Typing supernova remnant G352.7\(-\)0.1 using XMM-Newton X-ray observations

• Published in: arXiv.org 2024-03
• Main Authors: Ling-Xiao, Dang, Zhou, Ping, Sun, Lei, Mao, Junjie, Vink, Jacco, Qian-Qian, Zhang, Domček, Vladimír
• Format: Article
• Language: English
• Subjects: Abundance; Astrochemistry; Iron; Molecular clouds; Morphology; Nuclear fusion; Supernova remnants; Thermal plasmas; X ray spectra; XMM (spacecraft)
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2403.11972

G352.7\(-\)0.1 is a mixed-morphology (MM) supernova remnant (SNR) with multiple radio arcs and has a disputed supernova origin. We conducted a spatially resolved spectroscopic study of the remnant with XMM-Newton X-ray data to investigate its explosion mechanism and explain its morphology. The global X-ray spectra of the SNR can be adequately reproduced using a metal-rich thermal plasma model with a temperature of \(\sim 2\) keV and ionization timescale of \(\sim 3\times 10^{10}~{\rm cm^{-3}~s}\). Through a comparison with various supernova nucleosynthesis models, we found that observed metal properties from Mg to Fe can be better described using core-collapse supernova models, while thermonuclear models fail to explain the observed high Mg/Si ratio. The best-fit supernova model suggests a \(\sim 13\) \(M_\odot\) progenitor star, consistent with previous estimates using the wind bubble size. We also discussed the possible mechanisms that may lead to SNR G352.7\(-\)0.1 being an MMSNR. By dividing the SNR into several regions, we found that the temperature and abundance do not significantly vary with regions, except for a decreased temperature and abundance in a region interacting with molecular clouds. The brightest X-ray emission of the SNR spatially matches with the inner radio structure, suggesting that the centrally filled X-ray morphology results from a projection effect.