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Title:
Scrutinizing Exotic Cosmological Models Using ESSENCE Supernova Data Combined with Other Cosmological Probes
Authors:
Davis, T. M.; Mörtsell, E.; Sollerman, J.; Becker, A. C.; Blondin, S.; Challis, P.; Clocchiatti, A.; Filippenko, A. V.; Foley, R. J.; Garnavich, P. M.; Jha, S.; Krisciunas, K.; Kirshner, R. P.; Leibundgut, B.; Li, W.; Matheson, T.; Miknaitis, G.; Pignata, G.; Rest, A.; Riess, A. G.; Schmidt, B. P.; Smith, R. C.; Spyromilio, J.; Stubbs, C. W.; Suntzeff, N. B.; Tonry, J. L.; Wood-Vasey, W. M.; Zenteno, A.
Affiliation:
AA(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark; .), AB(Department of Astronomy, Stockholm University, AlbaNova, S-10691 Stockholm, Sweden; .), AC(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark; .; Department of Astronomy, Stockholm University, AlbaNova, S-10691 Stockholm, Sweden; .), AD(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AG(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile.), AH(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AI(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AJ(Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.), AK(Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Center, Menlo Park, CA 94025.), AL(Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.; Department of Physics, Texas A&M University, College Station, TX 77843-4242.), AM(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AN(European Southern Observatory, D-85748 Garching, Germany.), AO(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AP(National Optical Astronomy Observatory, Tucson, AZ 85719-4933.), AQ(Fermilab, Batavia, IL 60510-0500.), AR(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile.), AS(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AT(Space Telescope Science Institute, Baltimore, MD 21218.; Johns Hopkins University, Baltimore, MD 21218.), AU(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), AV(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AW(European Southern Observatory, D-85748 Garching, Germany.), AX(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.; Department of Physics, Harvard University, Cambridge, MA 02138.), AY(Department of Physics, Texas A&M University, College Station, TX 77843-4242.; Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AZ(Institute for Astronomy, University of Hawaii, Honolulu, HI 96822.), BA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), BB(Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL 61801-3080.)
Publication:
The Astrophysical Journal, Volume 666, Issue 2, pp. 716-725. (ApJ Homepage)
Publication Date:
09/2007
Origin:
UCP
ApJ Keywords:
Cosmology: Observations, Stars: Supernovae: General
DOI:
10.1086/519988
Bibliographic Code:
2007ApJ...666..716D

Abstract

The first cosmological results from the ESSENCE supernova survey (Wood-Vasey and coworkers) are extended to a wider range of cosmological models including dynamical dark energy and nonstandard cosmological models. We fold in a greater number of external data sets such as the recent Higher-z release of high-redshift supernovae (Riess and coworkers), as well as several complementary cosmological probes. Model comparison statistics such as the Bayesian and Akaike information criteria are applied to gauge the worth of models. These statistics favor models that give a good fit with fewer parameters. Based on this analysis, the preferred cosmological model is the flat cosmological constant model, where the expansion history of the universe can be adequately described with only one free parameter describing the energy content of the universe. Among the more exotic models that provide good fits to the data, we note a preference for models whose best-fit parameters reduce them to the cosmological constant model.
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