//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11622 SUBJECT: GRB 110201A: Swift detection of a burst DATE: 11/02/01 09:49:06 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU), A. P. Beardmore (U Leicester), S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester), J. M. Gelbord (PSU), D. Grupe (PSU), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC), C. Pagani (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-OAB/IASFPA) and G. Stratta (ASDC) report on behalf of the Swift Team: At 09:35:08 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 110201A (trigger=444230). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 137.065, +88.608 which is RA(J2000) = 09h 08m 16s Dec(J2000) = +88d 36' 27" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 17 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 09:36:15.5 UT, 66.6 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source with an enhanced position: RA, Dec 137.5802, 88.6054 which is equivalent to: RA(J2000) = 09h 10m 19.25s Dec(J2000) = +88d 36' 19.3" with an uncertainty of 2.3 arcseconds (radius, 90% containment). This location is 45 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 (7.08 x 10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.1 (+3.40/-2.79) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 250 seconds with the U filter starting 126 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 19.2 mag. The coverage of the XRT error circle by the 8'x8' region for the list of sources generated on-board is uncertain because the large number of sources filled the available telemetry. No correction has been made for the expected extinction corresponding to E(B-V) of 0.35. Burst Advocate for this burst is M. H. Siegel (siegel AT astro.psu.edu). 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: 11623 SUBJECT: GRB 110201A: MASTER optical observations DATE: 11/02/01 09:59:43 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina Blagoveschensk Educational State University, Blagoveschensk 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 K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres, S.Yazev, N.M.Budnev, Irkutsk State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in MASTER-Amur was pointed to the GRB110201A 21 sec s after notice time and 46 sec after GRB time at 2011-02-01 09:35:54.771 UT. On our first (10s exposure) set we haven`t found optical transient within SWIFT-XRT error-box. The 3-sigma upper limit has been about V = 14.5mag The message may be cited. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11624 SUBJECT: GRB 110201A: Swift-BAT refined analysis DATE: 11/02/01 15:17:14 GMT FROM: Scott Barthelmy at NASA/GSFC H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. H. Siegel (PSU), 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+878 sec from the recent telemetry downlink, we report further analysis of BAT GRB 110201A (trigger #444230) (Siegel, et al., GCN Circ. 11622). The BAT ground-calculated position is RA, Dec = 137.489, 88.610 deg, which is RA(J2000) = 09h 09m 57.3s Dec(J2000) = +88d 36' 36.9" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 97%. The mask-weighted light curve shows 3 or 4 overlapping peaks starting at ~T-2 sec, peaking at ~T_zero, and ending at ~T+30 sec. T90 (15-350 keV) is 13.0 +- 2.2 sec (estimated error including systematics). The time-averaged spectrum from T-2.8 to T+13.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.09 +- 0.11. The fluence in the 15-150 keV band is 7.0 +- 0.5 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.28 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/444230/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11625 SUBJECT: Swift/UVOT observations of GRB110201A DATE: 11/02/01 16:11:22 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (MSSL-UCL) and M.H Siegel (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 110201A 127 s after the BAT trigger (Siegel et al., GCN Circ. 11622). No optical afterglow consistent with the XRT position is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag u_FC 127 377 246 >20.0 u 127 2348 627 >20.4 v 433 2424 253 >19.5 b 382 2373 272 >20.4 w1 482 2324 233 >19.7 m2 457 2449 233 >19.6 w2 408 2400 253 >19.1 We note that a bright star (V=7) is a few arcminutes from the GRB position. The values quoted above are not corrected for the strong Galactic extinction due to the reddening of E(B-V) = 0.35 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11626 SUBJECT: