Recurrent Outbursts Revealed in 3XMM J031820.8-663034

• Published in: The Astrophysical journal Vol. 859; no. 2; pp. 106 - 113
• Main Authors: Zhao, Hai-Hui, Weng, Shan-Shan, Wang, Jun-Xian
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.06.2018; IOP Publishing
• Subjects: accretion, accretion disks; Astrophysics; black hole physics; Black holes; Blackbody; Deposition; Emission; Luminosity; Outbursts; Temperature; Temperature rise; X ray sources; X-ray emissions; X-rays: binaries; X-rays: individual (3XMM J031820.8-663034); X-rays: stars; XMM (spacecraft)
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aac176

3XMM J031820.8-663034, first detected by ROSAT in NGC 1313, is one of a few known transient ultraluminous X-ray sources (ULXs). In this paper, we present decades of X-ray data of this source from ROSAT, XMM-Newton, Chandra, and the Neil Gehrels Swift Observatory. We find that its X-ray emission experienced four outbursts since 1992, with a typical recurrent time ∼1800 days, an outburst duration ∼240-300 days, and a nearly constant peak X-ray luminosity ∼1.5 × 1039 erg s−1. The upper limit of X-ray luminosity at the quiescent state is ∼5.6 × 1036 erg s−1, and the total energy radiated during one outburst is ∼1046 erg. The spectra at the high luminosity states can be described with an absorbed disk blackbody, and the disk temperature increases with the X-ray luminosity. We compare its outburst properties with other known transient ULXs including ESO 243-49 HLX-1. As its peak luminosity only marginally puts it in the category of ULXs, we also compare it with normal transient black hole binaries. Our results suggest that the source is powered by an accreting massive stellar-mass black hole, and the outbursts are triggered by the thermal-viscous instability.