//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8462 SUBJECT: GRB 081102: Swift detection of a burst DATE: 08/11/02 18:10:16 GMT FROM: Scott Barthelmy at NASA/GSFC T. N. Ukwatta (GSFC/GWU), S. D. Barthelmy (GSFC), J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), C. Gronwall (PSU), C. Guidorzi (INAF-OAB), S. T. Holland (CRESST/USRA/GSFC), W.B Landsman (GSFC), V. Mangano (INAF-IASFPA), J. Mao (INAF-OAB), P. T. O'Brien (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU) and H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team: At 17:44:39 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 081102 (trigger=333427). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 331.182, +52.993 which is RA(J2000) = 22h 04m 44s Dec(J2000) = +52d 59' 36" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows multiple peaks with a duration of about 40 sec. The peak count rate was ~1800 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 17:46:11.5 UT, 92.0 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading uncatalogued X-ray source located at RA, Dec 331.17357, 52.99345 which is equivalent to: RA(J2000) = 22h 04m 41.66s Dec(J2000) = +52d 59' 36.4" with an uncertainty of 3.3 arcseconds (radius, 90% containment). This location is 18 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 consistent with the Galactic value of 4.95e+21 cm^-2 (Kalberla et al. 2005). The initial flux in the 2.5 s image was 2.85e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White (160-650 nm) filter starting 99 seconds after the BAT trigger. No afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers all of the XRT error circle. The image is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.81. Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 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: 8463 SUBJECT: GRB 081102: OPTIMA-Burst optical upper limit DATE: 08/11/02 21:32:24 GMT FROM: Alexander Stefanescu at MPE A. Stefanescu, N. Primak, F. Schrey, G. Kanbach, A. Slowikowska, H. Steinle, A. Updike and N. Lewandowski of the OPTIMA-Burst Team report the following: OPTIMA-Burst at the 1.3m Skinakas Observatory, of the University of Crete and the Foundation for Research and Technolgy -- Hellas observed the location of the XRT error-circle of GRB 081102 (GCN Circ 8462, T. N. Ukwatta et al.), starting at 2008-11-02 18:02:23 UT (~18 min after the burst). We did not detect any source inside the XRT error-circle in several co-added short (10-50s) white-light target acquisition frames taken under adverse conditions. Our limit is as follows: t-t_0 (mid-exp) t_exp limit (white light) 1276s 210s 18.5 Observations are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8464 SUBJECT: GRB 081102: MASTER VWF promt observation DATE: 08/11/02 22:34:37 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs MASTER-Net Team (http://observ.pereplet.ru): V. Lipunov, V.Kornilov, E.Gorbovskoy, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, I.Golubov Kislovodsk Solar Station of the Pulkovo observatory V.Krushinski, I.Zalognikh Ural State University, Kourovka S.Yazev, K.Ivanov Irkutsk State University MASTER Very Wide Field Camera located at Kislovodsk (2000 m) (http://apollo.sai.msu.ru/, D=50 mm, 4000 square degrees, 35'' per pix) has observed the Swift-BAT GRB081102 error box (Ukwatta et al., GCN Circ 8642) with 5s exposures starting before, during and after the GRB time. These unfiltered images are calibrated relative to USNO A2.0 (R). The limit of the each image is aboute 11.1 (S/N=3). The reduction is continuing. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8467 SUBJECT: GRB 081102: Enhanced Swift-XRT position DATE: 08/11/03 05:12:54 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 4108 s of XRT Photon Counting mode data and 2 UVOT images for GRB 081102, 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 = 331.1724, +52.9942 which is equivalent to: RA (J2000): 22h 04m 41.38s Dec (J2000): +52d 59' 39.3" with an uncertainty of 1.5 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 http://www.swift.ac.uk/xrt_positions/Goad.pdf), the current algorithm is an extension of this method. This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8468 SUBJECT: GRB 081102: Swift-BAT refined analysis DATE: 08/11/03 13:22:28 GMT FROM: Scott Barthelmy at NASA/GSFC E. E. Fenimore (LANL), 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/UMD), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), M. Stamatikos (GSFC/ORAU), 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 081102 (trigger #333427) (Ukwatta, et al., GCN Circ. 8462). The BAT ground-calculated position is RA, Dec = 331.178, 52.991 deg, which is RA(J2000) = 22h 04m 42.6s Dec(J2000) = +52d 59' 27.7" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 36%. The mask-weighted light curve shows two overlapping peaks, the first starting at ~T-20 sec, peaking at ~T-15 sec, and hitting a minimum between the two