March 2023 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 31354] GRB 230328B : GRANDMA/Kilonova-Catcher optical detection
by GCN Circulars 31 Mar '23

31 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33550 SUBJECT: GRB 230328B : GRANDMA/Kilonova-Catcher optical detection DATE: 23/03/31 20:37:22 GMT FROM: Damien Turpin at NAOC (CAS) <dturpin-astro(a)hotmail.com> F. Kugel (KNC), D. Turpin (CEA), S. Karpov (FZU), T. Hussenot-Desenonges (IJCLab), S. Antier (OCA/Artemis), P.A. Duverne (APC, U. Paris Cit�), P. Hello (IJCLab), A. Klotz (OMP/IRAP) report on behalf of the GRANDMA/Kilonova-Catcher collaboration: The Kilonova-Catcher telescope network responded to the alert of GRB 230328B (Swift detection: Gropp et al., GCN 33527; Fermi GBM detection: Veres et al., GCN 33526). The KNC observations were taken by F. Kugel with an ARTEMIS CCD ATIK-460ex camera mounted in the 0.4-m f/2.8 reflector telescope in the Chante-Perdrix Observatory (France). The afterglow is detected in the 36x60s unfiltered coadded images at about 5.2 hours (midtime of the exposure) after the Swift/BAT trigger time. Below, we report our photometric measurement in Rc magnitude. ------------------------------------------------------------- T-T0 (day) |Exposure| Filter | Mag +/- err |Mag.Lim. (AB) ------------------------------------------------------------- 0.22172 | 36 x 60s | Rc | 20.19 +/- 0.10 | 21.4 (3 sigma) Our detection is consistent with the detections and limits previously reported in Pankov et al., GCN 33528.; Belkin, GCN 33530; Lu et al., GCN 33534; Catapano et al., GCN 33535; Suresh et al., GCN 33536.; Adami et al., GCN 33537; Gompertz et al., GCN 33538; Komesh et al., GCN 33539; Lu et al., GCN 33540; Ror et al., GCN 33547; Agui Fernandez et al., GCN 33549 The GRANDMA/Kilonova-Cacther images have been calibrated using field stars from the PanSTARRS-DR1 catalog using the STDpipe pipeline (Karpov 2022) and the ps1/r to Rc mag conversion from (Pancino et al. 2022). GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).

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[vsnet-grb-info 31353] GRB 23038B: CAHA 2.2m/CAFOS detection
by GCN Circulars 31 Mar '23

31 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33549 SUBJECT: GRB 23038B: CAHA 2.2m/CAFOS detection DATE: 23/03/31 19:29:32 GMT FROM: J. F. Agui Fernandez at IAA-CSIC <feli(a)iaa.es> J. F. Agui Fernandez (IAA-CSIC), A. de Ugarte Postigo (OCA/CNRS), C. C. Thoene (ASU-CAS), M. Blazek (CAHA) , Ana Guijarro (CAHA) and S. Cikota (CAHA) report: We observed the afterglow of GR230328B (Fermi/GBM Detection: Fermi GBM Team GCN 33526, Swift detection: Gropp et al. GCN 33527) with CAFOS mounted on the 2.2 m telescope at the Calar Alto Observatory (Almeria, Spain). The observations consisted of 5 x 360 s in Rc-band and were obtained at mean epoch of 0.4717 days after the GRB. The afterglow is clearly detected with Rc = 21.00 ± 0.06 (AB) mag measured against comparison stars from the PanSTARRS catalogue.

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[vsnet-grb-info 31352] IceCube-Cascade 230329A: Upper limits from a search for additional neutrino events in IceCube
by GCN Circulars 31 Mar '23

