The Influence of Concentration and Dynamical State on Scatter in the Galaxy Cluster Mass-Temperature Relation
Abstract
Using a hydrodynamics plus N-body simulation of galaxy cluster formation within a large volume and mock Chandra X-ray observations, we study the form and evolution of the intrinsic scatter about the best-fit X-ray temperature-mass relation for clusters. We investigate the physical origin of the scatter by correlating it with quantities that are closely related to clusters' formation and merging histories. We also examine the distribution of the scatter for merging and non-merging populations, identified using halo merger trees derived from the simulation as well as X-ray substructure measures. We find a strong correlation between the scatter in the M-TX relation and the halo concentration, in the sense that more concentrated clusters tend to be cooler than clusters with similar masses. No bias is found between the merging and relaxed clusters, but merging clusters generally have greater scatter, which is related to the properties of the distribution of halo concentrations. We also detect a signature of non-lognormality in the distribution of scatter for our simulated clusters both at z = 0 and at z = 1. A detailed comparison of merging clusters identified by substructure measures and by halo merger trees is given in the discussion. Finally we conclude that, whenmore »
- Authors:
-
- Univ. of Illinois, Urbana, IL (United States)
- Univ. of Illinois, Urbana, IL (United States); National Center for Supercomputing Applications, Urbana, IL (United States)
- Publication Date:
- Research Org.:
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF); Krell Institute, Ames, IA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1564657
- Grant/Contract Number:
- FG02-97ER25308
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal
- Additional Journal Information:
- Journal Volume: 699; Journal Issue: 1; Journal ID: ISSN 0004-637X
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; galaxies; clusters; hydrodynamics; intergalactic medium; X-rays
Citation Formats
Yang, Hsiang-Yi Karen, Ricker, Paul M., and Sutter, P. M. The Influence of Concentration and Dynamical State on Scatter in the Galaxy Cluster Mass-Temperature Relation. United States: N. p., 2009.
Web. doi:10.1088/0004-637x/699/1/315.
Yang, Hsiang-Yi Karen, Ricker, Paul M., & Sutter, P. M. The Influence of Concentration and Dynamical State on Scatter in the Galaxy Cluster Mass-Temperature Relation. United States. https://doi.org/10.1088/0004-637x/699/1/315
Yang, Hsiang-Yi Karen, Ricker, Paul M., and Sutter, P. M. Thu .
"The Influence of Concentration and Dynamical State on Scatter in the Galaxy Cluster Mass-Temperature Relation". United States. https://doi.org/10.1088/0004-637x/699/1/315. https://www.osti.gov/servlets/purl/1564657.
@article{osti_1564657,
title = {The Influence of Concentration and Dynamical State on Scatter in the Galaxy Cluster Mass-Temperature Relation},
author = {Yang, Hsiang-Yi Karen and Ricker, Paul M. and Sutter, P. M.},
abstractNote = {Using a hydrodynamics plus N-body simulation of galaxy cluster formation within a large volume and mock Chandra X-ray observations, we study the form and evolution of the intrinsic scatter about the best-fit X-ray temperature-mass relation for clusters. We investigate the physical origin of the scatter by correlating it with quantities that are closely related to clusters' formation and merging histories. We also examine the distribution of the scatter for merging and non-merging populations, identified using halo merger trees derived from the simulation as well as X-ray substructure measures. We find a strong correlation between the scatter in the M-TX relation and the halo concentration, in the sense that more concentrated clusters tend to be cooler than clusters with similar masses. No bias is found between the merging and relaxed clusters, but merging clusters generally have greater scatter, which is related to the properties of the distribution of halo concentrations. We also detect a signature of non-lognormality in the distribution of scatter for our simulated clusters both at z = 0 and at z = 1. A detailed comparison of merging clusters identified by substructure measures and by halo merger trees is given in the discussion. Finally we conclude that, when cooling-related effects are neglected, the variation in halo concentrations is a more important factor for driving the intrinsic scatter in the M-TX relation, while departures from hydrostatic equilibrium due to cluster mergers have a minor effect.},
doi = {10.1088/0004-637x/699/1/315},
journal = {The Astrophysical Journal},
number = 1,
volume = 699,
place = {United States},
year = {Thu Jun 11 00:00:00 EDT 2009},
month = {Thu Jun 11 00:00:00 EDT 2009}
}
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