The baryonic assembly of dark matter haloes

By C. Faucher-Giguére, D. Keres̆, Chung-Pei Ma. 2011

232 citations recorded by the source corpus.

We use a suite of cosmological hydrodynamic simulations to systematically quantify the accretion rates of baryons into dark matter haloes and the resulting baryon mass fractions, as a function of halo mass, redshift and baryon type (including cold and hot gas). We find that the net baryonic accretion rates through the virial radius are sensitive to galactic outflows and explore a range of outflow parameters to illustrate the effects. We show that the cold gas accretion rate is in general not a simple universal factor of the dark matter accretion rate, and that galactic winds can cause star formation rates to deviate significantly from the external gas accretion rates, both via gas ejection and re-accretion. Furthermore, galactic winds can inject enough energy and momentum in the surrounding medium to slow down accretion altogether, especially in low-mass haloes and at low redshift, but the impact of outflows is suppressed with increasing halo mass. By resolving the accretion rates versus radius from the halo centres, we show how cold streams penetrate the hot atmospheres of massive haloes at z≥ 2, but gradually disappear at lower redshift. The total baryon mass fraction is also strongly suppressed by outflows in low-mass haloes, but is nearly universal in the absence of feedback in haloes above the UV background suppression scale, corresponding to circular velocities vc∼ 50 km s−1. The transition halo mass, at which the gas mass in haloes is equal for the cold and hot components, is roughly constant at ∼1011.5 M⊙ and does not depend sensitively on the wind prescription. We provide simple fitting formulae for the cold gas accretion rate and the corresponding efficiency with which dark matter channels cold gas into haloes in the no-wind case. Finally, we show that cold accretion is broadly consistent with driving the bulk of the highly star-forming galaxies observed at z∼ 2, but that the more intense star formers likely sample the high end of the accretion rate distribution, and may be additionally fuelled by a combination of gas recycling, gas re-accretion, hot mode cooling and mergers.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/66fb6719f75670d3222d54843424c490938ac0ce

