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 0.13 keV with a hydrogen column density of ( ) × 1020 cm−2. HST imaging allows us to measure a semimajor axis of 0.78 0.10 arcsec ( ) and a semiminor axis of arcsec ( ). This precise size helps to constrain the age and velocity of the shock to be ( ) × 103 yr and km s−1. We also fit photometry of the surrounding stars to infer the age and mass of the progenitor star to be 8 1 Myr and M . Based on measured radio properties of the source and assuming equipartition, the estimated radio luminosity of ∼1.7 × 1034 erg s−1 over the 108-1011 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 × 1049 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.
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 (\(9.7^{+6.4}_{-4.8}\))\(\times 10^{20}\) 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 \(0.69^{+0.14}_{-0.12}\) arcsec (\(6.7^{+1.2}_{-1.4}\) pc). This precise size helps to constrain the age and velocity of the shock to be (\(3.3^{+0.7}_{-0.6}\))\(\times 10^{3}\) yr and \(411^{+275}_{-122}\) 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 \(25^{+1}_{-5}\) 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.
PDF