//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12578 SUBJECT: GRB 111121A: Swift detection of a short hard burst DATE: 11/11/21 16:43:39 GMT FROM: Scott Barthelmy at NASA/GSFC V. D'Elia (ASDC), S. D. Barthelmy (GSFC), A. P. Beardmore (U Leicester), D. N. Burrows (PSU), S. Campana (INAF-OAB), M. M. Chester (PSU), N. Gehrels (NASA/GSFC), B. Gendre (ASDC), C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL), V. Mangano (INAF-IASFPA), C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA), T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC), R. L. C. Starling (U Leicester), G. Stratta (ASDC), C. A. Swenson (PSU), E. Troja (NASA/GSFC/ORAU), T. N. Ukwatta (MSU) and B.-B. Zhang (PSU) report on behalf of the Swift Team: At 16:26:24 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 111121A (trigger=508161). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 154.751, -46.637 which is RA(J2000) = 10h 19m 00s Dec(J2000) = -46d 38' 13" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single spike with a duration of about 1 sec. The peak count rate was ~38000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 16:27:41.3 UT, 76.9 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 154.7612, -46.6709 which is equivalent to: RA(J2000) = 10h 19m 2.68s Dec(J2000) = -46d 40' 15.1" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 124 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 (1.20 x 10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4 (+2.62/-2.25) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 4.58e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 85 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 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18.0 mag.No correction has been made for the expected extinction corresponding to E(B-V) of 0.26. We note that the XRT centroid is close to a known 14th magnitude star, which may complicate the analysis. Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 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: 12579 SUBJECT: GRB 111121A: Enhanced Swift-XRT position DATE: 11/11/21 21:22:07 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 2196 s of XRT Photon Counting mode data and 4 UVOT images for GRB 111121A, 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 = 154.76137, -46.67064 which is equivalent to: RA (J2000): 10h 19m 2.73s Dec (J2000): -46d 40' 14.3" with an uncertainty of 1.8 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: 12581 SUBJECT: GRB 111121A: Swift-BAT refined analysis DATE: 11/11/22 01:15:03 GMT FROM: Scott Barthelmy at NASA/GSFC J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), J. Norris (BSU), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), 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 recent telemetry downlinks, we report further analysis of BAT GRB 111121A (trigger #508161) (D'Elia, et al., GCN Circ. 12578). The BAT ground-calculated position is RA, Dec = 154.746, -46.670 deg, which is RA(J2000) = 10h 18m 59.1s Dec(J2000) = -46d 40' 10.7" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 64%. The mask-weighted light curve shows an inital strong pulse composed of two overlapping peaks, the first starting at ~T-0.3 sec and peaking at ~T+0.17 sec (at 2.6 cnts/det/sec). The second peaks at ~T+0.3 sec and is done by ~T+0.6 sec. This is followed by two episodes of extended emission. The first is roughly constant (~0.02 to 0.03 cnts/det/sec) out to ~T+65sec. The second episode is ~0.006 cnts/det/sec out to ~T+130 sec. T90 (15-350 keV) is 119 +- 16 sec (estimated error including systematics). This T90 includes the extended emission. The spectral lag is 10.2 ms +2.6-1.8 ms (for the 100-350 to 25-50 keV band) and 12.7 ms +6.8-8.7 ms (for the 50-100 to 15-25 keV band). This puts it on the long end of the distribution for spectral lag for short GRBs. The time-averaged spectrum from T-0.34 to T+141.08 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.66 +- 0.12. The fluence in the 15-150 keV band is 2.2 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.26 sec in the 15-150 keV band is 7.1 +- 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/508161/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12582 SUBJECT: GRB 111121A: Swift-XRT refined Analysis DATE: 11/11/22 04:43:03 GMT FROM: Phil Evans at U of Leicester B. Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC), M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), P.A. Evans (U. Leicester), O.M. Littlejohns (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB) and V.D'Elia report on behalf of the Swift-XRT team: We have analysed 10 ks of XRT data for GRB 111121A (D'Elia et al. GCN Circ. 12578), from 66 s to 24.1 ks after the BAT trigger. The data comprise 180 s in Windowed Timing (WT) mode (the first 9 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 Evans et al. (GCN. Circ 12579). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=1.85 (+/-0.09). At T+217 s the decay steepens to an alpha of 3.7 (+1.2, -0.7). The light curve breaks again at T+378 s to a decay with alpha=0.93 (+0.07, -0.08), before a final break at T+9772 s s after which the decay index is 2.1 (+0.5, -0.4). