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The Vela and Puppis A supernova remnants (SNRs) comprise a large emissionregion of $\sim 8^{\circ}$ diameter in the soft X-ray sky. The HaloSat CubeSatmission provides the first soft X-ray ($0.4-7$ keV) observation of the entireVela SNR and Puppis A SNR region with a single pointing and moderate spectralresolution. HaloSat observations of the Vela SNR are best fit with atwo-temperature thermal plasma model consisting of a cooler component with$kT_{1} = 0.19^{+0.01}_{-0.01}$ keV in collisional ionization equilibrium and ahotter component with $kT_{2} = 1.06^{+0.45}_{-0.27}$ keV in non-equilibriumionization. Observations of the Puppis A SNR are best fit with asingle-component plane-parallel shocked plasma model with $kT =0.86^{+0.06}_{-0.05}$ keV in non-equilibrium ionization. For the first time, wefind the total X-ray luminosities of both components of the Vela SNR spectrumin 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 $L_X = 4.1^{+1.8}_{-1.5} \times10^{34}$ erg s$^{-1}$ for the hotter component. We find the total X-rayluminosities of the Vela and Puppis A SNRs to be $L_{\text{X}} = 8.4 \times10^{34}$ erg s$^{-1}$ and $L_X = 6.7^{+1.1}_{-0.9} \times 10^{36}$ ergs$^{-1}$.

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