GRB240905B

This page lists all entries on GRB240905B in GRBweb

Summary Fermi GBM IPN GCN 37389 GCN 37393 GCN 37417 GCN 37418 GCN 37421 GCN 37433 GCN 37436 GCN 37455 GCN 37601 GCN 37613

Summary table
Variable Value Source
GRB_name_Fermi GRB240905186
T0 4:27:16 UTC GCN_circulars,Fermi GBM final loc
ra 268.0000° IPN
decl 14.2000° IPN
pos_error 2.00e-01° IPN
T90 1.28 s Fermi_GBM
T90_error 0.202 s Fermi_GBM
T90_start 4:27:16.140 UTC Fermi_GBM
fluence 7.85e-06 erg/cm² Fermi_GBM
fluence_error 9.66e-09 erg/cm² Fermi_GBM
T100 1.42 s
GBM_located False
mjd 60558.18560185185 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB240905186
trigger_name bn240905186
ra 268.0000°
decl 14.2000°
pos_error 3.58e+00°
datum 2024-09-05
t_trigger 4:27:16.140 UTC
T90 1.28 s
T90_error 0.202 s
T90_start 4:27:16.140 UTC
fluence 7.85e-06 erg/cm²
fluence_error 9.66e-09 erg/cm²
flux_1024 1.84e+01 erg/cm²/s
flux_1024_error 3.52e-01 erg/cm²/s
flux_1024_time -6.40e-02 erg/cm²/s
flux_64 3.02e+01 erg/cm²/s
flux_64_error 1.42e+00 erg/cm²/s
IPN table
GRB_name GRB240905B
ra 268.0000°
decl 14.2000°
pos_error 2.00e-01°
GCN 37389 table
GRB_name GRB240905B
GCN_number 37389
Detection_method Fermi GBM final loc
t_trigger 4:27:16 UTC
ra 266.1000°
decl 16.9000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37389 SUBJECT: GRB 240905B: Fermi GBM Final Real-time Localization DATE: 24/09/05 04:37:48 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely SHORT GRB At 04:27:16 UT on 5 Sep 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240905B (trigger 747203241.139826 / 240905186). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 266.1, Dec = 16.9 (J2000 degrees, equivalent to J2000 17h 44m, 16d 53'), with a statistical uncertainty of 1.0 degrees. The angle from the Fermi LAT boresight is 25.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240905186/quicklook/glg_skymap_all_bn240905186.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/bn240905186/quicklook/glg_healpix_all_bn240905186.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240905186/quicklook/glg_lc_medres34_bn240905186.gif
GCN 37393 table
GRB_name GRB240905B
GCN_number 37393
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37393 SUBJECT: Fermi GRB 240905B: Global MASTER-Net observations report DATE: 24/09/05 11:30:40 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-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240905B ( Fermi GBM team, GCN 37389) errorbox 23620 sec after notice time and 23653 sec after trigger time at 2024-09-05 11:01:29 UT, with upper limit up to 16.2 mag. Observations started at twilight. The observations began at zenith distance = 35 deg. The sun altitude is -9.3 deg. The galactic latitude b = 22 deg., longitude l = 41 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2589953 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 23684 | 2024-09-05 11:01:29 | MASTER-Amur | (17h 37m 46.69s , +16d 24m 43.3s) | C | 60 | 16.2 | 23763 | 2024-09-05 11:02:49 | MASTER-Amur | (17h 46m 01.25s , +16d 24m 00.3s) | C | 60 | 16.1 | 23865 | 2024-09-05 11:04:31 | MASTER-Amur | (17h 48m 50.82s , +18d 19m 37.2s) | C | 60 | 15.8 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 37417 table
GRB_name GRB240905B
GCN_number 37417
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 37417 SUBJECT: GRB 240905B: Swift ToO observations DATE: 24/09/07 02:31:03 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/LAT GRB 240905B. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021711 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the Fermi/LAT event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team.
