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Title:
Forming disc galaxies in ΛCDM simulations
Authors:
Governato, F.; Willman, B.; Mayer, L.; Brooks, A.; Stinson, G.; Valenzuela, O.; Wadsley, J.; Quinn, T.
Affiliation:
AA(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA; INAF, Osservatorio Astronomico di Brera, via Brera 29, 20121 Milano, Italy), AB(NYU, Department of Physics, 4 Washington Place, New York, NY 10003, USA), AC(ETH, Ramistrasse 101, CH-8092 Zurich, Switzerland), AD(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AE(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AF(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AG(Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L88 4M1, Canada), AH(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 374, Issue 4, pp. 1479-1494. (MNRAS Homepage)
Publication Date:
02/2007
Origin:
MNRAS
MNRAS Keywords:
methods: N-body simulations, galaxies: evolution, galaxies: formation
DOI:
10.1111/j.1365-2966.2006.11266.x
Bibliographic Code:
2007MNRAS.374.1479G

Abstract

We used fully cosmological, high-resolution N-body + smooth particle hydrodynamic (SPH) simulations to follow the formation of disc galaxies with rotational velocities between 135 and 270kms-1 in a Λ cold dark matter (CDM) universe. The simulations include gas cooling, star formation, the effects of a uniform ultraviolet (UV) background and a physically motivated description of feedback from supernovae (SNe). The host dark matter haloes have a spin and last major merger redshift typical of galaxy-sized haloes as measured in recent large-scale N-body simulations. The simulated galaxies form rotationally supported discs with realistic exponential scalelengths and fall on both the I band and baryonic Tully-Fisher relations. An extended stellar disc forms inside the Milky Way (MW)-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 MW-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. We discuss how 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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