GRB240805A

This page lists all entries on GRB240805A in GRBweb

Summary Fermi GBM IPN Swift GCN 37031 GCN 37032 GCN 37041 GCN 37042 GCN 37045 GCN 37047 GCN 37048 GCN 37054 GCN 37056 GCN 37075 GCN 37077 GCN 37083 GCN 37099

Summary table
Variable Value Source
GRB_name_Fermi GRB240805085
T0 2:02:20 UTC GCN_circulars,Fermi GBM final loc
ra 190.9110° Swift
decl -53.6220° Swift
pos_error 2.33e-02° Swift
T90 10.752 s Fermi_GBM
T90_error 0.362 s Fermi_GBM
T90_start 2:02:21.077 UTC Fermi_GBM
fluence 2.80e-05 erg/cm² Fermi_GBM
fluence_error 2.43e-08 erg/cm² Fermi_GBM
T100 11.829 s
GBM_located False
mjd 60527.08495370371 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB240805085
trigger_name bn240805085
ra 190.9108°
decl -53.6219°
pos_error 2.60e+00°
datum 2024-08-05
t_trigger 2:02:20.309 UTC
T90 10.752 s
T90_error 0.362 s
T90_start 2:02:21.077 UTC
fluence 2.80e-05 erg/cm²
fluence_error 2.43e-08 erg/cm²
flux_1024 1.43e+01 erg/cm²/s
flux_1024_error 2.85e-01 erg/cm²/s
flux_1024_time 5.76e+00 erg/cm²/s
flux_64 1.86e+01 erg/cm²/s
flux_64_error 1.19e+00 erg/cm²/s
IPN table
GRB_name GRB240805A
ra 190.9125°
decl -53.6167°
pos_error 5.00e-02°
Swift table
GRB_name GRB240805A
t_trigger 2:02:22 UTC
ra 190.9110°
decl -53.6220°
pos_error 2.33e-02°
GCN 37031 table
GRB_name GRB240805A
GCN_number 37031
Detection_method Fermi GBM final loc
t_trigger 2:02:20 UTC
ra 192.1000°
decl -52.9000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37031 SUBJECT: GRB 240805A: Fermi GBM Final Real-time Localization DATE: 24/08/05 02:12:51 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 02:02:20 UT on 5 Aug 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240805A (trigger 744516145.309414 / 240805085). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 192.1, Dec = -52.9 (J2000 degrees, equivalent to J2000 12h 48m, -52d 53'), with a statistical uncertainty of 1.5 degrees. The angle from the Fermi LAT boresight is 59.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240805085/quicklook/glg_skymap_all_bn240805085.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240805085/quicklook/glg_healpix_all_bn240805085.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240805085/quicklook/glg_lc_medres34_bn240805085.gif
GCN 37032 table
GRB_name GRB240805A
GCN_number 37032
Detection_method Swift Det
t_trigger 2:02:22 UTC
ra 190.9110°
decl -53.6220°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37032 SUBJECT: GRB 240805A: Swift detection of a burst DATE: 24/08/05 02:26:17 GMT FROM: David Palmer at LANL S. Dichiara (PSU), R. Gupta (NASA GSFC) and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift Observatory Team: At 02:02:22 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 240805A (trigger=1246907). Swift slewed immediately to the burst but the observations was cut short almost immediately after the end of slew due to an observing constraint. The BAT on-board calculated location is RA, Dec 190.911, -53.622 which is RA(J2000) = +12h 43m 39s Dec(J2000) = -53d 37' 17" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve is not immediately available. However, the original BAT trigger shows an excess of 3.3k counts in 1.024 s (25-100 keV) at the time of the trigger. The XRT and UVOT observations were only a few seconds long, so X-ray and optical positions and lightcurves will not be available until the GRB comes out of constraint around 02:58 UT. Burst Advocate for this burst is S. Dichiara (sbd5667 AT psu.edu). 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 37041 table
GRB_name GRB240805A
GCN_number 37041
Detection_method INTEGRAL
Circular_text TITLE: GCN CIRCULAR NUMBER: 37041 SUBJECT: GRB 240805A: INTEGRAL spectral analysis DATE: 24/08/05 14:00:00 GMT FROM: Diego Gotz at CEA D. Götz (CEA Irfu), S. Mereghetti (INAF, IASF Milano), C.Ferrigno, E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC, Versoix) and J.Borkowski (CAMK, Torun) report: we performed futher analysis of GRB 240805A detected by GBM, Swift, and INTEGRAL (GCN 37031, 37032, 37037). Our spectral analysis provides a preliminary peak flux, integrated over 1 s, of 4.2 photons (4e-7 erg)/cmsq/s and a fluence of 2.4e-6 erg/cmsq in the 20-200 keV energy band. We note that both these values are lower limits due to telemetry limitations at satellite level.
