paper

Dust temperature in ALMA $\hbox{[C $\scriptstyle\rm II $]}$-detected high- galaxies

arXiv:2102.08950 · doi:10.1093/mnras/stab720

Abstract

At redshift the far-infrared (FIR) continuum spectra of main-sequence galaxies are sparsely sampled, often with a single data point. The dust temperature thus has to be assumed in the FIR continuum fitting. This introduces large uncertainties regarding the derived dust mass (), FIR luminosity, and obscured fraction of the star formation rate. These are crucial quantities to quantify the effect of dust obscuration in high- galaxies. To overcome observations limitations, we introduce a new method that combines dust continuum information with the overlying $\hbox{[C $\scriptstyle\rm II $]} 158μ$m line emission. By breaking the degeneracy, with our method, we can reliably constrain the dust temperature with a single observation at m. This method can be applied to all ALMA and NOEMA $\hbox{[C $\scriptstyle\rm II $]}$ observations and exploited in ALMA Large Programs such as ALPINE and REBELS targeting $\hbox{[C $\scriptstyle\rm II $]}$ emitters at high-. We also provide a physical interpretation of the empirical relation recently found between gas mass and $\hbox{[C $\scriptstyle\rm II $]}$ luminosity. We derive an analogous relation linking the gas surface density and $\hbox{[C $\scriptstyle\rm II $]}$ surface brightness. By combining the two, we predict the cosmic evolution of the surface density ratio . We find that slowly increases with redshift, which is compatible with current observations at .

arXiv comment14 pages, 5 figures, submitted to MNRAS

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