//////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4533 SUBJECT: GRB 060117: Swift-BAT detection of a bright burst DATE: 06/01/17 07:22:11 GMT FROM: Scott Barthelmy at NASA/GSFC S. Campana (INAF-OAB), S. Barthelmy (GSFC), N. Gehrels (GSFC), C. Gronwall (PSU), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. Page (U Leicester), D. Palmer (LANL), M. Perri (ASDC) on behalf of the Swift team: At 06:50:01 UT, Swift-BAT triggered and located GRB 060117 (trigger=177666). The spacecraft did not slew because of the Sun observing constraint. It will come out of the Swift observing constraint on 07 Feb 2006. The BAT on-board calculated location is RA,Dec 327.926d,-59.980d {21h 51m 42s,-59d 58' 49"} (J2000), with an uncertainty of 3 arcmin (radius, 90% containment, stat+sys). The BAT light curve shows a bright multi-peak structure with a total duration of ~25 sec. The peak count rate was ~40,000 counts/sec (15-350 keV), at ~12 seconds after the trigger. We note that this is within 3 arcmin of the bright (J=13.0 mag) galaxy IRAS 21482-6015. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4534 SUBJECT: GRB 060117: nearby galaxy DATE: 06/01/17 07:39:54 GMT FROM: Nial Tanvir at IofA U.Cambridge N.R. Tanvir (U. Hertfordshire) notes: The galaxy that is within 2.7 arcmin of the BAT position of GRB 060117 (GCN 4533) is at redshift z=0.042, and there are other galaxies visible on DSS2 in the same field, which could well be at similar redshift. Given the high luminosity of this burst, it is therefore a candidate to be at low-redshift, and followup observations are encouraged, despite the poor location on the sky. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4535 SUBJECT: GRB 060117: FRAM optical afterglow candidate DATE: 06/01/17 09:41:08 GMT FROM: Martin Jelinek at Inst.Astrophys.Andalucia,Granada Petr Kubanek, (ASU Ondrejov, Czech Rep. and ISDC Versoix, Switzerland) Martin Jelinek (IAA Greanada, Spain), Michael Prouza (FZU Praha, Czech Rep., Martin Nekola and Rene Hudec (ASU Ondrejov, Czech Rep.) Report: The wide field camera of the telescope FRAM located at Pierre Auger observatory in Malargue, Argentina, observed the field of Swift trigger 177666 (Cmpana et al., GCN 4533) starting 123s after the GRB (10s after GCN). We detect an optical source at coordinates: 21:51:36.1 -59:58:58 (J2000) The object faded during few exposures from the reach of the telescope. Note that this object is within few arcseconds from the galaxy LEDA 128172. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4536 SUBJECT: GRB 060117: FRAM refined analysis DATE: 06/01/17 10:50:00 GMT FROM: Martin Jelinek at Inst.Astrophys.Andalucia,Granada Martin Jelinek (IAA Greanada, Spain), Petr Kubanek, (ASU Ondrejov, Czech Rep. and ISDC Versoix, Switzerland) Michael Prouza (FZU Praha, Czech Rep., Martin Nekola and Rene Hudec (ASU Ondrejov, Czech Rep.) Report: The observation of the GRB060117 (GCN 4533, 4534, 4535) started with a 10s R-band exposure at 06:52:05.4 UT, i.e. 124s after the GRB. The afterglow magnitude is 11.5+/-0.3 (calibration noise) and faded by 1.4mag during the first 120s of observation. The optical candidate is at a refined position: 21:51:36.13 -59:58:39.1 +/-1.5" (J2000) We note that the originally reported position was wrong by 20" in declination. [GCN OPS NOTE(07apr10): As pointed out by F.Marshall, the missing minus sign on the declination was added.] //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4538 SUBJECT: GRB 060117: Refined analysis of the Swift-BAT burst DATE: 06/01/17 19:16:15 GMT FROM: Hans Krimm at NASA-GSFC J. Cummings (GSFC/NRC), L. Barbier (GSFC), S. Barthelmy (GSFC) E. Fenimore (LANL), N. Gehrels (GSFC), K. Gendreau (GSFC), D. Hullinger (GSFC/UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), P. Meszaros (PSU), J. Norris (GSFC), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS), J. Tueller (GSFC) on behalf of the Swift-BAT team: Using the data set from T-60 to T+120 sec from the recent telemetry downlink, we report further analysis of BAT GRB 060117 (trigger #177666) (Campana, et al., GCN 4533). The BAT