Show simple item record

Author
dc.contributor.author
Zehavi, I 
Author
dc.contributor.author
Weinberg, D H 
Author
dc.contributor.author
Zheng, Z 
Author
dc.contributor.author
Berlind, A A 
Author
dc.contributor.author
Frieman, J A 
Author
dc.contributor.author
Scoccimarro, R 
Author
dc.contributor.author
Sheth, R K 
Author
dc.contributor.author
Blanton, M R 
Author
dc.contributor.author
Tegmark, M 
Author
dc.contributor.author
Mo, H J J 
Availability Date
dc.date.accessioned
2020-08-08T20:15:40Z
Availability Date
dc.date.available
2020-08-08T20:15:40Z
Release
dc.date.issued
2004
uri
dc.identifier.uri
http://hdl.handle.net/10831/49218
Abstract
dc.description.abstract
We measure the projected correlation function w(p)(r(p)) from the Sloan Digital Sky Survey for a flux-limited sample of 118,000 galaxies and a volume-limited subset of 22,000 galaxies with absolute magnitude M-r < - 21. Both correlation functions show subtle but systematic departures from the best-fit power law, in particular a change in slope at r(p) similar to 1-2 h(-1) Mpc. These departures are stronger for the volume-limited sample, which is restricted to relatively luminous galaxies. We show that the inflection point in w(p)(r(p)) can be naturally explained by contemporary models of galaxy clustering, according to which it marks the transition from a large-scale regime dominated by galaxy pairs in separate dark matter halos to a small-scale regime dominated by galaxy pairs in the same dark matter halo. For example, given the dark halo population predicted by an inflationary cold dark matter scenario, the projected correlation function of the volume-limited sample can be well reproduced by a model in which the mean number of M-r < - 21 galaxies in a halo of mass M > M-1 = 4.74 x 10(13) h(-1) M-. is [N](M)=(M/M-1)(0.89), with 75% of the galaxies residing in less massive, single-galaxy halos and simple auxiliary assumptions about the spatial distribution of galaxies within halos and the fluctuations about the mean occupation. This physically motivated model has the same number of free parameters as a power law, and it fits the w(p)(r(p)) data better, with a chi(2)/dof = 0.93, compared to 6.12 (for 10 degrees of freedom, incorporating the covariance of the correlation function errors). Departures from a power-law correlation function encode information about the relation between galaxies and dark matter halos. Higher precision measurements of these departures for multiple classes of galaxies will constrain galaxy bias and provide new tests of the theory of galaxy formation.
Language
dc.language
Angol
Title
dc.title
On departures from a power law in the galaxy correlation function
Type
dc.type
folyóiratcikk
Date Change
dc.date.updated
2020-06-05T11:48:04Z
Scope
dc.format.page
16-24
Doi ID
dc.identifier.doi
10.1086/386535
Wos ID
dc.identifier.wos
000221881200003
ID Scopus
dc.identifier.scopus
3142750641
MTMT ID
dc.identifier.mtmt
1064340
Issue Number
dc.identifier.issue
1
abbreviated journal
dc.identifier.jabbrev
ASTROPHYS J
Journal
dc.identifier.jtitle
ASTROPHYSICAL JOURNAL
Volume Number
dc.identifier.volume
608
Release Date
dc.description.issuedate
2004
department of Author
dc.contributor.institution
Fizikai Intézet
department of Author
dc.contributor.institution
Komplex Rendszerek Fizikája Tanszék
Author institution
dc.contributor.department
Komplex Rendszerek Fizikája Tanszék


Files in this item

On departures from a power law in the galaxy correlation function
 

This item appears in the following Collection(s)

Show simple item record