The hot circumgalactic medium in the eROSITA All-Sky Survey II. Scaling relations between X-ray luminosity and galaxies' mass

Abstract

Understanding how the properties of galaxies relate to the properties of the hot circum-galactic medium (CGM) around them can constrain galaxy evolution models. We measured the X-ray luminosity of the hot CGM based on the surface brightness profiles of central galaxy samples measured from Spectrum Roentgen Gamma (SRG)/eROSITA all-sky survey data. We related the X-ray luminosity to the galaxies' stellar and halo mass, and we compared the observed relations to the self-similar model and intrinsic (i.e., not forward-modeled) output of the IllustrisTNG, EAGLE, and SIMBA simulations. The average hot CGM X-ray luminosity ($L_{\mathrm{X},\mathrm{CGM}}$) correlates with the galaxy's stellar mass ($M_{\ast }$). It increases from $(1.6\pm 2.1)\times 10^{39}\mathrm{erg}{\mathrm{s}}^{-1}$ to $(3.4\pm 0.3)\times 10^{41}\mathrm{erg}{\mathrm{s}}^{-1}$, when $\log (M_{\ast })$ increases from 10.0 to 11.5. A power law describes the correlation as $\log (L_{\mathrm{X},\mathrm{CGM}})=(2.4\pm 0.1)\times \log (M_{\ast })+(14.6\pm 1.5)$. The hot CGM X-ray luminosity as a function of halo mass is measured within $\log (M_{500c})=11.3-13.7$, extending our knowledge of the scaling relation by more than two orders of magnitude. $L_{\mathrm{X},\mathrm{CGM}}$ increases with $M_{500c}$ from $(3.0\pm 1.6)\times 10^{39}\mathrm{erg}{\mathrm{s}}^{-1}$ at $\log (M_{500c})=11.3$ to $(1.3\pm 0.1)\times 10^{42}\mathrm{erg}{\mathrm{s}}^{-1}$ at $\log (M_{500c})=13.7$. The relation follows a power law of $\log (L_{\mathrm{X},\mathrm{CGM}})=(1.32\pm 0.05)\times \log (M_{500c})+(24.1\pm 0.7)$. Our observations highlight the necessity of non-gravitational processes at the galaxy group scale while suggesting these processes are sub-dominant at the galaxy scale. We show that the outputs of current cosmological galaxy simulations generally align with the observational results uncovered here but with possibly important deviations in selected mass ranges.

Abstract abridged for arXiv submission, accepted by A&A

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