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2010MNRAS.407.2091G - Mon. Not. R. Astron. Soc., 407, 2091-2108 (2010/October-1)
A study of the gas-star formation relation over cosmic time.
GENZEL R., TACCONI L.J., GRACIA-CARPIO J., STERNBERG A., COOPER M.C., SHAPIRO K., BOLATTO A., BOUCHE N., BOURNAUD F., BURKERT A., COMBES F., COMERFORD J., COX P., DAVIS M., FORSTER SCHREIBER N.M., GARCIA-BURILLO S., LUTZ D., NAAB T., NERI R., OMONT A., SHAPLEY A. and WEINER B.
Abstract (from CDS):
In contrast, very luminous and ultraluminous, gas-rich major mergers at both low and high z produce on average four to 10 times more far-infrared luminosity per unit gas mass. We show that only some fraction of this difference can be explained by uncertainties in gas mass or luminosity estimators; much of it must be intrinsic. A possible explanation is a top-heavy stellar mass function in the merging systems but the most likely interpretation is that the star formation relation is driven by global dynamical effects. For a given mass, the more compact merger systems produce stars more rapidly because their gas clouds are more compressed with shorter dynamical times, so that they churn more quickly through the available gas reservoir than the typical normal disc galaxies. When the dependence on galactic dynamical time-scale is explicitly included, disc galaxies and mergers appear to follow similar gas-to-star formation relations. The mergers may be forming stars at slightly higher efficiencies than the discs.
Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS
Journal keyword(s): stars: formation - ISM: molecules - galaxies: evolution - galaxies: ISM - galaxies: starbursts
Simbad objects: 43
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