GRB200227A

This page lists all entries on GRB200227A in GRBweb

Summary Fermi GBM IPN Swift GCN 27233 GCN 27234 GCN 27236 GCN 27239 GCN 27243 GCN 27244 GCN 27246 GCN 27249 GCN 27251 GCN 27257 GCN 27265

Summary table
Variable Value Source
GRB_name_Fermi GRB200227306
T0 7:20:08 UTC GCN_circulars,Fermi GBM final loc
ra 56.4327° Swift
decl 9.4823° Swift
pos_error 3.24e-04° Swift
T90 24.32 s Fermi_GBM
T90_error 1.196 s Fermi_GBM
T90_start 7:20:10.047 UTC Fermi_GBM
fluence 1.13e-05 erg/cm² Fermi_GBM
fluence_error 6.08e-08 erg/cm² Fermi_GBM
T100 32.8 s
GBM_located False
mjd 58906.30564814815 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB200227306
trigger_name bn200227306
ra 56.4329°
decl 9.4825°
pos_error 2.56e+00°
datum 2020-02-27
t_trigger 7:20:08.703 UTC
T90 24.32 s
T90_error 1.196 s
T90_start 7:20:10.047 UTC
fluence 1.13e-05 erg/cm²
fluence_error 6.08e-08 erg/cm²
flux_1024 8.82e+00 erg/cm²/s
flux_1024_error 3.54e-01 erg/cm²/s
flux_1024_time 7.10e+00 erg/cm²/s
flux_64 1.14e+01 erg/cm²/s
flux_64_error 1.63e+00 erg/cm²/s
IPN table
GRB_name GRB200227A
ra 56.4375°
decl 9.4833°
pos_error 5.00e-02°
Swift table
GRB_name GRB200227A
t_trigger 7:20:08 UTC
ra 56.4327°
decl 9.4823°
pos_error 3.24e-04°
T90 32.8 s
fluence 7.10e-06 erg/cm²
GCN 27233 table
GRB_name GRB200227A
GCN_number 27233
Detection_method Fermi GBM final loc
t_trigger 7:20:08 UTC
ra 56.9000°
decl 6.3000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27233 SUBJECT: GRB 200227A: Fermi GBM Final Real-time Localization DATE: 20/02/27 07:30:29 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 07:20:08 UT on 27 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200227A (trigger 604480813.702942 / 200227306). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 56.9, Dec = 6.3 (J2000 degrees, equivalent to J2000 03h 47m, 6d 17'), with a statistical uncertainty of 1.0 degrees. The angle from the Fermi LAT boresight is 19.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200227306/quicklook/glg_skymap_all_bn200227306.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/bn200227306/quicklook/glg_healpix_all_bn200227306.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200227306/quicklook/glg_lc_medres34_bn200227306.gif
GCN 27234 table
GRB_name GRB200227A
GCN_number 27234
Detection_method Swift Det
t_trigger 7:20:08 UTC
ra 56.4360°
decl 9.4910°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27234 SUBJECT: GRB 200227A: Swift detection of a burst DATE: 20/02/27 07:37:50 GMT FROM: Sibasish Laha at GSFC S. Laha (GSFC/UMBC/CRESST), C. Gronwall (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 07:20:08 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 200227A (trigger=958592). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 56.436, +9.491 which is RA(J2000) = 03h 45m 45s Dec(J2000) = +09d 29' 27" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 40 sec. The peak count rate was ~4500 counts/sec (15-350 keV), at ~8 sec after the trigger. The XRT began observing the field at 07:21:30.1 UT, 82.2 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 56.43302, 9.48264 which is equivalent to: RA(J2000) = 03h 45m 43.92s Dec(J2000) = +09d 28' 57.5" with an uncertainty of 3.5 arcseconds (radius, 90% containment). This location is 31 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 consistent with the Galactic value of 2.12 x 10^21 cm^-2 (Willingale et al. 2013). The initial flux in the 2.5 s image was 3.08e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 93 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 0.27. Burst Advocate for this burst is S. Laha (sib.laha AT gmail.com). 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 27236 table
