Galaxies in a simulated ΛCDM universe – II. Observable properties and constraints on feedback

By D. Kerevs, Neal Katz, R. Dav'e, Mark A. Fardal, David H. Weinberg HarvardCFA, Umass, U. Arizona, Ohio-State. 2009

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We compare the properties of galaxies that form in a cosmological simulation without strong feedback to observations of the z = 0 galaxy population. We confirm previous findings that models without strong feedback overproduce the observed galaxy baryonic mass function, especially at the low- and high-mass extremes. Through post-processing we investigate what kinds of feedback would be required to reproduce the statistics of observed galaxy masses and star formation rates. To mimic an extreme form of ‘preventive’ feedback, such as a highly efficient active galactic nucleus ‘radio mode’, we remove all baryonic mass that was originally accreted from shock-heated gas (‘hot-mode’ accretion). This removal does not bring the highmass end of the galaxy mass function into agreement with observations because much of the stellar mass in these systems formed at high redshift from baryons that originally accreted via ‘cold mode’ on to lower mass progenitors. An efficient ‘ejective’ feedback mechanism, such as supernova-driven galactic winds, must reduce the masses of these progenitors before they merge to form today’s massive galaxies. Feedback must also reduce the masses of lower mass z = 0 galaxies, which assemble at lower redshifts and have much lower star formation rates. If we monotonically remap galaxy masses to reproduce the observed mass function, but retain the simulation-predicted star formation rates, we obtain fairly good agreement with the observed sequence of star-forming galaxies. However, we fail to recover the observed population of passive, low star formation rate galaxies, especially at the high-mass end. Suppressing all hotmode accretion improves the agreement for high-mass galaxies, but it worsens the agreement at intermediate masses. Reproducing these z = 0 observations requires a feedback mechanism that dramatically suppresses star formation in a fraction of galaxies, increasing with mass, while leaving star formation rates of other galaxies essentially unchanged.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

