Discovery of a very young high-mass X-ray binary associated with the supernova remnant MCSNRJ0513-6724 in the LMC

• Published in: arXiv.org 2019-10
• Main Authors: Maitra, C, Haberl, F, Filipovic, M D, Udalski, A, Kavanagh, P J, Carpano, S, Maggi, P, Sasaki, M, Norris, R P, O'Brien, A, Hotan, A, E Lenc M K Szymanski, Soszynski, I, Poleski, R, Ulaczyk, K, Pietrukowicz, P, Kozlowski, S, Skowron, J, Mroz, P, Rybicki, K, Iwanek, P, Wrona, M
• Format: Article
• Language: English
• Subjects: Deposition; Emission; Evolution; Light curve; Luminosity; Magellanic clouds; Magnetic fields; Optical counterparts (astronomy); Orbits; Periodic variations; Pulsars; Soft x rays; Supernova remnants; Supernovae; X ray binaries; X ray stars; XMM (spacecraft)
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1910.02792

We report the discovery of a very young high-mass X-ray binary (HMXB) system associated with the supernova remnant (SNR) MCSNRJ0513-6724 in the Large Magellanic Cloud (LMC), using XMM-Newton X-ray observations. The HMXB is located at the geometrical centre of extended soft X-ray emission, which we confirm as an SNR. The HMXB spectrum is consistent with an absorbed power law with spectral index ~1.6 and a luminosity of 7x10^{33} ergs/s (0.2--12 keV). Tentative X-ray pulsations are observed with a periodicity of 4.4 s and the OGLE I-band light curve of the optical counterpart from more than 17.5 years reveals a period of 2.2324\pm0.0003 d, which we interpret as the orbital period of the binary system. The X-ray spectrum of the SNR is consistent with non-equilibrium shock models as expected for young/less evolved SNRs. From the derived ionisation time scale we estimate the age of the SNR to be