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Title:
Observational Constraints on the Nature of Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey
Authors:
Wood-Vasey, W. M.; Miknaitis, G.; Stubbs, C. W.; Jha, S.; Riess, A. G.; Garnavich, P. M.; Kirshner, R. P.; Aguilera, C.; Becker, A. C.; Blackman, J. W.; Blondin, S.; Challis, P.; Clocchiatti, A.; Conley, A.; Covarrubias, R.; Davis, T. M.; Filippenko, A. V.; Foley, R. J.; Garg, A.; Hicken, M.; Krisciunas, K.; Leibundgut, B.; Li, W.; Matheson, T.; Miceli, A.; Narayan, G.; Pignata, G.; Prieto, J. L.; Rest, A.; Salvo, M. E.; Schmidt, B. P.; Smith, R. C.; Sollerman, J.; Spyromilio, J.; Tonry, J. L.; Suntzeff, N. B.; Zenteno, A.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .), AB(Fermilab, Batavia, IL 60510-0500.), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .; Department of Physics, Harvard University, Cambridge, MA 02138.), AD(Department of Astronomy, University of California, Berkeley, CA 94720-3411.; Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Center, MS 29, Menlo Park, CA 94025.), AE(Space Telescope Science Institute, Baltimore, MD 21218.; Johns Hopkins University, Baltimore, MD 21218.), AF(Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.), AG(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .), AH(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AI(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AJ(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), AK(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .), AL(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .), AM(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile.), AN(Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada.), AO(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AP(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark.), AQ(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AR(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AS(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .; Department of Physics, Harvard University, Cambridge, MA 02138.), AT(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .; Department of Physics, Harvard University, Cambridge, MA 02138.), AU(Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.; Department of Physics, Texas A&M University, College Station, TX 77843-4242.), AV(European Southern Observatory, D-85748 Garching, Germany.), AW(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AX(National Optical Astronomy Observatory, Tucson, AZ 85719-4933.), AY(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AZ(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138; .; Department of Physics, Harvard University, Cambridge, MA 02138.), BA(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile.), BB(Department of Astronomy, Ohio State University, Columbus, OH 43210.), BC(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), BD(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), BE(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), BF(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), BG(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark.; Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden.), BH(European Southern Observatory, D-85748 Garching, Germany.), BI(Institute for Astronomy, University of Hawaii, Honolulu, HI 96822.), BJ(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.; Department of Physics, Texas A&M University, College Station, TX 77843-4242.), BK(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.)
Publication:
The Astrophysical Journal, Volume 666, Issue 2, pp. 694-715. (ApJ Homepage)
Publication Date:
09/2007
Origin:
UCP
ApJ Keywords:
Cosmology: Cosmological Parameters, Cosmology: Observations, Stars: Supernovae: General
DOI:
10.1086/518642
Bibliographic Code:
2007ApJ...666..694W

Abstract

We present constraints on the dark energy equation-of-state parameter, w=P/(ρc2), using 60 SNe Ia from the ESSENCE supernova survey. We derive a set of constraints on the nature of the dark energy assuming a flat universe. By including constraints on (ΩM, w) from baryon acoustic oscillations, we obtain a value for a static equation-of-state parameter w=-1.05+0.13-0.12 (stat 1 σ)+/-0.13 (sys) and ΩM=0.274+0.033-0.020 (stat 1 σ) with a best-fit χ2/dof of 0.96. These results are consistent with those reported by the Supernova Legacy Survey from the first year of a similar program measuring supernova distances and redshifts. We evaluate sources of systematic error that afflict supernova observations and present Monte Carlo simulations that explore these effects. Currently, the largest systematic with the potential to affect our measurements is the treatment of extinction due to dust in the supernova host galaxies. Combining our set of ESSENCE SNe Ia with the first-results Supernova Legacy Survey SNe Ia, we obtain a joint constraint of w=-1.07+0.09-0.09 (stat 1 σ)+/-0.13 (sys), ΩM=0.267+0.028-0.018 (stat 1 σ) with a best-fit χ2/dof of 0.91. The current global SN Ia data alone rule out empty (ΩM=0), matter-only ΩM=0.3, and ΩM=1 universes at >4.5 σ. The current SN Ia data are fully consistent with a cosmological constant.
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