31 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33548 SUBJECT: IceCube-Cascade 230329A: Upper limits from a search for additional neutrino events in IceCube DATE: 23/03/31 15:37:30 GMT FROM: Jessie Thwaites at IceCube/U Wisc-Madison <thwaites(a)wisc.edu> The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search [1] for additional track-like muon neutrino events arriving from the direction of IceCube-Cascade 230329A (https://gcn.gsfc.nasa.gov/notices_amon_icecube_cascade/137786_1524801.amon) in a time range of 1000 seconds centered on the alert event time (2023-03-29 20:21:48.310 UTC to 2023-03-29 20:38:28.310 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero track-like events are found within the 90% containment region of IceCube-Cascade 230329A. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-Cascade 230329A ranges from 1.0e+01 to 1.9e+01 GeV cm^-2 in a 1000 second time window. 90% of events IceCube would detect from a source at this declination with an E^-2.5 spectrum have energies in the approximate energy range between 4e+04 GeV and 4e+06 GeV. A subsequent search was performed including 2 days of data centered on the alert event time (2023-03-28 20:30:08.310 UTC to 2023-03-30 20:30:08.310 UTC). In this case, we report a p-value of 0.89, consistent with no significant excess of track events. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-Cascade 230329A ranges from 1.0e+01 to 1.9e+01 GeV cm^-2 in a 2 day time window. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc(a)icecube.wisc.edu. [1] IceCube Collaboration, R. Abbasi et al., ApJ 910 4 (2021)

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[vsnet-grb-info 31351] GRB 230328B: 3.6m DOT multiband optical observation
by GCN Circulars 31 Mar '23

31 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33547 SUBJECT: GRB 230328B: 3.6m DOT multiband optical observation DATE: 23/03/31 07:49:48 GMT FROM: Amit Kumar Ror at ARIES <mitturor77894(a)gmail.com> Amit K. Ror, Rahul Gupta, S. B. Pandey, A. Ghosh, A. Aryan, and K. Misra (ARIES) report: GRB 230328B was triggered by Swift-BAT at 14:54:48 UT and Fermi-GBM at 14:54:47.43 UT on 28-03-2023 (Gropp et al. 2023 GCN 33527, Dalessi et al. 2023 GCN 33531). The prompt emission was also detected by other space-based facilities like AstroSat-CZTI (Waratkar et al. 2023, GCN 33532), GRBAlpha (Dafcikova et al. 2023, GCN 33543), and Konus-Wind (Svinkin et al. 2023, GCN 33544). We searched for extended GeV emission for a temporal window of 10 ks since the GBM trigger, based on available LAT data. However, we did not find the detection of any GeV photons, and an upper limit was obtained for an energy flux < 5.2 x 10^{-10} erg/cm2/s in the energy range 100 MeV - 100 GeV with TS < 20. We observed the field of GRB 230328B using the 3.6m Devasthal Optical Telescope located at the Devasthal observatory of the Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India. We have taken multiple frames with an exposure time of 300 sec each in several optical passbands. We clearly detect the optical afterglow discovered by Swift-UVOT in each individual image. The estimated preliminary magnitude is as follows: Date Start_UT T_start-T0 (days) Filter Exp time (sec) magnitude ============================================================== 2023-03-28 21:51:54.44 ~0.29 R 300 sec 20.30 +/- 0.08 The magnitude quoted is not corrected for the galactic and host extinctions in the direction of the burst. Photometric calibration is performed using the standard stars from the USNO-B1 catalog. The detection of the optical afterglow is consistent with the observation of Gropp et al. 2023 (GCN 33527), Pankov et al. 2023 (GCN 33528), Belkin et al. 2023 (GCN 33530), Lu et al. 2023 (GCN 33534), Catapano et al. (33535), Suresh et al. (GCN 33536), Adami et al. (GCN 33537), Gompertz et al. (GCN 33538), Komesh et al. (GCN 33539), Lu et al. 2023 (GCN 33540) By combining our R-band magnitude with the observations of Pankov et al. 2023 (GCN 33528) and Belkin et al. 2023 (GCN 33530), we have determined the preliminary flux decay index of 0.55 +/-0.06. This circular may be cited. The 3.6m Devasthal Optical Telescope (DOT) is a recently commissioned facility in the Northern Himalayan region of India (long: 79 41 04E, lat: 29 21 40N, alt: 2540m) owned and operated by the Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital ( https://www.aries.res.in). The authors of this GCN circular thankfully acknowledge the consistent support from the staff members to run and maintain the 3.6m DOT.

