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(abridged) In this work we have a closer look at the gas content or fractionand the associated star formation rate in main sequence and starburst galaxiesat z=0 and z~1-2 by applying an analytical model of galactic clumpy gas disksto samples of local spiral galaxies, ULIRGs, submillimeter (smm), and high-zstarforming galaxies. The model gas and dust temperatures are determined by theheating and cooling equilibrium. Dense clouds are heated by turbulentmechanical and cosmic ray heating. The molecular abundances of individual gasclouds are determined by a detailed chemical network involving the cloudlifetime, density, and temperature. Molecular line emission is calculated withan escape probability formalism. The model calculates simultaneously the totalgas mass, HI/H_2 mass, the gas velocity dispersion, IR luminosity, IR spectralenergy distribution, CO spectral line energy distribution (SLED), HCN(1-0), andHCO+(1-0) emission of a galaxy given its size, integrated star formation rate,stellar mass radial profile, rotation curve, and Toomre Q parameter. The modelreproduces the observed CO luminosities and SLEDs of all sample galaxies withinthe model uncertainties (~0.3 dex). Whereas the CO emission is robust againstthe variation of model parameters, the HCN and HCO+ emission is sensitive tothe chemistry of the interstellar medium. The CO and HCN mass-to-lightconversion factors including CO-dark H_2 are given and compared to the valuesfound in the literature. Both, the HCN and HCO+ emission trace the densemolecular gas to a factor of ~2 for the local spiral galaxies, ULIRGs andsmm-galaxies. About 80% of the molecular line emission of compact starburstgalaxies originates in non-selfgravitating gas clouds. The integratedKennicutt-Schmidt law has a slope of ~1 for the local spirals, ULIRGs, andsmm-galaxies, whereas the slope is 1.7 for high-z starforming galaxies.

astronomy and astrophysics

Predicting HCN, HCO+, multi-transition CO, and dust emission of  star-forming galaxies From local spiral and ultraluminous infrared galaxies  to high-z star-forming and submillimeter galaxies