GRB230903A

This page lists all entries on GRB230903A in GRBweb

Summary Fermi GBM IPN Swift GCN 34608 GCN 34610 GCN 34611 GCN 34618 GCN 34619 GCN 34623 GCN 34624 GCN 34625 GCN 34626 GCN 34650

Summary table
Variable Value Source
GRB_name_Fermi GRB230903724
T0 17:22:56 UTC GCN_circulars,Swift Det
ra 9.9106° Swift
decl -40.9500° Swift
pos_error 2.85e-04° Swift
T90 2.816 s Fermi_GBM
T90_error 3.167 s Fermi_GBM
T90_start 17:22:56.511 UTC Fermi_GBM
fluence 4.05e-07 erg/cm² Fermi_GBM
fluence_error 3.56e-08 erg/cm² Fermi_GBM
T100 3.327 s
GBM_located False
mjd 60190.72425925926 GCN_circulars,Swift Det
Fermi GBM table
GRB_name_Fermi GRB230903724
trigger_name bn230903724
ra 9.9258°
decl -40.9239°
pos_error 1.04e+01°
datum 2023-09-03
t_trigger 17:22:58.815 UTC
T90 2.816 s
T90_error 3.167 s
T90_start 17:22:56.511 UTC
fluence 4.05e-07 erg/cm²
fluence_error 3.56e-08 erg/cm²
flux_1024 2.06e+00 erg/cm²/s
flux_1024_error 2.41e-01 erg/cm²/s
flux_1024_time -1.02e+00 erg/cm²/s
flux_64 4.31e+00 erg/cm²/s
flux_64_error 1.32e+00 erg/cm²/s
IPN table
GRB_name GRB230903A
ra 9.9250°
decl -40.9167°
pos_error 5.00e-02°
Swift table
GRB_name GRB230903A
t_trigger 17:22:56 UTC
ra 9.9106°
decl -40.9500°
pos_error 2.85e-04°
T90 2.54 s
fluence 2.20e-07 erg/cm²
GCN 34608 table
GRB_name GRB230903A
GCN_number 34608
Detection_method Fermi GBM final loc
t_trigger 17:22:58 UTC
ra 13.4000°
decl -13.5000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 34608 SUBJECT: GRB 230903A: Fermi GBM Final Real-time Localization DATE: 23/09/03 17:33:32 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 17:22:58 UT on 3 Sep 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230903A (trigger 715454583.81493 / 230903724). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 13.4, Dec = -13.5 (J2000 degrees, equivalent to J2000 00h 53m, -13d 30'), with a statistical uncertainty of 16.6 degrees. The angle from the Fermi LAT boresight is 70.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230903724/quicklook/glg_skymap_all_bn230903724.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230903724/quicklook/glg_healpix_all_bn230903724.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230903724/quicklook/glg_lc_medres34_bn230903724.gif
GCN 34610 table
GRB_name GRB230903A
GCN_number 34610
Detection_method Swift Det
t_trigger 17:22:56 UTC
ra 9.9260°
decl -40.9240°
Circular_text TITLE: GCN CIRCULAR NUMBER: 34610 SUBJECT: GRB 230903A: Swift detection of a burst DATE: 23/09/03 17:46:24 GMT FROM: K.L. Page at U Leicester A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), J.D. Gropp (PSU), J. A. Kennea (PSU), A. Y. Lien (U Tampa), A. Melandri (INAF-OAR), M. J. Moss (GWU), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 17:22:56 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 230903A (trigger=1189514). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 9.926, -40.924 which is RA(J2000) = 00h 39m 42s Dec(J2000) = -40d 55' 25" 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 10 sec. The peak count rate was ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 17:24:47.9 UT, 111.7 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source with an enhanced position: RA, Dec 9.91169, -40.94930 which is equivalent to: RA(J2000) = 00h 39m 38.81s Dec(J2000) = -40d 56' 57.5" with an uncertainty of 1.9 arcseconds (radius, 90% containment). This location is 99 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 (2.68 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.6 (+2.17/-1.93) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 250 seconds with the U filter starting 117 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 19.2 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 18.0 mag. Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it). 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 34611 table
GRB_name GRB230903A
GCN_number 34611
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 34611 SUBJECT: GRB 230903A: LCOGT Optical Upper Limits DATE: 23/09/03 22:06:53 GMT FROM: Robert Strausbaugh at Eastern Illinois University R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on behalf of a larger collaboration: We observed the Swift GRB 230903A (D'ai et al., GCN 34610) field with the LCOGT 1-meter Sinistro instrument at the South African Astronomical Observatory site, on September 3, from 20:08 to 20:41 UT (corresponding to 2.77 to 3.32 hours from the GRB trigger time) with the Bessel R and I filters. We performed a series of 3x300s exposures in each band. We do not detect a source within the Swift-XRT error region (D'Ai et al., GCN 34610) in either band. The following upper limits are calculated using the USNO-B1.0 catalog as reference: R > 20.5 I > 19.0 These magnitudes are not corrected for galactic extinction.