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[vsnet-grb-info 31350] Fermi trigger No 701883729: Global MASTER-Net observations report
by GCN Circulars 30 Mar '23

30 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33546 SUBJECT: Fermi trigger No 701883729: Global MASTER-Net observations report DATE: 23/03/30 18:30:29 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D.Cheryasov, Ya.Kechin (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. Gres, N.M. Budnev (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), A. Gabovich, V.Yurkov (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 GRB230330.65 (trigger No 701883729,23h 36m 48.00s , -71d 23m 24.0s, R=7.86) errorbox 6587 sec after notice time and 6594 sec after trigger time at 2023-03-30 17:31:58 UT, with upper limit up to 18.1 mag. Observations started at twilight. The observations began at zenith distance = 70 deg. The sun altitude is -12.3 deg. The galactic latitude b = -45 deg., longitude l = 311 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2207407 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 6624 | 2023-03-30 17:31:58 | MASTER-SAAO | (23h 07m 13.46s , -70d 58m 57.0s) | C | 60 | 17.3 | 6704 | 2023-03-30 17:33:18 | MASTER-SAAO | (23h 31m 43.34s , -71d 00m 16.9s) | C | 60 | 17.6 | 6979 | 2023-03-30 17:37:53 | MASTER-SAAO | (00h 51m 09.70s , -70d 59m 16.2s) | C | 60 | 14.0 | 7069 | 2023-03-30 17:39:23 | MASTER-SAAO | (23h 00m 59.38s , -72d 54m 49.2s) | C | 60 | 17.4 | 7148 | 2023-03-30 17:40:42 | MASTER-SAAO | (23h 28m 12.92s , -72d 54m 18.3s) | C | 60 | 17.8 | 7318 | 2023-03-30 17:43:33 | MASTER-SAAO | (00h 12m 20.13s , -72d 53m 05.7s) | C | 60 | 18.0 | 7410 | 2023-03-30 17:45:05 | MASTER-SAAO | (23h 13m 46.69s , -69d 04m 36.6s) | C | 60 | 17.5 | 8133 | 2023-03-30 17:57:07 | MASTER-SAAO | (23h 36m 16.46s , -69d 04m 57.2s) | C | 60 | 18.0 | 8213 | 2023-03-30 17:58:27 | MASTER-SAAO | (23h 07m 27.72s , -71d 00m 29.9s) | C | 60 | 18.1 | 8303 | 2023-03-30 17:59:58 | MASTER-SAAO | (23h 32m 01.71s , -70d 58m 49.1s) | C | 60 | 18.1 | 8702 | 2023-03-30 18:06:37 | MASTER-SAAO | (23h 01m 23.47s , -72d 54m 03.2s) | C | 60 | 17.7 | 8782 | 2023-03-30 18:07:56 | MASTER-SAAO | (23h 28m 25.09s , -72d 54m 52.0s) | C | 60 | 18.1 | 9155 | 2023-03-30 18:14:10 | MASTER-SAAO | (23h 14m 08.69s , -69d 06m 31.0s) | C | 60 | 17.3 | 9327 | 2023-03-30 18:17:01 | MASTER-SAAO | (23h 07m 37.78s , -70d 58m 54.7s) | C | 60 | 17.5 | 9406 | 2023-03-30 18:18:20 | MASTER-SAAO | (23h 32m 14.04s , -70d 59m 44.3s) | C | 60 | 17.8 | 9705 | 2023-03-30 18:23:19 | MASTER-SAAO | (23h 01m 30.56s , -72d 53m 37.1s) | C | 60 | 17.9 | 9795 | 2023-03-30 18:24:49 | MASTER-SAAO | (23h 28m 40.59s , -72d 54m 58.7s) | C | 60 | 17.6 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.

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[vsnet-grb-info 31349] GRB 230330B: Fermi GBM Final Localization
by GCN Circulars 30 Mar '23

30 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33545 SUBJECT: GRB 230330B: Fermi GBM Final Localization DATE: 23/03/30 16:48:56 GMT FROM: Joshua Wood at MSFC/Fermi-GBM <joshua.r.wood(a)nasa.gov> The Fermi GBM team reports the detection of a likely LONG GRB "At 00:26:04 UT on 30 March 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230330B (trigger 701828769/230330018). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 65.05, Dec = -35.22 (J2000 degrees, equivalent to J2000 4h 20m, -35d 13'), with a statistical uncertainty of 8.61 degrees. The angle from the Fermi LAT boresight is 32 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230330018/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230330018/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230330018/…"