GCN 37042 table
GRB_name GRB240805A
GCN_number 37042
Detection_method Fermi LAT Det
t_trigger 2:02:20.310 UTC
ra 190.4500°
decl -54.0200°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37042 SUBJECT: GRB 240805A: Fermi-LAT detection DATE: 24/08/05 14:41:11 GMT FROM: Rahul Gupta at NASA GSFC R. Gupta (NASA GSFC), A. Holzmann (DF, University of Buenos Aires, Argentina), and F. Longo (University and INFN, Trieste) report on behalf of the Fermi-LAT Collaboration: At 02:02:20.31 UT on August 05, 2024, Fermi-LAT detected high-energy emission from GRB 240805A which was also detected by Fermi-GBM (trigger 744516145 / 240805085, GCN 37031), Swift/BAT (GCN 37032), and INTEGRAL (GCN 37037). The best LAT on-ground location is found to be RA, Dec = 190.45, -54.02 (J2000) with an error radius of 0.45 deg (90% containment, statistical error only). This was 59 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. The photon flux above 100 MeV in the time interval 0-100 s after the GBM trigger is (3.6 +/- 1.3) E-5 ph/cm2/s. The estimated photon index above 100 MeV is -2.0 +/- 0.3. The highest-energy photon is a 1.6 GeV event which is observed about 17 seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is Lorenzo Scotton (lorenzo.scotton AT uah.edu) 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 37045 table
GRB_name GRB240805A
GCN_number 37045
Detection_method Swift-XRT Other
ra 190.9147°
decl -53.5953°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37045 SUBJECT: GRB 240805A: Swift-XRT refined Analysis DATE: 24/08/05 16:15:13 GMT FROM: Phil Evans at U of Leicester J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAR), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), D.N. Burrows (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 1.7 ks of XRT data for GRB 240805A, from 89 s to 5.1 ks after the BAT trigger. The data comprise 75 s in Windowed Timing (WT) mode (the first 6 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. Using 1639 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 = 190.91475, -53.59526 which is equivalent to: RA (J2000): 12h 43m 39.54s Dec(J2000): -53d 35' 42.9" with an uncertainty of 2.1 arcsec (radius, 90% confidence). The light curve can be modelled with an initial power-law decay with an index of alpha=7.82 (+0.18, -2.12), followed by a break at T+97.3 s to an alpha of 1.292 (+0.027, -0.026). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.79 (+/-0.08). The best-fitting absorption column is 5.1 (+/-0.5) x 10^21 cm^-2, in excess of the Galactic value of 2.3 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.52 (+0.23, -0.22) and a best-fitting absorption column of 3.8 (+1.5, -1.2) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.3 x 10^-11 (6.6 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.8 (+1.5, -1.2) x 10^21 cm^-2 Galactic foreground: 2.3 x 10^21 cm^-2 Excess significance: 2.0 sigma Photon index: 1.52 (+0.23, -0.22) If the light curve continues to decay with a power-law decay index of 1.292, the count rate at T+24 hours will be 0.020 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-12 (1.4 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01246907. This circular is an official product of the Swift-XRT team.
GCN 37047 table
GRB_name GRB240805A
GCN_number 37047
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37047 SUBJECT: Swift GRB 240805A: Global MASTER-Net observations report DATE: 24/08/05 16:56:41 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 240805A ( S. Dichiara et al., GCN 37032) errorbox 53063 sec after notice time and 53081 sec after trigger time at 2024-08-05 16:47:04 UT, with upper limit up to 16.1 mag. Observations started at twilight. The observations began at zenith distance = 33 deg. The sun altitude is -9.3 deg. The galactic latitude b = 9 deg., longitude l = 302 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2551196 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 53172 | MASTER-SAAO | C | 180 | 16.1 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 37048 table
