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Title:
First-Year Sloan Digital Sky Survey-II Supernova Results: Hubble Diagram and Cosmological Parameters
Authors:
Kessler, Richard; Becker, Andrew C.; Cinabro, David; Vanderplas, Jake; Frieman, Joshua A.; Marriner, John; Davis, Tamara M.; Dilday, Benjamin; Holtzman, Jon; Jha, Saurabh W.; Lampeitl, Hubert; Sako, Masao; Smith, Mathew; Zheng, Chen; Nichol, Robert C.; Bassett, Bruce; Bender, Ralf; Depoy, Darren L.; Doi, Mamoru; Elson, Ed; Filippenko, Alexei V.; Foley, Ryan J.; Garnavich, Peter M.; Hopp, Ulrich; Ihara, Yutaka; Ketzeback, William; Kollatschny, W.; Konishi, Kohki; Marshall, Jennifer L.; McMillan, Russet J.; Miknaitis, Gajus; Morokuma, Tomoki; Mörtsell, Edvard; Pan, Kaike; Prieto, Jose Luis; Richmond, Michael W.; Riess, Adam G.; Romani, Roger; Schneider, Donald P.; Sollerman, Jesper; Takanashi, Naohiro; Tokita, Kouichi; van der Heyden, Kurt; Wheeler, J. C.; Yasuda, Naoki; York, Donald
Affiliation:
AA(Department of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA ; Kavli Institute for Cosmological Physics, The University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA ; ), AB(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA ), AC(Department of Physics and Astronomy, Wayne State University, Detroit, MI 48202, USA ), AD(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA ), AE(Department of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA ; Kavli Institute for Cosmological Physics, The University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA ; Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ), AF(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ), AG(School of Mathematics and Physics, University of Queensland, QLD 4072, Australia ; Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark ), AH(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA ), AI(Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003, USA ), AJ(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA ), AK(Institute of Cosmology and Gravitation, Dennis Sciama Building, Burnaby Road, University of Portsmouth, Portsmouth PO1 3FX, UK ), AL(Department of Physics and Astronomy, University of Pennsylvania, 203 South 33rd Street, Philadelphia, PA 19104, USA ), AM(Institute of Cosmology and Gravitation, Dennis Sciama Building, Burnaby Road, University of Portsmouth, Portsmouth PO1 3FX, UK ; Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701, South Africa ), AN(Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, Stanford, CA 94305-4060, USA ), AO(Institute of Cosmology and Gravitation, Dennis Sciama Building, Burnaby Road, University of Portsmouth, Portsmouth PO1 3FX, UK ), AP(Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701, South Africa ; South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa ), AQ(Universitäts-Sternwarte, Ludwig-Maximilians Universität München, Germany ), AR(Department of Physics, Texas A&M University, College Station, TX 77843, USA ), AS(Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka-shi, Tokyo, 181-0015, Japan ; Institute for the Physics and Mathematics of the Universe, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba 277-8568, Japan ), AT(Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701, South Africa ), AU(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA ), AV(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA ; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA ), AW(University of Notre Dame, 225 Nieuwland Science, Notre Dame, IN 46556-5670, USA ), AX(Universitäts-Sternwarte, Ludwig-Maximilians Universität München, Germany ), AY(Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka-shi, Tokyo, 181-0015, Japan ; Department of Astronomy, Graduate School of Science, University of Tokyo, Bunkyo-Ku, Tokyo, 113-0033, Japan ), AZ(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA ), BA(Institut für Astrophysik, Universität Göttingen, Friedrich-Hund Platz 1, D-37077 Göttingen, Germany ), BB(Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka-shi, Tokyo, 181-0015, Japan ), BC(Department of Physics, Texas A&M University, College Station, TX 77843, USA ), BD(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA ), BE(Center for Neighborhood Technology, 2125 W. North Ave., Chicago, IL 60647, USA ; Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ), BF(National Astronomical Observatory of Japan, Mitaka, 181-8588, Japan ), BG(Department of Physics, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden ), BH(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA ), BI(Department of Astronomy, Ohio State University, 140 West 18th Ave., Columbus, OH 43210-1173, USA ), BJ(Physics Department, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623-5603, USA ), BK(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ; Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA ), BL(Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, Stanford, CA 94305-4060, USA ), BM(Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA ), BN(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark ; The Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden ), BO(National Astronomical Observatory of Japan, Mitaka, 181-8588, Japan ), BP(Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka-shi, Tokyo, 181-0015, Japan ; Department of Astronomy, Graduate School of Science, University of Tokyo, Bunkyo-Ku, Tokyo, 113-0033, Japan ), BQ(Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa ), BR(Department of Astronomy, McDonald Observatory, University of Texas, Austin, TX 78712, USA ), BS(Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ), BT(Department of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA ; Enrico Fermi Institute, University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA)
Publication:
The Astrophysical Journal Supplement, Volume 185, Issue 1, pp. 32-84 (2009). (ApJS Homepage)
Publication Date:
11/2009
Origin:
IOP
ApJ Keywords:
cosmological parameters, cosmology: observations, distance scale, methods: data analysis, supernovae: general, surveys
DOI:
10.1088/0067-0049/185/1/32
Bibliographic Code:
2009ApJS..185...32K

Abstract

We present measurements of the Hubble diagram for 103 Type Ia supernovae (SNe) with redshifts 0.04 < z < 0.42, discovered during the first season (Fall 2005) of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. These data fill in the redshift "desert" between low- and high-redshift SN Ia surveys. Within the framework of the MLCS2K2 light-curve fitting method, we use the SDSS-II SN sample to infer the mean reddening parameter for host galaxies, RV = 2.18 ± 0.14stat ± 0.48syst, and find that the intrinsic distribution of host-galaxy extinction is well fitted by an exponential function, P(AV ) = exp(-AVV), with τV = 0.334 ± 0.088 mag. We combine the SDSS-II measurements with new distance estimates for published SN data from the ESSENCE survey, the Supernova Legacy Survey (SNLS), the Hubble Space Telescope (HST), and a compilation of Nearby SN Ia measurements. A new feature in our analysis is the use of detailed Monte Carlo simulations of all surveys to account for selection biases, including those from spectroscopic targeting. Combining the SN Hubble diagram with measurements of baryon acoustic oscillations from the SDSS Luminous Red Galaxy sample and with cosmic microwave background temperature anisotropy measurements from the Wilkinson Microwave Anisotropy Probe, we estimate the cosmological parameters w and ΩM, assuming a spatially flat cosmological model (FwCDM) with constant dark energy equation of state parameter, w. We also consider constraints upon ΩM and ΩΛ for a cosmological constant model (ΛCDM) with w = -1 and non-zero spatial curvature. For the FwCDM model and the combined sample of 288 SNe Ia, we find w = -0.76 ± 0.07(stat) ± 0.11(syst), ΩM = 0.307 ± 0.019(stat) ± 0.023(syst) using MLCS2K2 and w = -0.96 ± 0.06(stat) ± 0.12(syst), ΩM = 0.265 ± 0.016(stat) ± 0.025(syst) using the SALT-II fitter. We trace the discrepancy between these results to a difference in the rest-frame UV model combined with a different luminosity correction from color variations; these differences mostly affect the distance estimates for the SNLS and HST SNe. We present detailed discussions of systematic errors for both light-curve methods and find that they both show data-model discrepancies in rest-frame U band. For the SALT-II approach, we also see strong evidence for redshift-dependence of the color-luminosity parameter (β). Restricting the analysis to the 136 SNe Ia in the Nearby+SDSS-II samples, we find much better agreement between the two analysis methods but with larger uncertainties: w = -0.92 ± 0.13(stat)+0.10 -0.33(syst) for MLCS2K2 and w = -0.92 ± 0.11(stat)+0.07 -0.15 (syst) for SALT-II.
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