Abstract
Object: Distances are found for four supernova remnants without previous distance measurements. H I spectra and H I channel maps are used to determine the maximum velocity of H I absorption for the four Supernova Remnants (SNRs). Method: We examined 13CO emission spectra and channel maps to look for possible molecular gas associated with each SNR, but did not find any. Result: The resulting distances for the SNRs are 3.5 ± 0.2 kpc (G24.7+0.6), 4.7 ± 0.3 kpc (G29.6+0.1), 4.1 ± 0.5 kpc (G41.5+0.4) and 4.5 ± 0 .4 - 9.0 ± 0.4 kpc (G57.2+0.8).
Highlights
Supernova remnants (SNRs) have a major impact on the state of the Interstellar Medium (ISM) of a galaxy
We examined 13CO emission spectra and channel maps to look for possible molecular gas associated with each Supernova Remnants (SNRs), but did not find any
Region 3 was chosen to extract the spectrum of the H II region G24.540+0.600 as a comparison for the SNR H I absorption spectra
Summary
Supernova remnants (SNRs) have a major impact on the state of the Interstellar Medium (ISM) of a galaxy (e.g. for a review see Cox [1]). They provide the thermal and kinetic energy that determines the structure of the ISM, and can drive outflows from the galaxy and trigger star formation. Determining the distance to an SNR is an important first step in determining its size, age, explosion energy and evolutionary state. Utilizing H I absorption spectra is one method of obtaining the distance to an SNR. For the construction of H I absorption spectra, we use the method presented by Leahy and Tian [2]. To determine the distance and resolve kinematic distance ambiguity, we use the step-by-step process described by Ranasinghe and Leahy [3]
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