//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11658 SUBJECT: GRB 110207A: Swift detection of a burst DATE: 11/02/07 11:26:09 GMT FROM: David Palmer at LANL O. M. Littlejohns (U Leicester), A. P. Beardmore (U Leicester), S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester), J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC), N. P. M. Kuin (UCL-MSSL), P. T. O'Brien (U Leicester), C. Pagani (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA), A. Rowlinson (U Leicester), T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU) and R. L. C. Starling (U Leicester) report on behalf of the Swift Team: At 11:17:20 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 110207A (trigger=444912). Swift could not slew to the burst due to a Moon constraint. The BAT on-board calculated location is RA, Dec 12.542, -10.806 which is RA(J2000) = 00h 50m 10s Dec(J2000) = -10d 48' 20" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex multi-peaked structure with a duration of about 40 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~0.5 sec after the trigger. Due to a Moon observing constraint, Swift cannot slew to the BAT position until 13:20 UT on 2011 February 08. There will thus be no XRT or UVOT data for this trigger before this time. Burst Advocate for this burst is O. M. Littlejohns (oml2 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: 11660 SUBJECT: GRB 110207A: MASTER prompt and early optical observations DATE: 11/02/07 13:52:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina Blagoveschensk Educational State University, Blagoveschensk K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres, S.Yazev, N.M.Budnev, Irkutsk State University E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov Sternberg Astronomical Institute, Moscow State University V.Krushinski, I.Zalozhnich, A. Popov Ural State University, Kourovka A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory Two MASTER II robotic telescopes (MASTER-Net: http://observ.pereplet.ru) located in Amur-Blagoveschensk and Tunka-Baykal was pointed to the GRB110207A 65 and 30 sec after GRB time correspondingly. On our first (10s exposure) set we haven`t found optical transient within SWIFT-BAT error-box (Littlejohns et al., GCN Curc 11658). Because GRB duration is 40 sec, the first images from Tunka is prompt. The obdervations was done at high zenith distance (>80 degrees). The 3-sigma upper limit has been about: ----------------------------------------------------------------------- Start Time mean time Exp Limit Filter Site after trigger after trigger (s) ----------------------------------------------------------------------- 30s 35s 10 13.0 V+P\/ Tunka-Baykal 65s 70s 10 14.1 V+P-| Amur-Blagoveschensk 65s 747s 1370 17.0 V+P-| Amur-Blagoveschensk 1700s 1790s 180 17.4 R Tunka-Baykal ------------------------------------------------------------------------ P - is polarization. The message may be cited. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11664 SUBJECT: GRB 110207A: Swift-BAT refined analysis DATE: 11/02/07 19:22:19 GMT FROM: Scott Barthelmy at NASA/GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), O. M. Littlejohns (U Leicester), C. B. Markwardt (GSFC), T. Sakamoto (GSFC/UMBC), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from recent telemetry downlinks, we report further analysis of BAT GRB 110207A (trigger #444912) (Littlejohns, et al., GCN Circ. 11658). The BAT ground-calculated position is RA, Dec = 12.540, -10.790 deg, which is RA(J2000) = 00h 50m 09.5s Dec(J2000) = -10d 47' 23.8" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows at least seven short peaks starting at ~T-0.1 sec and ending at ~T+20 sec with a long decay extending out to ~T+110 sec. T90 (15-350 keV) is 80.3 +- 16.2 sec (estimated error including systematics). The time-averaged spectrum from T-0.1 to T+108.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.30 +- 0.12. The fluence in the 15-150 keV band is 1.6 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.11 sec in the 15-150 keV band is 1.1 +- 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/444912/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11667 SUBJECT: GRB 110207A: TAROT Calern observatory optical observations DATE: 11/02/07 23:00:01 GMT FROM: Alain Klotz at CESR-CNRS Klotz A. (CESR-OMP), Gendre B. (ASDC), Laas-Bourez M. (UWA) Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report: We imaged the field of GRB 110207A detected by SWIFT (trigger 444912) with the TAROT robotic telescope (D=25cm) located at the Calern observatory, France. The observations started 6.62h after the GRB trigger (beginning of the night). The elevation of the field decreased from 25 degrees above horizon and weather conditions were good. We co-added a series of exposures. No OT was detected : t0+6.62h to t0+7.79h : R > 19.8 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. N.B. Galactic coordinates are lon=121.8238 lat=-73.6747 and the galactic extinction in R band is 0.1 magnitude estimated from D. Schlegel et al. 1998ApJ...500..525S. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11671 SUBJECT: GRB 110207A: Fermi GBM observation DATE: 11/02/08 16:02:07 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 11:17:20.29 UT on 07 February 2011, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 110207A (trigger 318770242/ 110207470), which was also detected by the Swift/BAT (Littlejohns et al. 2011, GCN 11658) The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 72.8 degrees. The GBM light curve shows a multi-peaked structure with a duration (T90) of about 39 s (50-300 keV). The time-averaged spectrum from T0-0.256 s to T0+38.912 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.09 (+0.13/-0.12) and the cutoff energy, parameterized as Epeak, is 450 (+290/-130) keV. The event fluence (10-1000 keV) in this time interval is (4.4 +/- 0.6)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+0.211 s in the 10-1000 keV band is 2.3 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11680 SUBJECT: GRB 110207A: Swift-XRT observations DATE: 11/02/09 14:44:37 GMT FROM: Phil Evans at U of Leicester P.A. Evans and O.M. Littlejohns (U. Leicester) report on behalf of the Swift team: Swift observed the field of GRB 110207A (Littlejohns et al., GCN Circ. 11658) for 5 ks from T0+99 ks to T0+112 ks; earlier observations were impossible due to the proximity of the GRB to the Moon. We find no X-ray sources in the BAT field of view, placing a 3-sigma upper limit on the afterglow brightness of 7.6e-14 erg/cm^2/sec during this interval (0.3-10 keV; assuming a typical GRB spectrum). Due to the proximity of the GRB to the Sun, no further observations are planned. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11695 SUBJECT: GRB 110207A: Suzaku WAM observation of the prompt emission DATE: 11/02/11 10:20:52 GMT FROM: Yuji Urata at Nat. Central U. P. Tsai, Y. Urata (NCU), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.), M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, T. Tamagawa, M. Serino (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The GRB 110207A (Swift/BAT trigger #444912 ; Littlejohns et al., GCN 11658; Palmer et al., GCN 11664) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2011/02/07 11:17:20.05 UT (=T0). The observed light curve shows a multi-peaked structure lasting from T0-0.2s to T0+3.2s with a duration (T90) of about 2.9 seconds. The fluence in 100 - 1000 keV was 5.98 (+/-0.54) x 10^-7 erg/cm^2. The 1-s peak flux measured from T0+0.32s was 0.27 (+/-0.06) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-0.2s to T0+3.2s is well fitted by a single power-law with a photon index of 1.53 (-0.24, +0.29) (chi^2/d.o.f = 34.22/34). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. 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