Studying dark energy with galaxy cluster surveys
dc.contributor.author | Mohr, J. J. | en_US |
dc.contributor.author | O'Shea, B. | en_US |
dc.contributor.author | Evrard, August E. | en_US |
dc.contributor.author | Bialek, J. J. | en_US |
dc.contributor.author | Haiman, Z. | en_US |
dc.date.accessioned | 2008-08-14T19:12:10Z | |
dc.date.available | 2008-08-14T19:12:10Z | |
dc.date.issued | 2003-07 | en_US |
dc.identifier.citation | Mohr, JJ; O'Shea, B; Evrard, AE; Bialek, J; Haiman, Z. (2003). Nuclear Physics B-Proceedings Supplements, 124: 63-67. <http://hdl.handle.net/2027.42/60610> | en_US |
dc.identifier.issn | 0920-5632 | en_US |
dc.identifier.uri | http://arxiv.org/abs/astro-ph/0208102 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/60610 | |
dc.description.abstract | Galaxy cluster surveys provide a powerful means of studying the density and nature of the dark energy. The redshift distribution of detected clusters in a deep, large solid angle SZE or X-ray survey is highly sensitive to the dark energy equation of state. Accurate constraints at the 5% level on the dark energy equation of state require that systematic biases in the mass estimators must be controlled at better than the similar to10% level. Observed regularity in the cluster population and the availability of multiple, independent mass estimators suggests these precise measurements are possible. Using hydrodynamical simulations that include preheating, we show that the level of preheating required to explain local galaxy cluster structure has a dramatic effect on X-ray cluster surveys, but only a mild effect on SZE surveys. This suggests that SZE surveys may be optimal for cosmology while X-ray surveys are well suited for studies of the thermal history of the intracluster medium. | en_US |
dc.format.extent | 354176 bytes | |
dc.format.extent | 18 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Elsevier Science Bv | en_US |
dc.title | Studying dark energy with galaxy cluster surveys | 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, Dept Astron, Ann Arbor, MI 48109 USA | en_US |
dc.contributor.affiliationother | Univ Illinois, Dept Astron, Urbana, IL 61801 USA | en_US |
dc.contributor.affiliationother | Univ Illinois, Dept Phys, Urbana, IL 61801 USA | en_US |
dc.contributor.affiliationother | Princeton Univ Observ, Princeton, NJ 08544 USA | en_US |
dc.contributor.affiliationumcampus | Ann Arbor | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/60610/1/Mohr2002Studying.pdf | |
dc.identifier.doi | http://dx.doi.org/10.1016/S0920-5632(03)02078-4 | en_US |
dc.identifier.source | Nuclear Physics B-Proceedings Supplements | en_US |
dc.owningcollname | Astrophysics (Physics, Department of) |
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