//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10348 SUBJECT: GRB 100119A: Swift detection of a burst DATE: 10/01/19 18:40:44 GMT FROM: Scott Barthelmy at NASA/GSFC V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), S. Campana (INAF-OAB), P.A. Curran (MSSL-UCL), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC), T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU), M. C. Stroh (PSU), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 18:25:25 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100119A (trigger=383063). Swift did not slew because of a Sun observing constraint. The BAT on-board calculated location is RA, Dec 299.327, -53.160 which is RA(J2000) = 19h 57m 18s Dec(J2000) = -53d 09' 36" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows multiple overlapping peaks with a duration of about 25 sec. The peak count rate was ~6000 counts/sec (15-350 keV), at T+5 sec. Due to an observing constraint, Swift cannot slew to the BAT position. There will thus be no XRT or UVOT data for this trigger. No observations with XRT or UVOT will be possible for approximately the next 26 days. Burst Advocate for this burst is V. Mangano (vanessa AT ifc.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/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10351 SUBJECT: GRB 100119A: Swift-BAT refined analysis DATE: 10/01/19 22:29:14 GMT FROM: Scott Barthelmy at NASA/GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA), C. B. Markwardt (GSFC/UMD), T. Sakamoto (GSFC/UMBC), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 100119A (trigger #383063) (Mangano, et al., GCN Circ. 10348). The BAT ground-calculated position is RA, Dec = 299.308, -53.149 deg which is RA(J2000) = 19h 57m 14.0s Dec(J2000) = -53d 08' 56.7" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 7%. The mask-weighted light curve shows several overlapping peaks starting at ~T-30 sec, peaking at ~T+3 sec, and ending at ~T+30 sec. T90 (15-350 keV) is 23.8 +- 4 sec (estimated error including systematics). The time-averaged spectrum from T-15.8 to T+15.5 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.01 +- 0.06. The fluence in the 15-150 keV band is 1.4 +- 0.0 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+2.12 sec in the 15-150 keV band is 7.7 +- 1.0 ph/cm2/sec. 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/383063/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10356 SUBJECT: Konus-Wind observation of GRB 100119A DATE: 10/01/23 17:39:23 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long GRB 100119A (Swift-BAT trigger=383063: Mangano et al., GCN 10348) triggered Konus-Wind at T0=66306.167s UT (18:25:06.167) The burst light curve shows a complex structure with a total duration of ~45 s. The emission is seen up to several MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB100119_T66306/ As observed by Konus-Wind the burst had a fluence of 6.1(+/-0.3)x10-5 erg/cm2, and a 256-ms peak flux measured from T0+18.176s of 4.3(+/-0.3)x10-6 erg/cm2/s (both in the 20 keV - 2 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+37.376 s) is well be fitted in the 20 keV - 10 MeV range by a power law with GRB (Band) model, for which: the low-energy photon index alpha = -0.73 (-0.08,+0.09), the high energy photon index beta = -2.8(-1.9, +0.4), the peak energy Ep = 377(-35, +35)keV (chi2 = 66/97 dof). The spectrum of the most intense part of the burst (measured from T0+15.360 to T0+21.504 s) is well fitted in the 20 keV - 10 MeV range by a power law with exponential cutoff model, for which alpha = -0.52(+/-0.11), and Ep = 387(-32, +37) keV (chi2 = 97/96 dof). All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10357 SUBJECT: GRB 100119A: Suzaku WAM observation of the prompt emission DATE: 10/01/28 05:12:04 GMT FROM: Nicolas Vasquez at Tokyo Inst of Tech ========================================================================= N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.), T. Uehara, Y.Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.) S. Sugita (Nagoya U), M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara, W. Iwakiri (Saitama U.), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, E. Sonoda, K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), Y. Urata, H. M. Lin (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The long GRB 100119A (Swift BAT trigger #383063; Mangano et al. GCN 10348) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 18:25:09.630 UT (=T0). The observed light curve shows a complicated structure, with overlapping pulses. The duration (T90) was about 24 seconds. The fluence in 100 - 1000 keV band is 4.55(-0.21, +0.17) x 10^-6 erg/cm2 with a 1-s peak flux measured from T0+18.5 sec of 6.94 (-0.63, +0.32) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-3.5 s to T0+37.5 s is well fitted by a cut off power-law model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.17 (-0.27, +0.26), and Epeak 510 (-45, +54) keV (chi^2/d.o.f. = 26.7/24). Due to the brightness of this burst, a 3% systematic error was added for low energy channels. All the quoted errors are at 90% confidence level. The light curves of this event are available at the following URL: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html =========================================================================