GCN 37418 table
GRB_name GRB240905B
GCN_number 37418
Detection_method Fermi LAT Det
t_trigger 4:27:16 UTC
ra 268.0000°
decl 14.2000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37418 SUBJECT: GRB 240905B: Fermi-LAT detection DATE: 24/09/07 03:07:29 GMT FROM: Rahul Gupta at NASA GSFC R. Gupta (NASA GSFC), N. Di Lalla (Stanford University), and D. Kocevski (NASA/MSFC) report on behalf of the Fermi-LAT Collaboration: On Sep 05, 2024, Fermi-LAT detected high-energy emission from GRB 240905B, which was also detected by Fermi-GBM (trigger 747203241.139826 / 240905186), and AstroSat CZTI (GCN 37391). The best LAT on-ground location is found to be: RA, Dec = 268.0, 14.2 (J2000) with an error radius of 0.2 deg (90 % containment, statistical error only). This was 28 deg from the LAT boresight at the time of the GBM trigger: T0 = 04:27:16 UT. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 0-10 s after the GBM trigger is (2.2 +/- 0.6) E-4 ph/cm2/s. The estimated photon index above 100 MeV is -2.0 +/- 0.3. The highest-energy photon is a 3 GeV event which is observed ~ 1.1 seconds after the GBM trigger. A Swift ToO has been approved for this burst. The Fermi-LAT point of contact for this burst is Niccolo' Di Lalla (niccolo.dilalla@stanford.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 37421 table
GRB_name GRB240905B
GCN_number 37421
Detection_method Swift-XRT Other
ra 267.9656°
decl 14.3317°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37421 SUBJECT: GRB 240905B: Swift-XRT observations DATE: 24/09/07 15:02:06 GMT FROM: Phil Evans at U of Leicester R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), S. Dichiara (PSU), J.A. Kennea (PSU), D.N. Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), A. Melandri (INAF-OAR) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 240905B, collecting 4.7 ks of Photon Counting (PC) mode data between T0+165.8 ks and T0+184.5 ks. Six uncatalogued X-ray sources have been detected, however none of them is above the RASS limit or shows definitive signs of fading. Therefore, at the present time we cannot identify which, if any, is the afterglow. Details of these sources are given below: Source 1: RA (J2000): 267.9656 = 17:51:51.73 Dec (J2000): +14.3317 = +14:19:54.0 Error: 5.3 arcsec (radius, 90% conf.) Count-rate: (7.5 [+1.7, -1.6])e-3 ct s^-1 Distance: 489 arcsec from Fermi/LAT position. Flux: (1.21 [+0.28, -0.26])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 2: RA (J2000): 267.8714 = 17:51:29.15 Dec (J2000): +14.1724 = +14:10:20.6 Error: 6.1 arcsec (radius, 90% conf.) Count-rate: (2.45 [+1.16, -0.91])e-3 ct s^-1 Distance: 459 arcsec from Fermi/LAT position. Source 3: RA (J2000): 268.0531 = 17:52:12.75 Dec (J2000): +14.1172 = +14:07:01.9 Error: 6.3 arcsec (radius, 90% conf.) Count-rate: (1.14 [+0.99, -0.76])e-3 ct s^-1 Distance: 351 arcsec from Fermi/LAT position. Source 4: RA (J2000): 268.1019 = 17:52:24.47 Dec (J2000): +14.0362 = +14:02:10.2 Error: 6.5 arcsec (radius, 90% conf.) Count-rate: (4.5 [+1.5, -1.3])e-3 ct s^-1 Distance: 688 arcsec from Fermi/LAT position. Flux: (1.10 [+0.38, -0.31])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 5: RA (J2000): 268.0524 = 17:52:12.56 Dec (J2000): +14.2532 = +14:15:11.5 Error: 5.9 arcsec (radius, 90% conf.) Count-rate: (1.11 [+0.86, -0.69])e-3 ct s^-1 Distance: 264 arcsec from Fermi/LAT position. Source 6: RA (J2000): 267.9614 = 17:51:50.74 Dec (J2000): +14.2308 = +14:13:51.0 Error: 7.4 arcsec (radius, 90% conf.) Count-rate: (1.41 [+0.93, -0.75])e-3 ct s^-1 Distance: 174 arcsec from Fermi/LAT position. Flux: (3.8 [+2.5, -2.0])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV) The results of the XRT-team automatic analysis of the XRT observations, including a position-specific upper limit calculator, are available at https://www.swift.ac.uk/ToO_GRBs/00021711. This circular is an official product of the Swift-XRT team.