ground-calculated position is RA,Dec = 327.917, -59.967 {21h 51m 40s, -59d 58' 1"} (J2000) +- 1.0 arcmin, (radius, sys+stat, 90% containment). This position includes a small correction for small BAT image distortions. We note that this error circle formally excludes the position of IRAS 21482-6015 (GCN 4533, GCN4534). We also note that fading afterglow discovered by the FRAM telescope group (Jelinek et al, GCN 4536) is 0.8 arc min from the center of the BAT 90% error circle. The partial coding was 25%. The light curve has multiple peaks, with the main peaks spanning the time range T-1 to T+17. T90 (15-350 keV) is (16 +- 1) sec (estimated error including systematics). There does appear to be weak emission extending out to T+100 seconds. The best fit to the spectral data for the time averaged period from T-1.98 to T+26.99 seconds is a power law with an exponential cutoff. This fit gives a photon index 1.51 +- 0.13, and Epeak of 71 +- 5 keV (chi squared 40 for 59 d.o.f). For this model the total fluence in the 15-150 keV band is (2.04 +- 0.04) x 10^-05 erg/cm2 and the 1-sec peak flux measured from T+11.12 sec is 48.9 +- 1.6 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.93 +- 0.03 (chi square 68 for 59 d.o.f.) All the quoted errors are at the 90% confidence level. Using the lag-luminosity method of Norris et al. (2000), and a lag measurement of 25 ms +- 5 ms (1 sigma; 100-350 keV to 25-50 keV bands), yields a pseudo-redshift of z ~ 1.3 +- 0.3 (includes spectral uncertainties). The remainder of the expected event data for this burst (from T-300 to T-60 sec and from T+120 to T+300) has not yet been received on the ground. If we see evidence for emission after T+120 sec in these data, we will issue another circular. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4542 SUBJECT: Konus-Wind observation of GRB 060117 DATE: 06/01/18 16:24:43 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and T. Cline on behalf of the Konus-Wind team report: The long soft GRB 060117 (Swift-BAT trigger #177666; Campana et al., GCN 4533; Cummings et al., GCN 4538) triggered Konus-Wind at T0=24597.852 s UT (06:49:57.852). The Konus-Wind light curve shows multiple peaks with a total duration of ~20 sec. As observed by Konus-Wind the burst had a fluence of (2.97+/-0.13)x10^-5 erg/cm2 and peak flux measured from T+11.12 on 16 msec time scale (1.28+/-0.18)x10^-5 erg/cm2/sec (both in the 20 keV - 1 MeV energy range). The time-integrated spectrum of the GRB (from T0 to T0+21.504 sec) is well fitted (in the 20 keV - 1 MeV range) by GRBM (Band) model for which: the low-energy photon index is alpha = -1.519 (-0.070,+0.082), the high energy photon index beta = -2.91(-0.50, +0.25), the break energy E0 = 184(-30, +34) keV (chi2 = 53/59 dof). The peak energy Ep = 89+/-5 keV. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4544 SUBJECT: GRB 060117: pseudo-z from spectral parameters of the prompt emission DATE: 06/01/18 17:45:03 GMT FROM: Jean-Luc Atteia at Lab d Astrophys.,OMP,Toulouse A. Pelangeon & J-L. Atteia (LATT-OMP) report: We have used the spectral parameters of GRB 060117 provided by Golenetskii et al. (GCNC 4542) to compute the spectral pseudo-redshift of this burst detected by SWIFT-BAT (Campana et al., GCNC 4533; Cummings et al., GCNC 4538). We find a pseudo-redshift pz= 0.45 +/- 0.2 This is significantly lower than the pseudo-redshift computed from the lag-luminosity relation (pz=1.3, GCNC 4538, Cummings et al.). This small pseudo-redshift suggests that the supernova associated with GRB 060117 could be detectable. We encourage observers to follow-up this GRB at various wavelengths to look for the possible emergence of the supernova. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4546 SUBJECT: GRB060117 - ATCA 3/6cm radio limits DATE: 06/01/18 22:43:28 GMT FROM: Brian Schmidt at RSAA, ANU (MSSSO) Brian Schmidt (ANU), Mark Wieringa (ATNF), Dale A. Frail (NRAO), and Alicia Soderberg (CalTech) report on behalf of a larger collaboration "We observed the field of GRB 061117 (GCN 4519) with the Australia Telescope Compact Array at 4.8 and 8.6GHz beginning January 18.4 UT. We detect no sources in a 20" box around the XRT/OT position (GCN 4522,4536) to an approximate 4 sigma limit of 0.6 mJy at both frequencies. " We would like to thank the Director and Staff of the Australia Telescope National Facility for obtaining these observations as part of a Target of Opportunity Program. