The warm-hot circumgalactic medium around EAGLE-simulation galaxies and its detection prospects with X-ray-line emission

Abstract

We estimate the detectability of X-ray metal-line emission from the circumgalactic medium (CGM) of galaxies over a large halo mass range (M200c = 1011 . 5 -10 14 . 5 M⊙), using the EA GLE simulations. W ith the XRISM Resolve instrument, a few bright (Kα or Fe L-shell) lines from M 200c ≥ 1013 M⊙ haloes should be detectable. Using the Athena X-IFU or the Lynx Main Array, emission lines (especially from O VIII and O VII) from the inner CGM of M 200c ≥ 10 12 .5 M⊙ haloes become detectable, and intragroup and intracluster gas will be detectable out to the virial radius. With the Lynx Ultra-high Resolution Array, the inner CGM of haloes hosting L∗ galaxies is accessible. These estimates do assume long exposure times (~1 Ms) and large spatial bins (~1-10 arcmin2). This emission is dominated by collisionally ionized (CI) gas, and tends to come from halo centres. The emission is biased towards temperatures close to the maximum emissivity temperature for CI gas (Tpeak), and high densities and metallicities. Ho we ver, for the Kα lines, emission can come from hotter gas in haloes where the virialized, volume-filling gas is hotter than Tpeak . Trends of emission with halo mass can largely be explained by differences in virial temperature. Differences in the mass trends of Kα, Heα-like, and Fe L-shell lines mirror differences in their emissivities as a function of temperature. We conclude that upcoming X-ray missions will open up a new window on to the hot CGM.