The properties of satellite galaxies in simulations of galaxy formation

By T. Okamoto, Carlos S. Frenk, Adrian Jenkins, Tom Theuns. 2009

133 citations recorded by the source corpus.

We investigate the properties of satellite galaxies in cosmological N-body/smooth particle hydrodynamics simulations of galaxy formation in Milky Way-sized haloes. Because of their shallow potential wells, satellite galaxies are very sensitive to heating processes which affect their gas content. Their properties can therefore be used to constrain the nature of feedback processes that regulate galaxy formation. In our simulations, we assume that all the energy produced by supernovae is used as kinetic energy to drive galactic winds. Several of our simulations produce bright, disc-dominated galaxies. We find that wind models in which the wind speed, ν w , is proportional to the local velocity dispersion of the dark matter, σ (and thus the wind mass-loading, η w ∝ σ ―2 ), make star formation in satellites sporadic, reproduce the observed satellite luminosity function reasonably well (down to M ν = -7) and match the luminosity-metallicity relation observed in the Local Group satellites. By contrast, models that assume a constant wind speed overproduce faint satellites and predict an incorrect luminosity-metallicity relation. Our simulations therefore suggest that the feedback processes that operate on the scale of satellite galaxies should generate galactic outflows whose mass-loading varies inversely with the depth of the potential.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/dfa38e19174f5e80cc225f3e00be3761be544a0f

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Citations in the corpus

A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “…allowed for star formation at lower densities (< 1 amu/cc), and hence found that baryons either steepened the inner densities or had little affect (Sales et al. 2007; Okamoto et al. 2010; Nickerson et al. 2011; Wadepuhl & Springel 2011; Parry et al. 2012; Di Cintio et al. 2012; Sawala et al. 2012).”
ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, background): “…and momentum injection, ∼ 50 − 100 pc, and On the interplay between star formation and feedback 13 the scale of measurement,∼ 2−20 kpc, and are therefore predictions of the simulations and not a result of any galactic wind model assumptions (see e.g. Okamoto et al. 2010; Vogelsberger et al. 2013).”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, result): “This is consistent with results of previous work (Bullock et al. 2000; Somerville 2002; Benson et al. 2003; Gnedin & Kravtsov 2006; Okamoto et al. 2010) We explore this point further in Fig.”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, methodology): “…Springel & Hernquist 2003a; Brook et al. 2004; Oppenheimer & Davé 2006; Stinson et al. 2006; Dubois & Teyssier 2008; Dalla Vecchia & Schaye 2008; Okamoto et al. 2010; Piontek & Steinmetz 2011; Dalla Vecchia & Schaye 2012; Stinson et al. 2013), and more recently also AGN feedback (e.g.,…”
Quenching and ram pressure stripping of simulated Milky Way satellite galaxies (2017, background): “…studies of MW analog satellite systems have typically focused either on one to a few high resolution cosmological models with gas physics (Okamoto et al. 2010; Zolotov et al. 2012; Wetzel et al. 2016) or have focused on a large suite of dark matter only models that better probe cosmic…”
The illustris simulation: Public data release (2015, background): “t al. (2013); Faucher-Giguere et al. (2009); Ferland et al. (1998); Katz et al. (1996); Cen (1992). Galactic-scale stellar feedback: Puchwein and Springel (2013); Oppenheimer and Dave (2008, 2006); Okamoto et al. (2010); Springel and Hernquist (2003). BH and AGN feedback: Di Matteo et al. (2008); Sp”
THE GHOSTS SURVEY. I. HUBBLE SPACE TELESCOPE ADVANCED CAMERA FOR SURVEYS DATA (2011, background): “…has sparked much debate as it places strong constraints on the nature of dark matter (e.g., Zentner & Bullock 2003; Strigari et al. 2007; Polisensky & Ricotti 2011) as well as the behavior of baryons in dark-matter potentials (e.g., Bullock et al. 2000; Ricotti & Gnedin 2005; Okamoto et al. 2010).”
How Stellar Feedback Simultaneously Regulates Star Formation and Drives Outflows (2015, background): “In SAMs (e.g.Croton et al. 2006; Somerville et al. 2008; Guo et al. 2011, 2013; White et al. 2015) and cosmological simulations (Okamoto et al. 2010; Vogelsberger et al. 2013; Torrey et al. 2014; cf. e.g.Oppenheimer & Davé 2008; Schaye et al. 2015), it is common to assume that the outflow…”
The properties of warm dark matter haloes (2013, methodology): “Recent hydrodynamic simulations have confirmed this conclusion originally deduced from semi-analytical models of galaxy formation (Okamoto et al. 2010; Wadepuhl & Springel 2011).”
The Aquila comparison project: the effects of feedback and numerical methods on simulations of galaxy formation (2011, methodology): “The TO model is described in Okamoto et al. (2010) and is based on an early version of the GADGET3 code.”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, background): “Okamoto et al. (2010) investigated the effect of different recipes for the kinetic feedback driving galactic winds, on the global properties of the Milky Way satellite model galaxies.”
The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time (2016, methodology): “We set the wind velocity equal to 3.46σ 1DDM , where σ 1D DM is the local 1D dark matter velocity dispersion (see e.g. Okamoto et al. 2010), which is calculated from the nearest 64 dark matter particles.”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, background): “…make the feedback depend on properties defined by the dark matter, such as its local velocity dispersion or halo mass (e.g. Oppenheimer & Davé 2006; Okamoto et al. 2010; Oppenheimer et al. 2010; Puchwein & Springel 2013; Vogelsberger et al. 2013, 2014b), which are generally better converged than…”
Shaping the galaxy stellar mass function with supernova- and AGN-driven winds (2012, unknown): “Okamoto et al. (2010) assumed an energy-driven wind scenario in which the wind properties scale according to vw ∼ σ and η ∼ 1/v 2 w ∼ 1/σ 2.”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, methodology): “They calculate η for winds also using the inner velocity dispersion, with a scaling of η ∝ v−2c for vc < 75 km s−1 and η ∝ v−1c for vc > 75 km s−1.6 The exact feedback 5 Okamoto et al. (2010) actually suggest that vmax is related to the velocity dispersion of gas.”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, methodology): “…wind mass loading scales with the inverse of the wind velocity squared, motivated by energy conservation arguments (see also Oppenheimer & Davé 2008; Okamoto et al. 2010; Puchwein & Springel 2013); and a model for black hole seeding, accretion and feedback that we will describe in more detail in…”
Theoretical Challenges in Galaxy Formation (2016, methodology): “Alternatively, an energy driven wind model has been proposed (Okamoto et al. 2010) to explain the low abundance of satellite galaxies in the Milky Way.”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, methodology): “…the popular convention of prescribing feedback parameters according to local conditions inferred from neighbouring dark matter particles (Oppenheimer & Davé 2006, 2008; Okamoto et al. 2010; Oppenheimer et al. 2010; Puchwein & Springel 2013; Vogelsberger et al. 2013, 2014a; Khandai et al. 2014).”