GRB_name GRB200227A
GCN_number 27236
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 27236 SUBJECT: GRB 200227A: MITSuME Akeno optical upper limit DATE: 20/02/27 11:59:48 GMT FROM: Motoki Oeda at Tokyo Inst. of Tech. M. Oeda, R. Adachi, K. L. Murata, K. Shiraishi, K. Iida, M. Niwano, F. Ogawa, S. Toma, R. Hosokawa, N. Nakamura, Y. Yatsu, and N. Kawai(TokyoTech) report on behalf of the MITSuME collaboration: We searched for the optical counterpart of GRB 200227A (Fermi GBM Team et al.,GCN Circular #27233, S. Laha et al., GCN Circular #27234) with the optical three color (g’, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 09:05:08 UT. We did not find any new point sources within the Swift/XRT circle (S. Laha et al., GCN Circular #27234) in all three bands. We obtained the 5-sigma limits as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 2.2 09:41:13 900 g’>18.4,Rc>18.2,Ic>17.5 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used UCAC4 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. ,in prep; https://github.com/MNiwano/Eclair)
GCN 27239 table
GRB_name GRB200227A
GCN_number 27239
Detection_method Fermi GBM Det
t_trigger 7:20:08.700 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 27239 SUBJECT: GRB 200227A: Fermi GBM observation DATE: 20/02/27 14:19:53 GMT FROM: Elisabetta Bissaldi at INFN,Bari E. Bissaldi (Politecnico and INFN Bari) reports on behalf of the Fermi GBM Team: "At 07:20:08.70 UT on 27 February 2020, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 200227A (trigger 604480813 / 200227306), which was also detected by the Swift/BAT (Laha et al. 2020, GCN 27234). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 19 degrees. The GBM light curve shows a single broad peak with a duration (T90) of about 24 s (50-300 keV). The time-averaged spectrum from T0 to T0+24 s is adequately fit by a Band function with Epeak = 139 +/- 10 keV, alpha = -0.95 +/- 0.05, and beta = -2.28 +/- 0.11. The event fluence (10-1000 keV) in this time interval is (1.41 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+7.1 s in the 10-1000 keV band is 8.8 +/- 0.4 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 27243 table
GRB_name GRB200227A
GCN_number 27243
Detection_method Swift-XRT Det
ra 56.4327°
decl 9.4823°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27243 SUBJECT: GRB 200227A: Enhanced Swift-XRT position DATE: 20/02/27 19:23:57 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 702 s of XRT Photon Counting mode data and 2 UVOT images for GRB 200227A, 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 = 56.43275, +9.48230 which is equivalent to: RA (J2000): 03h 45m 43.86s Dec (J2000): +09d 28' 56.3" with an uncertainty of 2.5 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 27244 table
GRB_name GRB200227A
GCN_number 27244
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27244 SUBJECT: GRB 200227A: Swift/UVOT Upper Limits DATE: 20/02/27 21:16:21 GMT FROM: Samantha Oates at MSSL S. R. Oates (U. Birmingham) and S. Laha (GSFC/UMBC/CRESST) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 200227A 93 s after the BAT trigger (Laha et al., GCN Circ. 27234). No optical afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 27243) 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 93 243 147 >20.3 u_FC 305 555 246 >19.7 white 93 1185 353 >20.8 v 634 1235 78 >18.3 b 560 1160 58 >19.2 u 305 1135 285 >19.8 w1 685 1284 58 >18.4 m2 659 1259 78 >18.4 w2 610 1210 78 >18.6 The magnitudes in the table are not corrected for the Galactic extinction due to the significant reddening of E(B-V) = 0.28 in the direction of the burst (Schlegel et al. 1998).