GRB_name GRB240805A
GCN_number 37048
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37048 SUBJECT: Fermi GRB 240805A: Global MASTER-Net observations report DATE: 24/08/05 17:15:29 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 240805A ( Fermi GBM team, GCN 37031) errorbox 53052 sec after notice time and 53084 sec after trigger time at 2024-08-05 16:47:04 UT, with upper limit up to 18.5 mag. Observations started at twilight. The observations began at zenith distance = 33 deg. The sun altitude is -9.3 deg. The galactic latitude b = 10 deg., longitude l = 303 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2551244 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 53174 | 2024-08-05 16:47:04 | MASTER-SAAO | (12h 43m 20.61s , -53d 36m 01.3s) | C | 180 | 16.1 | 53354 | 2024-08-05 16:47:04 | MASTER-SAAO | (12h 43m 20.63s , -53d 36m 01.3s) | C | 540 | 17.2 | Coadd 53373 | 2024-08-05 16:50:23 | MASTER-SAAO | (12h 43m 15.26s , -53d 36m 55.1s) | C | 180 | 16.9 | 53573 | 2024-08-05 16:53:42 | MASTER-SAAO | (12h 43m 23.40s , -53d 36m 25.3s) | C | 180 | 17.4 | 53772 | 2024-08-05 16:57:02 | MASTER-SAAO | (12h 43m 20.45s , -53d 34m 46.4s) | C | 180 | 17.9 | 53971 | 2024-08-05 17:00:21 | MASTER-SAAO | (12h 43m 21.17s , -53d 36m 24.1s) | C | 180 | 18.2 | 54171 | 2024-08-05 17:03:41 | MASTER-SAAO | (12h 43m 24.63s , -53d 34m 49.4s) | C | 180 | 18.5 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 37054 table
GRB_name GRB240805A
GCN_number 37054
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 37054 SUBJECT: GRB 240805A: SVOM/GRM observation DATE: 24/08/06 00:04:37 GMT FROM: Chenwei Wang at IHEP SVOM/GRM team: Chen-Wei Wang, Yong-Wei Dong, Jiang-Tao Liu, Shi-Jie Zheng, Jian-Chao Sun, Wen-Jun Tan, Jiang He, Min Gao, Hao-Xuan Guo, Yue Huang, Lu Li, Yong-Ye Li, Hong-Wei Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, You-Li Tuo, Hao-Xi Wang, Jin Wang, Jin-Zhou Wang, Ping Wang, Rui-Jie Wang, Yu-Xi Wang, Bo-Bing Wu, Shao-Lin Xiong, Jian-Ying Ye, Yi-Tao Yin, Wen-Hui Yu, Fan Zhang, Li Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Yan-Ting Zhang, Shu-Min Zhao, Xiao-Yun Zhao, Chao Zheng (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laurent Bouchet (IRAP), David Corre (CEA), Patrick Maeght (LUPM), Frédéric Piron (LUPM) , Stéphane Schanne (CEA), Jingwei Wang (IAP) SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), JeanLuc Attéia (IRAP), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Bing Zhang (UNLV) report on behalf of the SVOM team: During the commissioning phase, the SVOM/GRM was triggered by a long GRB 240805A at 2024-08-05T02:02:21.400 UT (T0), which also triggered Fermi/GBM (GCN 37031), Swift/BAT (GCN 37032), INTEGRAL (GCN 37037), and Fermi/LAT (GCN 37042). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a duration of about 12 s. The GRM light curve can be found here: https://www.bursthub.cn/admin/static/svgrb240805A.png At the time of this burst ECLAIRs was not in operational mode. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM point of contact for this burst is: Chen-Wei Wang (IHEP)(cwwang@ihep.ac.cn)
GCN 37056 table
GRB_name GRB240805A
GCN_number 37056
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37056 SUBJECT: GRB 240805A: Swift/UVOT Upper Limits DATE: 24/08/06 01:34:23 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and S. Dichiara (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 240805A 105 s after the BAT trigger (Dichiara et al., GCN Circ. 37032). No optical afterglow consistent with the XRT position (Osborne, GCN Circ. 37045) 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 initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 105 4086 269 >20.4 v 4297 4497 197 >18.7 b 3681 5128 205 >19.5 u 3476 5113 393 >19.5 w1 4708 4908 197 >19.1 m2 4502 4701 197 >19.1 w2 4092 4292 197 >19.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.191 in the direction of the burst (Schlegel et al. 1998).
