//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16520 SUBJECT: GRB 140705A: Swift detection of a short burst DATE: 14/07/05 09:47:43 GMT FROM: Kim Page at U.of Leicester M. Stamatikos (OSU/NASA/GSFC), D. Malesani (DARK/NBI), K. L. Page (U Leicester) and T. Sakamoto (AGU) report on behalf of the Swift Team: At 09:32:48 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 140705A (trigger=603488). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 293.725, +21.899 which is RA(J2000) = 19h 34m 54s Dec(J2000) = +21d 53' 57" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a short spike with a duration of about 0.2 sec. The peak count rate was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 09:33:49.6 UT, 61.0 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 293.7318, 21.8979 which is equivalent to: RA(J2000) = 19h 34m 55.64s Dec(J2000) = +21d 53' 52.4" with an uncertainty of 2.9 arcseconds (radius, 90% containment). This location is 23 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at http://www.swift.ac.uk/sper. No spectrum from the promptly downlinked event data is yet available to determine the column density. UVOT took a finding chart exposure of 150 seconds with the White filter starting 64 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the large, but uncertain extinction expected. Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 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: 16521 SUBJECT: GRB 140705A: Enhanced Swift-XRT position DATE: 14/07/05 13:23:22 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 886 s of XRT Photon Counting mode data and 1 UVOT images for GRB 140705A, 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 = 293.73199, +21.89673 which is equivalent to: RA (J2000): 19h 34m 55.68s Dec (J2000): +21d 53' 48.2" 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) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16522 SUBJECT: GRB 140705A: Swift-BAT refined analysis of a possible newly discovered SGR 1935+2154 DATE: 14/07/05 14:24:49 GMT FROM: Takanori Sakamoto at AGU A. Y. Lien (NASA/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-61 to T+242 sec from the recent telemetry downlink, we report further analysis of BAT GRB 140705A (trigger #603488) (Stamatikos, et al., GCN Circ. 16520). The BAT ground-calculated position is RA, Dec = 293.751, 21.912 deg which is RA(J2000) = 19h 35m 00.3s Dec(J2000) = +21d 54' 41.7" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 94%. The 2 ms mask-weighted light curve shows at least two spikes peaking at T+0 sec and T+0.05 sec. T90 (15-350 keV) is 0.08 +- 0.01 sec (estimated error including systematics). The time-averaged spectrum from T-0.02 to T+0.06 sec fit by a simple power-law model shows the power law index of 2.74 +- 0.15 (chi squared 75.65 for 57 d.o.f.). The fluence in the 15-150 keV band is 3.8 +- 0.4 x 10^-8 erg/cm2. The 1-sec peak photon flux measured from T-0.48 sec in the 15-150 keV band is 0.9 +- 0.2 ph/cm2/sec. A single blackbody fit to the time-averaged spectrum shows the blackbody temperature of 8.2 +- 1.0 keV (chi squared 74.30 for 57 d.o.f.). A thermal bremsstrahlung model fit shows the temperature of 35.7 +- 6.1 keV (chi squared 56.05 for 57 d.o.f.). A double blackbody fit shows the lower temperature of 4.8 +1.3 keV and the higher temperature of 13.7 (error not unconstrained) keV (chi squared 54.60 for 55 d.o.f.). All the quoted errors are at the 90% confidence level. Because 1) the burst is located at the galactic plane (l, b) = (57.25 deg, 0.83 deg.) and 2) the BAT burst spectrum is rather soft, we believe this could be a short event from a newly discovered SGR 1935+2154. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/603488/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16523 SUBJECT: GRB 140705A: Swift/UVOT Upper Limits DATE: 14/07/05 21:41:14 GMT FROM: Margaret Chester at PSU M. M. Chester (PSU) and M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140705A 65 s after the BAT trigger (Stamatikos et al., GCN Circ. 16520). No optical afterglow consistent with the XRT position (Osborne et al. GCN Circ. 16521) 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 first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 65 215 147 >20.6 u_FC 277 527 246 >20.2 white 65 6023 498 >21.5 v 607 6434 432 >19.8 b 532 7088 268 >21.1 u 277 7048 659 >20.6 w1 656 6843 432 >20.6 m2 5004 6638 393 >20.9 w2 582 6229 432 >21.