//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18659 SUBJECT: GRB 151205B: Swift detection of a burst DATE: 15/12/05 21:51:08 GMT FROM: David Palmer at LANL F. E. Marshall (NASA/GSFC), P. D'Avanzo (INAF-OAB), C. Gronwall (PSU), L. M. Z. Hagen (PSU), H. A. Krimm (CRESST/GSFC/USRA), A. Melandri (INAF-OAB), D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the Swift Team: At 21:43:14 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 151205B (trigger=666378). Swift could not slew immediately to the burst due to an observing contraint. The BAT on-board calculated location is RA, Dec 41.158, -43.481 which is RA(J2000) = 02h 44m 38s Dec(J2000) = -43d 28' 49" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 5 sec. The peak count rate was ~1800 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to an observing constraint, Swift will not slew until T0+50.6 minutes. There will be no XRT or UVOT data until this time. Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.nasa.gov). 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: 18661 SUBJECT: GRB 151205B: Swift-XRT observations DATE: 15/12/05 23:07:32 GMT FROM: Phil Evans at U of Leicester J.A. Kennea (PSU), G. Tagliaferri (INAF-OAB), S. Campana (INAF-OAB), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and D.N. Burrows (PSU) report on behalf of the Swift-XRT team: The XRT began observing the field of GRB 151205B at 22:35:21.5 UT, 3127.1 seconds after the BAT trigger. No source was detected in 245 s of promptly downlinked data. We are waiting for the full dataset to detect and localise the XRT counterpart. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18662 SUBJECT: GRB151205B: Initial UVOT observations DATE: 15/12/05 23:09:33 GMT FROM: Lea Hagen at PSU L. M. Z. Hagen (PSU) reports on behalf of the Swift/UVOT team: UVOT took a finding chart exposure of 150 seconds with the White filter starting 3131 seconds after the BAT trigger (Marshall et al., GCN Circ. 18659). No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the BAT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02. [GCN OPS NOTE(20jan16): Per author's request, the burst name in the Subject-line was changed from "A" to "B".] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18665 SUBJECT: GRB 151205B: MASTER-NET early optical observations DATE: 15/12/06 00:26:57 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov, P.Balanutsa, A.Kuznetsov, D.Kuvshinov, Lomonosov Moscow State University, Sternberg Astronomical Institute D.Buckley, S. Potter, A.Kniazev, M.Kotze South African Astronomical Observatory K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk 21:43:14.53 V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres The Instituto de Astrofisica de Canarias MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in SAAO was pointed to the GRB151205B (Marshall et. al. GCN 18659) 28 sec after notice time and 63 sec after trigger time at 21:44:18 UT in two polarisations. On our first (10s exposure) set we haven`t found optical transient within SWIFT error-box (ra=02 44 38 dec=-43 28 50 r=0.050000). The 5-sigma upper limit has been about 17.0 mag. We obtain a following early upper limits at a single an coadd images T_start T-Ts T-Tm Expt. Mlimit Coadd --------|----|-----|-----|-------|-------| 21:44:18 63 68 10 17.0 1 21:44:18 63 115 60 18.7 3 21:44:18 63 501 680 20.6 10 21:44:51 96 106 20 17.8 1 21:45:32 137 152 30 18.1 1 21:46:21 187 207 40 18.3 1 21:47:21 246 271 50 18.7 1 21:48:31 316 346 60 19.0 1 21:49:51 396 436 80 19.3 1 21:51:47 513 563 100 19.6 1 21:53:45 630 695 130 19.9 1 21:56:13 778 858 160 20.0 1 ... Ts - is exposure start time Tm - is exposure middle time T - is trigger time The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18670 SUBJECT: GRB 151205B, Swift-BAT refined analysis DATE: 15/12/06 17:03:30 GMT FROM: Hans Krimm at NASA-GSFC T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),H. A. Krimm (GSFC/USRA),A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), F. E. Marshall (NASA/GSFC),D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 15120B (trigger #666378) (Marshall, et al., GCN Circ. 18659). The BAT ground-calculated position is RA, Dec = 41.190, -43.461 deg which is RA(J2000) = 02h 44m 45.6s Dec(J2000) = -43d 27' 39.8" with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 96%. The mask-weighted light curve shows a single peak starting at T-2 sec with total duration of ~5 seconds. The spacecraft slewed away from the burst location at about T+350 seconds. T90 (15-350 keV) is 1.4 +- 0.2 sec (estimated error including systematics). The time-averaged spectrum from T-0.2 to T+1.