Textures and clusters

James G. Bartlett; Andrew K. Gooding; David N. Spergel

doi:10.1086/172175

Textures and clusters

James G. Bartlett, Andrew K. Gooding, David N. Spergel

Research output: Contribution to journal › Article › peer-review

2 Scopus citations

Abstract

We discuss the properties of galaxy clusters expected in a texture-seeded, CDM-dominated, Ω = 1 universe. Assuming that the textures are spherical, we use the spherical collapse model to compute the cluster velocity dispersion (or temperature) distribution function. For objects of mass 10¹¹ to 10¹⁵ M_⊙, we find v ∝ M_γ with γ ≃ 0.25. An unbiased (b = 1) texture model predicts too many high-velocity dispersion clusters. A biased texture model (b ∼ 3-4) appears to be compatible with cluster properties inferred from optical and X-ray observations. In the texture model, the cluster velocity distribution function does not evolve rapidly; thus, the model predicts the existence of rich clusters at moderate redshift (z ≈ 1-2).

Original language	English (US)
Pages (from-to)	1-6
Number of pages	6
Journal	Astrophysical Journal
Volume	403
Issue number	1
DOIs	https://doi.org/10.1086/172175
State	Published - 1993

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Cosmology: theory
Dark matter
Galaxies: clustering
Large-scale structure of universe

Access to Document

10.1086/172175

Cite this

@article{1d1b50d6437b41b5b7e8b33c5c1818a2,

title = "Textures and clusters",

abstract = "We discuss the properties of galaxy clusters expected in a texture-seeded, CDM-dominated, Ω = 1 universe. Assuming that the textures are spherical, we use the spherical collapse model to compute the cluster velocity dispersion (or temperature) distribution function. For objects of mass 1011 to 1015 M⊙, we find v ∝ Mγ with γ ≃ 0.25. An unbiased (b = 1) texture model predicts too many high-velocity dispersion clusters. A biased texture model (b ∼ 3-4) appears to be compatible with cluster properties inferred from optical and X-ray observations. In the texture model, the cluster velocity distribution function does not evolve rapidly; thus, the model predicts the existence of rich clusters at moderate redshift (z ≈ 1-2).",

keywords = "Cosmology: theory, Dark matter, Galaxies: clustering, Large-scale structure of universe",

author = "Bartlett, {James G.} and Gooding, {Andrew K.} and Spergel, {David N.}",

year = "1993",

doi = "10.1086/172175",

language = "English (US)",

volume = "403",

pages = "1--6",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

}

TY - JOUR

T1 - Textures and clusters

AU - Bartlett, James G.

AU - Gooding, Andrew K.

AU - Spergel, David N.

PY - 1993

Y1 - 1993

N2 - We discuss the properties of galaxy clusters expected in a texture-seeded, CDM-dominated, Ω = 1 universe. Assuming that the textures are spherical, we use the spherical collapse model to compute the cluster velocity dispersion (or temperature) distribution function. For objects of mass 1011 to 1015 M⊙, we find v ∝ Mγ with γ ≃ 0.25. An unbiased (b = 1) texture model predicts too many high-velocity dispersion clusters. A biased texture model (b ∼ 3-4) appears to be compatible with cluster properties inferred from optical and X-ray observations. In the texture model, the cluster velocity distribution function does not evolve rapidly; thus, the model predicts the existence of rich clusters at moderate redshift (z ≈ 1-2).

AB - We discuss the properties of galaxy clusters expected in a texture-seeded, CDM-dominated, Ω = 1 universe. Assuming that the textures are spherical, we use the spherical collapse model to compute the cluster velocity dispersion (or temperature) distribution function. For objects of mass 1011 to 1015 M⊙, we find v ∝ Mγ with γ ≃ 0.25. An unbiased (b = 1) texture model predicts too many high-velocity dispersion clusters. A biased texture model (b ∼ 3-4) appears to be compatible with cluster properties inferred from optical and X-ray observations. In the texture model, the cluster velocity distribution function does not evolve rapidly; thus, the model predicts the existence of rich clusters at moderate redshift (z ≈ 1-2).

KW - Cosmology: theory

KW - Dark matter

KW - Galaxies: clustering

KW - Large-scale structure of universe

UR - http://www.scopus.com/inward/record.url?scp=12044258619&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=12044258619&partnerID=8YFLogxK

U2 - 10.1086/172175

DO - 10.1086/172175

M3 - Article

AN - SCOPUS:12044258619

SN - 0004-637X

VL - 403

SP - 1

EP - 6

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

ER -

Textures and clusters

Abstract

All Science Journal Classification (ASJC) codes

Keywords

Access to Document

Other files and links

Fingerprint

Cite this