Virial scaling of massive dark matter halos: Why clusters prefer a high normalization cosmology
dc.contributor.author | Evrard, August E. | en_US |
dc.contributor.author | Bialek, J. J. | en_US |
dc.contributor.author | Busha, Michael Travis | en_US |
dc.contributor.author | White, M. | en_US |
dc.contributor.author | Habib, S. | en_US |
dc.contributor.author | Heitmann, K. | en_US |
dc.contributor.author | Warren, M. | en_US |
dc.contributor.author | Rasia, E. | en_US |
dc.contributor.author | Tormen, G. | en_US |
dc.contributor.author | Moscardini, L. | en_US |
dc.contributor.author | Power, C. | en_US |
dc.contributor.author | Jenkins, A. R. | en_US |
dc.contributor.author | Gao, L. | en_US |
dc.contributor.author | Frenk, C. S. | en_US |
dc.contributor.author | Springel, Volker | en_US |
dc.contributor.author | White, S. D. M. (Simon D. M.) | en_US |
dc.contributor.author | Diemand, J. | en_US |
dc.date.accessioned | 2008-08-14T19:11:46Z | |
dc.date.available | 2008-08-14T19:11:46Z | |
dc.date.issued | 2008-01-01 | en_US |
dc.identifier.citation | Evrard, AE; Bialek, J; Busha, M; White, M; Habib, S; Heitmann, K; Warren, M; Rasia, E; Tormen, G; Moscardini, L; Power, C; Jenkins, AR; Gao, L; Frenk, CS; Springel, V; White, SDM; Diemand, J. (2008). Astrophysical Journal, 672:(1) 122-137. <http://hdl.handle.net/2027.42/60603> | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://arxiv.org/abs/astro-ph/0702241 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/60603 | |
dc.description.abstract | We present a precise estimate of the bulk virial scaling relation of halos formed via hierarchical clustering in an ensemble of simulated cold dark matter cosmologies. The result is insensitive to cosmological parameters; the presence of a trace, dissipationless gas component; and numerical resolution down to a limit of similar to 1000 particles. The dark matter velocity dispersion scales with total mass as log sigma(DM)(M, z) = log(1082.9 +/- 4.0 km s(-1)) + (0.3361 +/- 0.0026) log [h(z)M-200/10(15) M-circle dot], with h(z) being the dimensionless Hubble parameter. At fixed mass, the velocity dispersion likelihood is nearly lognormal, with scatter sigma (ln) (sigma) = 0.0426 +/- 0.015, except for a tail with higher dispersions containing 10% of the population that are merger transients. We combine this relation with the halo mass function in Lambda CDM models and show that a low normalization condition, S-8 = sigma(8)(Omega(m)/0.3)(0.35) = 0.69, favored by recent WMAP and SDSS analysis requires that galaxy and gas-specific energies in rich clusters be 50% larger than that of the underlying dark matter. Such large energetic biases are in conflict with the current generation of direct simulations of cluster formation. A higher normalization, S-8 = 0.80, alleviates this tension and implies that the hot gas fraction within r(500) is (0.71 +/- 0.09) h(70)(-3/2) Omega(b)/Omega(m), a value consistent with recent Sunyaev-Zel'dovich observations. | en_US |
dc.format.extent | 1150717 bytes | |
dc.format.extent | 18 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Univ Chicago Press | en_US |
dc.subject | Cosmology : Miscellaneous | en_US |
dc.subject | Cosmology : Theory | en_US |
dc.subject | Dark Matter | en_US |
dc.subject | Galaxies : Clusters : General | en_US |
dc.subject | Gravitation | en_US |
dc.subject | Intergalactic Medium | en_US |
dc.title | Virial scaling of massive dark matter halos: Why clusters prefer a high normalization cosmology | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Physics | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA | en_US |
dc.contributor.affiliationum | Univ Michigan, Ctr Theoret Phys, Ann Arbor, MI 48109 USA | en_US |
dc.contributor.affiliationother | Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA | en_US |
dc.contributor.affiliationother | Los Alamos Natl Lab, Los Alamos, NM 87545 USA | en_US |
dc.contributor.affiliationother | Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy | en_US |
dc.contributor.affiliationother | Univ Padua, Dipartimento Astron, I-35122 Padua, Italy | en_US |
dc.contributor.affiliationother | INFN, Natl Inst Nucl Phys, Sez Bologna, I-40127 Bologna, Italy | en_US |
dc.contributor.affiliationother | Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia | en_US |
dc.contributor.affiliationother | Univ Durham, Dept Phys, Durham DH1 3LE, England | en_US |
dc.contributor.affiliationother | Max Planck Inst Astrophys, D-85740 Garching, Germany | en_US |
dc.contributor.affiliationother | Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA | en_US |
dc.contributor.affiliationumcampus | Ann Arbor | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/60603/1/Evrard2007Virial.pdf | |
dc.identifier.doi | http://dx.doi.org/10.1086/521616 | en_US |
dc.owningcollname | Astrophysics (Physics, Department of) |
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