Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0405189)
· References in the article
· Citations to the Article (135) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
The Effect of Gas Cooling on the Shapes of Dark Matter Halos
Authors:
Kazantzidis, Stelios; Kravtsov, Andrey V.; Zentner, Andrew R.; Allgood, Brandon; Nagai, Daisuke; Moore, Ben
Affiliation:
AA(Institute for Theoretical Physics, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland; .; Department of Astronomy and Astrophysics, Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, University of Chicago, Chicago, IL 60637.), AB(Department of Astronomy and Astrophysics, Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, University of Chicago, Chicago, IL 60637.), AC(Department of Astronomy and Astrophysics, Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, University of Chicago, Chicago, IL 60637.), AD(Department of Physics, University of California at Santa Cruz, 1156 High Street, Santa Cruz, CA 95064.), AE(Department of Astronomy and Astrophysics, Kavli Institute for Cosmological Physics, 5640 South Ellis Avenue, University of Chicago, Chicago, IL 60637.), AF(Institute for Theoretical Physics, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland; .)
Publication:
The Astrophysical Journal, Volume 611, Issue 2, pp. L73-L76. (ApJL Homepage)
Publication Date:
08/2004
Origin:
UCP
ApJ Keywords:
Cosmology: Theory, Cosmology: Dark Matter, Galaxies: Halos, Methods: Numerical
DOI:
10.1086/423992
Bibliographic Code:
2004ApJ...611L..73K

Abstract

We analyze the effect of dissipation on the shapes of dark matter (DM) halos using high-resolution cosmological gasdynamics simulations of clusters and galaxies in the ΛCDM cosmology. We find that halos formed in simulations with gas cooling are significantly more spherical than corresponding halos formed in adiabatic simulations. Gas cooling results in an average increase of the principle axis ratios of halos by ~0.2-0.4 in the inner regions. The systematic difference decreases slowly with radius but persists almost to the virial radius. We argue that the differences in simulations with and without cooling arise both during periods of quiescent evolution, when gas cools and condenses toward the center, and during major mergers. We perform a series of high-resolution N-body simulations to study the shapes of remnants in major mergers of DM halos and halos with embedded stellar disks. In the DM halo-only mergers, the shape of the remnants depends only on the orbital angular momentum of the encounter and not on the internal structure of the halos. However, significant shape changes in the DM distribution may result if stellar disks are included. In this case the shape of the DM halos is correlated with the morphology of the stellar remnants.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints