Distances to the Supernova Remnants in the Inner Disk

Abstract

Distance measurements of supernova remnants (SNRs) are essential and important. Accurate estimates of physical size, dust masses, and some other properties of SNRs depend critically on accurate distance measurements. However, the determination of SNR distances is still a tough task. Red clump stars (RCs) have a long history been used as standard candles. In this work, we take RCs as tracers to determine the distances to a large group of SNRs in the inner disk. We first select RC stars based on the near-infrared (IR) color-magnitude diagram (CMD). Then, the distance to and extinction of RC stars are calculated. To extend the measurable range of distance, we combine near-IR photometric data from the 2MASS survey with the deeper UKIDSS and VVV surveys. With the help of the Gaia parallaxes, we also remove contaminants including dwarfs and giants. Because an SN explosion compresses the surrounding interstellar medium, the SNR region would become denser and exhibit higher extinction than the surroundings. The distance of a SNR is then recognized by the position where the extinction and its gradient is higher than that of the ambient medium. A total of 63 SNRs' distances in the Galactic inner disk are determined and divided into three Levels A, B, and C with decreasing reliability. The distances to 43 SNRs are well determined with reliability A or B. The diameters and dust masses of SNRs are estimated with the obtained distance and extinction.

31 pages, 25 figures, 2 tables, accepted for publication in A&A

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• The UKIDSS Galactic Plane Survey
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• Near-infrared [Fe II] and H${}_2$ Emission-line Study of Galactic Supernova Remnants in the First Quadrant
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• New method for estimating molecular cloud distances based on Gaia, 2MASS, and the TRILEGAL galaxy model
• Dust Mass Associated with the Supernova Remnant IC 443 when Emission Meets Extinction
• The distances of 61 PGCCs in the Second Galactic Quadrant
• A look at the high energy aspects of the supernova remnant G309.8+00.0 with eROSITA and Fermi-LAT
• Dependence of pulsation mode of Cepheids on metallicity