Galaxies in a simulated ΛCDM Universe – I. Cold mode and hot cores

By D. Kerevs, Neal Katz, Mark A. Fardal, R. Dav'e, David H. Weinberg HarvardCFA, Umass, U. Arizona, Ohio-State. 2008

592 citations recorded by the source corpus.

We study the formation of galaxies in a large volume (50 h −1 Mpc, 2 × 288 3 particles) cosmological simulation, evolved using the entropy and energy-conserving smoothed particle hydrodynamics (SPH) code GADGET-2. Most of the baryonic mass in galaxies of all masses is originally acquired through filamentary ‘cold mode’ accretion of gas that was never shock heated to its halo virial temperature, confirming the key feature of our earlier results obtained with a different SPH code. Atmospheres of hot, virialized gas develop in haloes above 2–3 × 10 11 M � , a transition mass that is nearly constant from z = 3 to 0. Cold accretion persists in haloes above the transition mass, especially at z ≥ 2. It dominates the growth of galaxies in low-mass haloes at all times, and it is the main driver of the cosmic star formation history. Our results suggest that the cooling of shock-heated virialized gas, which has been the focus of many analytic models of galaxy growth spanning more than three decades, might be a relatively minor element of galaxy formation. At high redshifts, satellite galaxies have gas accretion rates similar to central galaxies of the same baryonic mass, but at z < 1t he accretion rates of low-mass satellites are well below those of comparable central galaxies. Relative to our earlier simulations, the GADGET-2 simulations predict much lower rates of ‘hot mode’ accretion from the virialized gas component. Hot accretion rates compete with cold accretion rates near the transition mass, but only at z ≤ 1. Hot accretion is inefficient in haloes

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4afe175dab03bbebb9c1c04cdb6424fc191708da

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. A. Dekel
6. Volker Springel
7. E. Quataert
8. D. Keres̆

Citations in the corpus

• The n ature of submillimetre galaxies in cosmological hydrodynamic simulations (2009, background): “It turns out this is not viable in a cold mode accretiondriven scenario, where the star formation rate is strongly limited by the gas supply rate, which in turn is set predominantly by the gravitational accretion rate (Kereš et al. 2005; Dekel & Birnboim 2006; Kereš et al. 2009).”
• The baryonic assembly of dark matter haloes (2011, methodology): “In addition to shocking, the decreasing cold gas accretion rates with decreasing radius are caused by accretion by satellite galaxies on the way down to the centre of the main halo (e.g. Kereš et al. 2009a; Simha et al. 2009).”
• Cosmic X-ray surveys of distant active galaxies (2015, background): “…halo models, ≈ 1013 M broadly corresponds to the maximum mass where a halo can support a large cold-gas supply—the gas in halos significantly more massive than this is mostly in a hot form, which is less easily accreted onto the SMBH (e.g., Cattaneo et al 2006; Croton 2009; Kereš et al 2009).”
• COLD FLOWS AND THE FIRST QUASARS (2011, background): “…this process of BH assembly is apparently facilited by the “cold flows” picture of galaxy formation which has revolutionized our understanding of galaxy assembly below the threshold dark matter mass of Mhalo ∼ 1012 M⊙ (Dekel & Birnboim 2006; Dekel et al. 2009; Kereš et al. 2005, 2009).”
• Evolution of density profiles in high-z galaxies: compaction and quenching inside-out (2015, background): “…halo mass grows above a threshold mass of ∼ 1012M , either via virial shock heating (Birnboim & Dekel 2003; Kereš et al. 2005; Dekel & Birnboim 2006; Kereš et al. 2009), or by gravitational infall heating (Dekel & Birnboim 2008; Birnboim & Dekel 2011; Khochfar & Ostriker 2008), which can be…”
• MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “…observed correlations between galaxy and halo mass – they overpredict the masses of both low and high mass galaxies, by a mass-dependent factor (i.e. predict a different magnitude and shape ofMgal(Mhalo); see Kereš et al. 2009a; Maller et al. 2006; Oppenheimer et al. 2010; Choi & Nagamine 2009).”
• What drives the growth of black holes (2011, background): “For example, the lack of significant AGN activity with dark-matter haloes 1013 M may be due to the halo virialising and shock heating the gas and suppressing vigorous mass accretion (e.g., Cattaneo et al., 2006, 2008; Dekel & Birnboim, 2006; Kereš et al., 2009).”
• SHORT-LIVED STAR-FORMING GIANT CLUMPS IN COSMOLOGICAL SIMULATIONS OF z ≈ 2 DISKS (2010, background): “In this picture, the high star-formation rates result from the high growth rates of cosmic structures atz ≈ 2 (Genel et al. 2008), as gas funnels directly from the cosmic web to the vicinity of galaxies in a ’cold-mode’ accretion (Kereš et al. 2005; Kereš et al. 2009; Dekel et al. 2009a).”
• KILOPARSEC-SCALE DUST DISKS IN HIGH-REDSHIFT LUMINOUS SUBMILLIMETER GALAXIES (2016, methodology): “Finally, some models propose that SMGs may simply represent the most massive extension of the normal z > 2 star–forming galaxy population (e.g., Kereš et al. 2005, 2009b,a; Davé et al. 2010).”
• EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, background): “…of hydrodynamical simulations which follow the gas accretion and buildup of stellar mass in galaxy halos formed in a cosmological context (e.g., Kereš et al. 2005, 2009; Oppenheimer et al. 2010) compare the predicted local galaxy stellar mass function to that observed (Bell et al. 2003),…”
• PHIBSS: MOLECULAR GAS CONTENT AND SCALING RELATIONS IN z ∼ 1–3 MASSIVE, MAIN-SEQUENCE STAR-FORMING GALAXIES (2012, background): “…mass end, may be fed by gradual and semi-continuous gas flows from the cosmic web, or by minor galaxy mergers, plausibly creating gas rich disks (Kereŝ et al. 2005, 2009, Bower et al. 2006, Kitzbichler & White 2007, Ocvirk, Pichon & Teyssier 2008, Dekel et al.2009, Genel et al. 2010, 2012,…”
• WHAT DOES A SUBMILLIMETER GALAXY SELECTION ACTUALLY SELECT? THE DEPENDENCE OF SUBMILLIMETER FLUX DENSITY ON STAR FORMATION RATE AND DUST MASS (2010, background): “The primary drawback of this approach for our present purposes is the lack of gas accretion, which cosmological hydrodynamic simulations show is a significant driver of star formation for the high-redshift, massive galaxies with which we are concerned (Kereš et al. 2005, 2009; Dekel et al. 2009).”
• Misaligned angular momentum in hydrodynamic cosmological simulations: warps, outer discs and thick discs (2010, background): “Several recent theoretical studies have addressed the process of gas delivery to galaxies (Birnboim & Dekel 2003; Kereš et al. 2005; Dekel & Birnboim 2006; Ocvirk, Pichon & Teyssier 2008; Brooks et al. 2009, hereafter B09; Dekel et al. 2009a; Dekel, Sari & Ceverino 2009b; Kereš et al. 2009).”
• What determines satellite galaxy disruption (2009, background): “While the assumption that satellite gas accretion rates are significantly lower than those of central galaxies may break down at z > 1 (Kereš et al. 2009), the significantly more recent infall times of satellites at high redshift mediates this concern.”