Forming disc galaxies in ΛCDM simulations

By Fabio Governato, B. Willman, Lucio Mayer, A. Brooks, G. Stinson, Octavio Valenzuela, James Wadsley, Thomas Quinn. 2006

492 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ba5648b71786a74d8bc072c4249261899b891b69

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A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “In more massive halos where gas is retained and star formation can begin, further suppression is expected from supernova feedback (Dekel & Silk 1986; Benson et al. 2002; Dekel & Woo 2003; Governato et al. 2007).”
The enrichment of the intergalactic medium with adiabatic feedback – I. Metal cooling and metal diffusion (2009, methodology): “This model has been calibrated via numerous galaxy formation studies (e.g., Governato et al. 2007).”
THE DUAL ORIGIN OF STELLAR HALOS (2009, methodology): “We focus here on MW1hr, as it was chosen to have a total mass and merger history similar to that of the Milky Way (Governato et al. 2007), making it a good candidate to compare with previous works which have also focused on simulating Milky Way-like stellar halos.”
THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND (2011, methodology): “…McGaugh & de Blok 1998a; Mo et al. 1998; Courteau & Rix 1999; Steinmetz & Navarro 1999; Courteau & Rix 1999; van den Bosch 2000; Bullock et al. 2001; Mo & Mao 2004; Mayer & Moore 2004; Gnedin et al. 2007; Governato et al. 2007; Trujillo-Gomez et al. 2010; de Rossi et al. 2010; Tonini et al. 2010).”
The kinematic connection between galaxies and dark matter haloes (2010, methodology): “However, as shown by Dutton & Courteau (2008) the simulated galaxies from Governato et al. (2007) do not fall on the TF relation (V2.”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, background): “This progress raises the question of what cut the Gordian knot that had allowed only incremental advances for many years (Governato et al. 2004, 2007; Robertson et al. 2004; Scannapieco et al. 2008, 2009, 2011; Sales c© 2013 RAS ar X iv :1 30 5.”
Idealized models for galactic disc formation and evolution in ‘realistic’ ΛCDM haloes (2012, background): “This should help us understand the failure or success of various fully cosmological simulations of disc galaxy formation, which still suffer from a multitude of uncertainties (e.g. Governato et al. 2007; CS09; Guedes et al. 2011; Scannapieco et al. 2012).”
The Evolution of Galaxy Structure Over Cosmic Time (2014, background): “Governato et al. (2007) show that disk galaxies can be simulated which have properties that match the morphological properties and kinematics of nearby disks, although this simulation is not in a cosmological context.”
The effects of gas on morphological transformation in mergers: implications for bulge and disc demographics (2009, background): “This has since been borne out in cosmological simulations (Governato et al. 2007, 2008), and may be seen in observations of high-redshift discs that are perhaps reforming after mergers (van Dokkum et al. 2004; Kassin et al. 2007; Genzel et al. 2008; Puech et al. 2008; Robertson & Bullock 2008a;…”
Theoretical Challenges in Galaxy Formation (2016, background): “The ’delayed cooling model significantly reduces the galaxy stellar masses and promotes the formation of disk dominated systems (Governato et al. 2007; Guedes et al. 2011; Keller, Wadsley & Couchman 2016).”
The Causes of Halo Shape Changes Induced by Cooling Baryons: Disks versus Substructures (2007, background): “Baryonic cooling inside substructures is strongly suppressed by feedback from supernovae (Dekel & Silk 1986; Governato et al. 2004, 2007).”
Evolution of magnetic fields in galaxies and future observational tests with the Square Kilometre Array (2008, background): “Recent models of disk formation have included hierarchical dark matter cosmology, gas cooling, star formation, and supernova (SN) feedback (Governato et al. 2007; Stringer & Benson 2007) and benefitted from the increased resolution of numerical simulations (Mayer et al. 2008).”
BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, background): “…1996; Navarro & Steinmetz 1997; Gnedin 2000; Hoeft et al. 2006; Okamoto et al. 2008; Madau et al. 2008), and supernova feedback further suppressing star formation at the more massive subhalo end (Dekel & Silk 1986; Benson et al. 2002; Dekel & Woo 2003; Governato et al. 2007; Busha et al. 2010).”
METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, background): “…and semi-analytic models (SAM) are not really satisfactory (Springel & Hernquist 2003; Kobayashi 2004; Cen & Ostriker 2006; Oppenheimer & Davé 2006; Governato et al. 2007), because they operate on scales too small to be resolved, and have to be incorporated via simplistic recipes that sometimes…”
HOW DO DISKS SURVIVE MERGERS? (2008, methodology): “THE EXISTENCE OF DISKS IN MAJOR MERGER REMNANTS Robertson et al. (2006a) and Springel & Hernquist (2005), and subsequently Governato et al. (2007) and Naab et al. (2006) have demonstrated that even major mergers can leave remnants with non-negligible disk components.”
The birth of a galaxy – II. The role of radiation pressure (2012, background): “One approach is to neglect radiative cooling within the blastwave, allowing it to adiabatically expand (e.g. Thacker & Couchman 2000; Governato et al. 2007; Guedes et al. 2011).”
The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs (2016, methodology): “Due to the computational cost, simulation studies have often relied on rerunning a small number of large volumes while only changing one parameter at a time (e.g. Schaye et al. 2015), only rarely running grids of simplified models (Governato et al. 2007).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, background): “For ex ample, Governato et al. (2007) produced disk galaxies spanning a decade in mass that seem to fit both the I-band TF relation and the baryonic TF relation very well, as well as the observed abundance of Milky Way (MW) type satellites.”