The C and CO cooling rates in nearby galaxies: A new tracers of star formation activity

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Scientific paper

We present a survey of the submillimeter lines of atomic carbon and of carbon monoxide in nearby galaxy nuclei (Bayet et al. 2004 and 2005a). By comparing observed and modelled data (using both LVG and PDR modelling codes), we derive the contribution of C and CO to the gas cooling rate for the sample galaxy nuclei. We show that the CO cooling rate is dominated by the contribution of the rotational lines (CO(6-5) and CO(7-6) especially) for starburst galaxies, and by slightly lower excitation lines for normal galaxies. We also show that the CO luminosity is tightly and linearly correlated with the far infrared luminosity (Bayet et al. 2005b and 2006), contrasting with the behaviour of other strong lines in galaxies (e.g. CO(1-0), [CII]) which do not scale linearly with the far infrared luminosity. The CO luminosity can therefore be used as a tracer of the star formation in galaxies.

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