The luminosity and color dependence of the galaxy correlation function

Idit Zehavi, Zheng Zheng, David H. Weinberg, Joshua A. Frieman, Andreas A. Berlind, Michael R. Blanton, Roman Scoccimarro, Ravi K. Sheth, Michael A. Strauss, Issha Kayo, Yasushi Suto, Masataka Fukugita, Osamu Nakamura, Neta A. Bahcall, Jon Brinkmann, James E. Gunn, Greg S. Hennessy, Željko Ivezić, Gillian R. Knapp, Jon Loveday & 7 others Avery Meiksin, David J. Schlegel, Donald P. Schneider, Istvan Szapudi, Max Tegmark, Michael S. Vogeley, Donald G. York

Research output: Contribution to journalArticle

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Abstract

We study the luminosity and color dependence of the galaxy two-point correlation function in the Sloan Digital Sky Survey, starting from a sample of ∼200,000 galaxies over 2500 deg2. We concentrate our analysis on volume-limited subsamples of specified luminosity ranges, for which we measure the projected correlation function wp(rp), which is directly related to the real-space correlation function ξ(r). The amplitude of wp(rp) rises continuously with luminosity from M r ≈ -17.5 to Mr ≈ -22.5, with the most rapid increase occurring above the characteristic luminosity L* (Mr ≈ -20.5). Over the scales 0.1 h-1 Mpc < rp < 10 h-1 Mpc, the measurements for samples with Mr > -22 can be approximated, imperfectly, by power-law three-dimensional correlation functions ξ(r) = (r/r0) with γ ≈ 1.8 and r0(L*) ≈ 5.0 h-1 Mpc. The brightest subsample, -23 < Mr < -22, has a significantly steeper ξ(r). When we divide samples by color, redder galaxies exhibit a higher amplitude and steeper correlation function at all luminosities. The correlation amplitude of blue galaxies increases continuously with luminosity, but the luminosity dependence for red galaxies is less regular, with bright red galaxies exhibiting the strongest clustering at large scales and faint red galaxies exhibiting the strongest clustering at small scales. We interpret these results using halo occupation distribution (HOD) models assuming concordance cosmological parameters. For most samples, an HOD model with two adjustable parameters fits the wp(rp) data better than a power law, explaining inflections at rp ∼ 1-3 h-1 Mpc as the transition between the one-halo and two-halo regimes of ξ(r). The implied minimum mass for a halo hosting a central galaxy more luminous than L grows steadily, with Mmin ∝ L at low luminosities and a steeper dependence above L*. The mass at which a halo has, on average, one satellite galaxy brighter than L is M1 ≈ 23Mmin(L), at all luminosities. These results imply a conditional luminosity function (at fixed halo mass) in which central galaxies lie far above a Schechter function extrapolation of the satellite population. The HOD model fits nicely explain the color dependence of wp(rp) and the cross correlation between red and blue galaxies. For galaxies with Mr < -21, halos slightly above M min have blue central galaxies, while more massive halos have red central galaxies and predominantly red satellite populations. The fraction of blue central galaxies increases steadily with decreasing luminosity and host halo mass. The strong clustering of faint red galaxies follows from the fact that nearly all of them are satellite systems in high-mass halos. The HOD fitting results are in good qualitative agreement with the predictions of numerical and semianalytic models of galaxy formation.

Original languageEnglish
Pages (from-to)1-27
Number of pages27
JournalAstrophysical Journal
Volume630
Issue number1 I
DOIs
Publication statusPublished - 2005 Sep 1
Externally publishedYes

Fingerprint

luminosity
halos
galaxies
color
occupation
power law
galactic evolution
cross correlation
extrapolation
distribution
prediction

Keywords

  • Cosmology: observations
  • Cosmology: theory
  • Galaxies: distances and redshifts
  • Galaxies: halos
  • Galaxies: statistics
  • Large-scale structure of universe

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Zehavi, I., Zheng, Z., Weinberg, D. H., Frieman, J. A., Berlind, A. A., Blanton, M. R., ... York, D. G. (2005). The luminosity and color dependence of the galaxy correlation function. Astrophysical Journal, 630(1 I), 1-27. https://doi.org/10.1086/431891

The luminosity and color dependence of the galaxy correlation function. / Zehavi, Idit; Zheng, Zheng; Weinberg, David H.; Frieman, Joshua A.; Berlind, Andreas A.; Blanton, Michael R.; Scoccimarro, Roman; Sheth, Ravi K.; Strauss, Michael A.; Kayo, Issha; Suto, Yasushi; Fukugita, Masataka; Nakamura, Osamu; Bahcall, Neta A.; Brinkmann, Jon; Gunn, James E.; Hennessy, Greg S.; Ivezić, Željko; Knapp, Gillian R.; Loveday, Jon; Meiksin, Avery; Schlegel, David J.; Schneider, Donald P.; Szapudi, Istvan; Tegmark, Max; Vogeley, Michael S.; York, Donald G.

