GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY

By Idit Zehavi, Zheng Zheng, D. Weinberg, M. Blanton, N. Bahcall, A. Berlind, J. Brinkmann, Joshua A. Frieman, James E. Gunn, Robert Lupton and 7 more. 2010

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We measure the luminosity and color dependence of galaxy clustering in the largest-ever galaxy redshift survey, the main galaxy sample of the Sloan Digital Sky Survey Seventh Data Release. We focus on the projected correlation function wp(rp) of volume-limited samples, extracted from the parent sample of ∼700,000 galaxies over 8000 deg2, extending up to redshift of 0.25. We interpret our measurements using halo occupation distribution (HOD) modeling assuming a ΛCDM cosmology (inflationary cold dark matter with a cosmological constant). The amplitude of wp(rp) grows slowly with luminosity for L < L* and increases sharply at higher luminosities, with a large-scale bias factor b(> L) × (σ8/0.8) = 1.06 + 0.21(L/L*)1.12, where L is the sample luminosity threshold. At fixed luminosity, redder galaxies exhibit a higher amplitude and steeper correlation function, a steady trend that runs through the “blue cloud” and “green valley” and continues across the “red sequence.” The cross-correlation of red and blue galaxies is close to the geometric mean of their autocorrelations, dropping slightly below at rp < 1 h−1 Mpc. The luminosity trends for the red and blue galaxy populations separately are strikingly different. Blue galaxies show a slow but steady increase of clustering strength with luminosity, with nearly constant shape of wp(rp). The large-scale clustering of red galaxies shows little luminosity dependence until a sharp increase at L > 4 L*, but the lowest luminosity red galaxies (0.04–0.25 L*) show very strong clustering on small scales (rp < 2 h−1 Mpc). Most of the observed trends can be naturally understood within the ΛCDM+HOD framework. The growth of wp(rp) for higher luminosity galaxies reflects an overall shift in the mass scale of their host dark matter halos, in particular an increase in the minimum host halo mass Mmin. The mass at which a halo has, on average, one satellite galaxy brighter than L is M1 ≈ 17 Mmin(L) over most of the luminosity range, with a smaller ratio above L*. The growth and steepening of wp(rp) for redder galaxies reflects the increasing fraction of galaxies that are satellite systems in high-mass halos instead of central systems in low-mass halos, a trend that is especially marked at low luminosities. Our extensive measurements, provided in tabular form, will allow detailed tests of theoretical models of galaxy formation, a firm grounding of semiempirical models of the galaxy population, and new constraints on cosmological parameters from combining real-space galaxy clustering with mass-sensitive statistics such as redshift-space distortions, cluster mass-to-light ratios, and galaxy–galaxy lensing.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/306090f1f6b0c67f4d4a735b6559e214ceae4dfa

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Citations in the corpus

The massive end of the luminosity and stellar mass functions: Dependence on the fit to the light profile (2013, background): “…in popular semi-empirical models for populating haloes with galaxies, such as the halo occupation and abundance matching techniques (e.g., Cooray & Sheth 2002; Berlind & Weinberg 2002; Vale & Ostriker 2004; Shankar et al. 2006; Zehavi et al. 2011; Leauthaud et al. 2012; Moster et al. 2013).”
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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): “…in luminosity or stellar 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…”
The LABOCA survey of the Extended Chandra Deep Field-South: clustering of submillimetre galaxies (2011, background): “Halo occupation distribution fits to galaxy clustering suggest that these haloes host galaxies with luminosities L ∼ 2–3L∗ (Zehavi et al. 2011), a population dominated by ellipticals with predominantly slow-rotating kinematics (e.g. Cappellari et al. 2011; Tempel et al. 2011).”
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