The Evolution of Disk Galaxies over Cosmic Ages

Details The Evolution of Disk Galaxies over Cosmic Ages The Evolution of Disk Galaxies over Cosmic Ages

Publishing date

Jun 2006

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.5303b&link_type=abstract

Journals

American Astronomical Society Meeting 208, #53.03; Bulletin of the American Astronomical Society, Vol. 38, p.133

Science

Mathematics

Field

Logic

Type

Scientific paper

Abstract

We used fully cosmological, high resolution N-body + SPH simulations to follow the formation of disk galaxies with rotational velocities between 135 and 270 km/sec in a Lambda CDM universe. The simulations include gas cooling, star formation, the effects of a uniform UV background and a physically motivated description of feedback from supernovae. The simulated galaxies form rotationally supported disks with realistic exponential scale lengths and fall on both the I-band and baryonic Tully Fisher relations. An extended stellar disk forms inside the Milky Way sized halo immediately after the last major merger. The combination of UV background and SN feedback drastically reduces the number of visible satellites orbiting inside a Milky Way sized halo, bringing it in fair agreement with observations. Our simulations predict that the average age of a primary galaxy's stellar population decreases with mass, because feedback delays star formation in less massive galaxies. Galaxies have stellar masses and current star formation rates as a function of total mass that are in good agreement with observational data. Both high mass and force resolution and a realistic description of star formation and feedback are important ingredients to match the observed properties of galaxies.

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