Forming disc galaxies in ΛCDM simulations

被引:519
作者
Governato, F.
Willman, B.
Mayer, L.
Brooks, A.
Stinson, G.
Valenzuela, O.
Wadsley, J.
Quinn, T.
机构
[1] Univ Washington, Dept Astron, Seattle, WA 98195 USA
[2] INAF, Osservatorio Astron Brera, I-20121 Milan, Italy
[3] NYU, Dept Phys, New York, NY 10003 USA
[4] ETH, CH-8092 Zurich, Switzerland
[5] McMaster Univ, Dept Phys & Astron, Hamilton, ON L88 4M1, Canada
关键词
methods : N-body simulations; galaxies : evolution; galaxies : formation;
D O I
10.1111/j.1365-2966.2006.11266.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 270 km s(-1) in a Lambda 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.
引用
收藏
页码:1479 / 1494
页数:16
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