//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8803 SUBJECT: GRB 090112: Fermi GBM detection DATE: 09/01/13 16:44:12 GMT FROM: Elisabetta Bissaldi at MPE E. Bissaldi (MPE) and A. von Kienlin (MPE) report on behalf of the Fermi GBM Team: "At 07:57:23.11 UT on 12 January 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090112 (trigger 253439845 / 090112332). The on-ground calculated location, using the GBM trigger data, is RA = 111.8, DEC = -30.3 (J2000 degrees, equivalent to 07h 27m, -30d 17'), with an uncertainty of 1.7 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 4 degrees. This burst was also independently detected by INTEGRAL SPI-ACS. The GRB lightcurve consists of two peaks with some substructure appearing at T0 and T0+4 s, respectively. A possible precursor is present around T0-20 s and additional weak emission is visible up to T0+50s. The event duration (T90) is about 65 s (8-1000 keV) and T50 is about 27 s (8-1000 keV). The time-averaged spectrum from T0-6 s to T0+18 s is best fit by a Band function with Epeak = 150 +/- 40 keV, alpha = -0.94 +/- 0.20 and beta = -2.01 +/- 0.19 (chi squared 464 for 456 d.o.f.). The event fluence (8-1000 keV) in this time interval is (5.2 +/- 1.0)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+4 s in the 8-1000 keV band is 7 +/- 2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8805 SUBJECT: GRB 090112B: Fermi GBM Detection DATE: 09/01/13 22:21:26 GMT FROM: Alexander van der Horst at NASA/MSFC A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM Team: "At 17:30:15.45 UT on 12 January 2009, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 090112B (trigger 253474217 / 090112.729). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 192.7, Dec = +22.2 (J2000 degrees, equivalent to J2000 12h51m, +22d12'), with a statistical uncertainty of 2.1 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 95 degrees. The GBM light curve shows one pulse with some substructure, with a duration (T90) of about 12 s (50-300 keV). The time-averaged spectrum from T0 to T0+8.70 s is best fit by a Band function with Epeak = 139 +/- 9 keV, alpha = -0.75 +/- 0.06 and beta = -2.43 +/- 0.14. The fluence (8-1000 keV) in this time interval is (5.4 +/- 0.3)E-6 erg/cm^2. The 1-sec peak photon flux measured starting from T0+2.6s in the 8-1000 keV band is 14 +/- 1 ph/s/cm^2. The spectral and temporal analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8815 SUBJECT: GRB 090112B: Suzaku WAM observation of the prompt emission DATE: 09/01/16 10:21:36 GMT FROM: Kazutaka Yamaoka at Aoyama Gakuin U M. Suzuki, M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, T. Tamagawa (RIKEN), H. Hayashi, E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara, N. Ohmori, K. Kono (Univ. of Miyazaki), A. Endo, M. Tashiro, Y. Terada, Y. Urata, K. Onda, N. Kodaka, K. Morigami, T. Sugasahara, W. Iwakiri (Saitama U.), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Sugita, K. Yamaoka (Aoyama Gakuin U.), Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira (Hiroshima U.), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The long GRB 090112B (van der Horst et al., GCN 8805) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2009-01-12 17:30:14 UT (=T0). The observed light curve shows multiple peaks and lasting from T0-1 s to T0+12 s with a duration (T90) of about 8 seconds. The fluence in 100 - 1000 keV was (5.2 +/- 0.3) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+3 s was 3.5 (+0.2/-0.3) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-1 s to T0+12 s is well fitted by a single power-law with a photon index of 2.46 +/- 0.14 (chi^2/d.o.f = 18/22). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html