//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12698 SUBJECT: IPN Triangulation of GRB 111215B (long/intense) DATE: 11/12/16 21:21:48 GMT FROM: Valentin Pal'shin at Ioffe Inst K. Hurley, on behalf of the Mars Odyssey and MESSENGER GRB teams, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, J. Goldsten, on behalf of the MESSENGER NS GRB team, K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long-duration, intense GRB 111215B was observed by Konus-Wind, Suzaku-WAM, MESSENGER (GRNS), and Mars Odyssey (HEND) at about 73686 s UT (20:28:06). We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 222.403 (14h 49m 37s) +16.439 (+16d 26' 21") Corners: 222.265 (14h 49m 04s) +16.514 (+16d 30' 51") 222.532 (14h 50m 08s) +16.665 (+16d 39' 53") 222.540 (14h 50m 10s) +16.364 (+16d 21' 49") 222.274 (14h 49m 06s) +16.212 (+16d 12' 43") --------------------------------------------- The error box area is 282 sq. arcmin, and its maximum dimension is 31 arcmin. This box can be improved. The time history and spectrum will be given in a forthcoming GCN Circular. A Swift ToO observation has been requested. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12700 SUBJECT: GRB 111215B: Swift-XRT observations DATE: 11/12/17 12:07:31 GMT FROM: Owen Littlejohns at U of Leicester O. M. Littlejohns (U. Leicester) reports on behalf of the Swift-XRT team: We have analysed 4.9 ks of XRT data for the IPN-detected burst: GRB 111215B (Hurley et al. et al. GCN Circ. 12698), from 113.3 ks to 130.4 ks after the IPN trigger. The data are entirely in Photon Counting (PC) mode. An X-ray source is detected within the IPN error circle. The refined XRT position is RA, Dec = 222.3994, +16.45412 which is equivalent to: RA (J2000): 14 49 35.86 Dec(J2000): +16 27 14.8 with an uncertainty of 3.7 arcsec (radius, 90% confidence). This position is 55 arcsec from the IPN position. The light curve is consistent with a constant source of mean count rate 2.6e-02 ct/sec. A power-law fit gives an index of 1.9 (+0.9, -2.8). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.5 (+0.5, -0.3). The best-fitting absorption column is 2 (+11, -1) x 10^20 cm^-2, consistent with the Galactic value of 1.6 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.9 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2 (+11, -1) x 10^20 cm^-2 Galactic foreground: 1.6 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.5 (+0.5, -0.3) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020193. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12701 SUBJECT: Konus-Wind observation of GRB 111215B DATE: 11/12/17 12:20:31 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 intense GRB 111215B (localized by IPN: Hurley et al., GCN 12698) triggered Konus-Wind at T0=72682.720s UT (20:28:02.720) The light curve shows multiple partly overlapping pulses with the brightest peak at ~T0+12s. A total duration of the burst is ~75 s. The emission is seen up to ~8 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB111215_T73682/ As observed by Konus-Wind the burst had a fluence of 5.3(-1.1,+1.1)x10-5 erg/cm2, and a 256-ms peak flux, measured from T0+11.776 s, of 6.1(-0.6,+0.6)x10-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+72.192 s) is best fitted in the 20 keV - 10 MeV range with the GRB (Band) model, for which: the low-energy photon index alpha = -1.18 (-0.12, +0.18), the high energy photon index beta = -2.3 (-0.6, +0.2), the peak energy Ep = 250(-60, +65) keV, chi2 = 88.2/88 dof. The spectrum at the maximum count rate (measured from T0+7.680 to T0+14.848 s) is best fitted in the 20 keV - 10 MeV range by a power law with exponential cutoff model, for which alpha = -1.03 (-0.10, +0.11), and Ep = 413(-57, +75) keV, chi2 = 101.9/89 dof. Fitting this spectrum by the GRB (Band) function yields the same alpha and Ep with a high energy photon index beta < -2.6 (chi2 = 101.9/88 dof). All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12702 SUBJECT: GRB 111215B: Swift/UVOT Upper Limits DATE: 11/12/17 16:33:03 GMT FROM: Samantha Oates at MSSL S. R .Oates (MSSL-UCL) and C. J. Saxton (MSSL-UCL) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of the IPN-detected burst: GRB 111215B, 31.5 hrs after the IPN trigger (Hurley et al. et al. GCN Circ. 12698) No optical afterglow consistent with the XRT position (Littlejohns et al. et al. GCN Circ. 12700) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag u 113,256 130,435 4889 >21.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12705 SUBJECT: GRB 111215B: Suzaku WAM observation of the prompt emission DATE: 11/12/20 06:18:49 GMT FROM: Makoto Tashiro at Saitama U/Swift W. Iwakiri, M. Tashiro, Y. Terada, T. Yasuda, K. Takahara, M. Asahina, S. Kobayashi, A. Sakamoto (Saitama U.) Y. Hanabata, T. Uehara, T. Kawano, K. Takaki, M. Mizuno, M. Ohno, Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa (Waseda U.), N. Ohmori, M. Akiyama, M. Yamauchi (Univ. of Miyazaki), C-J. Chuang, Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), The long bright GRB 111215B (localized by IPN: Hurley et al., GCN 12698) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 20:28:05.704 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-0.5 s, followed by a long weak tail seen up to T0+75 s with a duration (T90) of about 61 seconds. The fluence in 100 - 1000 keV was 2.81(-0.06, +0.09) x 10^-5 erg/cm^2. The 1-s peak flux measured from T0+13 s was 8.68 (-0.52, +0.36) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-0.5 s to T0+74.5 s is well fitted by a single power-law with a photon index of 2.05 (-0.06, +0.07) (chi^2 / d.o.f = 19.7/25). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst will be available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html