MAXI/GSC detection of X-ray outburst from Be/X-ray binary pulsar H1145-619
M. Nakajima, H. Negoro (Nihon U.), M. Ishikawa, S. Ueno, H. Tomida, S. Nakahira, Y. Sugawara (JAXA), T. Mihara, M. Sugizaki, M. Serino, W. Iwakiri, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Kawai, N. Isobe, S. Sugita, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara, S. Harita, Y. Muraki (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), H. Tsunemi, R. Shomura, T. Yoneyama (Osaka U.), K. Tanaka, T. Masumitsu, T. Kawase, A. Sakamaki (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto, S. Oda (Kyoto U.), Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), M. Yamauchi, K. Furuya (Miyazaki U.), Y. E. Nakagawa (JAMSTEC), K. Yamaoka (Nagoya U.)
The MAXI/GSC nova-alert system (Negoro et al. 2016) detected a weak X-ray enhancement from the position (RA,DEC) = (176.2, -62.5) on 2017-03-19 (MJD 57831). At this position, there are two X-ray pulsars, 1E 1145.1-6141 and H 1145-619, separated by 0.25 deg. Although the MAXI/GSC can not distinguish these sources due to the low spatial resolution, the current brightening nicely matched with the onset of the quasi-periodic outburst from H 1145-619, which recurs with the orbital period of 186.5 day (Warwick et al. 1985). In addition, another all-sky monitor Swift/BAT also detected the current brightening from H 1145-619. Thus the current event triggered by the MAXI/GSC nova-alert system can be considered as a normal outburst from Be/X-ray pulsar H 1145-619. The latest source flux can be checked at the following pages; MAXI(http://134.160.243.77/pubdata/v3.rkn/J1148-622/index.html), Swift/BAT(https://swift.gsfc.nasa.gov/results/transients/weak/H1145-619/), the BeXRB monitor page(http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php).
x-ray,binary,neutron star,nova,pulsar,star,transient