//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18657 SUBJECT: GRB 151205A: Swift detection of a burst DATE: 15/12/05 16:01:30 GMT FROM: Scott Barthelmy at NASA/GSFC J. R. Cummings (NASA/UMBC), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), P. D'Avanzo (INAF-OAB), C. Gronwall (PSU), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the Swift Team: At 15:46:00 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 151205A (trigger=666352). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 229.282, +35.769, which is RA(J2000) = 15h 17m 08s Dec(J2000) = +35d 46' 09" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a couple overlapping peaks with a total duration of about 25 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 15:47:32.7 UT, 91.8 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 229.2892, 35.7439 which is equivalent to: RA(J2000) = 15h 17m 09.41s Dec(J2000) = +35d 44' 38.0" with an uncertainty of 2.3 arcseconds (radius, 90% containment). This location is 92 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 (1.58 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.7 (+3.55/-2.93) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 1.31e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 100 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 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 XRT 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. Burst Advocate for this burst is J. R. Cummings (jayc 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: 18658 SUBJECT: GRB 151205A: Enhanced Swift-XRT position DATE: 15/12/05 20:26:56 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 2174 s of XRT Photon Counting mode data and 3 UVOT images for GRB 151205A, 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 = 229.28861, +35.74392 which is equivalent to: RA (J2000): 15h 17m 9.27s Dec (J2000): +35d 44' 38.1" 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: 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: 18660 SUBJECT: GRB 151205A: Swift/UVOT Upper Limits DATE: 15/12/05 23:00:57 GMT FROM: Lea Hagen at PSU L. M. Z. Hagen (PSU) and J. R. Cummings (NASA/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 151205A 101 s after the BAT trigger (Cummings et al., GCN Circ. 18657). No optical afterglow consistent with the XRT position (Osborne et al. GCN Circ. 18658) is detected in the initial UVOT exposures. 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: Filter T_start(s) T_stop(s) Exp(s) Mag white 101 5796 383 >21.15 v 590 6207 236 >19.25 b 514 5591 236 >20.14 u 259 6713 552 >20.21 w1 639 6617 413 >20.10 m2 4776 6412 393 >20.07 w2 565 6002 236 >19.95 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// 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: 18663 SUBJECT: GRB 151205A: Garching Telescope Upper Limit DATE: 15/12/05 23:49:31 GMT FROM: Alexander Kann at TLS Tautenburg T. Schweyer (MPE Garching) and D. A. Kann (TLS Tautenburg) report on behalf of the GROND team: We observed the field of GRB 151205A (Swift trigger 666352; J. R. Cummings et al., GCN #18657) with the Garching 0.6m telescope. Observations started at 16:24:57 UT on 2015-12-05, about 39 min after the GRB trigger. They were performed at an average airmass of 3.4 during evening twilight. We obtained 6 images of 180s exposure time in R (for a total exposure time of 18 min) with the midtime at 16:35:18 UT (MJD=57361.691180). We do not detect a source within the 1".8 enhanced XRT error circle (J. P. Osborne et al., GCN #18658), down to a limiting magnitude of R(AB) > 19.4 mag. The R band is calibrated against SDSS DR8. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18664 SUBJECT: GRB 151205A: Fermi GBM detection DATE: 15/12/06 00:08:29 GMT FROM: Matthew Stanbro at UAH/Fermi Matthew Stanbro (UAH) reports on behalf of the Fermi GBM Team: "At 15:46:01.90 UT on 05 December 2015, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 151205A (trigger 471023165 / 151205657) which was also detected by the Swift/BAT (Cummings et al. 2015, GCN 18657). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 76 degrees. The GBM light curve consists of several episodes with a duration (T90) of about 56 s (50-300 keV). The time-averaged spectrum from T0-2.05 s to T0+55.30 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is 1.06 +/- 0.48 and the cutoff energy, parameterized as Epeak, is 153 +/- 12 keV The event fluence (10-1000 keV) in this time interval is (2.56 +/- 0.21)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-1.34 s in the 10-1000 keV band is 1.36 +/- 0.15 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." -- Matthew C. Stanbro Fermi GBM Graduate Research Assistant University of Alabama in Huntsville //////////////////////////////////////////////////////////////////////// 