Massive Warm/Hot Galaxy Coronae: II. Isentropic Model

Abstract

We construct a new analytic phenomenological model for the extended circumgalactic material (CGM) of $L^{\ast }$ galaxies. Our model reproduces the OVII/OVIII absorption observations of the Milky Way (MW) and the OVI measurements reported by the COS-Halos and eCGM surveys. The warm/hot gas is in hydrostatic equilibrium in a MW gravitational potential, and we adopt a barotropic equation of state, resulting in a temperature variation as a function of radius. A pressure component with an adiabatic index of $\gamma =4/3$ is included to approximate the effects of a magnetic field and cosmic rays. We introduce a metallicity gradient motivated by the enrichment of the inner CGM by the Galaxy. We then present our fiducial model for the corona, tuned to reproduce the observed OVI-OVIII column densities, and with a total mass of $M_{\mathrm{gas}}\approx 5.5\times 10^{10}{\mathrm{M}}_{\odot }$ inside $r_{\mathrm{cgm}}\approx 280$ kpc. The gas densities in the CGM are low ($n_{\mathrm{H}}=10^{-5}-3\times 10^{-4}\mathrm{c}{\mathrm{m}}^{-3}$) and its collisional ionization state is modified by the metagalactic radiation field (MGRF). We show that for OVI-bearing warm/hot gas with typical observed column densities $N_{\mathrm{OVI}}\sim 3\times 10^{14}\mathrm{c}{\mathrm{m}}^{-2}$ at large ($\gtrsim 100$ kpc) impact parameters from the central galaxies, the ratio of the cooling to dynamical times, $t_{\mathrm{cool}}/t_{\mathrm{dyn}}$, has a model-independent upper limit of $\lesssim 4$. In our model, $t_{\mathrm{cool}}/t_{\mathrm{dyn}}$ at large radii is $\sim 2-3$. We present predictions for a wide range of future observations of the warm/hot CGM, from UV/X-ray absorption and emission spectroscopy, to dispersion measure (DM) and Sunyaev-Zeldovich CMB measurements. We provide the model outputs in machine-readable data files, for easy comparison and analysis.

arXiv comment24 pages, 15 figures. Accepted to ApJ

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