Tobias Prinz, Werner Becker
Aims: We present a detailed X-ray and radio wavelength study of G308.4-1.4, a
candidate supernova remnant (SNR) in the ROSAT All Sky Survey and the MOST
supernova remnant catalogue.
Methods: The SNR candidate and its central point sources were studied using
observations from the Chandra X-ray Observatory, SWIFT, the Australian
Telescope Compact Array (ATCA) at 1.4 and 2.5 GHz and WISE infrared observation
at 24 $\mu$m.
Results: We conclude that G308.4-1.4 is indeed a supernova remnant by means
of its morphology matching at X-ray, radio and infrared wavelength, its
spectral energy distribution in the X-ray band and its emission characteristics
in the radio band. G308.4-1.4 is a shell-type SNR. X-ray, radio and infrared
emission is seen only in the eastern part of the remnant due to a strong
spatial density variation of the interstellar medium around the remnant. The
X-ray emission can best be described by an absorbed non-equilibrium collisional
plasma with a hydrogen density of $n_\text{H}=(1.02\pm 0.04)$ cm$^{-2}$, a
plasma temperature of $6.3^{+1.2}_{-0.7}$ million Kelvin and an under-abundance
of Iron, Neon and Magnesium, as well as an overabundance in Sulfur with respect
to the solar values. A Sedov analysis revealed that the remnant is at a
distance of $ \approx 10$ kpc and the progenitor star exploded $\sim 5000$ to
7500 years ago. Two faint X-ray point sources located near to the remnant's
geometrical center are detected. Both sources have no counterpart at other
wavelengths, leaving them as candidates for the compact remnant of the
supernova explosion.
View original:
http://arxiv.org/abs/1202.4677
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