Epeak, is 1.4 +/- 0.2 MeV. The event fluence (10-1000 keV) in this time interval is (2.8 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux measured starting from T0+0.192 s in the 10-1000 keV band is 16.1 +/- 1.1 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN 27138 table
GRB_name GRB200219A
GCN_number 27138
Detection_method Swift-XRT Det
ra 342.6384°
decl -59.1195°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27138 SUBJECT: GRB 200219A: Enhanced Swift-XRT position DATE: 20/02/19 16:48:09 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 1921 s of XRT Photon Counting mode data and 1 UVOT images for GRB 200219A, 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 = 342.63837, -59.11954 which is equivalent to: RA (J2000): 22h 50m 33.21s Dec (J2000): -59d 07' 10.4" with an uncertainty of 1.8 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 27139 table
GRB_name GRB200219A
GCN_number 27139
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27139 SUBJECT: GRB 200219A: Swift-XRT refined Analysis DATE: 20/02/19 16:50:13 GMT FROM: Phil Evans at U of Leicester V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), D.N. Burrows (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB) and A.Y. Lien report on behalf of the Swift-XRT team: We have analysed 6.7 ks of XRT data for GRB 200219A (Lien et al. GCN Circ. 27125), from 57 s to 13.6 ks after the BAT trigger. The data comprise 28 s in Windowed Timing (WT) mode (the first 8 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 27138). We cannot determine at the present time whether the source is fading. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00957271. This circular is an official product of the Swift-XRT team.
GCN 27142 table
GRB_name GRB200219A
GCN_number 27142
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 27142 SUBJECT: GRB 200219A: Swift-XRT refined Analysis correction DATE: 20/02/19 19:03:51 GMT FROM: Elena Ambrosi at INAF-IASF A. D'Ai (INAF-IASFPA), B. Sbarufatti (PSU), D.N. Burrows (PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB) and A. Y. Lien (GSFC/UMBC) report on behalf of the Swift-XRT team: We have analysed 9.8 ks of XRT data for GRB 200219A (Lien et al. GCN Circ. 27125), from 57 s to 24.9 ks after the BAT trigger. The data comprise 165 s in Windowed Timing (WT) mode (the first 8 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 27138). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=1.10 (+/-0.16). At T+136 s the decay steepens to an alpha of 4.7 (+3.3, -0.4) before breaking again at T+444 s to a final decay with index alpha=1.2 (+0.4, -0.6). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.36 (+/-0.06). The best-fitting absorption column is 1.26 (+0.26, -0.24) x 10^21 cm^-2, in excess of the Galactic value of 1.9 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 4.9 x 10^-11 (5.4 x 10^-11) erg cm^-2 count^-1. A summary of the WT-mode spectrum is thus: Total column: 1.26 (+0.26, -0.24) x 10^21 cm^-2 Galactic foreground: 1.9 x 10^20 cm^-2 Excess significance: 7.2 sigma Photon index: 1.36 (+/-0.06) If the light curve continues to decay with a power-law decay index of 1.2, the count rate at T+24 hours will be 2.1 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x 10^-14 (1.1 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00957271. Due to data delivery problems, the GCN Circ. 27139 (D'Elia et al.) was sent while the analysis was still running, which is why it was incomplete. This circular is an official product of the Swift-XRT team.
