//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11509 SUBJECT: GRB 110102A: Swift detection of a burst with an optical detection DATE: 11/01/02 19:06:24 GMT FROM: Scott Barthelmy at NASA/GSFC S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Gronwall (PSU), C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC), V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), C. J. Saxton (UCL-MSSL), B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU) and G. Stratta (ASDC) report on behalf of the Swift Team: At 18:52:25 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 110102A (trigger=441454). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 245.879, +7.619 which is RA(J2000) = 16h 23m 31s Dec(J2000) = +07d 37' 09" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a weak precursor at T_zero and then a bright FRED-like pulse at T+130 sec with a total duration of about 170 sec. The peak count rate was ~6000 counts/sec (15-350 keV), at ~130 sec after the trigger. The XRT began observing the field at 18:54:54.0 UT, 148.6 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 245.8821, +7.6160 which is equivalent to: RA(J2000) = 16h 23m 31.70s Dec(J2000) = +07d 36' 57.5" with an uncertainty of 6.3 arcseconds (radius, 90% containment). This location is 15 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. UVOT took a finding chart exposure of 150 seconds with the White filter starting 149 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 16:23:31.43 = 245.88096 DEC(J2000) = +07:36:50.0 = 7.61390 with a 90%-confidence error radius of about 0.62 arc sec. This position is 8.6 arc sec. from the center of the XRT error circle. The estimated magnitude is 17.93 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.08. Burst Advocate for this burst is S. R. Oates (sro AT mssl.ucl.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: 11510 SUBJECT: GRB 110102A: Enhanced Swift-XRT position DATE: 11/01/02 23:49:13 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 3361 s of XRT Photon Counting mode data and 7 UVOT images for GRB 110102A, 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 = 245.88117, +7.61377 which is equivalent to: RA (J2000): 16h 23m 31.48s Dec (J2000): +07d 36' 49.6" 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: 11511 SUBJECT: GRB 110102A: Swift-BAT refined analysis DATE: 11/01/03 03:07:48 GMT FROM: Scott Barthelmy at NASA/GSFC T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), S. R. Oates (UCL-MSSL), D. M. Palmer (LANL), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from recent telemetry downlinks, we report further analysis of BAT GRB 110102A (trigger #441454) (Oates, et al., GCN Circ. 11509). The BAT ground-calculated position is RA, Dec = 245.877, 7.617 deg, which is RA(J2000) = 16h 23m 30.5s Dec(J2000) = +07d 37' 00.1" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 66%. The mask-weighted light curve shows a pair of small precursor peaks starting at ~T-50 sec and ending at ~T+50 sec. The main emission occurs with four peaks that start at ~T+100 sec and ending at ~T+340 with the maximum at ~T+210 sec. T90 (15-350 keV) is 264 +- 8 sec (estimated error including systematics). The time-averaged spectrum from T-49.2 to T+294.9 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.60 +- 0.04. The fluence in the 15-150 keV band is 1.65 +- 0.03 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+208.76 sec in the 15-150 keV band is 8.4 +- 0.3 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/441454/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11512 SUBJECT: GRB 110102A: Fermi GBM observation DATE: 11/01/03 05:45:05 GMT FROM: Lin Lin at UAH/NAOC Lin Lin (UAH) report on behalf of the Fermi GBM Team: "At 18:54:36.00 UT on 2 Jan. 2011, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 110102A (trigger 315687278 / 110102788). which was also detected by the Swift/BAT (S. R. Oates et al. 2011, GCN 11509) The GBM on-ground location is consistent with the Swift position. The GBM light curve shows of several peaks with a duration (T90) of about 254 s (50-300 keV). The T90 starts at T0-119 s. The time-averaged spectrum from T0-123 s to T0+149 s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -1.49 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 476.6 +/- 68.7 keV The event fluence (10-1000 keV) in this time interval is (4.39 +/- 0.09)E-5 erg/cm^2. The 1 sec peak photon flux measured starting from T0+78 s in the 10-1000 keV band is 14.07 +/- 0.35 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: 11513 SUBJECT: GRB110102A: MITSuME Okayama Optical Observation DATE: 11/01/03 10:09:15 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 110102A (Oates et al., GCN 11509) with the optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. The observation started on 2011-01-02 20:08:45 UT (~1.3 hours after the burst). We detected the