Simulations of the formation, evolution and clustering of galaxies and quasars
dc.contributor.author | Springel, Volker | en_US |
dc.contributor.author | White, S. D. M. (Simon D. M.) | en_US |
dc.contributor.author | Jenkins, A. R. | en_US |
dc.contributor.author | Frenk, C. S. | en_US |
dc.contributor.author | Yoshida, N. | en_US |
dc.contributor.author | Gao, L. | en_US |
dc.contributor.author | Navarro, J. | en_US |
dc.contributor.author | Thacker, R. | en_US |
dc.contributor.author | Croton, D. | en_US |
dc.contributor.author | Helly, J. | en_US |
dc.contributor.author | Peacock, J. A. | en_US |
dc.contributor.author | Cole, S. | en_US |
dc.contributor.author | Thomas, P. A. | en_US |
dc.contributor.author | Couchman, H. M. P. | en_US |
dc.contributor.author | Evrard, August E. | en_US |
dc.contributor.author | Colberg, Jorg M. | en_US |
dc.contributor.author | Pearce, Frazer R. | en_US |
dc.date.accessioned | 2008-08-14T19:13:18Z | |
dc.date.available | 2008-08-14T19:13:18Z | |
dc.date.issued | 2005-06-01 | en_US |
dc.identifier.citation | Springel, V; White, SDM; Jenkins, A; Frenk, CS; Yoshida, N; Gao, L; Navarro, J; Thacker, R; Croton, D; Helly, J; Peacock, JA; Cole, S; Thomas, P; Couchman, H; Evrard, AE; Colberg, J; Pearce, F. (2005). Nature, 435: 629-636. <http://hdl.handle.net/2027.42/60629> | en_US |
dc.identifier.issn | 0028-0836 | en_US |
dc.identifier.uri | http://arxiv.org/abs/astro-ph/0504097 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/60629 | |
dc.description.abstract | The cold dark matter model has become the leading theoretical picture for the formation of structure in the Universe. This model, together with the theory of cosmic inflation, makes a clear prediction for the initial conditions for structure formation and predicts that structures grow hierarchically through gravitational instability. Testing this model requires that the precise measurements delivered by galaxy surveys can be compared to robust and equally precise theoretical calculations. Here we present a simulation of the growth of dark matter structure using 2,1603 particles, following them from redshift z = 127 to the present in a cube-shaped region 2.230 billion lightyears on a side. In postprocessing, we also follow the formation and evolution of the galaxies and quasars. We show that baryon-induced features in the initial conditions of the Universe are reflected in distorted form in the low-redshift galaxy distribution, an effect that can be used to constrain the nature of dark energy with future generations of observational surveys of galaxies. | en_US |
dc.format.extent | 798831 bytes | |
dc.format.extent | 18 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Macmillan Magazines Ltd | en_US |
dc.title | Simulations of the formation, evolution and clustering of galaxies and quasars | 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.affiliationumcampus | Ann Arbor | en_US |
dc.identifier.pmid | 15931216 | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/60629/1/Springel2005Simulating.pdf | |
dc.identifier.doi | http://dx.doi.org/10.1038/nature03597 | en_US |
dc.owningcollname | Astrophysics (Physics, Department of) |
Files in this item
Remediation of Harmful Language
The University of Michigan Library aims to describe library materials in a way that respects the people and communities who create, use, and are represented in our collections. Report harmful or offensive language in catalog records, finding aids, or elsewhere in our collections anonymously through our metadata feedback form. More information at Remediation of Harmful Language.
Accessibility
If you are unable to use this file in its current format, please select the Contact Us link and we can modify it to make it more accessible to you.