THE TWO PHASES OF GALAXY FORMATION (2010, background): “…development of the internal structures of galaxies has been far more difficult to achieve with respect to the galactic stellar mass fractions (e.g. Kereš et al. 2009a; Guo et al. 2010b) as well as kinematics and morphologies (e.g. Abadi et al. 2003; Governato et al. 2010; Feldmann et al. 2010).”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, background): “Without strong dynamical effects from SNe that could generate galactic outflows, the star formation rates (SFRs) and stellar masses found in many cosmological galaxy simulations remain systematically too high (e.g. 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).”
Feedback and recycled wind accretion: assembling the z= 0 galaxy mass function (2009, background): “…gas dominates the halo gas, although dense filaments at high redshifts (z & 2) still allow cold mode accretion to proceed even above this threshold mass (K05; Dekel & Birnboim 2006; Kereš 2007; Ocvirck et al. 2008; Kereš et al. 2009a, hereafter K09a; Brooks et al. 2009; Dekel et al. 2009).”
Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “The no-wind case (nw; blue), where resolutionconverged, shows the classic behavior that the GSMF well exceeds observations at all masses (see e.g. Kereš et al. 2009b, for a more detailed discussion).”
The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations (2016, background): “…their surrounding gas, where intergalactic accretion feeds galaxies from the cosmic web (Kereš et al. 2005; Brooks et al. 2009; Dekel et al. 2009; Kereš et al. 2009a; Faucher-Giguère et al. 2011; van de Voort et al. 2011), powerful winds evacuate gas from galaxies (Oppenheimer & Davé 2008;…”
METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, methodology): “…estimated the fraction of gas inflow from outside the virial radius that actually reaches the galaxy at the halo center, in, using analytic arguments and hydro cosmological simulations (Birnboim & Dekel 2003; Kereš et al. 2005, 2009b; Dekel & Birnboim 2006; Ocvirk et al. 2008; Dekel et al. 2009).”
Galaxies in a simulated ΛCDM Universe – I. Cold mode and hot cores (2008, background): “Many of the results in this paper and its companions (Paper II, and Keres et al. 2009b (in preparation)) first appeared as part of D. Kereš’s PhD thesis at University of Massachusetts, Amherst (Keres 2007).”
Galaxies on FIRE (Feedback In Realistic Environments): stellar feedback explains cosmologically inefficient star formation (2013, background): “…stellar feedback, gas in cosmological models cools rapidly and inevitably turns into stars, predicting galaxies with far larger masses than are observed (e.g. Katz et al. 1996; Somerville & Primack 1999; Cole et al. 2000; Springel & Hernquist 2003b; Kereš et al. 2009, and references therein).”
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): “The virial temperature for galaxies with halos of mass∼ 1012 M⊙ is expected to beTvir ≃ 106 K (van de Voort et al. 2011b), and Kereš et al. (2009) suggest that this hot gas may fill the volume surrounding galaxies to a fewrvir .”
Galaxy Alignments: An Overview (2015, background): “Numerical simulations of individual (spiral) galaxies have shown the presence of cold gas accretion streams (Dekel et al. 2009; Kereš et al. 2009; Sales et al. 2012), which have a significant impact on the orientation of the disc and are able to tilt the orientation away from the initial one (Kimm e”
Feedback from winds and supernovae in massive stellar clusters – I. Hydrodynamics (2012, background): “For instance, without strong stellar feedback, cosmological models predict around 10 times the stellar mass found in real galaxies (e.g. Cole et al. 2000; Kereš et al. 2009).”
The rates and modes of gas accretion on to galaxies and their gaseous haloes (2010, methodology): “Contrary to our results and those of Kereš et al. (2009a), Kereš et al. (2005) find that the hot fraction continues to increase with the halo mass and that there is no significant evolution.”
Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies (2012, background): “Core creation should then be a common outcome of any feedback scheme that can create such flows (Springel et al. 2005; Kereš et al. 2009; Oppenheimer et al. 2010; Choi & Nagamine 2011; Hopkins et al. 2011) as long as sufficient spatial resolution and high SF surface densi- c© 2002 RAS, MNRAS 000,…”
DIFFUSE Lyα EMITTING HALOS: A GENERIC PROPERTY OF HIGH-REDSHIFT STAR-FORMING GALAXIES (2011, background): “…theoretical investigations focusing primarily on diffuse and extended Lyα from the outer parts of galaxies or LAEs have deliberately neglected the scattering of Lyα from the inside out (Dijkstra et al. 2006; Dijkstra & Loeb 2009; Kereš et al. 2009; Faucher-Giguere et al. 2010; Goerdt et al. 2009).”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, background): “…the baryons turning into stars, producing galaxies much more massive than observed (Katz et al. 1996; Somerville & Primack 1999; Cole et al. 2000; Springel & Hernquist 2003b; Kereš et al. 2009), regardless of the details of star formation in the simulation (White & Frenk 1991; Kereš et al. 2009).”
Self-regulated star formation in galaxies via momentum input from massive stars (2011, background): “…the net stellar mass formed from cooled baryons exceeds that observed by an order of magnitude or more, particularly in lower mass haloes (e.g. Katz, Weinberg & Hernquist 1996; Somerville & Primack 1999; Cole et al. 2000; Springel & Hernquist 2003b; Kereš et al. 2009, and references therein).”
Lyα COOLING EMISSION FROM GALAXY FORMATION (2010, background): “Since cold accretion likely fuels star formation in halo centers, at rates similar to the cold gas accretion rates (e.g., Kereš et al. 2005, 2009b; Faucher-Giguère et al. in prep.)”
DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4 (2012, background): “In Section 1 we discused gas inflows in the context of a popular model whereby the gas accretion rate regulates the galactic SFR (Dekel & Birnboim 2006; Keres̃ et al. 2009a; Keres̃ et al. 2009b; Bouché et al. 2010; Davé, Finlator, & Oppenheimer 2012).”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, background): “However, many discrepancies between observations and predictions persist (e.g., Fontana et al. 2006; Fontanot et al. 2009; Kereš et al. 2009; Davé et al. 2011a,b; Lu et al. 2012; Weinmann et al. 2012).”