The edge of galaxy formation II: evolution of Milky Way satellite analogues after infall

Abstract

In the first paper we presented 27 hydrodynamical cosmological simulations of galaxies with total masses between $5\times 10^8$ and $10^{10}{\mathrm{M}}_{\odot }$. In this second paper we use a subset of these cosmological simulations as initial conditions (ICs) for more than forty hydrodynamical simulations of satellite and host galaxy interaction. Our cosmological ICs seem to suggest that galaxies on these mass scales have very little rotational support and are velocity dispersion ($\sigma$) dominated. Accretion and environmental effects increase the scatter in the galaxy scaling relations (e.g. size - velocity dispersion) in very good agreement with observations. Star formation is substantially quenched after accretion. Mass removal due to tidal forces has several effects: it creates a very flat stellar velocity dispersion profiles, and it reduces the dark matter content at all scales (even in the centre), which in turn lowers the stellar velocity on scales around 0.5 kpc even when the galaxy does not lose stellar mass. Satellites that start with a cored dark matter profile are more prone to either be destroyed or to end up in a very dark matter poor galaxy. Finally, we found that tidal effects always increase the "cuspyness" of the dark matter profile, even for haloes that infall with a core.

13 pages, 15 figures, accepted to be published in MNRAS (with minor changes to the published version). This is the second paper of a series of two. The first paper can be found here arXiv:1707.01106

References in corpus (11)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• Introducing the Illustris Project: Simulating the coevolution of dark and visible matter in the Universe
• Too big to fail? The puzzling darkness of massive Milky Way subhaloes
• Astrophysics Source Code Library
• Star Formation and Feedback in Smoothed Particle Hydrodynamic Simulations--I. Isolated Galaxies
• The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time
• High-resolution mass models of dwarf galaxies from LITTLE THINGS
• Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter
• The edge of galaxy formation I: formation and evolution of MW-satellites analogues before accretion
• Spectroscopy of the three distant Andromedan satellites Cassiopeia III, Lacerta I, and Perseus I
• The Effects of Ram-pressure Stripping and Supernova Winds on the Tidal Stirring of Disky Dwarfs: Enhanced Transformation into Dwarf Spheroidals

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• Structure and kinematics of tidally limited satellite galaxies in LCDM
• Tucana B: A Potentially Isolated and Quenched Ultra-faint Dwarf Galaxy at D$\approx$1.4 Mpc
• Creating a galaxy lacking dark matter in a dark matter dominated universe
• The effect of tides on the Sculptor dwarf spheroidal galaxy
• Self-interacting dark matter interpretation of Crater II
• The cusp-core problem in gas-poor dwarf spheroidal galaxies
• The edge of galaxy formation III: The effects of warm dark matter on Milky Way satellites and field dwarfs
• The Stellar Kinematics of Void Dwarf Galaxies Using KCWI
• Trial by FIRE: Probing the dark matter density profile of dwarf galaxies with GraphNPE
• Coupled DM heating in SCDEW cosmologies
• Warm dark matter model with a few keV mass is bad for the too-big-to-fail problem
• Clues to the nature of dark matter from first galaxies
• LYRA II: Cosmological dwarf galaxy formation with inhomogeneous Population III enrichment
• Galactic tides and the Crater II dwarf spheroidal: a challenge to LCDM?