First study of the supernova remnant population in the Large Magellanic Cloud with eROSITA: II. Spectral analysis and X-ray luminosity function

Zangrandi F, Sasaki M, Long KS, Maggi P, Filipović MD, Haberl F, Kavanagh P, Mayer M, Koribalski B, Maitra C, Points S, Staveley-Smith L, Jurk K, Smeaton ZJ, Saeedi S (2026)

Publication Type: Journal article

Publication year: 2026

Journal

Book Volume: 709

Article Number: A207

DOI: 10.1051/0004-6361/202557834

Abstract

Aims. Supernova remnants (SNRs) are responsible for the injection of energy and chemical elements into the interstellar medium (ISM). The emission from SNRs can be studied to infer information about the supernova (SN) explosion itself as well as about the properties of the surrounding ISM. Studying a sample of SNRs in a galaxy provides an opportunity to better understand stellar feedback, and the best laboratory for such an investigation is the Large Magellanic Cloud (LMC). The LMC is the nearest star-forming galaxy, it lies outside the Galactic plane line of sight, and therefore its foreground absorption is low. Methods. The eROSITA telescopes are the best instruments currently available to perform a survey of the SNRs in the entire LMC due to their large field of view and their high sensitivity towards soft X-rays. We used the sample of SNRs reported in the previous paper and performed a spectral analysis on a part of the sample. We estimated the flux and the luminosity of the fainter sources using the energy conversion factor obtained assuming a non-equilibrium ionisation plasma model. Results. The X-ray luminosity function (XLF) of SNRs in the LMC shows a relatively large number of SNRs at high luminosities. We fitted the distribution with two Gaussian components, which yielded best-fit maxima for the LX[0.3-8.0keV] distribution at m1 = 10^34.7±0.2 erg s⁻¹ and m2 = 10^36.5±0.4 erg s⁻¹. We compared the XLF of the LMC with the XLFs of the Small Magellanic Cloud (SMC), M31, and M33 using a power-law fit and an Anderson-Darling (DA) test. The power indices of the XLFs of the LMC and SMC appear consistent with each other, while those of M33 and M31 are larger. Thus, the latter have steeper power laws, indicating a lower number of X-ray luminous SNRs with respect to the Magellanic Clouds. The DA test showed that the luminosity distributions of SNRs in the SMC and LMC are compatible with being extracted from the same underlying distribution. They are also compatible for different galaxies if we consider the same lower limit for LX [0.3-8.0 keV] for the entire distribution. Finally, we compared the luminosity and the X-ray sizes (diameter) of the SNRs in our sample. We observed a general trend of anti-correlation between size and X-ray luminosity that can be interpreted as a result of fading with time.

Authors with CRIS profile

Involved external institutions

Space Telescope Science Institute (STScI) United States (USA) (US) Université de Strasbourg (UDS) France (FR) University of Western Sydney Australia (AU) Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics Germany (DE) Maynooth University Ireland (IE) Commonwealth Scientific and Industrial Research Organisation (CSIRO) Australia (AU) Cerro Tololo Inter-American Observatory (CTIO) Chile (CL) University of Western Australia (UWA) Australia (AU)

How to cite

APA:

Zangrandi, F., Sasaki, M., Long, K.S., Maggi, P., Filipović, M.D., Haberl, F.,... Saeedi, S. (2026). First study of the supernova remnant population in the Large Magellanic Cloud with eROSITA: II. Spectral analysis and X-ray luminosity function. Astronomy & Astrophysics, 709. https://doi.org/10.1051/0004-6361/202557834

MLA:

Zangrandi, Federico, et al. "First study of the supernova remnant population in the Large Magellanic Cloud with eROSITA: II. Spectral analysis and X-ray luminosity function." Astronomy & Astrophysics 709 (2026).

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