//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14127 SUBJECT: GRB 130102A: Swift detection of a burst DATE: 13/01/02 18:27:44 GMT FROM: Scott Barthelmy at NASA/GSFC K. L. Page (U Leicester), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf of the Swift Team: At 18:10:53 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 130102A (trigger=544784). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 311.464, +49.835 which is RA(J2000) = 20h 45m 51s Dec(J2000) = +49d 50' 06" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). As per usual for an image trigger, the TDRSS lightcurve does not show anything significant. The XRT began observing the field at 18:12:50.3 UT, 116.5 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 311.4233, 49.8174 which is equivalent to: RA(J2000) = 20h 45m 41.60s Dec(J2000) = +49d 49' 02.6" with an uncertainty of 2.1 arcseconds (radius, 90% containment). This location is 113 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 7.96 x 10^21 cm^-2 (Kalberla et al. 2005). The initial flux in the 2.5 s image was 5.62e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 125 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. We note that this event is at galactic coordinates: l = 88.33 deg, b = 4.22 deg. It has the characteristics of a GRB, but could be a galactic transient since it is close to the galactic plane. Burst Advocate for this burst is K. L. Page (kpa AT star.le.ac.uk). 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: 14128 SUBJECT: GRB 130102A: IAC80 I-band observations DATE: 13/01/03 01:21:50 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (IAA-CSIC) & L. Toribio (IAC), report on behalf of a larger collaboration: "We observed the Swift/XRT location of GRB 130102A (Page et al., GCNC 14127) using the 82cm IAC80 telescope at the Observatorio del Teide (Tenerife, Spain). We took a set of I-band images on Jan 2.7924--2.8340 UT (0.84--1.83 hours post burst). No optical source brighter than I~21 (Vega) is detected inside the XRT error circle." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14129 SUBJECT: GRB 130102A: Enhanced Swift-XRT position DATE: 13/01/03 05:22:38 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 1933 s of XRT Photon Counting mode data and 2 UVOT images for GRB 130102A, 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 = 311.42346, +49.81764 which is equivalent to: RA (J2000): 20h 45m 41.63s Dec (J2000): +49d 49' 03.5" with an uncertainty of 1.6 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: 14131 SUBJECT: GRB 130102A: Swift-XRT refined Analysis DATE: 13/01/03 06:27:03 GMT FROM: Phil Evans at U of Leicester P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), A. Maselli (INAF-IASFPA) and K.L. Page report on behalf of the Swift-XRT team: We have analysed 10 ks of XRT data for GRB 130102A (Page et al. GCN Circ. 14127), from 109 s to 24.6 ks after the BAT trigger. The data comprise 66 s in Windowed Timing (WT) mode (the first 5 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN. Circ 14129). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=1.33 (+0.21, -0.20). At T+456 s the decay steepens to an alpha of 5.5 (+1.9, -1.2) before breaking again at T+924 s to a final decay with index alpha=0.88 (+0.31, -0.28). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.0 (+0.4, -0.3). The best-fitting absorption column is 1.13 (+0.34, -0.29) x 10^22 cm^-2, in excess of the Galactic value of 8.0 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.8 x 10^-11 (1.2 x 10^-10) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.13 (+0.34, -0.29) x 10^22 cm^-2 Galactic foreground: 8.0 x 10^21 cm^-2 Excess significance: 1.9 sigma Photon index: 2.0 (+0.4, -0.3) If the light curve continues to decay with a power-law decay index of 0.88, the count rate at T+24 hours will be 5.2 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x 10^-14 (6.4 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00544784. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14132 SUBJECT: GRB 130102A: MASTER-Net optical observations DATE: 13/01/03 08:05:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Denisenko Lomonosov Moscow State University, Sternberg Astronomical Institute A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Kislovodsk was pointed to the GRB130102A (Page et. al. GCN14127) 104 sec after GRB time at 2013-01-02 18:12:37 UT in two polarizations. On our first (20s exposure) set we haven`t found optical transient within SWIFT error-box. The 5-sigma upper limit has been about 17.9 mag MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located near Blagoveschensk was pointed to the GRB130102A (Page et. al. GCN 14127) 107 sec after GRB time at 2013-01-02 18:12:40 UT in two diagonal polarizations. On our first (20s exposure) set we haven`t found optical transient within SWIFT error-box. The 5-sigma upper limit has been about 13.9 mag. The low limit is the resultsa of the high zenit distance. We note that there are no objects in any catalogs 10" around center of the Swift XRT error box (Osborne et. al. GCN 14129). The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14133 SUBJECT: GRB 130102A: Swift-BAT refined analysis DATE: 13/01/03 14:19:24 GMT FROM: Scott Barthelmy at NASA/GSFC C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 130102A (trigger #544784) (Page, et al., GCN Circ. 14127). The BAT ground-calculated position is RA, Dec = 311.435, 49.838 deg which is RA(J2000) = 20h 45m 44.4s Dec(J2000) = +49d 50' 16.4" with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 99%. The mask-weighted light curve shows a peak starting at ~T+10 sec, peaking at ~T+22 sec, and ending around T+180 sec. There is a possibility of emission out to at least T+230 sec. T90 (15-350 keV) is 77.5 +- 18.2 sec (estimated error including systematics). The time-averaged spectrum from T+12.51 to T+100.43 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.39 +- 0.18. The fluence in the 15-150 keV band is 7.2 +- 0.9 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+23.54 sec in the 15-150 keV band is 0.4 +- 0.1 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/544784/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14134 SUBJECT: GRB 130102A: P60 Observations DATE: 13/01/03 19:26:41 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration: We have imaged the field of GRB130102A (Page et al., GCN 14127) with the robotic Palomar 60 inch telescope (P60). Observations began at 01:56 on 2013 January 3 (~ 7.8 hours after the Swift trigger), and were obtained under poor seeing conditions in the r', i', and z' filters. We do not detect any sources within the enhanced XRT error localization (Osborne et al., GCN 14129). Using nearby point sources from the AAVSO Photometric All-Sky Survey (APASS) for calibration, we measure limiting magnitudes of r' > 20.9, i' > 20.5 at this time. We note that these limits do not include a correction for the large Galactic extinction along this line of sight. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 14136 SUBJECT: GRB 130102A: Swift/UVOT Upper Limits DATE: 13/01/04 22:36:12 GMT FROM: Tyler Pritchard at PSU T. A. Pritchard (PSU) and K. L. Page (U Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 130102A 126 s after the BAT trigger (Page et al., GCN Circ. 14127). No optical afterglow consistent with the XRT position (Osborne et al. GCN Circ. 14129) 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 126 276 147 >21.1 u_FC 284 534 246 >20.4 white 126 7587 844 >22.4 v 614 12045 1343 >20.9 b 540 7382 549 >20.8 u 284 7177 775 >20.5 w1 664 6972 549 >20.2 m2 639 12641 934 >20.7 w2 590 7794 568 >20.7 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 1.90 in the direction of the burst (Schlegel et al. 1998).