//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11345 SUBJECT: GRB 101017A: Swift detection of a burst with optical counterpart DATE: 10/10/17 10:45:42 GMT FROM: David Palmer at LANL M. H. Siegel (PSU), J. M. Gelbord (PSU), D. Grupe (PSU), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), C. B. Markwardt (NASA/GSFC), P. T. O'Brien (U Leicester) and D. M. Palmer (LANL) report on behalf of the Swift Team: At 10:32:47 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 101017A (trigger=436429). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 291.378, -35.141 which is RA(J2000) = 19h 25m 31s Dec(J2000) = -35d 08' 26" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a complex series of peaks in a FRED envelope about 40 seconds long, with possible further emission out to T+100 seconds. The peak count rate was ~12000 counts/sec (15-350 keV), at ~3 sec after the trigger. The XRT began observing the field at 10:34:08.4 UT, 81.0 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 291.38546, -35.14513 which is equivalent to: RA(J2000) = 19h 25m 32.51s Dec(J2000) = -35d 08' 42.5" with an uncertainty of 3.9 arcseconds (radius, 90% containment). This location is 26 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 (7.69 x 10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.8 (+3.15/-2.65) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 8.79e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 88 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 19:25:32.56 = 291.38565 DEC(J2000) = -35:08:41.4 = -35.14482 with a 90%-confidence error radius of about 0.72 arc sec. This position is 2.7 arc sec. from the center of the XRT error circle. The estimated magnitude is 19.98 with a 1-sigma error of about 0.19. No correction has been made for the expected extinction corresponding to E(B-V) of 0.17. 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: 11346 SUBJECT: GRB 101017A: ROTSE-III Optical Limits DATE: 10/10/17 11:41:31 GMT FROM: Shashi Bhushan Pandey at ROTSE S. B. Pandey (U Mich), report on behalf of the ROTSE collaboration: ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded to GRB 101017A (Swift trigger 436429; M. H. Siegel et al. GCN 11345), producing images soon after the GCN notice time. We took 10 5-sec, 10 20-sec and 20 60-sec exposures. These unfiltered images are calibrated relative to USNO A2.0 (R). Comparison to the DSS (second epoch) reveals no new sources within the 3-sigma Swift/BAT error circle or at the UVOT position, for both single images and coadding into sets of 10. Individual images have limiting magnitudes ranging from 15.6-16.4; we set the following specific limits. start UT end UT t_exp(s) mlim t_start-tGRB(s) Coadd? -------------------------------------------------------------------- 10:34:55.2 10:35:15.2 20 16.4 127.8 N 10:37:49.3 10:42:31.6 282 17.5 301.9 Y //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11347 SUBJECT: GRB 101017A: Swift-BAT refined analysis DATE: 10/10/17 16:32:05 GMT FROM: Craig Markwardt at NASA/GSFC/UMD D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), 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-60 to T+240 sec from the recent telemetry downlink, we report further analysis of BAT GRB 101017A (trigger #436429) (Siegel, et al., GCN Circ. 11345). The BAT ground-calculated position is RA, Dec = 291.377, -35.141 deg which is RA(J2000) = 19h 25m 30.5s Dec(J2000) = -35d 08' 25.9" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 43%. The mask-weighted light curve resembles an overall FRED-like profile, starting at T-5 sec, peaking at T+2 sec, but with multiple shorter spikes superimposed. An extended tail is detectable out to at least T+160 sec. T90 (15-350 keV) is 70.0 +- 3.0 sec (estimated error including systematics). The time-averaged spectrum from T-5.5 to T+111 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.45 +- 0.03. The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+2.58 sec in the 15-150 keV band is 9.4 +- 0.4 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/436429/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11348 SUBJECT: GRB 101017A: Enhanced Swift-XRT position DATE: 10/10/17 17:59:49 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 1922 s of XRT Photon Counting mode data and 1 UVOT images for GRB 101017A, 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 = 291.38586, -35.14514 which is equivalent to: RA (J2000): 19h 25m 32.61s Dec (J2000): -35d 08' 42.5" with an uncertainty of 2.6 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: 11350 SUBJECT: Konus-Wind observation of GRB 101017A DATE: 10/10/18 07:50:50 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 101017A, (Swift/BAT trigger=436429: Siegel et.al, GCN 11345; Palmer et.al, GCN 11347) triggered Konus-Wind at T0=37961.692s UT (10:32:41.692) The burst light curve shows a jagged FRED-like structure with a total duration of ~45 s. The emission is seen up to 2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB101017_T37961/ As observed by Konus-Wind the burst had a fluence of (6.7 ± 0.4)x10-5 erg/cm2, and a 256-ms