THREE-DIMENSIONAL HYDRODYNAMIC SIMULATIONS OF MULTIPHASE GALACTIC DISKS WITH STAR FORMATION FEEDBACK. II. SYNTHETIC H I 21 cm LINE OBSERVATIONS

Abstract

We use three-dimensional numerical hydrodynamic simulations of the turbulent, multiphase atomic interstellar medium ( ISM) to construct and analyze synthetic H I 21 cm emission and absorption lines. Our analysis provides detailed tests of 21 cm observables as physical diagnostics of the atomic ISM. In particular, we construct (1) the “observed” spin temperature, T-s,(obs)(nu(ch)) = T-B (nu(ch))/[1 - e(-tau(nu ch))], and its optical-depth weighted mean T-s,T-obs; (2) the absorption-corrected “observed” column density, N-H,(obs) alpha integral d nu T-ch(B) (nu(ch)) tau(nu(ch))/[1 - e(-tau(nu ch))]; and (3) the “observed” fraction of cold neutral medium (CNM), f(c,obs) T-c/T-s, obs for T-c the CNM temperature; we compare each observed parameter with true values obtained from line-of-sight (LOS) averages in the simulation. Within individual velocity channels, T-s,T-obs(nu(ch)) is within a factor 1.5 of the true value up to tau(nu(ch)) similar to 10. As a consequence, N-H,N-obs and T-s,T-obs are, respectively, within 5% and 12% of the true values for 90% and 99% of LOSs. The optically thin approximation significantly underestimates N-H for tau > 1. Provided that Tc is constrained, an accurate observational estimate of the CNM mass fraction can be obtained down to 20%. We show that Ts, obs cannot be used to distinguish the relative proportions of warm and thermally unstable atomic gas, although the presence of thermally unstable gas can be discerned from 21 cm lines with 200 K less than or similar to T-s,T-obs(nu(ch)) less than or similar to 1000 K. Our mock observations successfully reproduce and explain the observed distribution of the brightness temperature, optical depth, and spin temperature in Roy et al. The threshold column density for CNM seen in observations is also reproduced by our mock observations. We explain this observed threshold behavior in terms of vertical equilibrium in the local Milky Way’s ISM disk.