MAXI/GSC detection of the outburst from Be/X-ray binary pulsar IGR J06074+2205
ATel #15294; M. Nakajima, H. Negoro (Nihon U.), T. Mihara (RIKEN), N. Kawai (Tokyo Tech), K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Tamagawa, J. Li, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga, J. Kohara (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, M. Kurihara (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC)
on 24 Mar 2022; 10:31 UT
Credential Certification: Motoki Nakajima (nakajima.motoki@nihon-u.ac.jp)
Subjects: X-ray, Binary, Neutron Star, Transient, Pulsar
The MAXI/GSC nova alert system triggered a faint X-ray transient source on 23 March 2022 (MJD 59661). Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (92.000 deg, 22.030 deg) = (06 08 00, +22 01 48) (J2000) with a statistical 90% C.L. elliptical error region with long and short radii of 0.69 deg and 0.49 deg, respectively. The roll angle of long axis from the north direction is 54.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). This position is consistent with that of the Be/X-ray binary pulsar IGR J06074+2205 (Chenevez et al. 2004, ATel#223; Halpern et al. 2005, ATel#682; Tomsick et al. 2006, ATel#959; Reig et al. 2018). This is the first firm detection of this source by MAXI/GSC since August 2009. The day-averaged X-ray fluxes in 4-10 keV band derived from the MAXI on-demand process are 0.022 ± 0.007 photons/s/cm2 (18 ± 5 mCrab, Mar. 22) and 0.019 ± 0.006 photons/s/cm2 (16 ± 5 mCrab, Mar. 23). These fluxes are comparable to the results of the INTEGRAL observations in 2004 (Chenevez et al. 2004, ATel#223; Reig et al. 2018). We searched all the data observed by MAXI/GSC since 2009 for the periodic X-ray activity related to the binary motion. However, no X-ray periodicities are found in the claimed binary orbital period of >100 days (Reig et al. 2018). We encourage multi-wavelength observations to reveal the nature of the poorly studied source, IGR J06074+2205.
The latest X-ray light-curve can be checked at the following pages;
MAXI ( http://maxi.riken.jp/pubdata/v7lrkn/J0607+220/index.html ) and
Swift/BAT ( https://swift.gsfc.nasa.gov/results/transients/weak/IGRJ06074p2205/ ).
