//////////////////////////////////////////////////////////////////////// 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: 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: 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).