Multiwavelength Study of the X-Ray Bright Supernova Remnant N300-S26 in NGC 300. (arXiv:1906.04531v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gross_J/0/1/0/all/0/1">Jacob Gross</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_B/0/1/0/all/0/1">Benjamin F. Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pannuti_T/0/1/0/all/0/1">Thomas G. Pannuti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Binder_B/0/1/0/all/0/1">Breanna Binder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garofali_K/0/1/0/all/0/1">Kristen Garofali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hanvey_Z/0/1/0/all/0/1">Zachary G. Hanvey</a>
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.
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.
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