GCN 37433 table
GRB_name GRB240905B
GCN_number 37433
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 37433 SUBJECT: GRB 240905B: GOTO optical upper limits DATE: 24/09/09 10:53:22 GMT FROM: Amit Kumar at University of Warwick, UK A. Kumar, D. O'Neill, B. P. Gompertz, J. Lyman, G. Ramsay, R. Starling, K. Ackley, M. J. Dyer, K. Ulaczyk, F. Jimenez-Ibarra, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Palle and D. Pollacco report on behalf of the GOTO collaboration: We report on observations with the Gravitational-wave Optical Transient Observer (GOTO, Steeghs et al. 2022) in response to GRB 240905B (Fermi GBM team, GCN 37389; Joshi et al., GCN 37391; Gupta et al., GCN 37418). Targeted observations of the GBM localisation were performed by GOTO North and South from 2024-09-05 09:29:19 UT to 2024-09-06 00:48:53 UT (respectively from +5.03 to +20.33 hours after trigger) distributed over four epochs. Each observation consisted of 4x90s exposures in the GOTO L-band (400-700 nm). Images were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using recent survey observations of the same pointings. Source candidates were initially filtered using a classifier (Killestein et al. 2021) and cross-matched against a variety of contextual and minor planet catalogues. Human vetting was carried out in real time on any candidates that passed the above checks. No candidate optical counterparts are identified within a circular region of radius 0.2 degrees centered on the Fermi/LAT localisation (Gupta et al., GCN 37418). The typical depth of the most constraining image is L > 20.7 mags (5-sigma), taken at 09:36:50 UT on 2024-09-05 (~5.1 hours after the GBM trigger). Forced photometry at the positions of 6 Swift/XRT detected uncatalogued X-ray sources (Brivio et al., GCN 37421) in this image similarly provides 5-sigma limiting L-band magnitudes of ~20.7 on each. Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and were not corrected for Galactic extinction. GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester and the Instituto de Astrofisica de Canarias (IAC).
GCN 37436 table
GRB_name GRB240905B
GCN_number 37436
Detection_method Fermi GBM Det
t_trigger 4:27:16.140 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 37436 SUBJECT: GRB 240905B: Fermi GBM Observation DATE: 24/09/09 16:29:13 GMT FROM: Sarah Dalessi at UAH S. Dalessi (UAH), A. Myers (NPP/GSFC) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 04:27:16.14 UT on 05 September 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240905B (trigger 747203241/240905186). which was also detected by AstroSat (J. Joshi et al. 2024, GCN 37391) and Fermi-LAT (R. Gupta et al. 2024, GCN 37418). The Fermi GBM on-ground location is consistent with the AstroSat and Fermi-LAT positions. The angle from the Fermi LAT boresight is 25 degrees. The GBM light curve single emission episode with a duration (T90) of about 1.3 s (50-300 keV). The time-averaged spectrum from T0+0 to T0+1.280 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.36 +/- 0.04 and the cutoff energy, parameterized as Epeak, is 1240 +/- 70 keV. The event fluence (10-1000 keV) in this time interval is (5.11 +/- 0.08)E-06 erg/cm^2. The 64-ms peak photon flux measured starting from T0+0.32 s in the 10-1000 keV band is 30 +/- 1 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 1223 +/- 70 keV, alpha = -0.36 +/- 0.04 and beta = -4.16 +/- 1.24. 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 37455 table
GRB_name GRB240905B
GCN_number 37455
Detection_method IPN Triangulation
t_trigger 4:27:16 UTC
ra 267.9220°
decl 14.2400°
Circular_text TITLE: GCN CIRCULAR NUMBER: 37455 SUBJECT: IPN triangulation of GRB 240905B (short) DATE: 24/09/11 15:24:31 GMT FROM: Dmitry Svinkin at Ioffe Institute A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin on behalf of the MGNS/BepiColombo team, J. Benkhoff on behalf of the BepiColombo team, D. Svinkin, D. Frederiks, A. Ridnaia, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, and E. Burns on behalf of the Fermi GBM team, E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and G. Waratkar, V. Jethwani, J.Joshi, V. Bhalerao, D. Bhattacharya, and S. Vadawale, on behalf of the Astrosat-CZTI team, report: The short-duration