Galaxy orbits and the intracluster gas temperature in clusters

doi:10.1111/j.1365-2966.2006.10490.x

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Wiley InterScience

Monthly Notices of the Royal Astronomical Society

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Monthly Notices of the Royal Astronomical Society: Letters

Volume 370 Issue 1, Pages 427 - 434

Published Online: 8 Jun 2006

A Journal of the Royal Astronomical Society

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Galaxy orbits and the intracluster gas temperature in clusters

L. Benatov ^1,2 , K. Rines ^2,3 , P. Natarajan ^1,2,3★ , A. Kravtsov ^4,5 and D. Nagai ^4,5,6

¹ Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA ² Department of Physics, Yale University, PO Box 208120, New Haven, CT 06520-8120, USA ³ Yale Centre of Astronomy and Astrophysics, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA ⁴ Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA ⁵ Kavli Institute for Cosmological Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA ⁶ Theoretical Astrophysics, California Institute of Technology, Mail Code 130-33, Pasadena, CA 91125, USA

Correspondence to ^★ E-mail: priyamvada.natarajan@yale.edu

KEYWORDS

gravitational lensing • galaxies: clusters: general • galaxies: general

ABSTRACT

In this paper, we examine how well galaxies and intracluster gas trace the gravitational potential of clusters. Utilizing mass profiles derived from gravitational lensing and X-ray observations, coupled with measured galaxy velocities, we solve for the velocity anisotropy parameter β_orb(r) using the anisotropic Jeans equation. This is done for five clusters, three at low redshift: A2199, A496 and A576 and two at high redshifts: A2390 and MS1358. We use X-ray temperature profiles obtained from Chandra and ASCA/ROSAT data to estimate β_X(r), the ratio of energy in the galaxies compared to the X-ray gas. We find that none of these clusters is strictly in hydrostatic equilibrium. We compare the properties of our sample with clusters that form in high-resolution cosmological N-body simulations that include baryonic physics. Simulations and data show considerable scatter in their β_orb(r) and β_X(r) profiles. We demonstrate the future feasibility and potential for directly comparing the orbital structure of clusters inferred from multiwavelength observations with high-resolution simulated clusters.