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 4.88 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16524 SUBJECT: GRB 140705A: MITSuME Okayama upper limits DATE: 14/07/05 23:21:57 GMT FROM: Daisuke Kuroda at OAO/NAOJ D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ), S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on behalf of MITSuME and OISTER collaboration: We observed the field of GRB 140705A (Stamatikos et al., GCNC 16520) with the optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. The observation started on 2014-07-05 14:57:48 UT (~5.4 h after the burst). We did not find any new point source within the enhanced XRT circle (Osborne et al., GCNC 16521) in all the three bands. Three sigma upper limits of the OT are listed below. We used GSC2.3 catalog for flux calibration. #T0+[day] MID-UT T-EXP[sec] g' Rc Ic ----------------------------------------------------- 0.30500 16:52:00 6540.0 >19.4 >19.1 >18.2 ----------------------------------------------------- T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec] [GCN OPS NOTE(06jul14): The Subject-line was changed to the correct GRB name.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16525 SUBJECT: GRB 140705A: Swift-XRT refined Analysis DATE: 14/07/05 23:47:04 GMT FROM: Phil Evans at U of Leicester C. Pagani (U. Leicester), B. Sbarufatti (INAF-OAB/PSU), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), D.N. Burrows (PSU), J.A. Kennea (PSU), V. Mangano (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester) and M. Stamatikos report on behalf of the Swift-XRT team: We have analysed 10 ks of XRT data for GRB 140705A (Stamatikos et al. GCN Circ. 16520), from 68 s to 35.0 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 16521). The light curve can be modelled with a power-law decay with a decay index of alpha=0.15 (+0.09, -0.10). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 3.7 (+0.6, -0.5). The best-fitting absorption column is 4.9 (+1.1, -1.0) x 10^22 cm^-2, in excess of the Galactic value of 1.3 x 10^22 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.7 x 10^-11 (1.7 x 10^-09) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 4.9 (+1.1, -1.0) x 10^22 cm^-2 Galactic foreground: 1.3 x 10^22 cm^-2 Excess significance: 6.0 sigma Photon index: 3.7 (+0.6, -0.5) If the light curve continues to decay with a power-law decay index of 0.15, the count rate at T+24 hours will be 0.022 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x 10^-12 (3.7 x 10^-11) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00603488. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16526 SUBJECT: GRB 140705A: MITSuME Ishigakijima upper limits DATE: 14/07/06 01:19:24 GMT FROM: Daisuke Kuroda at OAO/NAOJ D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ), K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on behalf of the MITSuME and OISTER collaboration: We observed the field of GRB 140705A (Stamatikos et al., GCNC 16520) with the optical three color (g', Rc and Ic) CCD camera attached to the Murikabushi 1m telescope of Ishigakijima Astronomical Observatory. The observation started on 2014-07-05 13:08:26 UT (~3.6 h after the burst). We did not find any new point source within the enhanced XRT circle (Osborne et al., GCNC 16521) in all the three bands. Three sigma upper limits of the OT are listed below. We used GSC2.3 catalog for flux calibration. #T0+[day] MID-UT T-EXP[sec] g' Rc Ic ----------------------------------------------------- 0.20844 14:32:57 6960.0 >22.1 >21.5 >20.5 ----------------------------------------------------- T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16527 SUBJECT: GRB 140705A: KAIT Optical Upper Limit DATE: 14/07/06 02:51:21 GMT FROM: Weikang Zheng at UC Berkeley WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to Swift GRB 140705A (Stamatikos et al., GCN 16520) starting at 09:34:02 UT, 74 s after the burst. Observations were performed with an automatic sequence in the clear (roughly R), V, and I filters, and the exposure time was 20 s per image. We do not detect any new source within the enhanced XRT error circle (Osborne et al. GCN 16521) in our individual images, nor in the coadded images of the first 5 or 10 clear band images. The typical limiting magnitude of our single clear image is about 19.2 calibrated to USNO B1.0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16528 SUBJECT: GRB 140705A / SGR 1935+2154: Optical observations from 10.4m GTC DATE: 14/07/06 03:47:32 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (IAA-CSIC/UPV-EHU), P. Rodriguez-Gil (IAC) and S. Campana (INAF-OAB) report on behalf of a larger collaboration: We have observed the field of GRB 140705A / SGR 1935+2154 (Stamatikos et al. GCN 16520, Lien et al. GCN 16522) using OSIRIS on the 10.4m GTC telescope. Observations started at 00:57 UT of the 6 July 2014 (15.42 hrs after the burst onset) and consisted of 10x120s in i-band and 20x60s in z-band. Within the enhanced XRT error box (Osborne et al. GCN 16521, updated to R.A.: 293.73169, Dec.: +21.89668, +/-1.5") we detect two sources. The first of them, which