afterglow candidate within the enhanced XRT error circle (Goad et al., GCNC 11510) in all the three bands. Photometric results are listed below. We used SDSS catalog for flux calibration. #T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err ---------------------------------------------------------------------- 0.06851 20:31:04 2340.0 20.0 0.4 19.6 0.3 18.3 0.2 ---------------------------------------------------------------------- T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11514 SUBJECT: GRB110102A: Swift/UVOT observations DATE: 11/01/03 12:41:16 GMT FROM: Samantha Oates at MSSL S. R. Oates (MSSL-UCL) and M. De Pasquale (MSSL-UCL) report on behalf of the Swift-UVOT team The Swift/UVOT began settled observations of the field of GRB 110102A 156 s after the BAT trigger (Oates et al., GCN Circ. 11509). The optical afterglow is detected in the white, v, b and u filters at a refined UVO position RA(J2000)= 245.88087 deg, DEC(J2000) = 7.61383, which is: RA (J2000) = 16:23:31.41 Dec (J2000) = +07:36:49.8 with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence). This position is consistent with the enhanced XRT position (Goad et al., GCN Circ. 11510). The detection in u suggests a redshift of <2.5. Preliminary magnitudes using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for single and summed exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag/3sigUL ##################################################### wh (FC) 156 306 147 17.97 +/- 0.06 wh 868 1018 147 18.39 +/- 0.08 u (FC) 314 564 246 17.98 +/- 0.09 u 1122 1315 39 18.89 +/- 0.62 v 816 835 19 17.86 +/- 0.53 b 597 589 19 17.60 +/- 0.20 uvw1 693 6331 452 > 20.09 uvm2 668 6126 292 > 19.87 uvw2 619 7152 471 > 20.35 ##################################################### The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.08 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11515 SUBJECT: Konus-Wind observation of GRB 110102A DATE: 11/01/03 15:46:18 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long GRB 110102A, (Swift/BAT trigger=441454: Oates, et al., GCN 11509; Sakamoto et.al, GCN 11511) triggered Konus-Wind at T0=68074.462s UT (18:54:34.462) The burst light curve consists of three major pulses, first two of them are much harder than the third one. The total duration of the burst is ~160 s. The emission is seen up to ~5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB110102_T68074/ As observed by Konus-Wind the burst had a fluence of (5.4 ± 0.9)x10-5 erg/cm2, and a 256-ms peak flux, measured from T0+76.032s, of (4.9 ± 0.8)x10-6 erg/cm2/s (both in the 20 keV - 5 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+164.096 s) is best fit in the 20 keV - 5 MeV range by the GRB (Band) model, for which: the low-energy photon index alpha = -1.22 (-0.16, +0.26), the high energy photon index beta = -2.3 (< -0.9), the peak energy Ep = 267(-91, +111) keV, chi2 = 65/76 dof. The spectrum at the maximum count rate (measured from T0+73.984 to T0+82.176 s) is best fit in the 20 keV - 5 MeV range by the GRB (Band) model, for which: the low-energy photon index alpha = -1.14 (-0.12, +0.15), the high energy photon index beta = -2.2 (-3.1, +0.3), the peak energy Ep = 436(-122, +180) keV, chi2 = 57/76 dof. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11517 SUBJECT: GRB 110102A: Swift-XRT refined Analysis DATE: 11/01/04 03:05:00 GMT FROM: Valerio D'Elia at ASDC V. D'Elia, G. Stratta (ASDC) and S. R. Oates (MSSL-UCL) report on behalf of the Swift-XRT team: We have analysed 18.8 ks of XRT data for GRB 110102A (Oates et al., GCN Circ. 11509), from 139 s to 47.5 ks after the BAT trigger. The data comprise 400 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ 11510). The light curve shows an intital flaring activity, possibly associated to the prompt event, followed by a canonical steep-flat-steep behaviour, which can be modelled with double broken power-law decay. The initial decay index is alpha= 8.6. At T+450 (+/- 0.05) s the decay flattens to an alpha of 0.49 (+/-0.03). At T+11.38 (+/- 0.01) ks the decay steepens again to an alpha of 1.53 (+0.07 -0.09). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.48 (+/-0.04). The best-fitting absorption column is 7.8 (+/- 1) x 10^20 cm^-2, in excess of the Galactic value of 4.8 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.27 (+/-0.07) and a best-fitting absorption column of 1.28 (+/- 0.17) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (5.8 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 1.6, the count rate at T+48 hours will be 0.012 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x 10^-13 (7.0 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00441454. This circular is an official product of the Swift-XRT team. [GCN OPS NOTE(04jan11): Per author's request, the "4.3 x 10^-12 (2.1 x 10^-13)" in the 4th paragraph was changed to "4.3 x 10^-13 (7.0 x 10^-13)".]