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.74 +- 0.33. The fluence in the 15-150 keV band is 7.7 +- 1.6 x 10^-8erg/cm2. The 1-sec peak photon flux measured from T+0.25 sec in the 15-150 keV band is 0.7 +- 0.2 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/666378/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18672 SUBJECT: GRB 151205B: further Swift-XRT observations DATE: 15/12/06 23:59:28 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Melandri (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), L.M. McCauley (PSU), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani (U. Leicester), A. Maselli (INAF-IASFPA), F. E. Marshall (NASA/GSFC) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 3.3 ks of Photon Counting (PC) mode XRT data for the Swift/BAT-detected burst GRB 151205B (Marshall et al. GCN Circ. 18659), collected between T0+3.1 ks and T0+68.9 ks. The first set of observations consists of 1.0 ks of data collected between T0+3.1 ks and T0+5.7 ks. No X-ray sources have been detected inside or close to the Swift/BAT error region. The 3-sigma upper limit in the field is 7.7e-3 ct s^-1, corresponding to a 0.3-10 keV observed flux of 2.7e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum). The second set of observations consists of 2.3 ks data collected between T0+39.8 ks and T0+68.9 ks. No X-ray sources have been detected inside or close to the Swift/BAT error region. The 3-sigma upper limit in the field is 3.7e-3 ct s^-1, corresponding to a 0.3-10 keV observed flux of 1.3e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum). The results of the XRT-team automatic analysis of the XRT observations, including a position specific upper limit calculator, are available at http://www.swift.ac.uk/ToO_GRBs/00666378. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18674 SUBJECT: GRB 151205B: Deep GROND Upper limits DATE: 15/12/08 22:02:39 GMT FROM: Alexander Kann at TLS Tautenburg R. Yates (MPE Garching) , D. A. Kann (TLS Tautenburg), C. Delvaux, and J. Greiner (both MPE Garching) report on behalf of the GROND team: We observed the field of GRB 151205B (Swift trigger 666378; Marshall et al., GCN #18659) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 01:21 UT on 06/12/2015, 3hrs 38 mins after the GRB trigger, and continued for several hours. We obtained a second epoch in the following night. We stacked the four deepest images of the first night (exposure times 7920 s in g'r'i'z' and 6600 s in JHK). They were performed at an average seeing of 0".77 and an average airmass of 1.04. The observations of the second night (exposure times 5760 s in g'r'i'z' and 5400 s in JHK) were obtained at 0".62 seeing and airmass 1.04. As there is no XRT detection for this GRB (Kennea et al., GCN #18661; D'Avanzo et al., GCN #18672), we performed image subtraction. We note that the g'r'i'z' images do not cover about 25% of the revised BAT error circle (Ukwatta et al., GCN #18670) to the north and east. The JHK images cover both the flight and the revised BAT error circle completely. No significantly variable sources are detected in any band. The formal upper limits (all in AB system) of our images, centered at 0.1939 days after the GRB, are: g' > 26.5 mag, r' > 26.5 mag, i' > 25.6 mag, z' > 25.0 mag, J > 22.7 mag, H > 22.2 mag, and K > 21.3 mag. The given limits are derived based on calibrating the images against GROND zero points and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.02 in the direction of the burst (Schlegel et al. 1998).