GCN 34618 table
GRB_name GRB230903A
GCN_number 34618
Detection_method Fermi GBM Det
t_trigger 17:22:58.810 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 34618 SUBJECT: GRB 230903A: Fermi GBM detection DATE: 23/09/04 16:40:58 GMT FROM: Oliver J Roberts at USRA/NASA O.J. Roberts (USRA), B. Mailyan (Florida Tech) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 17:22:58.81 UT on the 3rd September 2023 , the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 230903A (trigger 715454583 / 230903724) which was also detected by the Swift/BAT (A. D'ai et al. 2023, GCN 34610). The Fermi GBM Final Real-time Localization (GCN 34608) is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 98 degrees. The GBM light curve consists of one pulse with a duration (T90) of about 3 s (50-300 keV). The time-averaged spectrum from T0-4.0 s to T0+1.0 s is best fit by a simple power law function with index -1.78 +/- 0.09. A power law function with an exponential high-energy cutoff fits the spectrum equally well. The power law index is -1.27 +/- 0.33 and the cutoff energy, parameterized as Epeak, is 95 +/- 31 keV. The event fluence (10-1000 keV) in this time interval is (5.87 +/- 0.85)E-07 erg/cm^2. The 1-sec peak photon flux measured starting from T0-1s in the 10-1000 keV band is 2.0 +/- 0.2 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 34619 table
GRB_name GRB230903A
GCN_number 34619
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 34619 SUBJECT: Fermi GRB 230903A: Global MASTER-Net observations report DATE: 23/09/04 19:31:00 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko, G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gress, N.M. Budnev, O.Ershova (Irkutsk State University, API), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich (Blagoveschensk Educational State University) MASTER-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 230903A ( Fermi GBM team, GCN 34608) errorbox 49439 sec after notice time and 49475 sec after trigger time at 2023-09-04 07:07:34 UT, with upper limit up to 18.3 mag. The observations began at zenith distance = 24 deg. The sun altitude is -47.1 deg. MASTER-Amur robotic telescope located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 230903A errorbox 83217 sec after notice time and 83253 sec after trigger time at 2023-09-04 16:30:32 UT, with upper limit up to 16.5 mag. The observations began at zenith distance = 50 deg. The sun altitude is -31.3 deg. The galactic latitude b = -76 deg., longitude l = 128 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2264968 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 49505 | 2023-09-04 07:07:34 | MASTER-OAFA | (23h 45m 07.73s , -21d 40m 56.2s) | C | 60 | 18.3 | 50337 | 2023-09-04 07:21:25 | MASTER-OAFA | (23h 45m 12.23s , -21d 40m 04.4s) | C | 60 | 18.3 | 83283 | 2023-09-04 16:30:32 | MASTER-Amur | (00h 45m 02.38s , +01d 03m 22.9s) | C | 60 | 16.4 | 83363 | 2023-09-04 16:31:51 | MASTER-Amur | (00h 52m 59.10s , +01d 05m 05.8s) | C | 60 | 16.5 | 83442 | 2023-09-04 16:33:11 | MASTER-Amur | (00h 44m 55.77s , +02d 58m 32.3s) | C | 60 | 16.5 | 83522 | 2023-09-04 16:34:30 | MASTER-Amur | (00h 52m 50.71s , +02d 58m 14.6s) | C | 60 | 16.2 | 83941 | 2023-09-04 16:41:29 | MASTER-Amur | (00h 44m 58.62s , +01d 04m 26.3s) | C | 60 | 16.2 | 84021 | 2023-09-04 16:42:49 | MASTER-Amur | (00h 52m 58.54s , +01d 03m 22.6s) | C | 60 | 16.2 | 84100 | 2023-09-04 16:44:08 | MASTER-Amur | (00h 44m 54.16s , +02d 58m 06.4s) | C | 60 | 16.2 | 84180 | 2023-09-04 16:45:28 | MASTER-Amur | (00h 52m 50.10s , +02d 57m 42.0s) | C | 60 | 15.9 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 34623 table
GRB_name GRB230903A
GCN_number 34623
Detection_method Swift-BAT Det
ra 9.8980°
decl -40.9100°
Circular_text TITLE: GCN CIRCULAR NUMBER: 34623 SUBJECT: GRB 230903A: Swift-BAT refined analysis DATE: 23/09/05 04:07:26 GMT FROM: Mike Moss at George Washington U M. J. Moss (GSFC), S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU), M. Stamatikos (OSU) (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 230903A (trigger #1189514) (D'Ai, et al., GCN Circ. 34610). The BAT ground-calculated position is RA, Dec = 9.898, -40.910 deg which is RA(J2000) = 00h 39m 35.5s Dec(J2000) = -40d 54' 34.5" with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 40%. The mask weighted light curve shows a single short pulse. T90 (15-350 keV) is 2.54 +- 0.27 sec (estimated error including systematics). The T90 and the spectral hardness of this burst places it on the border of the long-soft and hard-short burst classifications. The time-averaged spectrum from T+0.20 to T+2.93 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index -0.66 +- 1.49, and Epeak of 63.4 +- 17.8 keV (chi squared 44.41 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 2.2 +- 0.4 x 10^-07 erg/cm2 and the 1-sec peak flux measured from T+0.50 sec in the 15-150 keV band is 1.3 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.40 +- 0.21 (chi squared 54.66 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/1189514/BA/