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: 18666 SUBJECT: GRB 151205C: MAXI/GSC detection DATE: 15/12/06 01:51:18 GMT FROM: H. Negoro at Nihon U. GRB 151205C: MAXI/GSC detection M. Nakajima, H. Negoro (Nihon U.), M. Serino (RIKEN), T. Sakamoto (AGU), S. Nakahira, S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Kawai, M. Arimoto, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara (Tokyo Tech), A. Yoshida, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, R. Imatani (Osaka U.), K. Tanaka, T. Masumitsu (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto (Kyoto U.), Y. Tsuboi, S. Kanetou, Y. Nakamura, R. Sasaki (Chuo U.), M. Yamauchi, D. Itoh (Miyazaki U.), K. Yamaoka (Nagoya U.), M. Morii (ISM) report on behalf of the MAXI team: The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at UT 2015/12/05 23:54:06. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (329.725 deg, 77.705 deg) = (21 58 54, +77 42 17) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.24 deg and 0.2 deg, respectively. The roll angle of long axis from the north direction is 102.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged over the scan was 152 +- 24 mCrab (4-10keV, 1 sigma error). Without assumptions on the source constancy, we obtain a rectangular error box for the transient source with the following corners: (326.621 deg, 76.996 deg) = (21 46 29, +76 59 46) (J2000) (328.465 deg, 76.767 deg) = (21 53 51, +76 46 02) (J2000) (333.174 deg, 78.383 deg) = (22 12 41, +78 23 00) (J2000) (331.143 deg, 78.636 deg) = (22 04 34, +78 38 08) (J2000) There was no significant excess flux in the previous transit at UT 22:21 and in the next transit at 12/6 01:26 UT with an upper limit of 20 mCrab for each. Detection Information: http://maxi.riken.jp/alert/novae/7361767105/7361767105.htm //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18667 SUBJECT: GRB 151205C: Tiled Swift observations DATE: 15/12/06 03:09:15 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the MAXI GRB 151205C. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00049 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the MAXI event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18668 SUBJECT: GRB 151205A, Swift-BAT refined analysis DATE: 15/12/06 05:09:17 GMT FROM: Scott Barthelmy at NASA/GSFC M. Stamatikos (OSU), 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), D. M. Palmer (LANL), T. Sakamoto (AGU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-315 to T+934 sec from the recent telemetry downlinks, we report further analysis of BAT GRB 151205A (trigger #666352) (Cummings, et al., GCN Circ. 18657). The BAT ground-calculated position is RA, Dec = 229.291, 35.767 deg, which is RA(J2000) = 15h 17m 09.7s Dec(J2000) = +35d 46' 01.7" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 93%. The mask-weighted light curve shows several overlapping peaks starting at ~T-10 sec, peaking at ~T+3 sec, with a long tail out to T+170 sec. T90 (15-350 keV) is 62.8 +- 12.3 sec (estimated error including systematics). The time-averaged spectrum from T-4.0 to T+69.5 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.17 +- 0.13. The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+1.98 sec in the 15-150 keV band is 0.6 +- 0.1 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/666352/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18669 SUBJECT: GRB 151205A: Swift-XRT refined Analysis DATE: 15/12/06 16:01:04 GMT FROM: Phil Evans at U of Leicester B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB) and J.R. Cummings report on behalf of the Swift-XRT team: We have analysed 7.1 ks of XRT data for GRB 151205A (Cummings et al. GCN Circ. 18657), from 81 s to 18.6 ks after the BAT trigger. The data comprise 133 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 Osborne et al. (GCN Circ. 18658). The light curve can be modelled with an initial power-law decay with an index of alpha=0.3 (+/-0.4), followed by a break at T+131 s to an alpha of 1.73 (+0.07, -0.06). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.23 (+0.14, -0.13). The best-fitting absorption column is 5.6 (+1.5, -1.3) x 10^21 cm^-2, in excess of the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.90 (+0.31, -0.29) and a best-fitting absorption column of 7.4 (+2.5, -2.1) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.7 x 10^-11 (7.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 7.4 (+2.5, -2.1) x 10^21 cm^-2 Galactic foreground: 1.6 x 10^20 cm^-2 Excess significance: 5.6 sigma Photon index: 1.90 (+0.31, -0.29) If the light curve continues to decay with a power-law decay index of 1.73, the count rate at T+24 hours will be 2.1 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.9 x 10^-15 (1.6 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/00666352. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// 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: 18671 SUBJECT: GRB 151205C: Swift-XRT observations DATE: 15/12/06 22:48:06 GMT FROM: Andrea Melandri at INAF-OAB A. Melandri, P. D'Avanzo (INAF-OAB) A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), K.L. Page (U. Leicester), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), A. Maselli (INAF-IASFPA) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the MAXI-detected burst GRB 151205C (Nakajima et al. GCN Circ. 18666) in a series of observations tiled on the sky. The total exposure time is 2.5 ks, distributed over 7 tiles; the maximum exposure at a single sky location was 790 s. The data were collected between T0+11.1 ks and T0+22.8 ks, and are entirely in Photon Counting (PC) mode. No X-ray sources have been detected. The 3-sigma upper limit in the field (not including the regions where the tiles overlap) ranges from ~0.02 to ~0.03 ct s^-1, corresponding to a 0.3-10 keV observed flux of 7.6e-13 to 1.1e-12 erg cm^-2 s^-1 (assuming a typical GRB spectrum). The results of the XRT-team automatic analysis of the tiled XRT observations, including a position-specific upper limit calculator, are available at http://www.swift.ac.uk/xrt_products/TILED_GRB00049. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// 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). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18676 SUBJECT: GRB 151205A: Khureltogot upper limit DATE: 15/12/09 10:19:21 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), S. Schmalz (AIP), E. Mazaeva (IKI), N. Tungalag (Research Center of Astronomy and Geophysics MAS), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of Swift GRB 151205A (Cummings et al., GCN 18657) with ORI-40 telescope of Khureltogot observatory starting on Dec., 5 (UT) 20:49:25, i.e. ~6 hours after the burst trigger. We do not detect any object within enhanced XRT error circle (Osborne et al., GCN 18658). Photometry of the field is following Date UT start t-T0 Filter Exp. Upper_Limit (3sigma) (mid, days) (s) 2015-12-05 20:49:25 0.24451 none 90*60 21.3 Photometry is based on nearby SDSS stars, R magnitude deduced from Lupton's transformations. SDSS id R(Lupton) J151723.45+354524.6 13.849 0.011 J151723.30+354351.0 14.562 0.012 J151718.79+354350.3 15.801 0.013 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 18677 SUBJECT: GRB 151205C: Optical follow-up observations at Kiso DATE: 15/12/10 03:00:06 GMT FROM: Masaomi Tanaka at NAOJ Yuki Kikuchi (U. of Tokyo), Masaomi Tanaka (NAOJ), Ryou Ohsawa, Makoto Ichiki, Shigeyuki Sako, Tomoki Morokuma, Mamoru Doi (U. of Tokyo), Nozomu Tominaga (Konan U.), Motoko Serino (RIKEN), Akihiro Suzuki, Keiichi Maeda (Kyoto U.), and Takanori Sakamoto (AGU) report: We performed optical non-filter imaging observations for the MAXI-detected burst GRB 151205C (Nakajima et al. GCN Circ. 18666) with a prototype model camera of Tomo-e Gozen (Tomo-e PM). Tomo-e Gozen is a wide-field optical imaging camera with 84 1kx2k CMOS sensors on the focal plane of the 1.05-m Kiso Schmidt telescope (Sako et al. in preparation, http://www.ioa.s.u-tokyo.ac.jp/tomoe/). The prototype model camera has 8 CMOS sensors along the RA direction with spatial gaps of 25 arcmin between the adjacent chips. The field-of-view of each chip is 39.7 arcmin (RA) x 22.4 arcmin (Dec). Thanks to the low dark current of the sensors in room temperature, we operate the CMOS sensors without coolers which enables us to make a light-weight camera system. By using 1 of 8 chips of Tomo-e PM, multiple regions which cover in total 95% of the localization area (with the following central coordinates) have been observed. RA | Dec | Obs. time | t-t0* | Exptime | (J2000) | (J2000) | (UT) | (days) | (sec) | 22:00:34 | +77:39:51 | 2015 Dec 6 14:08 | 0.59 | 150 | 21:58:01 | +77:41:46 | 2015 Dec 6 14:25 | 0.60 | 150 | 22:05:23 | +78:26:45 | 2015 Dec 7 09:12 | 1.39 | 180 | 22:02:51 | +78:06:14 | 2015 Dec 7 09:15 | 1.39 | 180 | 21:55:36 | +77:28:11 | 2015 Dec 7 09:22 | 1.39 | 180 | 21:58:37 | +77:45:37 | 2015 Dec 7 09:26 | 1.40 | 180 | 22:08:11 | +78:19:44 | 2015 Dec 8 14:22 | 2.60 | 150 | 22:04:56 | +78:03:18 | 2015 Dec 8 14:25 | 2.61 | 144 | 22:02:25 | +77:42:13 | 2015 Dec 8 14:29 | 2.61 | 144 | 21:58:14 | +77:22:13 | 2015 Dec 8 14:31 | 2.61 | 180 | 21:55:13 | +77:04:13 | 2015 Dec 8 14:34 | 2.61 | 180 | * time after the burst We performed image subtraction using PTF R-band data taken on 2011 Jul 17 as references (obtained through IPAC, Law et al. 2009, PASP, 121, 1395; Laher et al. 2014, PASP, 126, 674). No new transient objects have been found within these fields. The limiting magnitudes of our data are about 20 mag (calibrated with USNO UCAC3 catalog, Zacharias et al. 2010, AJ, 139, 2184).