Fig. 2: Observed and simulated shell structures in the supernova remnant 0509.
From: Calcium in a supernova remnant as a fingerprint of a sub-Chandrasekhar-mass explosion
Left: reverse shocked ejecta emitting in [Ca XV] in SNR 0509 obtained by integrating over a slice from 5,626 Å to 5,752 Å (for more details, see ‘Data analysis and visualization’ section). The intensity ranges from 0.05 to 0.9 × 10−17 erg s−1 cm−2 arcsec−2 Å−1. The area within the eastern (left) white highlighted rectangle shows the region picked for examining the double-shell structure. The region within the western (right) rectangle is the extraction aperture for the spectrum shown in Fig. 1. Left centre: integrated column (along the line of sight) of density × density × X(Ca), which shows a double-shell structure of calcium in the model M10_03 after 100 s of explosion (the plotted value range is 7 × 10−20 to 5 × 10−13 density2 X(Ca)). Right centre: reverse shocked ejecta emitting in [S XII] in SNR 0509, obtained by integrating over a spectral slice from 7,502 Å to 7,726 Å. The bright point sources in the figure are not sulfur clumps but rather stars that have strong emission lines in the wavelength range of [S XII] (for more details, see ‘Data analysis and visualization’ section). A highly red-shifted background galaxy can be observed at the same wavelength in the centre of the remnant as a diffuse red spot. The intensity ranges from 0.18 to 2.0 × 10−17 erg s−1 cm−2 arcsec−2 Å−1. Right: integrated column of density × densit × X(S), which shows a single-shell structure of sulfur in the model M10_03 (the plotted value range is 3 × 10−19 to 1 × 10−13 density2 X(Ca)). X(Ca) and X(S) represent mass fraction for the specific element. Vx, Vz, velocity in the x and z axis, respectively.