GCN 27246 table
GRB_name GRB200227A
GCN_number 27246
Detection_method Swift-BAT Det
ra 56.4330°
decl 9.4890°
Circular_text TITLE: GCN CIRCULAR NUMBER: 27246 SUBJECT: GRB 200227A: Swift-BAT refined analysis DATE: 20/02/28 05:04:40 GMT FROM: Scott Barthelmy at NASA/GSFC J. R. Cummings (CPI), S. D. Barthelmy (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-61 to T+243 sec from recent telemetry downlinks, we report further analysis of BAT GRB 200227A (trigger #958592) (Laha, et al., GCN Circ. 27234). The BAT ground-calculated position is RA, Dec = 56.433, 9.489 deg, which is RA(J2000) = 03h 45m 43.9s Dec(J2000) = +09d 29' 22.0" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 46%. The mask-weighted light curve a couple overlapping peaks starting at T-10 sec, peaking at T+8 sec, and ending at T+90 sec. T90 (15-350 keV) is 32.8 +- 9.7 sec (estimated error including systematics). The time-averaged spectrum from T-0.50 to T+87.64 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.15 +- 0.19, and Epeak of 156.4 +- 88.9 keV (chi squared 55.3 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 7.1 +- 0.2 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T+8.54 sec in the 15-150 keV band is 5.7 +- 0.4 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.46 +- 0.05 (chi squared 63.6 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/958592/BA/
GCN 27249 table
GRB_name GRB200227A
GCN_number 27249
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 27249 SUBJECT: GRB 200227A: Swift-XRT refined Analysis DATE: 20/02/28 07:49:20 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU) and S. Laha (GSFC/UMBC/CRESST) report on behalf of the Swift-XRT team: We have analysed 6.1 ks of XRT data for GRB 200227A (Laha et al. GCN Circ. 27234), from 72 s to 29.1 ks after the BAT trigger. The data comprise 288 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 Beardmore et al. (GCN Circ. 27243). The light curve can be modelled with an initial power-law decay with an index of alpha=3.86 (+0.21, -0.16), followed by a break at T+169 s to an alpha of 1.09 (+0.07, -0.05). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.88 (+0.08, -0.07). The best-fitting absorption column is 5.9 (+/-0.5) x 10^21 cm^-2, in excess of the Galactic value of 2.1 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.83 (+0.17, -0.16) and a best-fitting absorption column of 5.6 (+1.1, -1.0) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.6 x 10^-11 (6.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 5.6 (+1.1, -1.0) x 10^21 cm^-2 Galactic foreground: 2.1 x 10^21 cm^-2 Excess significance: 5.7 sigma Photon index: 1.83 (+0.17, -0.16) If the light curve continues to decay with a power-law decay index of 1.09, the count rate at T+24 hours will be 4.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x 10^-13 (3.3 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00958592. This circular is an official product of the Swift-XRT team.
GCN 27251 table
GRB_name GRB200227A
GCN_number 27251
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 27251 SUBJECT: GRB 200227A: Insight-HXMT/HE detection DATE: 20/02/28 08:57:43 GMT FROM: Qi Luo at IHEP Q. Luo, Y. G. Zheng, C. Cai, S. Xiao, Q. B. Yi, Y. F. DU, W. C. Xue, Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong, C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: At 2020-02-27T07:20:16.15 (T0), Insight-HXMT/HE detected GRB 200227A (trigger ID: HEB200227305) in a routine search of the data, which was also detected by Fermi/GBM (GCN #27233) and Swift-BAT (GCN #27234). The Insight-HXMT/HE light curve mainly consists of two pulses with a duration (T90) of 37.71 s measured from T0-6.92 s. The 1-ms peak rate, measured from T0+1.169 s, is 1862 cnts/sec. The total counts from this burst is 19259 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB200227305_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 (deposited 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. 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.
GCN 27257 table
GRB_name GRB200227A
GCN_number 27257
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 27257 SUBJECT: GRB 200227A: Mondy optical upper limit DATE: 20/02/28 14:30:50 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), E. Mazaeva (IKI), A. Volnova (IKI) report on behalf of IKI-GRB-FuN: We observed the field of GRB 200227A (Fermi GBM Team et al., GCN 27233; Laha et al., GCN 27234) with AZT-33IK telescope of Sayan observatory (Mondy) starting on Feb. 27 (UT) 12:47:07. Within enhanced Swift-XRT position of afterglow (Beardmore et al., GCN 27243) we did not detect optical afterglow in agreement with previously reported non-detection (Oeda et al., GCN 27236; Oates et al., GCN 27244). Preliminary photometry of the field is following. Date UT start, t-T0 Filter Exp. OT UL(3sigma) (mid, days) (s) 2020-02-27 12:47:07 0.24582 R 27*120 n/d 23.2 Photometry is based on the SDSS-DR12 nearby stars (Lupton’s transformation) SDSS-DR12_id R(Lupton) J034542.04+092727.3 18.56 J034546.87+092955.7 17.19 J034534.13+092646.2 17.32
GCN 27265 table
GRB_name GRB200227A
GCN_number 27265
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 27265 SUBJECT: GRB 200227A: RATIR Optical Observations DATE: 20/02/28 20:22:19 GMT FROM: Alan M Watson at UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 200227A (Laha et al., GCN Circ. 27234) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2020/02 28.17 to 2020/02 28.24 UTC (20.84 to 22.53 hours after the BAT trigger), obtaining a total of 0.69 hours exposure in the r and i bands. For a source within the Swift-XRT enhanced error circle (Beardmore et al., GCN Circ. 27243), in comparison with the SDSS DR9, we obtain the following upper limits (3-sigma): r > 19.73 i > 20.33 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.