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4543 SUBJECT: Correction to GCN 4542 on GRB 060117 DATE: 06/01/18 16:54:51 GMT FROM: Valentin Pal'shin at Ioffe Inst V. Pal'shin on behalf of the Konus-Wind team: The time of the measured peak flux quoted in GCN 4542 is wrong. Actually, the peak flux was measured from T0+11.392 sec. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4547 SUBJECT: GRB060117 - ATCA 3/6cm radio limits - correction DATE: 06/01/18 23:06:53 GMT FROM: Brian Schmidt at RSAA, ANU (MSSSO) Brian Schmidt (ANU), Mark Wieringa (ATNF), Dale A. Frail (NRAO), and Alicia Soderberg (CalTech) report on behalf of a larger collaboration "We observed the field of GRB 061117 (GCN 4533, GCN 4538) with the Australia Telescope Compact Array at 4.8 and 8.6GHz beginning January 18.4 UT. We detect no sources in a 20" box around the OT position (GCN 4536) of 21:51:36.13 -59:58:39.1 (J2000) to an approximate 4 sigma limit of 0.6 mJy at both frequencies. " We would like to thank the Director and Staff of the Australia Telescope National Facility for obtaining these observations as part of a Target of Opportunity Program. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4548 SUBJECT: GRB 060117: PROMPT Observations DATE: 06/01/19 17:49:26 GMT FROM: Melissa Nysewander at UNC,Chapel Hill M. Nysewander, A. LaCluyze, D. Reichart, J.A. Crain, A. Foster, K. Ivarson report on behalf of the UNC team of the FUN GRB collaboration: We observed the error region of GRB 060117 (Campana et al., GCN 4533) with four of the PROMPT telescopes simultaneously in Ur'Iz' beginning 18.0 hours after the burst under the automated control of SkyNet at very high airmass. Each exposure is 80 s long; the table below gives details of the observations: Filter Telescope Start (UT) Stop (UT) # Exp Total (hr) U P2 00:47:39 02:17:47 61 1.36 r' P4 00:47:39 02:18:44 63 1.40 I P1 00:47:36 02:13:03 59 1.31 z' P5 00:47:38 02:14:16 61 1.36 We do not see the afterglow reported by Jelinek et al. (GCN 4536) in r'Iz' to r' > 20.2, I > 21.2, and z' > 20.2 (3-sigma). The magnitudes have been calibrated to 5 USNO NOMAD catalogue stars using the transformation equations of Smith et al. 2002. PROMPT is currently being built and commissioned at CTIO. //////////////////////////////////////////////////////////////////////// TITLE: GCN GRB OBSERVATION REPORT NUMBER: 4573 SUBJECT: GRB 060117: Suzaku WAM observation of the prompt emission DATE: 06/01/24 17:45:26 GMT FROM: Kazutaka Yamaoka at Aoyama Gakuin U Y.Terada (RIKEN), K.Yamaoka, S.Sugita (Aoyama Gakuin U.), M.Ohno, T.Takahashi, Y.Fukazawa (Hiroshima U.), K.Abe, Y.Endo, S. Hong, K.Onda, M.Tashiro (Saitama U.), G.Sato, K.Nakazawa, T.Takahashi (ISAS/JAXA), R.Miyawaki, M.Kokubun, K.Makishima (Univ. of Tokyo) and the HXD-II team The bright and long burst, GRB 060117 (Swift-BAT trigger #177666; Campana et al., GCN 4533), triggered the Suzaku Wide-band All-sky Monitor (WAM) which is sensitive to an energy band of 50 keV - 5 MeV at 06:50:00 (UT). The observed light curve shows multi-peak structures with a duration (T90) of 16 seconds. The fluence in 100 - 1000 keV was (1.5 +/- 0.1)X10^-5 erg/cm2. The 1-s peak flux was 9.2 +/- 0.4 photons/cm2/s in the same energy range. Preliminary result shows that the time-averaged spectrum is well fitted by a single power law with a photon index of 2.5 +/- 0.2. All the quoted errors are at statistical 90% confidence level. The WAM in-flight calibration is still under way, and systematic errors, such as the flux calibration uncertainties of about 20%, are not included in the errors. The WAM light curve of this event is available at http://www.astro.isas.ac.jp/suzaku/research/HXD-WAM/WAM-GRB/grb/grb_table.html Further detailed analysis and the refinement are in progress.