//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17131 SUBJECT: IPN Triangulation of GRB 141202A (short/hard) DATE: 14/12/03 12:02:29 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team, V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM 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. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, report: The short-duration, hard-spectrum GRB 141202A has been observed by Fermi (GBM trigger 439211828), MESSENGER (GRNS), INTEGRAL (SPI-ACS), Konus-Wind, and Swift (BAT), so far, at about 40626 s UT (11:17:06). This burst occurred just after Swift started a preplanned slew maneuver. There are no BAT event data covering the burst interval, but from the energy response of the quadrant rates, it appears that the source was partially coded in BAT. We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 143.073 (09h 32m 17s) +54.161 (+54d 09' 38") Corners: 142.732 (09h 30m 56s) +52.555 (+52d 33' 17") 143.092 (09h 32m 22s) +53.247 (+53d 14' 51") 143.397 (09h 33m 35s) +55.706 (+55d 42' 22") 143.039 (09h 32m 09s) +55.054 (+55d 03' 15") --------------------------------------------- The error box area is 1439 sq. arcmin, and its maximum dimension is 3.2 deg (the minimum one is 10 arcmin). The Sun distance was 117 deg. This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB141202_T40626/IPN/ The time history and spectrum will be given in forthcoming GCN Circulars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17132 SUBJECT: GRB 141202A Tiled Swift observations DATE: 14/12/03 13:24:03 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the IPN GRB 141202A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00033 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the IPN event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17133 SUBJECT: GRB 141202A: Fermi GBM Detection DATE: 14/12/03 13:53:27 GMT FROM: Oliver Roberts at UCD/Fermi O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team: "At 11:17:05.61 UT on the 2nd of December 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 141202A (trigger 439211828 / 141202470 ). The GBM on-ground location, using the Fermi GBM trigger data, is RA = 145.0, Dec =+59.9, with an uncertainty of 3.3 degrees (radius, 1-sigma containment,statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The GBM location is consistent with the IPN Triangulation (Golenetskii et al. 2014, GCN 17131). The angle from the Fermi LAT boresight is about 78 degrees. The GBM light curve consists of a single peak with a duration (T90) of about 1.3 s (50-300 keV). The time-averaged spectrum from T0+0.0 s to T0+1.3 s is adequately fit by a power law function with an exponential high-energy cutoff. The power law index is -0.11 +/- 0.08 and the cutoff energy, parameterized as Epeak, is 596 +/- 40 keV. The event fluence (10-1000 keV) in this time interval is (4.2 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.1 s in the 10-1000 keV band is 8.4 +/- 0.3 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: 17134 SUBJECT: GRB 141202A: Swift XRT observations DATE: 14/12/04 13:27:51 GMT FROM: Claudio Pagani at U of Leicester C. Pagani and P. A. Evans (U. Leicester) report on behalf of the Swift team: Swift-XRT has observed the error box of the IPN GRB 141202A (Golenetskii et al., GCN Circ. 17131) in a series of observations tiled on the sky. The total exposure time is 12.3 ks spread over 7 fields; the maximum exposure within the sky observed was 2.7 ks. The observations started 93.5 ks after the IPN trigger and extended over ~50.8 ks. Within these data no credible X-ray afterglow is detected. The 3-sigma upper limit is 5.2E-03 cts s^-1 (0.3-10 keV). The automated analysis of the XRT data detects three X-ray sources that are classified as possible afterglow candidates, but inspection of the data shows these to be artifacts due to contamination by the bright Earth. The automated analysis is reported online at http://www.swift.ac.uk/xrt_products/TILED_GRB00033 This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17136 SUBJECT: Konus-Wind observation of GRB 141202A DATE: 14/12/04 18:01:42 GMT FROM: Anastasia Tsvetkova at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The short-duration, hard-spectrum GRB 141202A (IPN triangulation: Golenetskii et al., GCN 17131; Fermi GBM detection: Roberts, GCN 17133) triggered Konus-Wind at T0=40626.305 s UT (11:17:06.305). The burst light curve shows a single pulse with a duration of ~1.4 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of 4.44(-1.02,+1.47)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0+0.624 s, of 7.37(-2.00,+2.67)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+8.448 s) is best fit 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 = -0.49(-0.35,+0.47), and Ep = 538(-150,+274) keV (chi2 = 77/84 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.0 (chi2 = 77/83 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB141202_T40626/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17139 SUBJECT: GRB 141202A: Swift/UVOT Detection of a Variable Source Near the IPN Error Box DATE: 14/12/05 15:43:31 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) and S. B. Cenko (NASA/GSFC) report on behalf of the Swift/UVOT team: The short/hard GRB 141202A was localized to a 1439 sq. arcmin error box with the IPN (Golenetskii et al. GCN Circ. 17131), and Swift tiled the error box with 7 fields starting 93.5 ks after the trigger. No credible afterglow was detected with the Swift/XRT (Pagani et al. GCN Circ. 17134). In two exposures with the U filter starting 128 ks after the trigger, Swift/UVOT finds a bright source just outside the IPN error region that is not seen in the DSS or the SDSS. In addition, no source at this position was found with the Minor Planet Checker. There is a dim SDSS galaxy with a g' magnitude (AB) of 23.0 +/- 0.2 coincident with the UVOT source. A 3-sigma upper limit for this galaxy in the u' band is 22.4 mag. The preliminary UVOT position is: RA (J2000) = 09:32:29.78 = 143.12408 (deg.) Dec (J2000) = 55:19:44.4 = 55.32899 (deg.) with an estimated uncertainty of 0.5 arcsec. (radius, 90% confidence). There is very marginal evidence (1.8-sigma) for variability between the two UVOT observations. The preliminary AB magnitudes using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is: Filter T_start(ks) T_stop(ks) Exp(ks) Mag (AB) u 127.9 128.6 0.69 20.43 +/- 0.09 u 129.4 130.3 0.88 20.69 +/- 0.13 No correction is made for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the source (Schlegel et al. 1998). The 3-sigma upper limit for the XRT count rate at the position of the UVOT source is 9.6e-3 counts/s in the 0.3-10 keV band. It would be very unusual for UVOT to find a bright optical afterglow for a short/hard GRB so long after the trigger, especially since XRT did not find an afterglow. The long-term increase in the optical flux by a factor of at least 6 indicates that this may nevertheless be an interesting object. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17153 SUBJECT: GRB141202A: Discovery Channel Telescope Optical Observations DATE: 14/12/09 04:09:42 GMT FROM: John Capone at UMD J. Capone (UMD), V. Toy (UMD), A. Cucchiara (NASA-GSFC), S.B. Cenko (NASA-GSFC), E. Troja (NASA-GSFC), A. Kutyrev (NASA-GSFC), and S. Veilleux (UMD) report on behalf of a larger collaboration: We observed the field of the variable source reported by Marshall and Cenko (GCN 17139) with the Large Monolithic Imager (LMI) on the 4.3m Discovery Channel Telescope (DCT) at Happy Jack, AZ from 2014/12/07 11:01 until 2014/12/07 11:08 UTC (starting 119.74 hours after the observations reported by Golenetskii et al. in GCN 17131). A source is clearly detected at the location of the source identified by UVOT in u', g', r', i' and z'. Using nearby point sources from SDSS for calibration we measure r' = 20.57 +/- 0.03. The coincident SDSS R10 source has r' = 22.65 +/- 0.20, confirming that the source is indeed transient. At 0.8 arcsecond seeing, the source is unresolved. This magnitude is reported in AB magnitude and is not corrected for Galactic extinction in the direction of the source. Further observations are planned to investigate possible variability of this source. We thank the staff of the Discovery Channel Telescope for assistance with these observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17192 SUBJECT: GRB 141202A: Suzaku WAM observation of the prompt emission DATE: 14/12/19 04:36:16 GMT FROM: Makoto Tashiro at Saitama U/Swift J. Enomoto, M. Tashiro, Y. Terada, T. Yasuda, S. Koyama, S. Takeda, S. Nakaya, T. Fujinuma, S. Matsuoka (Saitama U.), M. Yamauchi, N. Ohmori, R. Kinoshita (Univ. of Miyazaki), W. Iwakiri (RIKEN), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.),Y. Hanabata (ICRR), M. Ohno, T. Kawano, S. Furui, Y. Fukazawa (Hiroshima U.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report: The short and IPN localized GRB 141202A (IPN localization: S. Golenetskii et al., GCN 17131; Fermi GBM Detection: O.J. Roberts et al., GCN 17133; Konus-Wind observation: S. Golenetskii et al., GCN 17136) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 11:17:5.508 UT (=T0). The observed light curve shows a multi-peaked structure lasting from T0s to T0+2s, followed by a weaker emission seen with a duration (T90) of about 1.8 seconds. The fluence in 100 - 1000 keV was 4.48 (-0.18, +0.10) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+0.5s was 7.61 (-2.44, -0.11) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0 s to T0+2 s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 0.28 (-0.56, +0.48), and Epeak 565 (-66, +96) keV (chi^2/d.o.f. = 24.5/25). 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