THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0–8

By P. Behroozi, Risa Wechsler, C. Conroy. 2012

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We present a robust method to constrain average galaxy star formation rates (SFRs), star formation histories (SFHs), and the intracluster light (ICL) as a function of halo mass. Our results are consistent with observed galaxy stellar mass functions, specific star formation rates (SSFRs), and cosmic star formation rates (CSFRs) from z = 0 to z = 8. We consider the effects of a wide range of uncertainties on our results, including those affecting stellar masses, SFRs, and the halo mass function at the heart of our analysis. As they are relevant to our method, we also present new calibrations of the dark matter halo mass function, halo mass accretion histories, and halo–subhalo merger rates out to z = 8. We also provide new compilations of CSFRs and SSFRs; more recent measurements are now consistent with the buildup of the cosmic stellar mass density at all redshifts. Implications of our work include: halos near 1012 M☉ are the most efficient at forming stars at all redshifts, the baryon conversion efficiency of massive halos drops markedly after z ∼ 2.5 (consistent with theories of cold-mode accretion), the ICL for massive galaxies is expected to be significant out to at least z ∼ 1–1.5, and dwarf galaxies at low redshifts have higher stellar mass to halo mass ratios than previous expectations and form later than in most theoretical models. Finally, we provide new fitting formulae for SFHs that are more accurate than the standard declining tau model. Our approach places a wide variety of observations relating to the SFH of galaxies into a self-consistent framework based on the modern understanding of structure formation in ΛCDM. Constraints on the stellar mass–halo mass relationship and SFRs are available for download online.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/54aefad629c70d0b2c534d14e874be18d44d512b

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Citations in the corpus

Systematic Identification of LAEs for Visible Exploration and Reionization Research Using Subaru HSC (SILVERRUSH). I. Program strategy and clustering properties of ∼2000 Lyα emitters at z = 6–7 over the 0.3–0.5 Gpc2 survey area (2017, methodology): “We adopt the HOD models of Harikane et al. (2016) based on the halo mass function of Behroozi, Wechsler, and Conroy (2013) that is a modification of the Tinker et al. (2008) halo mass function.”
THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, methodology): “The slope of the relation between stellar mass and halo mass does not evolve significantly out to z ∼ 1.6 (Leauthaud et al. 2012; Behroozi et al. 2013).”
Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, background): “We find these results to be in good qualitative agreement at z 3 with the relations found by Behroozi et al. (2013b) in that the peak of the baryon conversion efficiency moves to higher masses at higher redshifts, the efficiency at masses larger than the peak is independent of redshift, and the…”
STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS (2014, background): “…) or ψ(t) ∝ t2/τ · exp(−t/τ ); 2. truncated SFH: ψ(t) = const if t < t0, ψ(t) = 0 otherwise; The Astrophysical Journal, 801:97 (17pp), 2015 March 10 Santini et al. and even more complex functional forms that have been proposed by previous works (e.g., Behroozi et al. 2013; Simha et al. 2014).”
The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, methodology): “The uncertainty on the stellar mass is comparable to our assumed uncertainty for the isolated dwarf galaxy sample described above of ∼25% (Oh et al. 2015), making the comparison between the stellar masses in Behroozi et al. (2013) and those taken from Zhang et al. (2012) entirely reasonable.”
Dark Matter Substructure in Numerical Simulations: A Tale of Discreteness Noise, Runaway Instabilities, and Artificial Disruption (2018, methodology): “…technique of subhalo abundance matching (e.g., Vale & Ostriker 2004; Conroy et al. 2006; Guo et al. 2010; Hearin et al. 2013; Moster et al. 2013; Behroozi et al. 2013), which has become a prime tool for interpreting galaxy clustering, galaxy-galaxy lensing, and group multiplicity functions, and…”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “By employing such a technique, Behroozi et al. (2013) constrain the average stellar mass of galaxies in haloes betweenMhalo = 1012–1013 M⊙ at z = 2 to range fromM∗ ≈ 5×109–1011 M⊙.”
GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS (2016, result): “In each of our survey volumes, the stellar mass to halo mass relation (also see Chen et al. 2014, for the Rarepeak) is consistent with the extrapolated fitting formula of Behroozi et al. (2013).”
Ultraviolet emission lines in young low-mass galaxies at z ≃ 2: physical properties and implications for studies at z > 7 (2014, background): “…in stars is thought to drop rapidly for dark matter halos less massivethan c© 2013 RAS ∼ 6×1011 M⊙ (e.g., Conroy & Wechsler 2009, Moster et al. 2010, Guo et al. 2010, Behroozi et al. 2013), likely implying that the efficiency of star formation and gas cooling is greatly reducedin low mass halos.”
Simulating galaxy formation with the IllustrisTNG model (2017, background): “…winds”) or wind velocity (“faster winds”), star forma- c© 0000 RAS, MNRAS 000, 000–000 0 2 4 6 8 10 redshift 10-2 10-1 SF R D [ M s un y r1 M pc -3 ] Behroozi et al. 2013 (comp) Oesch et al. 2015 (comp) fiducial TNG stronger winds (x2) faster winds (x2) faster winds (fiducial loading)…”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, methodology): “Here, we use the parameterization of Behroozi et al. (2013a), who provide simple functions to track the number density evolution of the progenitors of galaxies.”
EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, methodology): “Merger trees were generated using the ConsistentTrees algorithm (Behroozi et al. 2013c), providing a physically consistent evolution of halo properties across time steps.”
THE EVOLUTION OF THE GALAXY STELLAR MASS FUNCTION AT z = 4–8: A STEEPENING LOW-MASS-END SLOPE WITH INCREASING REDSHIFT (2015, background): “This corresponds to a typical stellar mass of a few times 107 M at z = 4–8 (e.g., Behroozi et al. 2013), similar to the minimum stellar mass in our real sample.”
Evolution of galaxy stellar masses and star formation rates in the eagle simulations (2014, methodology): “The Behroozi et al. (2013) estimate is divided into star forming and passive galaxies due to the reduced sensitivity of passive galaxies to the assumed form of the star formation history.”
WHY BARYONS MATTER: THE KINEMATICS OF DWARF SPHEROIDAL SATELLITES (2012, background): “In the field, galaxies display a clear trend of increasing stellar mass with halo mass (e.g., Behroozi et al. 2010; Moster et al. 2012; Leauthaud et al. 2012; Behroozi et al. 2013), yet satellites that span two orders of magnitude in luminosity seem to show no trend in their central vc with mass.”