//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8817 SUBJECT: GRB 090117 - SuperAGILE Localization of a long GRB DATE: 09/01/17 17:35:37 GMT FROM: Marco Feroci at IASF/INAF I. Donnarumma, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda (INAF/IASF Rome), A. Giuliani, S. Vercellone, A. Chen, S. Mereghetti, A. Pellizzoni, F. Perotti, P. Caraveo (INAF/IASF Milan), A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Marisaldi, M. Galli, (INAF/IASF Bologna), M. Tavani, G. Pucella, F. D'Ammando, V. Vittorini, A. Argan, A. Trois, G. Piano, S. Sabatini (INAF/IASF Rome), G. Barbiellini, F. Longo, E. Moretti (INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2), M. Prest, E. Vallazza (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), and P. Giommi, C. Pittori, B. Preger, P. Santolamazza, F. Verrecchia (ASDC) and L. Salotti (ASI), on behalf of the AGILE Team, report: "SuperAGILE detected a gamma ray burst on 17 January 2009, at 15:21:54 UT. The event had a duration of about 10.0 s in the 20-60 keV energy range, with a precursor followed by the main peak. Assuming a crab-like energy spectrum, the peak flux on 1-s timescale was about 2.7E-07 erg/cm2/s. The burst position was reconstructed as (RA, Dec) (164.003 deg, -58.249 deg), which is: RA(J2000) = 10h 56m 00.75s Dec(J2000) = -58d 14' 57.84" with an uncertainty of 3' radius. The given uncertainty accounts for both the statistical and systematic errors. An analysis of the AGILE Gamma Ray Imager (GRID) data is in progress." This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8818 SUBJECT: GRB090117: Swift-XRT detection of a possible candidate afterglow DATE: 09/01/18 00:04:10 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team : The Swift-XRT began observing the field of the SuperAGILE GRB 090117 at 2009-01-17 19:10:13 UT, 13.7 ks after the burst. In a 1.9 ks Photon Counting mode X-ray image covering the 0.3-10 keV band, we detect an uncatalogued source within the SuperAGILE error circle at the astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue) of RA, Dec = 164.0444, -58.2336 which is equivalent to: RA (J2000): 10 56 10.66 Dec (J2000): -58 14 00.8 with an uncertainty of 2.4 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. The position enhancement is described by Goad et al. (2007, A&A, 476, 1401 http://www.swift.ac.uk/xrt_positions/Goad.pdf), the current algorithm is an extension of this method. At this stage we cannot tell if the source is fading to confirm that it is the X-ray counterpart of the SuperAGILE burst. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8819 SUBJECT: GRB090117 Swift/UVOT upper limits DATE: 09/01/18 03:23:36 GMT FROM: Patricia Schady at MSSL/Swift P. Schady (MSSL-UCL) reports on behalf of the Swift/UVOT team: The Swift/UVOT began observing the field of SuperAGILE GRB 090117 (Donnarumma et al., GCN 8817) at 2009-01-017 19:10:14 UT, 13.7 ks after the burst. We do not detect any source at the Swift XRT position (Beardmore et al., GCN 8818), although we note that there is a bright star with v-band magnitude v = 17.7 that lies within the XRT error circle. The UVOT 3-sigma upper limits are reported below: Filter T_start Exp(s) Mag (3-sigma upper limit) ------------------------------------------------------------- white 14.4 455 > 17.18 v 15.1 595 > 16.18 b 13.8 627 > 17.08 u 13.7 63 > 17.27 ------------------------------------------------------------- The quoted upper limits have not been corrected for the expected Galactic extinction along the line of sight of E_(B-V) = 1.63 mag. All photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8820 SUBJECT: GRB 090117: GROND Upper Limits DATE: 09/01/18 04:13:15 GMT FROM: Andrea Rossi at TLS Tautenburg A. Rossi (Tautenburg Obs.), F. Olivares (MPE Garching), A. Kupcu Yoldas (ESO), J. Greiner, and A. Yoldas (both MPE Garching) report on behalf of the GROND team: We observed the field of GRB 090117 (SuperAGILE trigger, Donnarumma et al. GCN #8817) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPI/ESO telescope at La Silla (Chile). Observations started at 01:40 UT, about 9 hrs after the GRB. We do not detect any new sources within the 5-sigma Swift/XRT error circle (Breadmore & Evans, GCN #8818). Note that there is a R~16 magnitude star within the XRT position contaminating the search for the GRB afterglow. Co-added images of the first 8 minutes yield the following specific limits (in AB magnitudes): g' > 23.7 r' > 24.1 i' > 23.2 z' > 22.2 J > 21.9 H > 20.9 K > 20.3 The magnitudes are calibrated against the GROND zeropoints and 2MASS field stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8821 SUBJECT: GRB 090117 - Fermi GBM Observations DATE: 09/01/18 05:58:26 GMT FROM: Valerie Connaughton at MSFC Valerie Connaughton (UAH) reports on behalf of the Fermi GBM Team: "At 15:22:01.05 UT on 17 Jan 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090117 (trigger 253898523 / 090117640) which was also detected by SuperAGILE (Donnarumma et al. 2009, GCN 8817). The GBM on-ground location is consistent with the reported position from SuperAGILE. The angle from the Fermi LAT boresight is 51 degrees. The GBM light curve shows a soft event with a single peak lasting about 2 seconds superimposed on a lower-level continuum. The burst duration (T90) is about 21 s (8-1000 keV). The time-averaged spectrum from T0-5 s to T0+4 s is best fit by a Band function with Epeak = 25 +/- 2 keV, alpha = -0.4 +/- 0.5, and beta = -2.5 +/- 0.1 The event fluence (8-1000 keV) in this time interval is (1.8 +/- 1.3)E-6 erg/cm^2, with a 1 sec peak flux starting at T0 of 9.6 +/- 4.2 ph/cm^2/s and a 0.256 sec peak flux starting at T0+0.256 sec of 18.6 +/- 8.0 ph/cm^2/s. In view of the soft spectrum and the position of the burster close to the Galactic plane, other spectral forms were investigated that are more typical of galactic transient sources. Of these, the best fit was obtained using a thermal Bremmstrahlung model with kT = 49. The Band GRB function was preferred statistically with delta chi2 = -5 for 1 extra parameter. It is likely, therefore, that this is a soft GRB rather than a new galactic transient. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8822 SUBJECT: GRB 090117C - Fermi GRB Detection DATE: 09/01/18 06:15:23 GMT FROM: Valerie Connaughton at MSFC Valerie Connaughton (UAH) reports on behalf of the Fermi GBM Team: "At 15:10:40.18 UT on 17 Jan 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090117C (trigger 253897842 / 090117632). The on-ground calculated location, using the GBM trigger data, is RA = 117.6, DEC = -40.3 (J2000 degrees, equivalent to 07h 50m, -40d 18'), with an uncertainty of 1.8 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 54 degrees. The GBM light curve consists of a precursor lasting tens of seconds until trigger time, followed by a single episode with substructure lasting a further 35 s. The total duration (T90) between 8 and 1000 keV is about 86 s. The time-averaged spectrum of the main emission from T0-2 s to T0+29 s is best fit by a Band function with Epeak = 247 +/- 41 keV, alpha = -1.0 +/- 0.1, and beta = -2.1 +/- 0.2, giving an 8-1000 keV fluence of (1.1 +/- 0.1) E-5 erg/cm^2. The precursor spectrum from T0-55 sec to T0-6 s is best fit using a power law function with an exponential high energy cutoff. The power law index is -1.3 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 147 +/- 38 keV. The 8-1000 keV fluence of the precursor is (3.9 +/- 0.5) E-6 erg/cm^2. A 1-sec peak photon flux of 4.2 +/- 0.7 ph/s/cm^2 in the 8-1000 keV band is measured starting at T0+22.5 s. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8823 SUBJECT: GRB 090117: confirmation of the X-ray afterglow DATE: 09/01/18 07:55:36 GMT FROM: Kim Page at U.of Leicester K.L. Page & A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team: Following the collection of further XRT data, we see that the source found by Beardmore & Evans (GCN Circ. 8818) is fading, so confirm it as the X-ray afterglow of GRB 090117 (Donnarumma et al., GCN Circ. 8817; Connaughton, GCN Circ. 8821). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8824 SUBJECT: GRB 090117B : Fermi GBM detection DATE: 09/01/18 12:31:04 GMT FROM: Andreas von Kienlin at MPE Andreas von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 08:02:02.23 UT on 17 January 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090117B (trigger 253872124 / 090117335) The on-ground calculated location, using the GBM trigger data, is RA = 232.9, DEC = 27.6 (J2000 degrees, equivalent to 15h 32m, 27d 36'), with an uncertainty of 9.4 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 49 degrees The GBM light curve consists of two separate peaks, the first from T0-0.768 to T0+0.768 sec and the second from T0+24.0643 sec to T0+26.368 sec. T90 (8-1000 keV) is about 27 sec. Both peaks were fit using a power-law function with index -1.55 +/- 0.08 (chi squared 272.27/245 d.o.f.) for the first and with index -1.55 +/- 0.07 (chi squared 249.72/245 d.o.f.)for the second peak. The event fluence (8-1000 keV) for both peaks is (2.1 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.768 s in the 8-1000 keV band is 4.6 +/- 0.2 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: 8836 SUBJECT: GRB 090117C: Suzaku WAM observation of the prompt emission DATE: 09/01/22 12:37:45 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.), N. Vasquez (Tokyo Tech.), on behalf of the Suzaku WAM team, report: The long GRB 090117C (Connaughton et al., GCN8822) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2009-01-17 15:10:40 UT (=T0). The observed light curve shows relatively strong emission from T0-6 s to T0+32 s with a precursor of about 1 min. long. The duration (T90) including the precursor is about 91 seconds. The fluence in 100 - 1000 keV was (1.18 +/- 0.11) x 10^-5 erg/cm^2. The 1-s peak flux measured from T0+22 s was 1.2 (+/-0.3) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-78 s to T0+32 s is fitted by a single power-law with a photon index of 1.72 +/- 0.18 (chi^2/d.o.f = 14/12). 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 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8954 SUBJECT: Radio observation of GRB 090117 with ATCA DATE: 09/03/09 06:29:00 GMT FROM: Aquib Moin at CIRA/ATNF Aquib Moin (Curtin Institute of Radio Astronomy / Australia Telescope National Facility), Steven Tingay (Curtin Institute of Radio Astronomy), Chris Phillips (Australia Telescope National Facility), Gregory Taylor (University of New Mexico), Mark Wieringa (Australia Telescope National Facility) and Ralph Martin (Perth Observatory) report: We observed the SuperAGILE-GRID position of the GRB090117 (GCN 8817) at 4.800 and 4.928 GHz with the Australia Telescope Compact Array (ATCA) between 01:00:00 UT and 22:00:00 UT on February 21/22, 2009. We did not detect a radio source at the position of the GRB090117 (GCN 8817). The data at 4.800 and 4.928 GHz were merged and the radio flux density at the GRB position found out to be -0.0109 +/- 0.189 mJy/beam (1-sigma). The Australia Telescope Compact Array (/ Parkes telescope / Mopra telescope / Long Baseline Array) is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. See the 4.800 & 4.928 GHz combined image at: http://cira.ivec.org/dokuwiki/doku.php/grb/grb090117/grb090117_field_image