GRB230510B

This page lists all entries on GRB230510B in GRBweb

Summary Fermi GBM IPN GCN 33759 GCN 33760 GCN 33763 GCN 33772 GCN 33806 GCN 33811

Summary table
Variable Value Source
GRB_name_Fermi GRB230510890
T0 21:21:34 UTC GCN_circulars,Fermi GBM final loc
ra 0.6917° IPN
decl 27.5333° IPN
pos_error 1.67e-01° IPN
T90 466.186 s Fermi_GBM
T90_error 22.018 s Fermi_GBM
T90_start 21:21:39.901 UTC Fermi_GBM
fluence 9.57e-05 erg/cm² Fermi_GBM
fluence_error 1.60e-07 erg/cm² Fermi_GBM
T100 472.087 s
GBM_located False
mjd 60074.88997685185 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB230510890
trigger_name bn230510890
ra 4.5300°
decl 30.0500°
pos_error 2.13e+00°
datum 2023-05-10
t_trigger 21:21:34.013 UTC
T90 466.186 s
T90_error 22.018 s
T90_start 21:21:39.901 UTC
fluence 9.57e-05 erg/cm²
fluence_error 1.60e-07 erg/cm²
flux_1024 8.12e+00 erg/cm²/s
flux_1024_error 2.65e-01 erg/cm²/s
flux_1024_time 1.94e+02 erg/cm²/s
flux_64 1.34e+01 erg/cm²/s
flux_64_error 1.17e+00 erg/cm²/s
IPN table
GRB_name GRB230510B
ra 0.6917°
decl 27.5333°
pos_error 1.67e-01°
GCN 33759 table
GRB_name GRB230510B
GCN_number 33759
Detection_method Fermi GBM final loc
t_trigger 21:21:34 UTC
ra 4.5000°
decl 30.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33759 SUBJECT: GRB 230510B: Fermi GBM Final Real-time Localization DATE: 23/05/10 21:32:13 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 21:21:34 UT on 10 May 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230510B (trigger 705446499.012602 / 230510890). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 4.5, Dec = 30.0 (J2000 degrees, equivalent to J2000 00h 18m, 30d 00'), with a statistical uncertainty of 1.0 degrees. The angle from the Fermi LAT boresight is 66.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230510890/quicklook/glg_skymap_all_bn230510890.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/bn230510890/quicklook/glg_healpix_all_bn230510890.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230510890/quicklook/glg_lc_medres34_bn230510890.gif
GCN 33760 table
GRB_name GRB230510B
GCN_number 33760
Detection_method MAXI Det
t_trigger 21:22:03 UTC
ra 0.6920°
decl 27.5410°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33760 SUBJECT: GRB 230510B: MAXI/GSC detection DATE: 23/05/10 23:29:07 GMT FROM: Satoshi Sugita at Aoyama Gakuin U. M. Nakajima (Nihon U.), Y. Kawakubo (LSU), S. Sugita, M. Serino (AGU), H. Negoro, K. Kobayashi, M. Tanaka, Y. Soejima, Y. Kudo (Nihon U.), T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, N. Kawai, M. Matsuoka (RIKEN), T. Sakamoto, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU), Y. Tsuboi, S. Urabe, S. Nawa, N. Nemoto (Chuo U.), M. Shidatsu (Ehime U.), I. Takahashi, M. Niwano, S. Sato, N. Higuchi, Y. Yatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, S. Ogawa, T. Kurihara (JAXA), Y. Ueda, K. Setoguchi, T. Yoshitake, Y. Nakatani (Kyoto U.), M. Yamauchi, Y. Hagiwara, Y. Umeki, Y. Otsuki (Miyazaki U.), K. Yamaoka (Nagoya U.), M. Sugizaki (NAOC), W. Iwakiri (Chiba U.) report on behalf of the MAXI team: The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 21:22:03 UT 10 May 2023. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (0.692 deg, 27.541 deg) = (00 02 46, +27 32 27) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.15 deg and 0.14 deg, respectively. The roll angle of long axis from the north direction is 139.0 deg counterclockwise. Without assumptions on the source constancy, we obtain a rectangular error box for the transient source with the following corners: (R.A., Dec) = (0.127, 28.437) deg = (00 00 30, +28 26 13) (J2000) (R.A., Dec) = (359.878, 28.290) deg = (23 59 30, +28 17 23) (J2000) (R.A., Dec) = (0.966, 26.843) deg = (00 03 51, +26 50 34) (J2000) (R.A., Dec) = (1.213, 26.988) deg = (00 04 51, +26 59 16) (J2000) There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The trigger time and position was consistent with that of GRB 230510B (Fermi GBM, GCN 33759) The X-ray flux averaged over the scan was 635 +- 75 mCrab (4.0-10.0keV, 1 sigma error). There was no significant excess flux in the previous transit at 19:49 UT and in the next transit at 22:54 UT with an upper limit of 20 mCrab for each.
GCN 33763 table
GRB_name GRB230510B
GCN_number 33763
