MAXI/GSC detection of a new X-ray outburst from XTE J1858+034 or a new X-ray transient MAXI J1900+037
ATel #15970; M. Nakajima, H. Negoro (Nihon U.), M. Serino (AGU), K. Kobayashi, M. Tanaka, Y. Soejima (Nihon U.), T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU), Y. Tsuboi, J. Kohara, S. Urabe, S. Nawa, N. Nemoto (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, T. Kurihara (JAXA), Y. Ueda, S. Ogawa, K. Setoguchi, T. Yoshitake, K. Inaba, Y. Nakatani (Kyoto U.), M. Yamauchi, T. Sato, R. Hatsuda, R. Fukuoka, Y. Hagiwara, Y. Umeki (Miyazaki U.), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) , W. Iwakiri (Chiba U.)
on 31 Mar 2023; 11:31 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 an X-ray transient source on March 30, 2023. Assuming that the source flux was constant over the transit, we obtain the source position at
(R.A., Dec) = (285.123 deg, 3.711 deg) = (19 00 29, +03 42 39) (J2000)
with a statistical 90% C.L. elliptical error region with long and short radii of 0.41 deg and 0.34 deg, respectively. The roll angle of long axis from the north direction is 128.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). The X-ray flux averaged for 2 days before and after trigger is 32 +- 6 mCrab (4.0-10.0keV).
The error region includes the Be/X-ray binary pulsar XTE J1858+034 discovered in 1998 (IAUC 6826 :2). Outbursts from XTE J1858+034 were observed in 2004 (ATel#274), 2010 (ATel#2846), 2011 (ATel#3766), and 2019 (ATel#13217). The Swift/BAT light curve of XTE J1853+034, however, does not shows any significant activity, yet (https://swift.gsfc.nasa.gov/results/transients/weak/XTEJ1858p034/).
Thus, we also tentatively name the source MAXI J1900+037 until the identification as XTE J1858+034.
Followup observations are encouraged.