GRB 240905B (Fermi-GBM detection: The Fermi GBM team, GCN 37389; Dalessi et al., GCN 37436; AstroSat-CZTI detection: Joshi et al., GCN 37391; Fermi-LAT detection: Gupta et al., GCN 37418) was detected by Fermi (GBM and LAT), Konus-Wind, INTEGRAL (SPI-ACS), Astrosat (CZTI), and BepiColombo (MGNS) at about 16036 s UT (04:27:16). We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 267.922 (17h 51m 41s) +14.240 (+14d 14' 24") Corners: 267.264 (17h 49m 03s) +12.544 (+12d 32' 40") 267.181 (17h 48m 43s) +12.565 (+12d 33' 54") 268.618 (17h 54m 28s) +15.927 (+15d 55' 37") 268.703 (17h 54m 49s) +15.906 (+15d 54' 21") --------------------------------------------- The error box area is 1087 sq. arcmin, and its maximum dimension is 3.65 deg (the minimum one is 5 arcmin). The Sun distance was 100 deg. This localization may be improved. The IPN localization is consistent with, but reduces the area of, the Fermi-LAT localization. Swift-XRT reported six afterglow candidates for this burst (Source 1-6, Brivio et. al., GCN 37421). Three candidates (Sources 1, 2, and 6) are inside the IPN box. A triangulation map and HEALPix FITS file are posted at http://www.ioffe.ru/LEA/GRBs/GRB240905_T16038/IPN/ The HEALPix triangulation map is the multi-order HEALPix in units of probability density. The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular.
GCN 37601 table
GRB_name GRB240905B
GCN_number 37601
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 37601 SUBJECT: GRB 240905B: VZLUSAT-2 detection DATE: 24/09/24 17:57:04 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 (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. Hroch, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo (Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida (ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe (Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes (VZLU), I. Vertat (FEL ZCU) -- the VZLUSAT-2/GRB payload collaboration. The short-duration GRB 240905B (Fermi/GBM detection: GCN 37389; AstroSat/CZTI detection: GCN 37391; Konus/Wind detection at 2024-09-05 04:27:18.558 UTC; INTEGRAL/SPI-ACS peak detection at 2024-09-05 ~04:27:16 UTC) was detected by the GRB detector on board of the VZLUSAT-2 3U CubeSat (https://www.vzlusat2.cz/en/). The data acquisition was performed by the GRB detector unit no. 1. The detection was confirmed at the peak time 2024-09-05 04:27:15 UTC. The T90 duration is 1 s and the significance during T90 reaches 11 sigma. The light curve obtained by VZLUSAT-2 is available here: https://vzlusat2.konkoly.hu/static/share/GRB240905B_GCN_VZLUSAT2.pdf All VZLUSAT-2 detections are listed at: https://monoceros.physics.muni.cz/hea/VZLUSAT-2/ The GRB detectors on VZLUSAT-2 are a demonstration payload for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Two GRB modules of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 January 13 from Cape Canaveral.
GCN 37613 table
GRB_name GRB240905B
GCN_number 37613
Detection_method Konus-Wind Det
t_trigger 4:27:18.558 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 37613 SUBJECT: Konus-Wind detection of GRB 240905B DATE: 24/09/26 15:50:34 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, 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 240905B (Fermi-GBM detection: The Fermi GBM team, GCN 37389; Dalessi et al., GCN 37436; AstroSat-CZTI detection: Joshi et al, GCN 37391; Fermi-LAT detection: Gupta et al., GCN 37418; IPN triangulation: Kozyrev et al., GCN 37455; VZLUSAT-2 detection: Dafcikova et al., GCN 37601) triggered Konus-Wind at T0=16038.558 s UT (04:27:18.558). The burst light curve shows a multipeaked structure which starts at ~T0-0.1 s and has a total duration of ~1 s. The emission is seen up ~5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240905_T16038/ As observed by Konus-Wind, the burst had a fluence of 1.68(-0.28,+0.35)x10^-5 erg/cm2, and a 16-ms peak flux, measured from T0+0.432 s, of 4.13(-1.05,+1.17)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+8.448 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.54(-0.18,+0.21) and Ep = 1229(-251,+357) keV (chi2 = 92/87 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.2 (chi2 = 92/86 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.