GCN 34624 table
GRB_name GRB230903A
GCN_number 34624
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 34624 SUBJECT: GRB 230903A: VLT/X-shooter optical observations DATE: 23/09/05 10:07:06 GMT FROM: Emeric Le Floc'h at CEA-Saclay D. Pieterse (Radboud University), D. B. Malesani (Radboud and DAWN/NBI), E. Le Floc’h (CEA-Saclay), A. Saccardi (GEPI, Obs. de Paris) and N. R. Tanvir (Univ. of Leicester) report on behalf of the Stargate collaboration : We observed the field of GRB230903A (Fermi GBM team, GCN 34608 ; D’Ai et al., GCN 34610) using the ESO VLT UT3 (Melipal) equipped with the X-shooter instrument. Three 60s exposures were obtained in the r-band on 2023 September 4.097 UT (T-To ~8.95h). The observations were performed under poor weather conditions, with a seeing of 3.2 arcsec measured in the data. We do not detect any source coinciding with the location of the X-ray afterglow detected by Swift/XRT (D’Ai et al., GCN 34610). We obtain the following upper limit, calibrated using a faint, nearby object from the Legacy Survey (Dey et al. 2019, ApJ, 257, 29). r > 22.7 mag (AB) This estimate is not corrected for Galactic extinction and is consistent with the non-detection reported earlier by LCOGT (Strausbaugh et al., GCN 34611). We acknowledge excellent support from the ESO observing staff in Paranal, in particular Claudia Paladini and Jonathan Smoker.
GCN 34625 table
GRB_name GRB230903A
GCN_number 34625
Detection_method Swift-XRT Det
ra 9.9106°
decl -40.9500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 34625 SUBJECT: GRB 230903A: Enhanced Swift-XRT position DATE: 23/09/05 12:44:15 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 832 s of XRT Photon Counting mode data and 2 UVOT images for GRB 230903A, 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 = 9.91061, -40.95001 which is equivalent to: RA (J2000): 00h 39m 38.55s Dec (J2000): -40d 57' 00.0" with an uncertainty of 2.2 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 34626 table
GRB_name GRB230903A
GCN_number 34626
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 34626 SUBJECT: GRB 230903A: Swift-XRT refined Analysis DATE: 23/09/05 14:09:08 GMT FROM: Phil Evans at U of Leicester K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti (INAF-OAB), A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), J. D. Gropp (PSU), S. Dichiara (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 2.3 ks of XRT data for GRB 230903A, from 97 s to 29.3 ks after the BAT trigger. The data comprise 8 s in Windowed Timing (WT) mode (taken while Swift was slewing), with the remainder in Photon Counting (PC) mode. The light curve can be modelled with a power-law decay with a decay index of alpha=1.17 (+/-0.09). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.00 (+0.24, -0.22). The best-fitting absorption column is 8.2 (+5.9, -5.0) x 10^20 cm^-2, in excess of the Galactic value of 2.7 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 3.3 x 10^-11 (3.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 8.2 (+5.9, -5.0) x 10^20 cm^-2 Galactic foreground: 2.7 x 10^20 cm^-2 Excess significance: 1.8 sigma Photon index: 2.00 (+0.24, -0.22) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01189514. This circular is an official product of the Swift-XRT team.
GCN 34650 table
GRB_name GRB230903A
GCN_number 34650
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 34650 SUBJECT: GRB 230903A: TESS observations of optical emission DATE: 23/09/10 14:31:37 GMT FROM: Rahul Jayaraman at MIT R. Jayaraman (MIT), M.M. Fausnaugh (TTU/MIT), R. Vanderspek (MIT), and G.R. Ricker (MIT) report: The Transiting Exoplanet Survey Satellite (TESS; Ricker et al. JATIS 2015) observed the location of the gamma-ray burst GRB230903A (GCN 34608, Fermi GBM Team et al.; GCN 34610, D’Ai et al.) at a 200 second cadence continuously from 2.8 days before the trigger to 3.75 days after the trigger. The GRB occurred during TESS observational Sector 69, in the field of view of Camera 2, CCD 3. We extracted a light curve from the calibrated TESS Full-Frame Images (FFIs) produced by TICA (Fausnaugh et al. RNAAS 2020), using difference imaging and forced photometry at the enhanced location provided by Swift-XRT in GCN 34625 (Beardmore et al.). Our analysis procedure is described in Fausnaugh et al. 2023 (arXiv:2307.11815). TESS observations show a flux excess of 5.1-sigma above the background in the 200s FFI exposure that encompasses the Fermi trigger time, corresponding to an apparent magnitude of 17.20 ± 0.05 in the TESS band (600 nm–1000 nm). Further analysis is ongoing. The TICA data are publicly available on the MAST archive at https://archive.stsci.edu/hlsp/tica.