- GCN/BACODINE POSITION NOTICE
TITLE: GCN/MAXI NOTICE
NOTICE_DATE: Sun 06 Dec 15 00:38:20 UT
NOTICE_TYPE: MAXI Unknown Source Position
EVENT_ID_NUM: 361767105
EVENT_RA: 0.00d {+00h 00m 00s} (J2000),
0.20d {+00h 00m 49s} (current),
359.36d {+23h 57m 26s} (1950)
EVENT_DEC: +0.00d {+00d 00' 00"} (J2000),
+0.09d {+00d 05' 19"} (current),
-0.28d {-00d 16' 41"} (1950)
EVENT_ERROR: 1.0 [deg radius, stat+sys, 90% containment]
EVENT_FLUX: 152.0 +- 0.0 [mCrab]
EVENT_DATE: 17361 TJD; 339 DOY; 15/12/05
EVENT_TIME: 86048.00 SOD {23:54:08.00} UT
EVENT_TSCALE: 10s
EVENT_EBAND: Low, 2-4 keV
SUN_POSTN: 252.17d {+16h 48m 40s} -22.42d {-22d 25' 26"}
SUN_DIST: 106.67 [deg]
MOON_POSTN: 192.26d {+12h 49m 02s} -3.91d {-03d 54' 36"}
MOON_DIST: 167.36 [deg]
MOON_ILLUM: 26 [%]
GAL_COORDS: 96.34,-60.19 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 0.00, 0.00 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: MAXI Unknown Source Position. GRB or unknown X-ray Transient.
- GCN Circular #18666
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
- GCN Circular #18667
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.
- GCN Circular #18671
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.
- GCN Circular #18677
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).
Previous IAU Circulars 