Computer Science
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..281..229f&link_type=abstract
The IGM/Galaxy Connection: The Distribution of Baryons at z=0, ASSL Conference Proceedings Vol. 281. Edited by Jessica L. Rosenb
Computer Science
Scientific paper
Using the standard prescription for the rates of supernovae type II and type Ia, we compare the predictions of a simple model of star formation in galaxies with the observed radial gradients of abundance ratios in a sample of early-type galaxies to infer the relative contribution of each type of supernova. The data suggests a correlation between the fractional contribution of Type Ia to the chemical enrichment of the stellar populations (1-xi) and central velocity dispersion of order 1-xi ~ -0.16log(sigma0)+0.40, so that the type Ia contribution in stars ranges from a negligible amount in massive (sigma0 ~ 300 km/s) galaxies up to 10% in low-mass (~100 km/s) elliptical galaxies. Our model is parametrized by a star formation timescale (tSF) which controls the duration of the starburst. A correlation with galaxy radius as a power law (tSF propto rbeta) translates into a radial gradient of the abundance ratios. The data implies a wide range of formation scenarios for a simple model that fixes the luminosity profile, ranging from inside-out (beta=2), to outside-in formation (beta=-1), as is consistent with numerical simulations of elliptical galaxy formation. An alternative scenario that links tSF to the dynamical timescale favours inside-out formation over a smaller range 0.4 < beta < 0.6. In both cases, massive galaxies are predicted to have undergone a more extended period of star formation in the outer regions with respect to their low-mass counterparts.
Ferreras Ignacio
Silk Joseph
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