Global X-Ray Properties of the Vela and Puppis A Supernova Remnants

Abstract

The Vela and Puppis A supernova remnants (SNRs) comprise a large emission region of $\sim 8^{\circ }$ diameter in the soft X-ray sky. The HaloSat CubeSat mission provides the first soft X-ray ($0.4-7$ keV) observation of the entire Vela SNR and Puppis A SNR region with a single pointing and moderate spectral resolution. HaloSat observations of the Vela SNR are best fit with a two-temperature thermal plasma model consisting of a cooler component with $k{T}_1=0.19_{-0.01}^{+0.01}$ keV in collisional ionization equilibrium and a hotter component with $k{T}_2=1.06_{-0.27}^{+0.45}$ keV in non-equilibrium ionization. Observations of the Puppis A SNR are best fit with a single-component plane-parallel shocked plasma model with $kT=0.86_{-0.05}^{+0.06}$ keV in non-equilibrium ionization. For the first time, we find the total X-ray luminosities of both components of the Vela SNR spectrum in the $0.5-7$ keV energy band to be $L_X=4.4_{-1.4}^{+1.4}\times 10^{34}$ erg s${}^{-1}$ for the cooler component and $L_X=4.1_{-1.5}^{+1.8}\times 10^{34}$ erg s${}^{-1}$ for the hotter component. We find the total X-ray luminosities of the Vela and Puppis A SNRs to be $L_{\text{X}}=8.4\times 10^{34}$ erg s${}^{-1}$ and $L_X=6.7_{-0.9}^{+1.1}\times 10^{36}$ erg s${}^{-1}$.

arXiv commentaccepted for publication in The Astronomical Journal, 8 pages, 4 figures

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Cited by in corpus (4)

• A global view of shocked plasma in the supernova remnant Puppis A provided by SRG/eROSITA
• Absorption Line Observations of H${}_3^{+}$ and CO in Sight Lines Toward the Vela and W28 Supernova Remnants
• Wide-field X-ray observations of the supernova remnant Puppis A with the SRG/ART-XC telescope
• The HaloSat and PolarLight CubeSat Missions for X-ray Astrophysics