How do galaxies get their gas

By Neal Katz, D. Keres̆, R. Dav'e, D. Weinberg. 2002

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Not the way one might have thought. In hydrodynamic simulations of galaxy formation, some gas follows the traditionally envisioned route, shock heating to the halo virial temperature before cooling to the much lower temperature of the neutral ISM. But most gas enters galaxies without ever heating close to the virial temperature, gaining thermal energy from weak shocks and adiabatic compression, and radiating it just as quickly. This “cold mode” accretion is channeled along filaments, while the conventional, “hot mode” accretion is quasi-spherical. Cold mode accretion dominates high redshift growth by a substantial factor, while at z < 1 the overall accretion rate declines and hot mode accretion has greater relative importance. The decline of the cosmic star formation rate at low z is driven largely by geometry, as the typical cross section of filaments begins to exceed that of the galaxies at their intersections.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Feedback and recycled wind accretion: assembling the z= 0 galaxy mass function (2009, background): “More recently, “cold mode” accretion was argued to be responsible for most of the gas supply into galaxies across cosmic time (Katz et al. 2003; Kereš et al. 2005, hereafter K05; Dekel & Birnboim 2006).”
Bursting and quenching in massive galaxies without major mergers or AGNs (2007, background): “The success of the spherical model in predicting the threshold mass as seen in cosmological hydrodynamical simulations (Kereš et al. 2005; Dekel & Birnboim 2006) is demonstrated in Fig.”
The physics driving the cosmic star formation history (2009, background): “…& Ostriker 2000; Pearce et al. 2001; Ascasibar et al. 2002; Murali et al. 2002; Sommer-Larsen, Götz & Portinari 2003; Springel & Hernquist 2003b; Kereš et al. 2005; Nagamine et al. 2006; Di Matteo et al. 2008; Oppenheimer & Davé 2008; Choi & Nagamine 2009; Crain et al. 2009; Booth & Schaye…”
Neutral hydrogen in nearby elliptical and lenticular galaxies: the continuing formation of early-type galaxies (2006, background): “Another possibility is that the neutral hydrogen comes from smooth, cool accretion of the IGM (see, e.g., Keres et al. 2005 and refs therein): in this case we do not expect a major star formation event that would leave a distinct marker in the stellar population as would be the case in a merger,…”
A study of the gas–star formation relation over cosmic time (2010, result): “This conclusion is consistent with other observational (e.g. Förster Schreiber et al. 2006, 2009; Erb 2008; Genzel et al. 2008) and theoretical findings (Kereš et al. 2005; C© 2010 The Authors.”
Lyα blobs as an observational signature of cold accretion streams into galaxies (2009, background): “…which show that baryons assemble into galaxies through a two-phase medium which contains filamentary streams of cold (T ∼ 104 K) gas embedded within a hot gaseous halo (e.g Kereš et al. 2005; Dekel & Birnboim 2006; Ocvirk et al. 2008; Dekel et al. 2009; Kereš et al. 2009; Agertz et al. 2009).”
Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, methodology): “We use SKID2 (Spline Kernel Interpolative Denmax) to identify galaxies as bound groups of star-forming gas and stars (Kereš et al. 2005; Oppenheimer et al. 2010).”
Disc formation and the origin of clumpy galaxies at high redshift (2009, background): “…a mass of Mvir ∼ 3.5 × 1011 M , while the total baryonic mass in the disc (disregarding the bulge) is Mbar ∼ 2.4 × 1010 M out of which 50 per cent is gas, putting it in a regime where both cold flows and stable shocks can exist (Kereš et al. 2005; Dekel & Birnboim 2006; Ocvirk et al. 2008).”
Chaotic cold accretion on to black holes (2013, background): “In recent years, there has been a revolution in the field of galaxy formation driven by the realization that many galaxies accrete primarily in the cold mode (e.g. Kereš et al. 2005), rather than in the hot mode.”
The impact of angular momentum on black hole accretion rates in simulations of galaxy formation (2013, background): “We can expect that this creates a difference in the mode by which gas is supplied to the central galaxy (White & Frenk 1991; Kereš et al. 2005; Dekel & Birnboim 2006; Van de Voort et al. 2010): in lower mass haloes, accreted gas flows almost directly on to the galaxy, fuelling a cold gas disc at…”
The neutral hydrogen content of galaxies in cosmological hydrodynamic simulations (2013, methodology): “The current paradigm for galaxy evolution rests on the tenet that gas flows into and out of galaxies are primarily responsible for governing galaxy growth (e.g. Kereš et al. 2005; Dekel et al. 2009; Davé, Finlator, & Oppenheimer 2012, and references therein).”
The correlation of star formation quenching with internal galaxy properties and environment (2008, background): “Galaxies in smaller mass haloes (Mhalo 1012 M ) likely accrete most of their gas in a ‘cold flow’, and never form a hot halo (Birnboim & Dekel 2003; Kereš et al. 2005; Dekel & Birnboim 2006).”
Galaxy bimodality versus stellar mass and environment (2006, background): “…for galaxies below and above the transition mass may be related to the balance between hydrostatic versus rapid cooling (Birnboim & Dekel 2003; Kereš et al. 2005; Bower et al. 2006; Croton et al. 2006), or to the diversity of star formation histories of satellite galaxies at low masses…”
Galaxy merger morphologies and time-scales from simulations of equal-mass gas-rich disc mergers (2008, background): “…degree present-day galaxies are assembled discretely via the merger of pre-existing galaxies (e.g. Kauffmann, White, & Guideroni 1993; Somerville, Primack, & Faber 2001) or through more continuous processes such as cold gas and dark matter accretion (e.g. Kereš et al. 2005; Dekel & Birnboim 2006).”
The properties of the star-forming interstellar medium at z = 0.84-2.23 from HiZELS : mapping the internal dynamics and metallicity gradients in high-redshift disc galaxies. (2012, background): “…halo, through minor mergers or by cold streams from the intergalactic medium (IGM), appears to dominate over that from major mergers and suggests that the star formation within the interstellar medium (ISM) of high-redshift galaxies is driven by internal dynamical processes (Kereš et al. 2005).”
Dynamical Properties of z ~ 2 Star-forming Galaxies and a Universal Star Formation Relation (2007, background): “Given that the kinematics of UVand optical star-forming galaxies are consistent with that of large protodisks, these systems may have evolved in a less violent fashion through a series ofminor mergers, or through cold gas flows from the halo (Keres et al. 2005; Dekel & Birnboim 2006).”
THE COSMOS2015 CATALOG: EXPLORING THE 1 < z < 6 UNIVERSE WITH HALF A MILLION GALAXIES (2016, background): “However, recent hydrodynamical simulations now suggest however now that most of the gas is accreted directly from cold dense filaments without being shockheated (Katz et al. 2003; Kereš et al. 2005; Ocvirk et al. 2008; Dekel et al. 2009) at least for lower-mass haloes at high redshift.”
The baryonic assembly of dark matter haloes (2011, background): “While previous work has investigated the detailed physics of gas accretion (e.g. Kereš et al. 2005, 2009a; Ocvirk et al. 2008), with some broad considerations of the accretion rates into haloes and galaxies, no previous study has systematically quantified the baryonic accretion rates a function of…”