GCN 37075 table
GRB_name GRB240805A
GCN_number 37075
Detection_method Fermi GBM Det
t_trigger 2:02:20.310 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 37075 SUBJECT: GRB240805A: Fermi GBM Observation DATE: 24/08/06 15:04:23 GMT FROM: Jacob Smith at Fermi-GBM Team M. Godwin (UAH), J. Smith (UAH), and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: At 02:02:20.31 UT on 05 August 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240805A (trigger 744516145/240805085),which was also detected by SVOM/GRM (SVOM/GRM team, 2024, GCN 37054), Fermi-LAT (R. Gupta et al. 2024, GCN 37042), INTEGRAL IBAS (S.Mereghetti et al. 2024, GCN 37037), and Swift-BAT (S. Dichiara et al. 2024, GCN 37032). The Final Real-time Localization (Fermi GBM Team 2024, GCN 37031) is consistent with the Fermi-LAT, Integral, and Swift positions. The angle from the Fermi LAT boresight is 59 degrees. The GBM light curve has many short peaks with a duration (T90) of about 10.8 s (50-300 keV). The time-averaged spectrum from T0-3.6 to T0+16.9 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.67 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 330 +/- 8 keV. The event fluence (10-1000 keV) in this time interval is (2.91 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+5.8 s in the 10-1000 keV band is 14.3 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 310 +/- 10 keV, alpha = -0.65 +/- 0.02 and beta = -2.9 +/- 0.3. 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 37077 table
GRB_name GRB240805A
GCN_number 37077
Detection_method Konus-Wind Det
t_trigger 2:02:22.029 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 37077 SUBJECT: Konus-Wind detection of GRB 240805A DATE: 24/08/06 15:53:16 GMT FROM: Anna Ridnaia at Ioffe Institute A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long-duration GRB 240805A (Fermi-GBM observation: The Fermi GBM team, GCN 27031; Godwin et al., GCN 37075; Swift-BAT detection: Dichiara et al., GCN 37032; INTEGRAL IBIS/ISGRI detection: Mereghetti et al., GCN 37037; Götz et al., GCN 37041; Fermi-LAT detection: Gupta et al., GCN 37042; SVOM/GRM observation: Wang et al., GCN 37054) triggered Konus-Wind at T0=7342.029 s UT (02:02:22.029). The burst light curve shows a multipeaked structure which starts at ~T0-2.3 s and has a total duration of ~15.6 s. The emission is seen up to ~4 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240805_T07342/ As observed by Konus-Wind, the burst had a fluence of 3.43(-0.31,+0.35)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+3.680 s, of 6.61(-1.44,+1.48)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+15.360 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 = -0.46(-0.11,+0.13), the high energy photon index beta = -2.76(-0.43,+0.26), the peak energy Ep = 272(-22,+22) keV (chi2 = 81/80 dof). The spectrum near the maximum count rate (measured from T0+0.256 to T0+7.168 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 = -0.51(-0.12,+0.14), the high energy photon index beta = -2.78(-0.61,+0.29), the peak energy Ep = 279(-26,+27) keV (chi2 = 70/71 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 37083 table
GRB_name GRB240805A
GCN_number 37083
Detection_method Swift-BAT Det
ra 190.9190°
decl -53.6030°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37083 SUBJECT: GRB 240805A: Swift-BAT refined analysis DATE: 24/08/06 20:26:06 GMT FROM: Rahul Gupta at NASA GSFC S. D. Barthelmy (GSFC), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 240805A (trigger #1246907) (Dichiara, et al., GCN Circ. 37032). The BAT ground-calculated position is RA, Dec = 190.919, -53.603 deg which is RA(J2000) = 12h 43m 40.6s Dec(J2000) = -53d 36' 10.3" with an uncertainty of 0.79 arcmin, (radius, sys+stat, 90% containment). The partial coding was 31%. The mask-weighted BAT light curve shows a complex structure. T90 (15-350 keV) is 37.34 +- 6.22 sec (estimated error including systematics). The time-averaged spectrum from T-3.936 to T+258.128 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.21 +- 0.06. The fluence in the 15-150 keV band is 8.7 +- 0.3 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T+3.28 sec in the 15-150 keV band is 8.0 +- 0.5 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1246907
GCN 37099 table
GRB_name GRB240805A
GCN_number 37099
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37099 SUBJECT: GRB 240805A: ATCA Radio Upper Limits DATE: 24/08/08 07:19:40 GMT FROM: agul8829@uni.sydney.edu.au A. Gulati (USyd), S. Chastain (UNM), G. E. Anderson (Curtin), J. K. Leung (UofT/HUJI), S. D. Ryder (Macquarie), A. J. van der Horst (GWU), and L. Rhodes (Oxford) on behalf of the ATCA PanRadio GRB collaboration We observed long GRB 240805A (Fermi GBM Collaboration, GCN 37031; S. Dichiara et al., GCN 37032) as part of the The Australia Telescope Compact Array (ATCA) "PanRadio GRB" Large Project C3542 (PI: G. Anderson) at 5.5 and 9 GHz 18-minutes post burst on 2024-08-05 (02:30-13:30 UT) and 2.7 days post-burst on 2024-08-07 (09:00-13:00 UT). No radio sources were detected near the Swift/XRT enhanced position (J. P. Osborne et al., GCN 37045) in either observation epoch. The 3-sigma upper limits for the 9 GHz observations are 45 and 42 uJy respectively. We thank the CSIRO Space and Astronomy staff for supporting these observations. We acknowledge the Gomeroi people as the traditional owners of the Observatory site. The Australia Telescope Compact Array is part of the Australia Telescope National Facility (https://ror.org/05qajvd42) which is funded by the Australian Government for operation as a National Facility managed by CSIRO.