Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering

By Zheng Zheng, A. Coil, Idit Zehavi. 2007

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We model the luminosity-dependent projected two-point correlation function of DEEP2 (z ~ 1) and SDSS (z ~ 0) galaxies within the HOD framework. At both epochs, there is a tight correlation between central galaxy luminosity and halo mass, with the slope and scatter decreasing for larger halo masses, and the fraction of satellite galaxies decreases at higher luminosity. We find little evolution in the relation between mass scales of host halos for central galaxies and satellite galaxies above the same luminosity threshold. Combining these HOD results with theoretical predictions of the typical growth of halos, we establish an evolutionary connection between the galaxy populations at the two redshifts by linking z ~ 0 central galaxies to z ~ 1 central galaxies that reside in their progenitor halos. We find that the stellar mass growth of galaxies depends on halo mass. On average, the majority of the stellar mass in central galaxies residing in z ~ 0 low-mass halos (~5 × 1011 h-1 M☉) and only a small fraction of the stellar mass in central galaxies of high-mass halos (~1013 h-1 M☉) result from star formation between z ~ 1 and z ~ 0. In addition, the mass scale of halos where the star formation efficiency reaches a maximum is found to shift toward lower mass with time. Future work that combines HOD modeling of the clustering of galaxies at different redshifts with the assembly history and dynamical evolution of dark matter halos can lead to an understanding of the stellar mass growth due to both mergers and star formation as a function of host halo mass and provide powerful tests of galaxy formation theories.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6b6a8f3152e294d2243bedf9328626ffd5fe3ef3

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Citations in the corpus

Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “(46), but integrating from rp out to rout ≡ √ r2p + r2max, where rmax is the same value as used for the data (e.g., Zehavi et al. 2004, 2005, 2011; Abazajian et al. 2005; Tinker et al. 2005; Zheng et al. 2007, 2009; Yoo et al. 2009).”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, background): “…mass (e.g., Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Bullock et al. 2002; Zehavi et al. 2002, 2005, 2011b; Zheng et al. 2005, 2007; Tinker et al. 2007; Skibba & Sheth 2009; Brown et al. 2008; Wake et al. 2011; Foucaud et al. 2010; White et al. 2011).”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, methodology): “The models of abundance matching, as well as halo occupation distribution modeling (Zheng et al. 2007; Wake et al. 2011) and conditional luminosity function modeling (Yang et al. 2012), agree in a low stellar-to-virial mass ratio, fstars(z = 3) = 0.06% − 0.6% for halos with masses ofMv = 1011 M⊙ at…”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, methodology): “Best-Fit Halo Occupancy Distribution The halo occupancy distribution (HOD) may be used, for instance, to predict or fit to galaxy clustering (Zheng et al. 2007; Watson et al. 2011; Zehavi et al. 2011).”
AGN heating and ICM cooling in the HIFLUGCS sample of galaxy clusters (2008, background): “Inherent scalings between BCGs and clusters have been implied in numerous observational studies (e.g. Lin & Mohr 2004; Brough et al. 2008) as well as cosmological simulations (Zheng et al. 2007; Cooray & Milosavljević 2005).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “This value is somewhat higher than the σlogL ∼ 0.12 found by Zheng et al. (2007), but is consistent within the uncertainties.”
THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, background): “…(per unit mass) give reasonably good predictions for clustering statistics by adopting fairly small dispersions in the mapping function (e.g. Zheng et al. 2007, Conroy & Wechsler 2009) and give a only factor of two discrepancy in the predicted major merger rates (e.g. Hopkins et al. 2010b,…”
Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, background): “…galaxy Nc and the satellite galaxies Ns: N(M) = Nc(M) × [1 + Ns(M)] , (10) where Nc(M) = 1 2 [ 1 + erf ( log M − log Mmin σlog M )] , (11) Ns(M) = ( M − M0 M1 )α · (12) The smooth transition for central galaxies expresses the uncertainties in the galaxy formation process (Zheng et al. 2007).”
A halo model of galaxy colours and clustering in the Sloan Digital Sky Survey (2008, methodology): “We use the parametrization of Zehavi et al. (2005) to illustrate the former case, and that of Zheng et al. (2007) to illustrate the latter.”
PROBING THE INTERGALACTIC MEDIUM/GALAXY CONNECTION. V. ON THE ORIGIN OF Lyα AND O vi ABSORPTION AT z < 0.2 (2011, background): “More modern treatments compare the clustering of galaxies as a function of luminosity to predictions for dark matter halos and thereby derive a relation between L and Mh (e.g. Zheng et al. 2007; The SDSS Collaboration et al. 2010).”
Galaxy Zoo: Disentangling the Environmental Dependence of Morphology and Colour ⋆ (2008, methodology): “We test this with a halo occupation model of galaxy clustering, (e.g., Zehavi et al. 2005, Zheng et al. 2007), in which the halo occupation distribution of central and satellite galaxies depends on halo mass and the luminosity threshold.”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, background): “…correction; i.e., mass growth is dominated by major mergers and star formation, as seen in cosmological simulations (Maller et al. 2006) and observations (Zheng et al. 2007; although it is possible that minor mergers become important for the most extreme, massive brightest cluster galaxies [BCGs]).”
The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity (2012, methodology): “Galaxies were placed in halos using the halo occupation distribution determined from measurements of the correlation function of CMASS galaxies and the parameterization of Zheng et al. (2007).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, methodology): “Other authors have reached a similar conclusion using HOD, CLF, or SHAM methods (e.g., Yang, Mo, & van den Bosch 2003; Tinker et al. 2005; Vale & Ostriker 2006; Zheng et al. 2007; Kim et al. 2008; Guo et al. 2010; Moster et al. 2010).”