The spatial distribution of satellite galaxies around host galaxies can illuminate the relationship between satellites and dark matter subhalos and aid in developing and testing galaxy formation models. Previous efforts to constrain the distribution attempted to eliminate interlopers from the measured projected number density of satellites and found that the distribution is generally consistent with the expected dark matter halo profile of the parent hosts, with a best-fit power-law slope of ≈ -1.7 between projected separations of ~$30\,h^{-1}$ kpc and $0.5\, h^{-1}$ Mpc. Here, I use the projected cross-correlation of bright and faint galaxies to analyze contributions from satellites and interlopers together, using a halo occupation distribution (HOD) analytic model for galaxy clustering. This approach is tested on mock catalogs constructed from simulations. I find that analysis of Sloan Digital Sky Survey (SDSS) data gives results generally consistent with interloper subtraction methods between the projected separations of $10\,h^{-1}$ kpc and $6.3\,h^{-1}$ Mpc, although the errors on the parameters that constrain the radial profile are large, and larger samples of data are required.

The galaxy cross-correlation function as a probe of the spatial distribution of galactic satellites

Westudytheluminosityandcolordependenceofthegalaxytwo-pointcorrelationfunctionintheSloanDigitalSky Survey, starting from a sample of � 200,000 galaxies over 2500 deg 2 . 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 � (r). The amplitude of wp(rp) rises continuously with luminosity from Mr �� 17: 5t oMr �� 22:5, with the most rapid increase occurring above the characteristic luminosity L� (Mr �� 20:5). Over the scales 0:1 h � 1 Mpc � 22 can be approximated, imperfectly, by power-law three-dimensional correlation functions � (r) ¼ (r/r0) � � with � � 1:8 and r0(L� ) � 5:0 h � 1 Mpc. The brightest subsample, � 23 < Mr < � 22, has a significantly steeper � (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 � (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 Mmin 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 offaint 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. Subject headingg cosmology: observations — cosmology: theory — galaxies: distances and redshifts — galaxies: halos — galaxies: statistics — large-scale structure of universe

The Luminosity and Color Dependence of the Galaxy Correlation Function

The astrocosmic databases for multi-wavelength and cosmological properties of extragalactic sources

Using our samples of I-type Active Galactic Nuclei (AGN) and blue galaxies from the SDSS DR7 and the WiggleZ DR1 surveys, parameters of their cross- and autocorrelation functions (ACF) were obtained. Analysis of the real-space ACF shows the presence of a steeper break for AGNs than for blue galaxies, which is in agreement with their evolution paradigm, according to which, in the late epoch, filaments are mainly populated by galaxies with star formation, while I-type AGNs are mainly formed in clusters. The value of β = 0.58 ± 0.08—which characterizes infall of objects onto matter overdensities—and the bias parameter for I-type AGNs bAGN = 1.38 ± 0.19 for $\bar z = 0.65$—which agrees well with the results of other authors for one of I-type AGN subclasses, quasars, and also with the results for X-ray selected samples of different-type AGN—was obtained from the redshift-space distortions of the ACF.

Cross-correlation function of SDSS DR7 I-type AGNs and WiggleZ galaxies

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Cross-correlation function of SDSS DR7 I-type AGNs and WiggleZ galaxies