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Title:
Type II-P Supernovae from the SDSS-II Supernova Survey and the Standardized Candle Method
Authors:
D'Andrea, Chris B.; Sako, Masao; Dilday, Benjamin; Frieman, Joshua A.; Holtzman, Jon; Kessler, Richard; Konishi, Kohki; Schneider, D. P.; Sollerman, Jesper; Wheeler, J. Craig; Yasuda, Naoki; Cinabro, David; Jha, Saurabh; Nichol, Robert C.; Lampeitl, Hubert; Smith, Mathew; Atlee, David W.; Bassett, Bruce; Castander, Francisco J.; Goobar, Ariel; Miquel, Ramon; Nordin, Jakob; Östman, Linda; Prieto, José L.; Quimby, Robert; Riess, Adam G.; Stritzinger, Maximilian
Affiliation:
AA(Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA ), AB(Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA ), AC(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA ), AD(Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellise Avenue, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellise Avenue, Chicago, IL 60637, USA ; Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA ), AE(Department of Astronomy, MSC 4500, New Mexico State University, P. O. Box 30001, Las Cruces, NM 88003, USA ), AF(Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellise Avenue, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellise Avenue, Chicago, IL 60637, USA ), AG(Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba, 277-8582, Japan ), AH(Department of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA ), AI(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 ), AJ(Department of Astronomy, McDonald Observatory, University of Texas, Austin, TX 78712, USA ), AK(Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba, 277-8582, Japan ), AL(Department of Physics and Astronomy, Wayne State University, Detroit, MI 48202, USA ), AM(Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA ), AN(Institute of Cosmology and Gravitation, Dennis Sciama Building, Burnaby Road, University of Portsmouth, Portsmouth PO1 3FX, UK ), AO(Institute of Cosmology and Gravitation, Dennis Sciama Building, Burnaby Road, University of Portsmouth, Portsmouth PO1 3FX, UK ), AP(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 ), AQ(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA ), AR(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 ), AS(Institut de Ciències de l'Espai, (IEEC - CSIC), Campus UAB, 08193 Bellaterra, Barcelona, Spain ), AT(Department of Physics, Stockholm University, Albanova University Center, SE-106 91 Stockholm, Sweden ; The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden ), AU(Institució Catalana de Recerca i Estudis Avançats, Barcelona, Spain ; Institut de Física d'Altes Energies, E-08193 Bellaterra, Barcelona, Spain ), AV(Department of Physics, Stockholm University, Albanova University Center, SE-106 91 Stockholm, Sweden ; The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden ), AW(Department of Physics, Stockholm University, Albanova University Center, SE-106 91 Stockholm, Sweden ; The Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, AlbaNova, Stockholm University, SE-106 91 Stockholm, Sweden ), AX(Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101, USA ; Hubble and Carnegie-Princeton Fellow.), AY(Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA ), AZ(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 ), BA(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark ; Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile )
Publication:
The Astrophysical Journal, Volume 708, Issue 1, pp. 661-674 (2010). (ApJ Homepage)
Publication Date:
01/2010
Origin:
IOP
ApJ Keywords:
cosmology: observations, distance scale, supernovae: general, surveys
DOI:
10.1088/0004-637X/708/1/661
Bibliographic Code:
2010ApJ...708..661D

Abstract

We apply the Standardized Candle Method (SCM) for Type II Plateau supernovae (SNe II-P), which relates the velocity of the ejecta of a SN to its luminosity during the plateau, to 15 SNe II-P discovered over the three season run of the Sloan Digital Sky Survey-II Supernova Survey. The redshifts of these SNe—0.027 < z < 0.144—cover a range hitherto sparsely sampled in the literature; in particular, our SNe II-P sample contains nearly as many SNe in the Hubble flow (z > 0.01) as all of the current literature on the SCM combined. We find that the SDSS SNe have a very small intrinsic I-band dispersion (0.22 mag), which can be attributed to selection effects. When the SCM is applied to the combined SDSS-plus-literature set of SNe II-P, the dispersion increases to 0.29 mag, larger than the scatter for either set of SNe separately. We show that the standardization cannot be further improved by eliminating SNe with positive plateau decline rates, as proposed in Poznanski et al. We thoroughly examine all potential systematic effects and conclude that for the SCM to be useful for cosmology, the methods currently used to determine the Fe II velocity at day 50 must be improved, and spectral templates able to encompass the intrinsic variations of Type II-P SNe will be needed.

Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.


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