GCN 27148 table
GRB_name GRB200219A
GCN_number 27148
Detection_method Swift-BAT Det
ra 342.5950°
decl -59.1010°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27148 SUBJECT: GRB 200219A, Swift-BAT refined analysis DATE: 20/02/20 04:14:14 GMT FROM: Amy Lien at GSFC S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), J. P. Norris (BSU), 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-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 200219A (trigger #957271) (Lien et al., GCN Circ. 27125). The BAT ground-calculated position is RA, Dec = 342.595, -59.101 deg which is RA(J2000) = 22h 50m 22.7s Dec(J2000) = -59d 06' 04.5" with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 99%. The mask-weighted light curve shows a short pulse that starts and peaks at ~T0, and ends at ~T+0.5 s. It is followed by an extended emission that lasting until ~T+90 s. In addition, there may be some even weaker emission until ~T+300 s. T90 (15-350 keV) is 288.0 +- 50.6 sec (estimated error including systematics). The time-averaged spectrum from T-0.2 to T+86.7 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.47 +- 0.25. The fluence in the 15-150 keV band is 7.4 +- 1.1 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.268 sec in the 15-150 keV band is 2.4 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. Because the burst seems to be similar to short GRBs with extended emission, we perform further spectral analysis for the short pulse and the extended emission. The short pulse from T-0.224 s to T+0.496 s (determined by the Bayesian block analysis) is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.69 +- 0.14. The fluence in the 15-150 keV band is 2.5 +- 0.2 x 10^-7 erg/cm2. The extended emission from T+0.496 s to T+86.704 s is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.78 +- 0.33. The fluence in the 15-150 keV band is 4.9 +- 1.0 x 10^-7 erg/cm2. The spectral lag of the short pulse is 14 (+5, -5) ms for the 100-350 keV to 25-50 keV bands, and 20 (+15, -10) ms for the 50-100 keV to 15-25 keV bands. These values are more consistent with those of long GRBs. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/957271/BA/
GCN 27164 table
GRB_name GRB200219A
GCN_number 27164
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 27164 SUBJECT: GRB 200219A: FRAM-Auger optical limit DATE: 20/02/21 16:41:40 GMT FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ), Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague, CZ) report: The 30cm robotic telescope FRAM-Auger in Malargue (Argentina) reacted robotically to the Swift/BAT alert of GRB200219A (Lien et al., GCNC 27125, D'Elia et al., GCNC 27139, and Bissaldi et al., GCNC 27137), starting with a series of 20s unfiltered images at 07:43:16 UT, i.e. 6.45 min post trigger. We do not detect any new or strongly variable source at or around the reported gamma-ray errorbox at single frames or a combined 20 x 20s image taken between 6.45 min and 15.39 min after the initial trigger. The combined exposure has a limiting magnitude r'(AB) = 18.9, as calibrated against the APASS Catalogue.
GCN 27165 table
GRB_name GRB200219A
GCN_number 27165
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 27165 SUBJECT: GRB 200219A: UVOT Upper Limits DATE: 20/02/21 18:02:34 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) 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 200219A 75 s after the BAT trigger (Lien et al., GCN Circ. 27125). No optical afterglow consistent with the XRT position (Osborne et al. GCN Circ. 27138) 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 75 225 147 >20.2 u_FC 287 537 246 >19.3 white 75 19365 1139 >21.2 v 617 30839 1770 >19.7 b 543 36572 2257 >20.9 u 287 25105 2431 >20.7 w1 666 40797 1248 >20.4 m2 641 40734 2104 >20.4 w2 592 28878 914 >20.2 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998).
GCN 27218 table
GRB_name GRB200219A
GCN_number 27218
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27218 SUBJECT: GRB 200219A: Chandra rapid ToO upper limit DATE: 20/02/26 06:32:01 GMT FROM: Takanori Sakamoto at AGU T. Sakamoto (AGU), E. Troja (NASA/GSFC/ORAU), J. Norris (BSU), S. D. Barthelmy (GSFC), J. L. Racusin (GSFC), N. Kawai (Tokyo Tech), A. Fruchter (STScI), M. Im (SNU) A Chandra ToO observation of GRB 200219A (Lien et al., GCN Circ. 27125; Bissaldi et al., GCN Circ. 27137) started on February 23 16:32 UT (~4.4 days after the GRB trigger) for a total of 19.2 ksec. We do not detect an X-ray afterglow at the location of the enhanced XRT position (Osborne et al., GCN Circ. 27138). The calculated 3-sigma upper limit is 3.3e-4 c/s in the 0.35-8 keV band using aprates of the CIAO software package. Using the best fit spectral parameters of the XRT PC mode data, we estimated an 3-sigma unabsorbed flux upper limit of 5.0e-15 erg/cm2/s in the 0.35-8 keV band. We would like to thank the Chandra operation team for rapidly approving and making this observation.
