//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12942 SUBJECT: GRB 120213A: Swift detection of a burst DATE: 12/02/13 00:40:47 GMT FROM: Scott Barthelmy at NASA/GSFC T. Sakamoto (NASA/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and M. C. Stroh (PSU) report on behalf of the Swift Team: At 00:27:19 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 120213A (trigger=514767). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 301.032, +65.397, which is RA(J2000) = 20h 04m 08s Dec(J2000) = +65d 23' 51" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single FRED pulse with a duration of about 40 sec. The peak count rate was ~3200 counts/sec (15-350 keV), at ~4 sec after the trigger. The XRT began observing the field at 00:28:09.0 UT, 49.5 seconds after the BAT trigger. XRT found a bright, uncatalogued, fading X-ray source located at RA, Dec 301.0105, 65.4092 which is equivalent to: RA(J2000) = +20h 04m 2.52s Dec(J2000) = +65d 24' 33.1" with an uncertainty of 5.2 arcseconds (radius, 90% containment). This location is 54 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 0.1 s image was 4.08e-08 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 58 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 expected extinction corresponding to E(B-V) of 0.22. Burst Advocate for this burst is T. Sakamoto (Taka.Sakamoto 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: 12944 SUBJECT: GRB 120213A: Prompt enhanced Swift-XRT position DATE: 12/02/13 01:28:23 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 120213A, we find an enhanced XRT position of the afterglow: RA, Dec: 301.0128, 65.4110 which is equivalent to: RA (J2000) = 20 04 03.07 Dec (J2000) = +65 24 39.6 with an uncertainty of 2.1 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/514767. Position enhancement is is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12945 SUBJECT: GRB 120213A: MASTER-NET early optical observations DATE: 12/02/13 03:39:37 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, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, M.Kornilov, A.Sankovich Sternberg Astronomical Institute, Moscow State University V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalozhnich, A. Popov Ural State University, Kourovka K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University H.Levato, C.Mallamaci, C.Saffe ICATE (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio), San Juan, San Juan University, Felix Aguilar Observatory, Argentina MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Kislovodsk was pointed to the GRB120213A 26 sec. after notice time and 49 sec. after GRB time at 2012-02-13 00:28:08.528 UT in two polarizations. On our first (10s exposure) set we haven`t found optical transient within SWIFT error-box (ra=20 04 07 dec=+65 23 59 r=0.050000). The 5-sigma upper limit has been about 16.15mag The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12946 SUBJECT: GRB 120213A: Swift-BAT refined analysis DATE: 12/02/13 04:19:01 GMT FROM: Scott Barthelmy at NASA/GSFC W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), 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-239 to T+841 sec from recent telemetry downlinks, we report further analysis of BAT GRB 120213A (trigger #514767) (Sakamoto, et al., GCN Circ. 12942). The BAT ground-calculated position is RA, Dec = 300.987, 65.413 deg, which is RA(J2000) = 20h 03m 56.8s Dec(J2000) = +65d 24' 48.0" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows a single FRED-like pulse starting at ~T-7 sec, peaking at ~T+5 sec, and ending at ~T+75 sec. T90 (15-350 keV) is 48.9 +- 12.0 sec (estimated error including systematics). The time-averaged spectrum from T-6.31 to T+74.46 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.37 +- 0.09. The fluence in the 15-150 keV band is 1.9 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+5.44 sec in the 15-150 keV band is 1.7 +- 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/514767/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12948 SUBJECT: GRB 120213A: Enhanced Swift-XRT position DATE: 12/02/13 06:29:22 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 2431 s of XRT Photon Counting mode data and 5 UVOT images for GRB 120213A, 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 = 301.01211, +65.41135 which is equivalent to: RA (J2000): 20h 04m 2.91s Dec (J2000): +65d 24' 40.9" with an uncertainty of 1.7 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: 12951 SUBJECT: GRB 120213A: Swift/UVOT Upper Limits DATE: 12/02/13 12:35:20 GMT FROM: Samantha Oates at MSSL S. R. Oates (MSSL-UCL) and T. Sakamoto (NASA/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 120213A 59 s after the BAT trigger (Sakamoto et al., GCN Circ. 12942). No optical afterglow consistent with the XRT position (Beardmore et al., GCN Circ. 12948) 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 59 209 147 >19.8 u_FC 271 521 246 >19.7 white 59 12944 1454 >21.6 v 602 6546 294 >20.4 b 527 12032 1219 >20.5 u 271 7161 717 >20.6 w1 653 6956 471 >19.8 m2 6551 6751 197 >19.8 w2 578 13010 332 >20.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.22 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12952 SUBJECT: GRB 120213A: Swift-XRT refined Analysis DATE: 12/02/13 12:40:03 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), O.M. Littlejohns (U. Leicester), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC) and T. Sakamoto report on behalf of the Swift-XRT team: We have analysed 6.5 ks of XRT data for GRB 120213A (Sakamoto et al. GCN Circ. 12942), from 53 s to 22.8 ks after the BAT trigger. The data comprise 886 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN. Circ 12944). The late-time light curve (from T0+5.3 ks) can be modelled with a power-law decay with a decay index of alpha=3.02 (+0.19, -0.18). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 3.28 (+/-0.07). The best-fitting absorption column is 3.52 (+0.15, -0.14) x 10^21 cm^-2, in excess of the Galactic value of 1.0 x 10^21 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.22 (+/-0.15) and a best-fitting absorption column of 1.7 (+/-0.4) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.4 x 10^-11 (5.4 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.7 (+/-0.4) x 10^21 cm^-2 Galactic foreground: 1.0 x 10^21 cm^-2 Excess significance: 3.2 sigma Photon index: 2.22 (+/-0.15) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00514767. This circular is an official product of the Swift-XRT team.