//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7978 SUBJECT: GRB 080714: Swift detection of a burst DATE: 08/07/14 18:11:28 GMT FROM: David Palmer at LANL M. Perri (ASDC), S. D. Barthelmy (GSFC), J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (INAF-IASFPA), F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester), D. M. Palmer (LANL), D. Perez (U Leicester), B. Preger (ASDC), P. Schady (MSSL-UCL), M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester), G. Stratta (ASDC), M. C. Stroh (PSU), D. E. Vanden Berk (PSU) and L. Vetere (PSU) report on behalf of the Swift Team: At 17:52:56 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 080714 (trigger=316910). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 188.109, -60.279 which is RA(J2000) = 12h 32m 26s Dec(J2000) = -60d 16' 42" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 40 sec. The peak count rate was ~5000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 17:54:16.4 UT, 79.7 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 188.10733, -60.27708 which is equivalent to: RA(J2000) = 12h 32m 25.76s Dec(J2000) = -60d 16' 37.5" with an uncertainty of 3.1 arcseconds (radius, 90% containment). This location is 7.5 arcseconds from the BAT onboard position, within the BAT error circle. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 5.44e+21 cm^-2 (Kalberla et al. 2005). The initial flux in the 2.5 s image was 5.01e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm) filter starting 89 seconds after the BAT trigger. No afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. Because of the density of catalogued stars, further analysis is required to report an upper limit for any afterglow in the sub-image. No correction has been made for the large, but uncertain extinction expected. Burst Advocate for this burst is M. Perri (perri AT asdc.asi.it). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7979 SUBJECT: GRB 080714: Swift-BAT refined analysis DATE: 08/07/15 02:59:58 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), M. Perri (ASDC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU) on behalf of the Swift-BAT team: Using the data set from T-240 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 080714 (trigger #316910) (Perri, et al., GCN Circ. 7978). The BAT ground-calculated position is RA, Dec = 188.104, -60.274 deg which is RA(J2000) = 12h 32m 24.9s Dec(J2000) = -60d 16' 28.2" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 43%. The mask-weighted lightcurve shows a single peak with a rise time of about 3 seconds and an exponential decay with a time constant of about 10 seconds. T90 (15-350 keV) is 33 +- 9 sec (estimated error including systematics). There is a small peak in the raw light curve, mostly above 25 keV, at about T-90 sec that appears to be from a different source, out of the field of view. The time-averaged spectrum from T-3.6 to T+50.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.52 +- 0.08. The fluence in the 15-150 keV band is 2.5 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T-0.37 sec in the 15-150 keV band is 4.2 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/316910/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7980 SUBJECT: GRB 080714: Enhanced Swift-XRT position DATE: 08/07/15 06:31:13 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 4736 s of XRT Photon Counting mode data and 4 UVOT images for GRB 080714, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 188.10601, -60.27775 which is equivalent to: RA (J2000): 12h 32m 25.44s Dec (J2000): -60d 16' 39.9" with an uncertainty of 2.3 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. 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. This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7981 SUBJECT: GRB 080714: Swift-XRT refined analysis DATE: 08/07/15 14:04:07 GMT FROM: Giulia Stratta at ASDC G. Stratta, M. Perri, B. Preger (ASDC) report on behalf of the Swift-XRT team: We analysed the first 3 orbits of XRT data for GRB 080714 (Perri et al., GCN Circ. 7978) taken from 88s after the trigger (T0) in Windowed Timing (WT) mode and then in Photon Counting (PC) mode from T0+233 s to T0+9874 s. The UVOT-enhanced XRT position was given by Goad et al. (GCN Circ. 7980). The X-ray light curve from T0+88s up to ~T0+300s shows an initial 40 seconds long flat segment followed by an increasingly steepening decay. Starting from T0+300s (PC data) the light curve can be fit with a power law model with a best fit slope of 1.0+/-0.1. The WT data spectrum from T0+88s to T0+231s is well fitted by