GRB110201A: MITSuME Okayama optical upper limits DATE: 11/02/02 09:39:55 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 the MITSuME collaboration: We observed the field of GRB 110201A (Siegel et al., GCN 11622) with the optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. The observation started on2011-02-01 09:59:39 UT (~25 min. after the burst). We did not find any new point source within the XRT error circle (Siegel et al., GCNC 11622) 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 ------------------------------------------------------ 0.16707 13:35:43 5880.0 >21.3 >21.3 >18.7 ------------------------------------------------------ T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11627 SUBJECT: GRB 110201A: Swift-XRT refined Analysis DATE: 11/02/02 16:02:43 GMT FROM: Dirk Grupe at PSU/Swift-XRT D. Grupe and M. H. Siegel (PSU) report on behalf of the Swift-XRT team: We have analyzed 21 ks of XRT data for GRB 110201A (Siegel et al. GCN Circ. 11622), from 54 s to 83.0 ks after the BAT trigger. The data comprise 6 s in Windowed Timing (WT) mode (taken while Swift was slewing), with the remainder in Photon Counting (PC) mode. The light curve can be modeled with a broken power-law model with an initial decay slope of alpha-1 = 3.25 (+0.40, -0.66) and a break at Tbreak-1 = 380 (+120, -55) s. After this break the afterglow decays with a slope of alpha-2 = 1.03 (+0.12, -0.11). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.04 (+0.26, -0.29). The best-fitting absorption column is 3.1 (+0.5, -1.0) x 10^21 cm^-2, in excess of the Galactic value of 2.8 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.3 x 10^-11 (7.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.1 (+0.5, -1.0) x 10^21 cm^-2 Galactic foreground: 2.8 x 10^20 cm^-2 Excess significance: 5.3 sigma Photon index: 2.04 (+0.26, -0.29) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00444230. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11688 SUBJECT: GRB 110201A: optical observations DATE: 11/02/10 10:58:01 GMT FROM: Alina Volnova at SAI MSU V. Rumyantsev (CrAO), A. Pozanenko (IKI),  A. Volnova (SAI MSU), E. Klunko (ISTP) report on behalf of larger GRB  follow-up collaboration: We observed  the field of the Swift GRB 110201A (Siegel et al., GCN 11622) with Shajn telescope of CrAO in filter R between  Feb. 01 (UT) 17:01 - 18:04, and with AZT-33IK telescope  between Feb. 01 (UT) 16:31 - 17:07. Using stacked image of CrAO observations we detect  a diffuse source (A) at ~4" offset of a center of the XRT error circle (Siegel et al., GCN 11622), see also http://www.swift.ac.uk/sper/444230/.  The coordinates of the center of the source (A) are (J2000) RA = 09:10:29.84, Dec =  +88:36:17.5 with uncertainty of 0.5" in both coordinates. The photometry of the source is based on the USNO-B1.0 star 1786-0003311 (09:12:09.70 +88:36:01.0) assuming R=17.64 is following: T0+         Filter,   Exposure,  source A, mag, UpperLimit (mid, d)              (s) 0.3305    R       45x60          21.9 +/- 0.1     23.4 Would be the source (A) a host galaxy of GRB 110201A, the galaxy could be a relatively close  (z <1) taking into account its brightness. The finding chart can be found at http://grb.rssi.ru/GRB110201A/GRB110201a_110201_R_ZTSh.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11698 SUBJECT: GRB 110201A: Subaru/MOIRCS Ks-band photometry DATE: 11/02/11 21:06:49 GMT FROM: Masato Onodera at ETH Zurich M. Onodera (ETH Zurich), E. Daddi (CEA/Saclay), I. Tanaka (Subaru Telescope), and Y. Yamada (NAOJ) report: We observed the field of GRB 110201A (Siegel et al., GCN Circ. 11622) in Ks-band with MOIRCS on the Subaru telescope. The observations was carried out on 2011-02-02 16:27:33 UT (~31 hours after the burst) for 200 seconds integration and on 2011-02-03 16:16:20 UT (~54.5 hours after the burst) for 520 seconds integration. Within the XRT error circle, we did not find any evidence for fading sources. On the other hand, a faint galaxy is detected at (RA, Dec)=(9:10:23.01, +88:36:21.82). Our preliminary photometry shows the galaxy is Ks=19.7 (Vega) or Ks=21.5 (AB) with an error of ~0.2 mag. There is another source slightly outside of the XRT error circle at (RA, Dec)=(9:10:31.5, +88:36:18.4) with an magnitude of Ks=19.3 (Vega) or Ks=21.1 (AB) with an error of ~0.15 mag. Flux calibration was carried out by using 2MASS sources. Images are provided for consultation at the following web site: http://www.astro.phys.ethz.ch/people/monodera/grb110201a/