//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10330 SUBJECT: GRB 100116A: Fermi GBM detection DATE: 10/01/17 02:29:49 GMT FROM: Michael S. Briggs at UAH and MSFC M. S. Briggs and V. Connaughton (UA Huntsville), report on behalf of the Fermi GBM Team: "At 21:31:00.24 UT on 16 January 2010, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 100116A (trigger 285370262 / 100116.897). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 301.48, Dec = +16.24 (J2000 degrees, equivalent to J2000 20h 06m, +16d 14'), with a statistical uncertainty of 1.0 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 29 degrees. The GBM light curve shows two peaks separated by over 60 seconds with little or no intervening emission. The total duration is approximately 110 seconds. Both peaks are best fit with a power law function with an exponential high-energy cutoff. The first peak, fit from -3.072 to 2.048 s, has Epeak = 240 (-40,+60) keV and an index of -0.92 +/- 0.15. The fluence of this peak is (1.5 +/- 0.1) E-6 ergs / cm**2. The second peak, fit from 82.949 to 101.38 s, has Epeak = 1240 +/- 90 keV and an index of -1.02 +/- 0.017. The fluence of this peak is (3.36 +/- 0.03) E-5 ergs / cm**2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10333 SUBJECT: GRB 100116A: Fermi LAT detection DATE: 10/01/17 05:04:12 GMT FROM: Julie McEnery at NASA/GSFC Julie McEnery (GSFC), Jim Chiang (SLAC), Nicola Omodei (Stanford) and Tak Nakamori (Tokyo Institute of Technology) report on behalf of the Fermi LAT team: At 21:32:36.00 (UT) on 16 Jan 2010, the Fermi Large Area Telescope (LAT) detected gamma rays from the long GRB 100116A, which was triggered and located by the Fermi Gamma-ray Burst Monitor (GBM) (trigger 285370262 / 100116.897, GCN10330). The angle of the GBM best position (RA, Dec= 301.48, 16.24) with respect to the LAT boresight was ~29 degrees at the time of the LAT detection, which is well within our field of view. The data from the Fermi LAT shows an increase in the event rate coincident with the second peak in the GBM lightcurve (around 90s after the GBM trigger) that is spatially correlated with the GBM emission. It is a relatively weak detection with less than 20 excess events, most with energy below 100 MeV. The best LAT on-ground localization is found to be (RA, Dec = 305.02, 14.45) (RA=20h 20' 04.80'', Dec=14d 27' 00.0'', J2000) with a 90% containment radius of 0.30 deg (statistical; 68% containment radius: 0.17 deg) which is consistent with the GBM localization. A Swift TOO request cannot be requested due to Sun constraints. Further analysis is ongoing. The point of contact for this burst is Julie McEnery: julie.mcenery@nasa.gov 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. This message can be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10347 SUBJECT: Konus-Wind observation of GRB 100116A DATE: 10/01/19 13:23:06 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 hard GRB 100116A (Fermi-GBM trigger 285370262: Briggs and Connaughton, GCN 10330; Fermi-LAT localization: McEnery et al., GCN 10333) triggered Konus-Wind at T0=77543.747s UT (21:32:23.747) The burst light curve shows a single-pulse structure with a total duration of ~30 s. A weaker precursor, reported by Fermi-GBM (GCN 10330) is clearly seen in the low-resolution background mode data at T0-88s. The emission is seen up to 10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB100116_T77543/ As observed by Konus-Wind the burst had a fluence of 5.7(+/-0.6)x10-5 erg/cm2, and a 256-ms peak flux measured from T0+6.144s of 4.2(+/-0.4)x10-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+23.296 s) is well be fitted 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 = -0.96(-0.06, +0.07), and Ep = 968(-130, +163) keV (chi2 = 105/98 dof). The spectrum of the most intense part of the burst (measured from T0+0.256 to T0+8.192 s) is well fitted in the 20 keV - 10 MeV range by a power law with exponential cutoff model, for which alpha = -0.96(+/-0.6), and Ep = 1015(-121, +146) keV (chi2 = 107/101 dof). All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10353 SUBJECT: GRB 100116A: Suzaku WAM observation of the prompt emission DATE: 10/01/21 13:06:25 GMT FROM: Takeshi Uehara at Hiroshima U T. Uehara, Y.Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.) K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U), Y. Terada, M. Tashiro, 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), N. Vasquez (Tokyo Tech.), 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 100116A (Fermi/GBM trigger #285370262 / 100116.89 Briggs et al., GCN 10330, McEnery et al., GCN 10333) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 21:31:00.15 UT (=T0). The observed light curve shows two separated pulses, a precursor at T0+0 to T0+4 sec and a main harder pulse at T0+81 to T0+111 sec, and the duration (T90) was about 96 seconds. The fluences in 100 - 1000 keV were 1.24(-0.16, +0.17) e-6 and 2.89 (-0.08, +0.06) e-5 erg/cm^2 in the precursor and the main pulse, respectively. The 1-s peak flux measured from T0+94 s was 7.26 (-0.43, +0.47) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0+81 s to T0+111 s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.15 (-0.10, +0.09), and Epeak 1119 (-135, +137) keV (chi^2/d.o.f. = 79.0/54). 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 -- Takeshi Uehara (Hiroshima Univ.) E-mail: uehara@hep01.hepl.hiroshima-u.ac.jp