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Citations in the corpus

THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “…forces and possibly dissipation and interaction with feedback-driven winds (Nelson et al. 2015), so that their radial distribution and fate can be quite different (Faucher-Giguère et al. 2011; van de Voort et al. 2011; van de Voort & Schaye 2012; Wetzel & Nagai 2015; Feldmann & Mayer 2015).”
THE BIMODAL METALLICITY DISTRIBUTION OF THE COOL CIRCUMGALACTIC MEDIUM AT z ≲ 1 (2013, background): “…Maller & Bullock 2004; Dekel & Birnboim 2006), while feedback from star formation and AGN activity can fuel massive outflows from a gas-rich galaxy that may choke off star formation (e.g., Kacprzak et al. 2008; Oppenheimer et al. 2010, 2012; Fumagalli et al. 2011b; Faucher-Giguère et al. 2011).”
The neutral hydrogen content of galaxies in cosmological hydrodynamic simulations (2013, background): “The third possibility is also unlikely to be happening in our simulations, since we do not explicitly add any sort of preheating, nor do we explicitly vary the dark matter accretion rates from the usual ΛCDM expectations (e.g. Neistein & Dekel 2008; Faucher-Giguere et al. 2011).”
Full-data Results of Hubble Frontier Fields: UV Luminosity Functions at z ∼ 6–10 and a Consistent Picture of Cosmic Reionization (2017, background): “The parameter range of Mtrunc is −16 to −10; Mtrunc = −16 mag corresponds to the detection limit of current observations, and Mtrunc = −10 mag is the magnitude of minimium halos which have star forming galaxies predicted by Faucher-Giguère et al. (2011).”
THE CHARACTERISTIC STAR FORMATION HISTORIES OF GALAXIES AT REDSHIFTS z ∼ 2–7 (2012, background): “104 K) is model dependent and highly uncertain, with suggested values of ǫ ≃ 0.4 − 0.8 (e.g., Bouché et al. 2010; Faucher-Giguère et al. 2011).”
Neutral hydrogen in galaxy haloes at the peak of the cosmic star formation history (2014, background): “…z = 4 and z = 3 have disappeared as virial shocks are no longer cooling rapidly relative to gas infall (e.g., Birnboim & Dekel 2003; Kereš et al. 2005, 2009; Faucher-Giguère et al. 2011; Nelson et al. 2013). c© 0000 RAS, MNRAS 000, 000–000 Neutral hydrogen in z = 2 − 4 galaxy halos 19 2.02.53.03.”
FIRE in the field: Simulating the threshold of galaxy formation (2016, background): “The corresponding 4 This is usually defined as the mass at which a typical halo has a baryon fraction that is suppressed by 50% relative to fb owing solely to UV background feedback (Gnedin 2000; Dijkstra et al. 2004; Hoeft et al. 2006; Okamoto et al. 2008; see also Faucher-Giguère et al. 2011).”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, methodology): “The sum of the baryon fraction and the expelled fraction is far below unity at all times, suggesting that the UV background plays a role in preventing accretion continuously, starting at very high redshifts (Gnedin 2000; Faucher-Giguère et al. 2011).”
Star formation sustained by gas accretion (2014, background): “Faucher-Giguère et al. (2011) showed from simulations that a factor of 2 increase in the mass loading factor or a factor of 2 increase in the wind speed affect most sensitively the accretion rate at the virial radius without much effect on the cold gas accretion rate to the center.”
Moving mesh cosmology: tracing cosmological gas accretion (2013, background): “The resulting maximum past temperature Tmax value is compared to some temperature threshold (Kereš et al. 2005, 2009; van de Voort et al. 2011; Faucher-Giguère et al. 2011).”
THE GASEOUS ENVIRONMENT OF HIGH-z GALAXIES: PRECISION MEASUREMENTS OF NEUTRAL HYDROGEN IN THE CIRCUMGALACTIC MEDIUM OF z ∼ 2–3 GALAXIES IN THE KECK BARYONIC STRUCTURE SURVEY (2012, background): “…have halo masses comparable to the theoretically expected transition mass between “cold mode” and “hot mode” accretion (van de Voort et al. 2011b; Faucher-Giguère et al. 2011; Kereš et al. 2009; Ocvirk et al. 2008); most of these authors predict that both hot and cold accretion occur in such…”
The impact of star formation feedback on the circumgalactic medium (2016, background): “…feedback models on the star formation rate, inflow and outflow rates, and the CGM structure and corresponding observables are studied (e.g., Faucher-Giguère et al. 2011; Oppenheimer et al. 2010; Nelson et al. 2015; Hummels et al. 2013; Suresh et al. 2015b; Marasco et al. 2015; Rahmati et…”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “…of galaxy stellar mass in the present–day Universe provides important clues to answering fundamental questions concerning the cosmic assembly of baryons in the Λ-cold dark matter (ΛCDM) paradigm (Fukugita et al. 1998; Kereš et al. 2005; Faucher-Giguère et al. 2011; Davé et al. 2012).”
A unified model for galactic discs: star formation, turbulence driving, and mass transport (2017, methodology): “The formula for in is the result of a fit to the results of a series of SPH simulations run by Faucher-Giguère et al. (2011), and it is calibrated to be most accurate for z > 2.”
HUBBLE FRONTIER FIELDS FIRST COMPLETE CLUSTER DATA: FAINT GALAXIES AT z ∼ 5–10 FOR UV LUMINOSITY FUNCTIONS AND COSMIC REIONIZATION (2014, background): “…in this study we assume two Mtrunc values that bracket the plausible range of the parameter; Mtrunc = −17 mag corresponding to the current observational limit and Mtrunc = −10 mag being the predicted magnitude of minimum-mass halos that can host star-forming galaxies (Faucher-Giguère et al. 2011).”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, background): “…much, if not most, of the fuel supply for massive galaxies at later times owes to recycled wind material trapped in the CGM in these hot halos (see Oppenheimer et al. 2010; Davé et al. 2011b; Faucher-Giguère et al. 2011; Christensen et al. 2016; Muratov et al. 2017; AnglésAlcázar et al. 2017a).”