//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12065 SUBJECT: GRB 110610A: Swift detection of a burst DATE: 11/06/10 15:36:34 GMT FROM: Scott Barthelmy at NASA/GSFC F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), S. Campana (INAF-OAB), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC), P. T. O\'Brien (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), A. Rowlinson (U Leicester), T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU), C. A. Swenson (PSU), G. Tagliaferri (INAF-OAB), E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (MSU) report on behalf of the Swift Team: At 15:21:32 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 110610A (trigger=455155). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 308.151, +74.823 which is RA(J2000) = 20h 32m 36s Dec(J2000) = +74d 49' 22" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows several peaks with a duration of about 60 sec. The peak count rate was ~6000 counts/sec (15-350 keV), at ~35 sec after the trigger. The XRT began observing the field at 15:22:43.9 UT, 71.8 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 308.17636, 74.82415 which is equivalent to: RA(J2000) = 20h 32m 42.33s Dec(J2000) = +74d 49' 26.9" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 24 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 in excess of the Galactic value (1.32 x 10^21 cm^-2, Kalberla et al. 2005), with an excess column of 9.4 (+4.45/-3.60) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 8.90e-10 erg cm^-2 s^-1 (0.2-10 keV). Due to a bright star in the field of view, UVOT products will be delayed. Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.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: 12066 SUBJECT: GRB 110610A: MASTER-NET optical observations DATE: 11/06/10 15:52:40 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev,E.Konstantinov, Irkutsk State University E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. Kornilov,A.Sankovich Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalozhnich, T.Kopytova, A. Popov Ural State University, Kourovka V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina Blagoveschensk Educational State University, Blagoveschensk MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Tunka(Siberia) was pointed to the GRB110610.64 30 sec s after notice time and 55 sec after GRB time at 2011-06-10 15:22:27.062 UT. On our first (10s exposure) set we haven`t found optical transient within SWIFT error-box (ra=20 32 35 dec=+74 49 11 r=0.050000). The 5-sigma upper limit has been about 15.0 mag The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12068 SUBJECT: GRB 110610A: Swift-BAT refined analysis DATE: 11/06/10 19:57:20 GMT FROM: Scott Barthelmy at NASA/GSFC J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), F. E. Marshall (NASA/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-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 110610A (trigger #455155) (Marshall, et al., GCN Circ. 12065). The BAT ground-calculated position is RA, Dec = 308.205, 74.827 deg, which is RA(J2000) = 20h 32m 49.1s Dec(J2000) = +74d 49' 37.3" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 71%. The mask-weighted light curve shows several overlapping peaks starting at ~T-15 sec, with the first peak at ~T+3 sec, the highest peak at ~T+35 sec, and ending at ~T+55 sec. Emission may continue (~1-sigma level) out to T+170 sec. T90 (15-350 keV) is 46.4 +- 5.7 sec (estimated error including systematics). The time-averaged spectrum from T-11.1 to T+58.0 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.51 +- 0.05. The fluence in the 15-150 keV band is 4.9 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+34.42 sec in the 15-150 keV band is 4.2 +- 0.2 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/455155/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12069 SUBJECT: GRB 110610A: Enhanced Swift-XRT position DATE: 11/06/10 20:10:29 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 916 s of XRT Photon Counting mode data and 1 UVOT images for GRB 110610A, 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 = 308.17906, +74.82533 which is equivalent to: RA (J2000): 20h 32m 42.97s Dec (J2000): +74d 49' 31.2" with an uncertainty of 1.9 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: 12070 SUBJECT: GRB 110610A: Swift/UVOT Upper Limits DATE: 11/06/10 22:11:43 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) reports on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 110610A 4561 s after the BAT trigger (Marshall et al., GCN Circ. 12065). No optical afterglow consistent with the XRT position (Goad et al. GCN Circ. 12069) is detected in the initial UVOT exposures. The usual UVOT finding chart exposures were not taken because of a nearby bright star. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag v 4561 6408 590 >19.7 w1 4971 6817 590 >20.5 m2 4766 6612 590 >20.8 w2 4356 6203 590 >20.5 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.44 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12071 SUBJECT: GRB 110610A: Swift-XRT refined Analysis DATE: 11/06/11 07:21:04 GMT FROM: Antonia Rowlinson at U.of Leicester A. Rowlinson (U. Leicester) and F. E. Marshall (NASA/GSFC) report on behalf of the Swift-XRT team: We have analysed 9.4 ks of XRT data for GRB 110610A (Marshall et al. GCN Circ. 12065), from 62 s to 24.2 ks after the BAT trigger. The data comprise 79 s in Windowed Timing (WT) mode (the first 8 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 Goad et al. (GCN. Circ 12069). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=2.8 (+/-0.4). At T+174 s the decay flattens to an alpha of 0.18 (+0.21, -0.32) before breaking again at T+984 s to a final decay with index alpha=1.33 (+0.12, -0.10). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.18 (+0.20, -0.19). The best-fitting absorption column is 8.2 (+1.3, -1.2) x 10^21 cm^-2, in excess of the Galactic value of 1.3 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 5.1 x 10^-11 (1.2 x 10^-10) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 8.2 (+1.3, -1.2) x 10^21 cm^-2 Galactic foreground: 1.3 x 10^21 cm^-2 Excess significance: 11.4 sigma Photon index: 2.18 (+0.20, -0.19) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00455155. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12072 SUBJECT: GRB 110610A: 1.23m CAHA optical observations DATE: 11/06/12 20:41:02 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (IAA-CSIC, Granada), P. Kubanek (IAA-CSIC, Granada & U. Valencia), report on behalf of a larger collaboration: "We have taken two optical data sets of the Swift GRB 110610A (Marshall et al., GCN 12065) field using the 1.23m Calar Alto telescope. The observations were carried out in the I-band on June 11.0013--11.1579 UT and June 11.9093--12.1599 UT (8.67-12.44 hours and 30.46-36.48 hours post trigger, respectively). We do not detect any optical source consistent with the XRT error circle (Goad et al., GCNC 12069) down to a limiting magnitude of I=20.6 (3 sigma, calibrated against USNO-B1.0)". //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12073 SUBJECT: GRB 110610A: Fermi GBM detection DATE: 11/06/15 00:42:24 GMT FROM: Shaolin Xiong at UAH Shaolin Xiong (UAH) reports on behalf of the Fermi GBM Team: "At 15:21:32.549 UT on 10 June 2011, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 110610A (trigger 329412094 / 110610640), which was also detected by the Swift/BAT (Marshall et al. 2011, GCN 12065). The GBM on-ground location is consistent with the Swift position. This burst was also detected by INTEGRAL SPI-ACS and Suzaku WAM. The angle from the Fermi LAT boresight is 59 degrees. The GBM light curve consists of multiple peaks with a duration (T90) of about 40 s (50-300 keV). The time-averaged spectrum from T0+0.0 s to T0+39.4 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.97 +/- 0.05 and the cutoff energy, parameterized as Epeak, is 189.9 +/- 14.0 keV. The event fluence (10-1000 keV) in this time interval is (8.70 +/- 0.35)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+33.7 s in the 10-1000 keV band is 5.97 +/- 0.25 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak = 170.0 +/- 19.8 keV, alpha = -0.93 +/- 0.07 and beta = -2.23 +/- 0.20. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12074 SUBJECT: GRB 110610A: Suzaku WAM observation of the prompt emission DATE: 11/06/15 09:43:15 GMT FROM: Satoshi Sugita at Aoyama Gakuin U. S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.), T. Uehara, Y. Hanabata, T. Takahashi, M. Ohno, Y. Fukazawa (Hiroshima U.), Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.), M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa (Waseda U.), N. Ohmori, M. Akiyama, M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai, C-J. Chuang (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The long GRB 110610A (Swift/BAT trigger #455155, GCN 12065; Marshall et al.,) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 15:22:6.198 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-53s, ending at T0+10s with a duration (T90) of 47 +/- 10 seconds. The fluence in 100 - 1000 keV was 4.57 (-0.60, +0.53) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+1s was 1.44 +/- 0.15 photons/cm^2/s in the same energy range. result shows that the time-averaged spectrum from T0-53s to T0+10s is well fitted by a single power-law with a photon index of 2.07 (-0.13, 0.15) (chi^2/d.o.f = 34.5/26). All the quoted errors are at statistical 90% confidence level. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html