In: Astrophysical Journal, Vol. 630, No. 1 I, 01.09.2005, p. 1-27.

Research output: Contribution to journalArticle

Zehavi, I, Zheng, Z, Weinberg, DH, Frieman, JA, Berlind, AA, Blanton, MR, Scoccimarro, R, Sheth, RK, Strauss, MA, Kayo, I, Suto, Y, Fukugita, M, Nakamura, O, Bahcall, NA, Brinkmann, J, Gunn, JE, Hennessy, GS, Ivezić, Ž, Knapp, GR, Loveday, J, Meiksin, A, Schlegel, DJ, Schneider, DP, Szapudi, I, Tegmark, M, Vogeley, MS & York, DG 2005, 'The luminosity and color dependence of the galaxy correlation function', Astrophysical Journal, vol. 630, no. 1 I, pp. 1-27. https://doi.org/10.1086/431891
Zehavi I, Zheng Z, Weinberg DH, Frieman JA, Berlind AA, Blanton MR et al. The luminosity and color dependence of the galaxy correlation function. Astrophysical Journal. 2005 Sep 1;630(1 I):1-27. https://doi.org/10.1086/431891
Zehavi, Idit ; Zheng, Zheng ; Weinberg, David H. ; Frieman, Joshua A. ; Berlind, Andreas A. ; Blanton, Michael R. ; Scoccimarro, Roman ; Sheth, Ravi K. ; Strauss, Michael A. ; Kayo, Issha ; Suto, Yasushi ; Fukugita, Masataka ; Nakamura, Osamu ; Bahcall, Neta A. ; Brinkmann, Jon ; Gunn, James E. ; Hennessy, Greg S. ; Ivezić, Željko ; Knapp, Gillian R. ; Loveday, Jon ; Meiksin, Avery ; Schlegel, David J. ; Schneider, Donald P. ; Szapudi, Istvan ; Tegmark, Max ; Vogeley, Michael S. ; York, Donald G. / The luminosity and color dependence of the galaxy correlation function. In: Astrophysical Journal. 2005 ; Vol. 630, No. 1 I. pp. 1-27.
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T1 - The luminosity and color dependence of the galaxy correlation function

AU - Zehavi, Idit

AU - Zheng, Zheng

AU - Weinberg, David H.

AU - Frieman, Joshua A.

AU - Berlind, Andreas A.

AU - Blanton, Michael R.

AU - Scoccimarro, Roman

AU - Sheth, Ravi K.

AU - Strauss, Michael A.

AU - Kayo, Issha

AU - Suto, Yasushi

AU - Fukugita, Masataka

AU - Nakamura, Osamu

AU - Bahcall, Neta A.

AU - Brinkmann, Jon

AU - Gunn, James E.

AU - Hennessy, Greg S.

AU - Ivezić, Željko

AU - Knapp, Gillian R.

AU - Loveday, Jon

AU - Meiksin, Avery

AU - Schlegel, David J.

AU - Schneider, Donald P.

AU - Szapudi, Istvan

AU - Tegmark, Max

AU - Vogeley, Michael S.

AU - York, Donald G.