GCN 27226 table
GRB_name GRB200219A
GCN_number 27226
Detection_method Konus-Wind Det
t_trigger 7:36:45.513 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 27226 SUBJECT: Konus-Wind observation of GRB 200219A DATE: 20/02/26 16:09:54 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, M. Ulanov, A. Tsvetkova, A. Lysenko, A. Ridnaia, and T. Cline on behalf of the Konus-Wind team, report: The short-duration GRB 200219A (Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27123; Bissaldi and Meegan, GCN Circ. 27137; Swift-BAT detection: Lien et al., GCN Circ. 27125; Laha et al., GCN Circ. 27148) triggered Konus-Wind at T0=27405.513 s UT (07:36:45.513). The burst light curve shows a single multi-peaked pulse which starts at ~T0-0.2 s and has a total duration of ~0.4 s. The emission is seen up to ~8 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB200219_T27405/ As observed by Konus-Wind, the burst had a fluence of 4.12(-0.61,+0.67)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0+0.182 s, of 2.34(-0.73,+0.76)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+0.256 s) is best fit in the 20 keV - 8 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.06(-0.28,+0.35) and Ep = 952(-173,+218) keV (chi2 = 29/27 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.6 (chi2 = 29/26 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 27245 table
GRB_name GRB200219A
GCN_number 27245
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27245 SUBJECT: GRB 200219A: ATCA 5/9 GHz radio observations DATE: 20/02/28 03:46:19 GMT FROM: Gemma Anderson at Curtin U D. d’Antonio (UTS), M. E. Bell (UTS), G. E. Anderson (Curtin), J. Stevens (CASS), P. J. Hancock (Curtin), J. C. A. Miller-Jones (Curtin), M. D. Aksulu (UvA), A. Bahramian (Curtin), K. W. Bannister (CASS), A. J, van der Horst (GWU), S. D. Ryder (Macquarie), J-P. Macquart (Curtin), R. M. Plotkin (UNR), A. Rowlinson (UvA), R. A. M. J. Wijers (UvA) We used the Australia Telescope Compact Array (ATCA) to perform a radio observation of the short GRB 200219A. The scheduled observations began on 2020 Feb 22.8 UT for 7.5 hours (3.5 days post-burst; Fermi GBM Team GCN 27123, A. Y. Lien et al., GCN 27125). No radio source was detected at the XRT position (J.P. Osborne et al., GCN 27138), with preliminary 3 sigma upper-limits of 53 microJy and 57 microJy at 5.5 and 9 GHz, respectively. We thank the ATCA and CSIRO Astronomy and Space Science (CASS) staff for scheduling these observations.
GCN 27305 table
GRB_name GRB200219A
GCN_number 27305
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 27305 SUBJECT: GRB 200219A: AstroSat CZTI detection DATE: 20/03/03 12:36:27 GMT FROM: Soumya Gupta at IUCAA/ASTROSAT S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed the detection of the short GRB 200219A, which was also detected by Fermi GBM Final Real-time (GCN #27123), Swift (Lien A. et al., GCN #27125), MASTER (Tiurina N. et al., GCN #27126), Swift-BAT (Laha S. et al., GCN #27148), FRAM-Auger (Jelinek M. et al., GCN #27164), UVOT (Siegel M. et al., GCN #27165), Konus-Wind (Svinkin D. et al., GCN #27226) and ATCA 5/9 GHz (Antonio D. et al., GCN #27245). The source was clearly detected in the 40-200 keV energy range. The light curve showed a single peak of emission peaking at 2020-02-19 07:36:49 UT. The measured peak count rate associated with the burst is 426 +/- 30.7 cts/s above the background in the combined data of four quadrants, with a total of 413 +/- 4.4 cts. The local mean background count rate was 489 +/- 2.2 cts/s. Using cumulative rates, we measure a T90 of 1.1 +/- 0.45 s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.