Forming disc galaxies in ΛCDM simulations
Fabio Governato,Fabio Governato,Beth Willman,Lucio Mayer,Alyson Brooks,Gregory S. Stinson,Octavio Valenzuela,James Wadsley,Thomas R. Quinn +8 more
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TL;DR: In this article, the authors 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 270km s -1 in a cold dark matter (CDM) universe.
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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 270km s -1 in a A 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 / 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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Citations
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Tommaso Zana,Pedro R. Capelo,Massimo Dotti,Massimo Dotti,Lucio Mayer,Alessandro Lupi,Francesco Haardt,Francesco Haardt,Silivia Bonoli,Silivia Bonoli,Sijing Shen +10 more
TL;DR: In this paper, the authors analyse and describe the outcome of two particular simulations taken from the Eris suite, ErisBH and Eris2k, which mainly differ in the prescriptions employed for gas cooling, star formation, and feedback from supernovae and black holes.
DM haloes in the fifth-force cosmology
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Empirically Constrained Predictions for Metal-Line Emission from the Circumgalactic Medium
TL;DR: In this paper, a high-resolution cosmological simulation of a Milky Way-like galaxy was used to examine the effect on the absorption and emission properties of metals in the CGM.
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The imprint of satellite accretion on the chemical and dynamical properties of disc galaxies
T. Ruiz-Lara,C. G. Few,Brad K. Gibson,I. Pérez,Estrella Florido,Ivan Minchev,Patricia Sanchez-Blazquez +6 more
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TL;DR: In this paper, a set of eight Milky Way-sized cosmological simulations performed using the AMR code Adaptive Refinement Tree + Hydrodynamics in a λCDM cosmology is presented.
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