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 33763 SUBJECT: GRB 230510B: CALET Gamma-Ray Burst Monitor detection DATE: 23/05/11 06:22:32 GMT FROM: Yuta Kawakubo at Louisiana State University P. S. Marrocchesi (U of Siena), A. Yoshida, T. Sakamoto, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), and the CALET collaboration: The long GRB 230510B (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 33759; MAXI/GSC detection: Nakajima et al., GCN Circ 33760) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 21:21:32.08 UTC on 10 May 2023 (http://cgbm.calet.jp/cgbm_trigger/flight/1367788853/index.html). The burst signal was seen by all CGBM detectors. The burst light curve shows a double-peaked structure that starts at T-45.5 sec, peaks at T+23.4 sec, and ends at T+263.9 sec. The T90 and T50 durations measured by the SGM data are 233.0 +/- 3.3 sec and 168.5 +/- 0.8 sec (40-1000 keV), respectively. The ground-processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1367788853/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.
GCN 33772 table
GRB_name GRB230510B
GCN_number 33772
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 33772 SUBJECT: GRB 230510B: AstroSat CZTI detection DATE: 23/05/11 15:03:27 GMT FROM: Gaurav Waratkar at IIT Bombay P K. Navaneeth (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long GRB 230510B which was also detected by Fermi (Fermi GBM Team, GCN Circ. 33759), MAXI/GSC (Nakajima et al., GCN Circ. 33760), and CALET (Marrocchesi et al., GCN Circ. 33763). The source was detected in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2023-05-10 21:21:52.50 UTC. The measured peak count rate associated with the burst is 98 (+43, -2) counts/s above the background in the combined data of three quadrants (out of four), with a total of 4971 (+1144, -1220) counts. The local mean background count rate was 313 (+1, -1) counts/s. Using cumulative rates, we measure a T90 of 270 (+36, -58) s. The source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.The light curve showed multiple peaks of emission with the strongest peak at 2023-05-10 21:21:52.50 UTC. The measured peak count rate associated with the burst is 316 (+77, -19) counts/s above the background in the combined data of all quadrants, with a total of 11559 (+2752, -3027) counts. The local mean background count rate was 1315 (+3, -3) counts/s. We measure a T90 of 202 (+36, -10) s from the cumulative Veto light curve. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project. CZTI GRB detections are reported regularly on the payload site at: http://astrosat.iucaa.in/czti/?q=grb
GCN 33806 table
GRB_name GRB230510B
GCN_number 33806
Detection_method Fermi GBM Det
t_trigger 21:21:34.010 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 33806 SUBJECT: GRB 230510B: Fermi GBM detection DATE: 23/05/16 21:23:02 GMT FROM: sumanbala2210@gmail.com O.J. Roberts (USRA/NASA-MSFC), S. Bala (USRA), J. Wood (NASA-MSFC) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 21:21:34.01 UT on 10 May 2023, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 230510B (trigger 705446499 /230510890), which was also detected by MAXI/GSC (M. Nakajima et al. 2023, GCN 33760), CALET (P.S. Marrocchesi et al. 2023, GCN 33763), and CZTI/AstroSat (P.K. Navaneeth et al. 2023, GCN 33772). The Fermi GBM Final Real-time Localization (GCN 33759) is consistent with the MAXI/GSC position. The angle from the Fermi LAT boresight at the GBM trigger time is 60 degrees. The GBM light curve consists of two distinct peaks with multiple short peaks in between with a duration (T90) of about 466 s (50-300 keV). The time-averaged spectrum from T0-5.12 s to T0+650.81 s is best fit by a Band function, with Epeak= 341 +/- 28 keV, alpha = -1.32 +/- 0.02, and beta = -2.01 +/- 0.06. The event fluence (10-1000 keV) in this time interval is (1.28 +/- 0.01)E-04 erg/cm^2. The 1-sec peak photon flux measured starting from T0+194 s in the 10-1000 keV band is 8.12 +/- 0.26 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 33811 table
GRB_name GRB230510B
GCN_number 33811
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 33811 SUBJECT: GRB 230510B: GRBAlpha detection DATE: 23/05/17 18:34:37 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration. The long-duration GRB 230510B (Fermi/GBM detection: GCN 33759; CALET/CGBM detection: GCN 33763; AstroSat detection: GCN 33772; Wind/Konus detection at 2023-05-10 21:21:35.995 UT; INTEGRAL/SPI-ACS detection at 2023-05-10 21:21:45 UT; GECAM-B trig. no. 178) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023; arXiv:2302.10048). The detection was confirmed at the peak time 2023-05-10 21:20:55 UTC. The T90 duration measured by GRBAlpha is 198 s and the overall significance during T90 reaches 14 sigma in the 80-400 keV band. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB230510B_GCN.pdf All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.