peaks at ~T-7 sec. The second peak peaks at ~T+1 sec, and returns to background at ~T+90 sec. T90 (15-350 keV) is 63 +- 16 sec (estimated error including systematics). The time-averaged spectrum from T-20.2 to T+62.8 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.73 +- 0.13. The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.08 sec in the 15-150 keV band is 1.4 +- 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/333427/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8469 SUBJECT: GRB 081102: Swift/UVOT refined analysis DATE: 08/11/03 15:13:14 GMT FROM: Stefan Immler at NASA/GSFC S. Immler (GSFC/CRESST/UMCP) and T. N. Ukwatta (GSFC/GWU) report on the behalf of the Swift UVOT team: The Swift Ultra-Violet/Optical Telescope (UVOT) began observing GRB 081102 (trigger 333427) 83 seconds after the BAT trigger (Ukwatta et al., GCN Circ. 8462). No afterglow is detected at the enhanced XRT position (Osborne et al., GCN Circ. 8467) in the initial v-filter finding chart or subsequent images. The limiting magnitudes (3-sigma in 3" radius apertures) in each of the UVOT filters are as follows: Filter T_start(s) T_stop(s) Exp(s) Mag UL (3sig) white 100 19051 1246 >21.9 v 83 35803 1423 >20.3 b 433 24833 1808 >21.3 u 408 30614 2717 >21.3 uvw1 383 29977 2922 >21.1 uvm2 359 36395 2701 >20.9 uvw2 309 34890 1434 >20.7 The values quoted above are in the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627). They are not corrected for the high (and unreliable) Galactic extinction at the low Galactic latitude of the burst of <5 degrees. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8470 SUBJECT: GRB 081102: Swift-XRT refined analysis DATE: 08/11/03 15:16:22 GMT FROM: Boris Sbarufatti at INAF-IASF-Pa V. Mangano, B. Sbarufatti, V. La Parola (INAF-IASF Pa), T. Ukwatta (GSFC/GWU) report on behalf of the Swift-XRT team: Swift-XRT began observing the field of GRB 081102 (trigger 333427, Ukwatta et al., GCN circ.8462) at 17:46:11.5 UT, 92.0 seconds after the BAT trigger. We analysed data from the first 10 orbits, consisting of 151 s in Windowed Timing mode, from T+98 s to T+251s and 14 ks in Photon Counting mode, from T+251s to T+42.1 ks. The lightcurve is best fit by a broken powerlaw model with slopes alpha_1 = -2.35 +/- 0.15 and alpha_2= -1.22 (-0.11 +0.22) and break time T_break = T+560 (-160 +500)s. After the break, we observe a strong flare at T+960 (-11+21) s with decay time 157 +/-15 s. The WT spectrum is best fit by a simple absorbed powerlaw with photon index 2.7 +/- 0.1 and an absorbing column consistent with the Galactic value of 4.9E21 cm^-2 (Kalberla et al. 2005). The observed (unabsorbed) flux in the 0.3 - 10 keV band is 4.0E-10 (1.3E-9) erg cm^-2 s^-1. The PC spectrum is best fit by a simple absorbed powerlaw with photon index 1.97 +/- 0.1 and an absorbing column consistent with the Galactic value. The observed (unabsorbed) flux in the 0.3 - 10 keV band is 1.1 (1.8)E-11 erg cm^-2 s^-1. The countrate to flux conversion factor is 7.1E-11. The predicted countrate for November 3, 17:45 UT (T+ 24h) is 1.3E-3 counts/s equivalent to a flux of 9.2E-14 erg cm^-2 s^-1. All quoted errors are at 90% confidence level. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8471 SUBJECT: GRB 081102: MASTER prompt optical limit DATE: 08/11/03 20:06:42 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs MASTER-Net Team (http://observ.pereplet.ru): V. Lipunov, V.Kornilov, E.Gorbovskoy, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.Parkhomenko Kislovodsk Solar Station of the Pulkovo observatory V.Krushinski, I.Zalognikh Ural State University, Kourovka S.Yazev, K.Ivanov Irkutsk State University MASTER Very Wide Field Camera located at Kislovodsk (2000 m) (http://apollo.sai.msu.ru/, D=50 mm, 4x1000 square degrees, 35'' per pix) has observed the Swift-BAT GRB081102 error box (Ukwatta et al., GCN Circ 8642) with 5s exposures during all night without windows between images. There are two separeted (~702m) mount with double cameras. Now we present results from North camera. These unfiltered images are calibrated relative to Tycho stars (V). We do not detect any new source at the XRT position reported in GCN Circ. 8467 ( Osborne et al.) brighter than 12.4 mag before and after trigger time. The photometry results +-4 min around trigger time: T-T_trigger m_lim (S/N=3) Exposure Coadd -255s... 0... 255 s 11.6 5s no -2min...0...+2 min 12.2 30s 6 -2min...0...+2 min 12.4 60s 12 The optical fluence during the 60s-GRburst is limited by <= 6x10_-9 erg/cm_2 including 2.5 magnitude absorbtion (Ukwatta et al., Circ 8462). The BAT-fluence is aboute 3 10_-6 erg/cm_2 (15-150 Kev) (http://gcn.gsfc.nasa.gov/notices_s/333427/BA/). So Optical Fluence/Gamma-Fluence ~ < 1/500 Same ratio for GRB080319B is ~ 1/200 (Naked Eye GRB). The light curve is available at http://observ.pereplet.ru/images/GRB081102/lc1.png The video are available at http://observ.pereplet.ru/images/GRB081102/grb.gif You can see 200 sets. Note: the GRB was at the edge of the FOW. The reduction is continuing. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8476 SUBJECT: Fermi Detection of GRB 081102 DATE: 08/11/04 16:32:24 GMT FROM: Chryssa Kouveliotou at MSFC C. Kouveliotou (NASA/MSFC) and M.S. Briggs (UAHuntsville) report on behalf of the Fermi GBM Team: At 17:44:21.6 UT on 02 November 2008, the Fermi GBM triggered and located an event (trigger 247340662 / 081102739) which was also seen by SWIFT (Ukwata et al. 2008, GCN 8462). The GBM on-ground location is consistent with the Swift position; the GBM trigger time is 17.4 s earlier than the Swift trigger. The GBM light curve shows a multiple peak event (three and possibly four peaks) with T90= 88 s (50-300 keV). The time-averaged spectrum from T0-2.048 s to T0+46.01 s is best fit by a exponentially cutoff power law model with Epeak = 88.7 +/- 8.3 keV, and index 0.0 +/- 0.3 (chi squared 278 for 238 d.o.f.). The event fluence (50-300 keV) in this time interval is (2.1 +/- 0.05)E-06 erg/cm^2. A Band function fit the spectrum equally well (chi squared 276 for 237 d.o.f.) with Epeak=72 +/- 13, alpha = 0.44 +/- 0.58 and beta = -2.36 +/- 0.32. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8496 SUBJECT: GRB 081102B: Fermi GBM detection DATE: 08/11/07 17:26:42 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) and E. Bissaldi (MPE) report on behalf of the Fermi GBM Team: "At 08:45:00.51 UT on 02 November 2008, the Fermi GBM triggered and located GRB 081102B (trigger 247308301/ 081102365). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 231.2, Dec = 35.2 (J2000 degrees, equivalent to J2000 15h 25m, 35d 12'), with a statistical uncertainty of 6.1 degrees (radius, 1-sigma containment; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 53 degrees. The GBM light curve shows a double peak with a duration (T90) of about 2.2 s (8-1000 keV). The time-averaged spectrum from T0-0.226 s to T0+0.798 s (first peak) is well fit by a simple power law function with index -1.07 +/- 0.06 (chi squared 247 for 243 d.o.f.). The event fluence (8-1000 keV) in the same time interval is (1.12 +/- 0.04)E-06 erg/cm^2. The 1-sec photon flux measured starting from T0-0.226 s in the 8-1000 keV band is 3.68 +/- 0.14 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: 8516 SUBJECT: GRB 081102: MASTER refind and final results DATE: 08/11/11 15:50:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.Parkhomenko Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalognikh Ural State University, Kourovka S.Yazev, K.Ivanov Irkutsk State University Two of the four MASTER Very Wide Field Cameras located at Kislovodsk (http://apollo.sai.msu.ru/, D=50 mm, 4x1000 square degrees, 35'' per pix) has observed the Swift-BAT GRB081102 error box (Mangano et al., GCN Circ 8470, Lipunov et al., GCN 8464, 8471) with 5s exposures during all night without time gap between images. There are two separeted (~702m) mount with double cameras. Now we present results from the North and South mounts. These unfiltered images are calibrated relative to Tycho stars (V). We do not detect any new source at the XRT position reported in GCN Circ. 8470 (Mangano et al.) brighter than 13.0 mag before and after trigger time. The photometry results +-4 min around trigger time: T-T_trigger m_lim (S/N=3) Exposure Coadd -255s... 0... 255 s 11.8 5s yes -2min...0...+2 min 12.7 2x30s 12 -2min...0...+2 min 13.0 2x60s 24 The optical fluence during the 40s-GRBurst is limited by <= 1.6x10_-8 erg/cm_2 including 2.8 magnitude absorbtion (Ukwatta et al., Circ 8462). The BAT-fluence is aboute 2.3x10_-6 erg/cm_2 (15-150 keV) (Fenimore et al., GCN 8468). So: Optical Fluence/Gamma-Fluence(15-150keV) ~ < 1/140 Same ratio for GRB080319B is ~ 1/25 (Naked Eye GRB) in 15-150 keV (Racusin, Karpov et al., Nature, vol.455, 183, 2008). Scientific Master Team Report are available at http://observ.pereplet.ru/images/GRB081102/grb_film.html Note: the GRB was at the edge of the FOW in both cameras. The message may be cited. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 8520 SUBJECT: GRB 081102: RTT150 Optical observations DATE: 08/11/13 18:30:53 GMT FROM: Irek Khamitov at TUG I. Khamitov, M.Parmaksizoglu (TUG), S.Alis, M.Hudaverdi (Istambul Uni.), Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.), R. Burenin, M. Pavlinsky, R. Sunyaev (IKI), I. Bikmaev, N. Sakhibullin (KSU/AST) report: We observed the field of the Swift-BAT GRB 081102 (Ukwatta et al., GCN8462) with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey), starting at 03 Nov, 17:44 UT, i.e. approximately 24.0 hours after the burst, using TFOSC CCD. We made 3x300s exposures in R-band. We do not detect any new source inside the XRT error circle (Osborne et al., GCN8467). Using USNO-B1 stars we estimated the limiting magnitude of combined image as m_R ~ 22. -- This message has been scanned for viruses and dangerous content by MailScanner, and is believed to be clean.