Spheroidal systems as a one-parameter family of mass at their birth

Details Spheroidal systems as a one-parameter family of mass at their birth Spheroidal systems as a one-parameter family of mass at their birth

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...188...13y&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 188, no. 1, Dec. 1987, p. 13-23. CNRS-supported research.

Astronomy and Astrophysics

Astrophysics

138

Galactic Evolution, Galactic Structure, Star Formation, Stellar Mass Ejection, Stellar Winds, Supernovae, Dwarf Galaxies, Elliptical Galaxies, Globular Clusters, Stellar Luminosity

Scientific paper

A supernova-driven wind model for spheroidal systems is constructed using an evolutionary method of population synthesis. An assumed relation between binding energy and mass for protoclouds gives a star formation rate (SFR) per unit mass which is proportional to a negative power of mass. With such a SFR and a universal initial mass function, the structural and chemical properties of elliptical galaxies, dwarf elliptical galaxies, and globular clusters were successfully reproduced. The chemical and photometric properties of the systems are monotonically related to their mass. The expansion of a system due to galactic mass loss changes the structural properties most significantly for dwarf elliptical galaxies, and brings about the distinct sequences of ellipticals, dwarfs, and globulars in the diameter-surface brightness (D-SB) diagram. It is suggested that the spheroidal systems were subject to a single relationship at their birth over the range of 10 billion in mass, although an extra parameter seems to be necessary for bright ellipticals to fit the sequence in the D-SB diagram. The previous criticism that the simple model of mass loss cannot reproduce the low metallicities of dwarf galaxies is removed if the observed metallicities are compared with the average of stellar metallicities weighted by their luminosities.

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