peak flux measured from T0+5.632s of (7.0 ± 0.9)x10-6 erg/cm2/s (both in the 20 keV - 2 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+40.448 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model, for which alpha = -1.18 ± 0.06, and Ep = 600(-45, +52) keV (chi2 = 66/58 dof). The spectrum at the maximum count rate (measured from T0+0.256 to T0+7.680 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model, for which alpha = -0.9 ± 0.1, and Ep = 742(-90, +113) keV (chi2 = 62/58 dof). All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11351 SUBJECT: GRB101017A: MITSuME Okayama optical upper limits DATE: 10/10/18 09:27:41 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 101017A (Siegel et al., GCN 11345) 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 2010-10-17 10:33:28 UT (~41 sec after the burst). We did not find any new point source within the enhanced XRT error circle (Goad et al., GCNC 11348) 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 ------------------------------------------------------ 0.01517 10:54:37 1800.0 >17.6 >17.9 >17.6 ------------------------------------------------------ T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11354 SUBJECT: GRB 101017A: Swift/UVOT Observations DATE: 10/10/18 14:20:49 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) reports on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 101017A 88s after the BAT trigger (Siegel et al., GCN Circ. 11345). The source reported by Siegel et al. is confirmed in the u and white filters but has not been detected since the first orbit. The 3-sigma upper limits for the finding chart (fc) and summed exposures are reported below: FILTER T_start(s) T_stop Exposure Mag/3uL ======================================================== white (fc) 88 238 147 19.85+-0.22 white 88 1724 409 20.09+-0.17 white 5660 7296 393 >21.03 v 630 1773 136 >18.81 v 6071 11723 1158 >19.93 b 556 1699 116 >19.66 b 5456 7091 393 >20.30 u 301 550 245 19.15+-0.23 u 301 1675 343 19.22+-0.20 u 5250 6886 393 >19.94 uvw1 679 1648 116 >19.22 uvw1 5046 13365 1112 >20.60 uvm2 654 1797 116 >19.08 uvm2 6276 12628 1082 >20.63 uvw2 605 1749 136 >19.52 uvw2 5866 7502 393 >20.22 ======================================================= The above magnitudes are not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0.17 (Schlegel et al., 1998, ApJS, 500, 525). The photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11355 SUBJECT: GRB 101017A: Swift XRT refined analysis DATE: 10/10/19 01:44:43 GMT FROM: Dirk Grupe at PSU/Swift-XRT D. Grupe and M. Siegel (PSU) report on behalf of the Swift-XRT team: We have analyzed 21.8 ks of XRT data for GRB 101017A (Siegel et al. GCN Circ. 11345), from 87 s to 82800 s after the BAT trigger. The data comprise 210 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The light curve can be modeled with a multiple broken power-law model. After an initial decay slope of 2.22+/-0.08 the light curve steepens at T_break=260+40-20 s with a slope of 3.85+1.13-0.34 and flattens again at T+527+52-69 s with a decay slope of 1.35+/-0.08. A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.38+/-0.06 and an absorption column density of 20.85+2.48-2.31 x 10^20 cm^-2 which is in excess of the Galactic column density of 7.69 x 10^20 cm^-2 (Kalberla et al. 2005). A fit to the pc mode data shows that the spectrum has steepened with a photon spectral index of 2.08+/-0.20. The absorption column density of this fit is consistent with the result from the WT data. The counts to 0.3-10 keV flux conversion factor deduced from the WT spectrum is 6.63 x 10^-11 and 7.70 x 10^-11 erg cm^-2 count^-1 for the observed and the absorption corrected count rates. For the pc mode we found conversion factors are 5.00 x 10^-11 and 7.57 x 10^-11 ergs cm^-2 counts^-1, respectively. If the light curve continues to decay with a power-law decay index of 1.35, the count rate at T+48 hours will be in the order of 3 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x 10^-14 (2.3 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00436429. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 11356 SUBJECT: GRB 101017A: miniTAO/ANIR NIR upper limits DATE: 10/10/19 05:34:13 GMT FROM: Takeo Minezaki at U.of Tokyo/Astro K. Motohara, T. Tanabe, S. Koshida, T. Morokuma, T. Minezaki, and Y. Yoshii (University of Tokyo) report on behalf of the TAO project team: We observed GRB 101017A (Siegel et al., GCN 11345) with the near-infrared camera ANIR mounted on the miniTAO 1.0m telescope at the University of Tokyo Atacama Observatory on the summit of Co. Chajnantor (5640 m altitude) in the northern Chile. The J- and Ks-band observations started from 2010-10-18 00:37 UT (14hours after the burst), and total exposure time was 300sec for each band. No object was detected within the enhanced XRT error circle (Goad et al., GCNC 11348). Three sigma upper limits are listed below, where the flux calibrations were carried out using 2MASS stars within the FoV. Band Mid-UT AB-Mag ---------------------------- Ks 00:40:25 >19.3 J 00:46:51 >19.9 ----------------------------