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[vsnet-grb-info 31348] Konus-Wind detection of GRB 230328B
by GCN Circulars 30 Mar '23

30 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33544 SUBJECT: Konus-Wind detection of GRB 230328B DATE: 23/03/30 14:13:25 GMT FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru> D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova, A. Lysenko, A. Ridnaia, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 230328B (Fermi-GBM detection: The Fermi GBM team, GCN Circ. 33526; Swift-BAT detection: Gropp et al., GCN Circ. 33527; Markwardt et al., GCN Circ. 33541; AstroSat-CZTI detection: Waratkar et al., GCN Circ. 33532; GRBAlpha detection: Dafcikova et al., GCN Circ. 33543;) triggered Konus-Wind at T0=53688.873 s UT (14:54:48.873). The burst light curve shows a multi-peaked structure which starts at ~T0-3.3 s and has a total duration of ~12 s. The emission is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB230328_T53688/ As observed by Konus-Wind, the burst had a fluence of 7.12(-0.51,+0.58)x10^-6 erg/cm2, and a 64-ms peak flux, measured from T0+0.430 s, of 2.87(-0.77,+0.78)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+8.448 s) is best fit in the 20 keV - 5 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.38(-0.13,+0.14) and Ep = 151(-21,+29) keV (chi2 = 73/75 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 = 74/24 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.

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[vsnet-grb-info 31347] GRB 230328B: GRBAlpha detection
by GCN Circulars 30 Mar '23

30 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33543 SUBJECT: GRB 230328B: GRBAlpha detection DATE: 23/03/30 11:54:37 GMT FROM: Marianna Dafcikova at Masaryk University <500025(a)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 230328B (Fermi/GBM detection: GCN 33526; Swift/BAT detection: GCN 33527; AstroSat/CZTI detection: GCN 33532; GECAM-B detection: trigger no. 165) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023; arXiv:2302.10048). The detection was confirmed at the peak time 2023-03-28 14:54:49 UTC. The T90 duration measured by GRBAlpha is 8 s and the overall significance during T90 reaches 13 sigma. GRBAlpha entered the outer Van Allen radiation belt during the tail part of the burst. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB230328B_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.

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[vsnet-grb-info 31346] GRB 230330A: Fermi GBM Final Real-time Localization
by GCN Circulars 30 Mar '23

30 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33542 SUBJECT: GRB 230330A: Fermi GBM Final Real-time Localization DATE: 23/03/30 04:44:38 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply(a)GIOC.nsstc.nasa.gov> The Fermi GBM team reports the detection of a likely LONG GRB At 04:34:29 UT on 30 Mar 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230330A (trigger 701843674.478352 / 230330191). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 282.7, Dec = -12.6 (J2000 degrees, equivalent to J2000 18h 50m, -12d 35'), with a statistical uncertainty of 4.0 degrees. The angle from the Fermi LAT boresight is 47.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230330191/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230330191/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230330191/…

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[vsnet-grb-info 31345] GRB 230328B: Swift-BAT refined analysis
by GCN Circulars 30 Mar '23

30 Mar '23

TITLE: GCN CIRCULAR NUMBER: 33541 SUBJECT: GRB 230328B: Swift-BAT refined analysis DATE: 23/03/30 03:44:23 GMT FROM: Tyler Parsotan at UMBC/GSFC/CRESST II <parsotat(a)umbc.edu> C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), 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-240 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 230328B (trigger #1162001) (Gropp, et al., GCN Circ. 33527). The BAT ground-calculated position is RA, Dec = 291.037, 80.013 deg which is RA(J2000) = 19h 24m 08.8s Dec(J2000) = +80d 00' 45.3" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 46%. The mask weighted light curve has a double peaked structure. The light curve does not show an early afterglow as was stated in the original GCN. T90 (15-350 keV) is 19.23 +- 3.82 sec (estimated error including systematics). The time-averaged spectrum from T-7.38 to T+25.49 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.22 +- 0.29, and Epeak of 99.7 +- 59.7 keV (chi squared 29.53 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 4.3 +- 0.2 x 10^-06 erg/cm2 and the 1-sec peak flux measured from T+0.26 sec in the 15-150 keV band is 8.4 +- 0.5 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.63 +- 0.07 (chi squared 35.85 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/1162001/BA/

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