an absorbed power law model with photon index Gamma=1.14+/-0.05 and a total equivalent hydrogen column density of NH=(0.3+/-0.1)e22 cm**-2. The Galactic NH is 5.44e21 cm**-2 (Kalberla et al. 2005). The 0.3-10 keV observed (unabsorbed) flux is (3.4+/-0.2)e-10 erg/cm**2/s ((3.9+/-0.2)e-10 erg/cm**2/s). If the light-curve continues to decay with the same rate, the count rate 24 hours after the trigger is estimated to be ~6e-3 counts/s, which corresponds to an observed flux of ~5e-13 erg/cm**2/s. This is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7982 SUBJECT: GRB 080714: Swift/UVOT Detection of an Optical Afterglow DATE: 08/07/15 16:06:40 GMT FROM: Frank Marshall at GSFC F.E. Marshall (NASA/GSFC) and M. Perri (ASDC) report on behalf of the Swift/UVOT team: The Swift/UVOT observed the field of GRB 080714 starting 90 s after the BAT trigger (Perri et al., GCN Circ. 7978). The burst is in a crowded field only 2.5 degrees from the Galactic Plane. We find a fading source inside the enhanced XRT error circle (Goad et al., GCN Circ. 7980) in observations with the White and V filters. The preliminary position for the afterglow is: RA(J2000) = 12:32:25.44 = 188.1060 DEC(J2000) = -60:16:40.4 = -60.2779 with a 90% confidence error radius of about 0.8 arcsec. The measured magnitudes in the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) and 3-sigma upper limits for detecting a source in the first two finding chart (FC) exposures and subsequent co-added exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white (FC) 90 189 98 20.2 +/- 0.2 white 4290 4489 197 >20.7 v (FC) 197 596 393 19.1 +/- 0.2 v 5896 6095 197 >19.7 b 677 4284 206 >20.2 u 652 12382 1137 >20.7 uvw1 628 6505 236 >19.7 uvm2 602 6300 236 >19.9 uvw2 707 16498 1007 >20.8 The values quoted above are not corrected for the predicted large, but uncertain, Galactic extinction the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7983 SUBJECT: Konus-Wind observation of GRB 080714 DATE: 08/07/15 18:22:34 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team report: The long GRB 080714 (Swift-BAT trigger #316910: Perri et al., GCN 7978, Barthelmy et al., GCN 7979) triggered Konus-Wind at T0=64378.478 s UT (17:52:58.478). The burst light curve shows a single pulse with a duration of ~20s. As observed by Konus-Wind the burst had a fluence of 3.64(-0.60, +0.87)x10^-6 erg/cm2, and a 256-ms peak flux measured from T0+0.544 s of 6.84(-1.79, +2.01)x10^-7 erg/cm2/s (both in the 20 keV - 1 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+16.640 s) is well fitted (in the 20 keV-1 MeV range) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.24(-0.39, +0.46) and Ep = 137(-34, +100) keV (chi2 = 48.3/52 dof). All the quoted errors are at the 90% confidence level. The Konus-Wind light curve of this GRB is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080714_T64378/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 7984 SUBJECT: GRB 080714: GROND confirmation of the optical/NIR afterglow DATE: 08/07/16 06:43:03 GMT FROM: Thomas Kruehler at MPE/MPI T. Kruehler, J. Greiner, C. Clemens, A. Yoldas (all MPE Garching), A. Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest) report on behalf of the GROND team: We observed the field of GRB 080714 (Swift trigger 316910; M. Perri et al., GCN #7978) in two epochs, simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m ESO/MPI telescope at La Silla Observatory (Chile). We detect the optical afterglow reported by Marshall & Perri (GCN #7982) at RA (J2000.0) = 13h 32m 25.49s DEC (J2000.0) = -60d 16' 39.3" with an absolute uncertainty of 0.6". Preliminary photometry yields the following magnitudes against USNO-B1 and 2MASS field stars in stacked images: Band T_mid(h) Exp(min) Mag g' 6.4058 50 > 24.3 g' 30.3847 32 > 23.4 r' 6.4058 50 22.76 +- 0.08 r' 30.3847 32 > 23.6 i' 6.4058 50 21.15 +- 0.07 i' 30.3847 32 22.68 +- 0.24 z' 6.4058 50 20.39 +- 0.06 z' 30.3847 32 21.82 +- 0.29 J 6.2827 40 18.58 +- 0.11 J 30.2958 30 20.00 +- 0.16 H 6.2827 40 17.25 +- 0.14 H 30.2958 30 18.52 +- 0.24 not corrected for the expected Galactic foreground reddening of around E(B-V) = 1.15 mag (Schlegel et al., 1998). Given the high foreground extinction, the non detection in g' is consistent with the powerlaw slope of the broad band SED derived from r to H and does not necessarily imply a high redshift. Additionally, we note the presence of a nearby, faint (r'~ 24.1 +- 0.2) source at RA (J2000.0) = 13h 32m 25.60s DEC (J2000.0) = -60d 16' 37.7" roughly 1.8" away from the afterglow, which may influence the photometry in the second epoch.