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.71 (+/-0.08). The best-fitting absorption column is 4.2 (+/-0.4) x 10^21 cm^-2, in excess of the Galactic value of 1.2 x 10^21 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 1.88 (+0.15, -0.17) and a best-fitting absorption column of 3.4 (+/-0.7) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.6 x 10^-11 (6.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.4 (+/-0.7) x 10^21 cm^-2 Galactic foreground: 1.2 x 10^21 cm^-2 Excess significance: 8.0 sigma Photon index: 1.88 (+0.15, -0.17) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00508161. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12583 SUBJECT: GRB 111121A: Magellan/Megacam observations DATE: 11/11/22 12:58:18 GMT FROM: Edo Berger at Harvard W. Fong (Harvard), A. Seth (U. Utah), R. Chornock and E. Berger (Harvard) report: "We imaged the field of the short GRB 111121A (GCN 12578) with Megacam on the Magellan/Clay 6.5-m telescope at a mid-time of 2011 November 22.27 UT (13.9 hours post-burst). We obtained 25x30-sec exposures in r-band at an airmass of 1.7 in ~0.7" seeing. The location of the latest enhanced XRT error circle (improved from GCN 12579 at http://www.swift.ac.uk/xrt_positions/ with RA(J2000) = 10:19:02.71, Dec(J2000) = -46:40:14.5, 1.4" uncertainty) is contaminated by emission from a nearby bright (R~12.5) star. However, we find a faint source on the southern edge of the XRT circle at (J2000): RA = 10:19:02.7 Dec = -46:40:15.6, with an uncertainty of ~0.5" in each coordinate that includes contributions from the centroiding error of the source and a 0.27" rms uncertainty from the astrometric tie to USNO-B. Due to the location of the source near a diffraction spike from the bright star, it is unclear at present whether it is extended or point-like. Additional analysis to extract a magnitude for the source is on-going, and additional observations to check for variability are planned." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12584 SUBJECT: GRB 111121A: Swift/UVOT Upper Limits DATE: 11/11/22 14:39:55 GMT FROM: Paul Kuin at MSSL N.P.M. Kuin, S. Oates (MSSL-UCL) and V. D'Elia (ASDC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 111121A 86 s after the BAT trigger (D'Elia et al., GCN Circ. 12578). No optical afterglow consistent with the XRT position (Evans et al, GCN Circ. 12579) is detected in the initial UVOT exposures. The XRT enhanced position falls within the PSF wings of a B~13.6 magnitude star. Inspection of the event mode data after correction for a slight wander in attitude shows no evidence for any transient source. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are dominated by the nearly star and are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 86 235 147 >14.8 u_FC 298 548 246 >15.5 white 86 990 296 >14.7 v 629 822 39 >13.1 b 554 748 39 >14.2 u 298 723 265 >15.5 w1 678 873 39 >16.5 m2 653 847 39 >18.5 w2 604 797 39 >17.9 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.26 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12585 SUBJECT: Konus-Wind observation of GRB 111121A DATE: 11/11/23 12:26:06 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 short hard intense GRB 111121A (Swift-BAT trigger #508161: D'Elia et al., GCN 12578; Cummings et al., GCN 12581) triggered Konus-Wind at T0=59182.640s UT (16:26:22.640) The light curve shows of a hard bright pulse with a total duration of ~600 ms followed by a tail of a weak soft extended emission for at 20 s. The emission is seen up to ~10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB111121_T59182/ As observed by Konus-Wind the burst had a fluence of (2.3 ± 0.3)x10-5 erg/cm2, and a 16-ms peak flux, measured from T0+0.160 s, of (8.4 ± 1.5)x10-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The spectrum of the burst (measured from T0 to T0+0.256 s) is best fitted in the 20 keV - 10 MeV range with the GRB (Band) model, for which: the low-energy photon index alpha = -0.44 (-0.07, +0.07), the high energy photon index beta = -3.0 (<-2.4), the peak energy Ep = 1780(-290, +310) keV, chi2 = 59.7/51 dof. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 12607 SUBJECT: GRB 111121A: Suzaku WAM observation of the prompt emission DATE: 11/12/01 10:39:34 GMT FROM: Yuji Urata at Nat. Central U. C-J. Chuang, Y. Urata, P. Tsai (NCU), Y. Hanabata, T. Uehara, T. Takahashi, M. Mizuno, M. Ohno, Y. Fukazawa (Hiroshima U.), T. Yasuda, Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, M. Asahina, S. Kobayashi, A. Sakamoto (Saitama U.), S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa (Waseda U.), N. Ohmori, M. Akiyama, M. Yamauchi (Univ. of Miyazaki), K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The bright short GRB 111121A (Swift/BAT trigger 508161 ; D'Elia et al., GCN 12578) was detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 16:26:24.488 UT (=T0). The observed light curve shows a single peak structure starting at T0, ending at T0+1 s with a duration (T90) of about 0.45 seconds. The fluence in 100 - 1000 keV was 4.29(-0.41, 0.23) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+1 s was 20.26 photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0 to T0+1 s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 0.58 (-0.19, 0.18), and Epeak 1678.97 (-210.66, 300.31) keV (chi^2/d.o.f. = 60.1/47). 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