Multiwavelength Study of the X-Ray Bright Supernova Remnant N300-S26 in NGC 300

Abstract

We present a multiwavelength examination of the supernova remnant (SNR) S26 in the nearby galaxy NGC 300 using data from Chandra X-ray Observatory, XMM-Newton X-ray Observatory, Hubble Space Telescope (HST), the Very Large Array, and the Australia Telescope Compact Array. We simultaneously fit all of the available X-ray data with a thermal plasma model and find a temperature of $0.77\pm 0.13$ keV with a hydrogen column density of ($9.7_{-4.8}^{+6.4}$)$\times 10^{20}$ cm${}^{-2}$. HST imaging allows us to measure a semimajor axis of $0.78\pm 0.10$ arcsec ($7.5\pm 1.0$ pc) and a semiminor axis of $0.69_{-0.12}^{+0.14}$ arcsec ($6.7_{-1.4}^{+1.2}$ pc). This precise size helps to constrain the age and velocity of the shock to be ($3.3_{-0.6}^{+0.7}$)$\times 10^3$ yr and $411_{-122}^{+275}$ km s${}^{-1}$. We also fit photometry of the surrounding stars to infer the age and mass of the progenitor star to be $8\pm 1$ Myr and $25_{-5}^{+1}$ M${}_{\odot }$. Based on measured radio properties of the source and assuming equipartition, the estimated radio luminosity of $\sim 1.7\times 10^{34}$ erg s${}^{-1}$ over the $10^8-10^{11}$ Hz frequency range results in a minimum magnetic field associated with this SNR of $0.067$ mG and the minimum energy needed to power the observed synchrotron emission of $1.5\times 10^{49}$ erg. The size and temperature of N300-S26 appear to be similar to the Galactic SNR G311.5-0.3 except that G311.5-0.3 has a significantly lower X-ray luminosity, is older, and has a slower shock velocity.

arXiv comment37 pages, 6 figures, 3 tables

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