Abstract
ABSTRACT We use the spectral synthesis code cloudy to tabulate the properties of gas for an extensive range in redshift (z = 0–9), temperature (log T[K] = 1–9.5), metallicity (log Z/Z⊙ = −4 – +0.5, Z = 0), and density ($\log n_{\mathrm{H}}[\, \mathrm{cm}^{-3}] = -8$ − +6). This therefore includes gas with properties characteristic of the interstellar, circumgalactic, and intergalactic media. The gas is exposed to a redshift-dependent UV/X-ray background, while for the self-shielded lower-temperature gas (i.e. ISM gas), an interstellar radiation field and cosmic rays are added. The radiation field is attenuated by a density- and temperature-dependent column of gas and dust. Motivated by the observed star formation law, this gas column density also determines the intensity of the interstellar radiation field and the cosmic ray density. The ionization balance, molecule fractions, cooling rates, line emissivities, and equilibrium temperatures are calculated self-consistently. We include dust, cosmic rays, and the interstellar radiation field step-by-step to study their relative impact. These publicly available tables are ideal for hydrodynamical simulations. They can be used stand alone or coupled to a non-equilibrium network for a subset of elements. The release includes a C routine to read in and interpolate the tables, as well as an easy-to-use python graphical user interface to explore the tables.
Highlights
Radiative processes are a critical ingredient for all models that include baryons
Radiative losses are crucial for the formation of stars and for the ignition of the cosmic baryon cycle, they are heavily used in observational astronomy to classify the properties of gas within galaxies, around galaxies and in between galaxies
Out of the 183 emission lines listed in Table 7 we show a few examples of soft X-ray emission lines in Fig. and farinfrared/(sub-)mm emission lines in Fig. In both figures the normalized emergent emissivities, /nH2, for the last cloudy zone of the shielding column ( Vol) as well as the emissivity calculated by dividing the line intensity of the full shielding column by the length of the shielding column ( Col) from the fiducial model “UV background (UVB) dust1 CR1 G1 shield1” are displayed
Summary
Radiative processes are a critical ingredient for all models that include baryons. Radiative losses are crucial for the formation of stars and for the ignition of the cosmic baryon cycle, they are heavily used in observational astronomy to classify the properties of gas within galaxies (interstellar medium, ISM), around galaxies (circumgalactic medium, CGM) and in between galaxies (intergalactic medium, IGM). Determining the radiative cooling rate of a parcel of gas relies on a series of intertwined chemical reactions of species that can interact with the ambient radiation field. Radiative cooling functions were calculated under the assumption of an optically thin gas in collisional ionization equilibrium The ionization rates in CIE (and the recombination rates and the radiative losses, Λ) are proportional to the number of colli-
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