we name S1, has an approximate magnitude of i(AB)~24 whereas S2 has i(AB)~25.5. Photometry is based on USNO-B1.0, and is still very preliminary. The coordinates of these sources are (J2000+/-0.5"): S1: 19:34:55.56, +21:53:48.2 S2: 19:34:55.68, +21:53:47.9 We have used UKIDSS nIR images for comparison, as there were not deep enough images available in the optical (there is no SDSS coverage in this field). S1 is clearly detected in J, H and K-band images of UKIDSS. S2, could be marginally detected in J-band. At this point we cannot claim variability of any of these sources and thus their relation with GRB 140705A / SGR 1935+2154 cannot be stated. We acknowledge excellent support from the GTC staff, in particular Riccardo Scarpa. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16529 SUBJECT: GRB 140705A / SGR 1935+2154: FTN observations DATE: 14/07/06 12:11:44 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi, S. Dichiara (U. Ferrara) on behalf of a large collaboration report: The 2-m Faulkes Telescope North began observing Swift GRB 140705A/ SGR 1935+2154 (Stamatikos et al. GCN Circ 16520; Lien et al. GCN Circ 16522) on July 05 at 10:10:46 UT, i.e. ~38 min after the BAT trigger, with the r' and i' filters. Within the enhanced XRT error circle (Osborne et al. GCN Circ. 16521) we found nothing down to the following limit: Mid time from Total Exp Filter Magnitude trigger (min) (s) -------------------------------------------------------------- 52.0 120x4 i' > 21 -------------------------------------------------------------- Magnitudes are calibrated against nearby USNO-B1 stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16533 SUBJECT: GRB 140705A / SGR 1935+2154: Probable association with supernova remnant G57.2+0.8 DATE: 14/07/07 08:19:25 GMT FROM: Bryan Gaensler at U of Sydney B. M. Gaensler (U. Sydney / CAASTRO) reports: I note that the newly identified magnetar SGR 1935+2154 (GCN 16522; ATel 6294) is coincident with the Galactic supernova remnant (SNR) G57.2+0.8 (Sun et al., 2011, A&A, 536, A83, and references therein). Specifically, the location of the SGR as determined by Swift XRT (ATel 6294) sits very close to the geometric centre of the SNR. A 1.4 GHz radio image of the SNR taken from the VLA Galactic Plane Survey (Stil et al., 2006, AJ, 132, 1158), and showing the position of the SGR, is available at: http://www.physics.usyd.edu.au/~bmg/fig_sgr1935+2154_snr.png This is a relatively uncrowded region of the Galactic plane, implying a high probability of a physical association between SGR 1935+2154 and SNR G57.2+0.8. The SGR's location at the centre of a SNR is similar to that previously found for other SGRs such as 1E 2259+586 in CTB 109, 1E 1841-045 in Kes 73 and 1E 1547.0-5408 in G327.2-0.1. No reliable age or distance estimate is available for SNR G57.2+0.8. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16542 SUBJECT: GRB 140705A / SGR 1935+2154: VLA 6 GHz observations DATE: 14/07/08 01:23:52 GMT FROM: Wen-fai Fong at CFA W. Fong and E. Berger (Harvard) report: "We observed the field of the Swift-detected SGR 1935+2154 (GRB 140705A; Stamatikos et al., GCN 16520) with the Karl G. Jansky Very Large Array (VLA) beginning on 2014 Jul 6.34 UT (22.69 hr after the BAT trigger) at a mean frequency of 6 GHz. In 1 hour of observations, we do not detect any radio emission within the enhanced XRT position (Osborne et al., GCN 16521) to a 3-sigma limit of 41 microJy." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16544 SUBJECT: GRB 140705A: Nishi-Harima NIR upper limits DATE: 14/07/08 12:30:45 GMT FROM: Akira Arai at Nishi-Harima Astro. Obs/U of Hyogo A. Arai, J. Takahashi, Y. Takagi, S. Honda, and K. Morihana (Univ. of Hyogo) report on behalf of the Nayuta team and the OISTER collaboration: We observed the field of GRB 140705A (Stamatikos et al., GCNC 16520) with Nishiharima Infrared Camera (NIC) attached to the Nayuta 2-m telescope at the Nishi-Harima Astronomical Observatory. The observations were conducted on 2014-07-05 at 12:53:36 -- 13:06:20 UT. We did not find any new point source within the enhanced XRT circle (Osborne et al., GCNC 16521) in all three bands. Three sigma upper limits of the object are listed below. We used 2MASS catalog for flux calibration. # MID-UT T0+[day] T-EXP J_mag H_mag Ks_mag -------------------------------------------------------------------------------- 12:59:59 0.14388 600 >16.6 >16.0 >15.4 -------------------------------------------------------------------------------- T0+: Elapsed time after the burst (day) T-EXP: Total Exposure time (seconds) -- ------------------------------------------------- Akira Arai, Nishi-Harima Astronomical Observatory, University of Hyogo mail : arai@nhao.jp -------------------------------------------------