PY - 2005/9/1

Y1 - 2005/9/1

N2 - We study the luminosity and color dependence of the galaxy two-point correlation function in the Sloan Digital Sky Survey, starting from a sample of ∼200,000 galaxies over 2500 deg2. We concentrate our analysis on volume-limited subsamples of specified luminosity ranges, for which we measure the projected correlation function wp(rp), which is directly related to the real-space correlation function ξ(r). The amplitude of wp(rp) rises continuously with luminosity from M r ≈ -17.5 to Mr ≈ -22.5, with the most rapid increase occurring above the characteristic luminosity L* (Mr ≈ -20.5). Over the scales 0.1 h-1 Mpc < rp < 10 h-1 Mpc, the measurements for samples with Mr > -22 can be approximated, imperfectly, by power-law three-dimensional correlation functions ξ(r) = (r/r0)-γ with γ ≈ 1.8 and r0(L*) ≈ 5.0 h-1 Mpc. The brightest subsample, -23 < Mr < -22, has a significantly steeper ξ(r). When we divide samples by color, redder galaxies exhibit a higher amplitude and steeper correlation function at all luminosities. The correlation amplitude of blue galaxies increases continuously with luminosity, but the luminosity dependence for red galaxies is less regular, with bright red galaxies exhibiting the strongest clustering at large scales and faint red galaxies exhibiting the strongest clustering at small scales. We interpret these results using halo occupation distribution (HOD) models assuming concordance cosmological parameters. For most samples, an HOD model with two adjustable parameters fits the wp(rp) data better than a power law, explaining inflections at rp ∼ 1-3 h-1 Mpc as the transition between the one-halo and two-halo regimes of ξ(r). The implied minimum mass for a halo hosting a central galaxy more luminous than L grows steadily, with Mmin ∝ L at low luminosities and a steeper dependence above L*. The mass at which a halo has, on average, one satellite galaxy brighter than L is M1 ≈ 23Mmin(L), at all luminosities. These results imply a conditional luminosity function (at fixed halo mass) in which central galaxies lie far above a Schechter function extrapolation of the satellite population. The HOD model fits nicely explain the color dependence of wp(rp) and the cross correlation between red and blue galaxies. For galaxies with Mr < -21, halos slightly above M min have blue central galaxies, while more massive halos have red central galaxies and predominantly red satellite populations. The fraction of blue central galaxies increases steadily with decreasing luminosity and host halo mass. The strong clustering of faint red galaxies follows from the fact that nearly all of them are satellite systems in high-mass halos. The HOD fitting results are in good qualitative agreement with the predictions of numerical and semianalytic models of galaxy formation.

AB - We study the luminosity and color dependence of the galaxy two-point correlation function in the Sloan Digital Sky Survey, starting from a sample of ∼200,000 galaxies over 2500 deg2. We concentrate our analysis on volume-limited subsamples of specified luminosity ranges, for which we measure the projected correlation function wp(rp), which is directly related to the real-space correlation function ξ(r). The amplitude of wp(rp) rises continuously with luminosity from M r ≈ -17.5 to Mr ≈ -22.5, with the most rapid increase occurring above the characteristic luminosity L* (Mr ≈ -20.5). Over the scales 0.1 h-1 Mpc < rp < 10 h-1 Mpc, the measurements for samples with Mr > -22 can be approximated, imperfectly, by power-law three-dimensional correlation functions ξ(r) = (r/r0)-γ with γ ≈ 1.8 and r0(L*) ≈ 5.0 h-1 Mpc. The brightest subsample, -23 < Mr < -22, has a significantly steeper ξ(r). When we divide samples by color, redder galaxies exhibit a higher amplitude and steeper correlation function at all luminosities. The correlation amplitude of blue galaxies increases continuously with luminosity, but the luminosity dependence for red galaxies is less regular, with bright red galaxies exhibiting the strongest clustering at large scales and faint red galaxies exhibiting the strongest clustering at small scales. We interpret these results using halo occupation distribution (HOD) models assuming concordance cosmological parameters. For most samples, an HOD model with two adjustable parameters fits the wp(rp) data better than a power law, explaining inflections at rp ∼ 1-3 h-1 Mpc as the transition between the one-halo and two-halo regimes of ξ(r). The implied minimum mass for a halo hosting a central galaxy more luminous than L grows steadily, with Mmin ∝ L at low luminosities and a steeper dependence above L*. The mass at which a halo has, on average, one satellite galaxy brighter than L is M1 ≈ 23Mmin(L), at all luminosities. These results imply a conditional luminosity function (at fixed halo mass) in which central galaxies lie far above a Schechter function extrapolation of the satellite population. The HOD model fits nicely explain the color dependence of wp(rp) and the cross correlation between red and blue galaxies. For galaxies with Mr < -21, halos slightly above M min have blue central galaxies, while more massive halos have red central galaxies and predominantly red satellite populations. The fraction of blue central galaxies increases steadily with decreasing luminosity and host halo mass. The strong clustering of faint red galaxies follows from the fact that nearly all of them are satellite systems in high-mass halos. The HOD fitting results are in good qualitative agreement with the predictions of numerical and semianalytic models of galaxy formation.

KW - Cosmology: observations

KW - Cosmology: theory

KW - Galaxies: distances and redshifts

KW - Galaxies: halos

KW - Galaxies: statistics

KW - Large-scale structure of universe

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