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Title:
Constraining Cosmic Evolution of Type Ia Supernovae
Authors:
Foley, Ryan J.; Filippenko, Alexei V.; Aguilera, C.; Becker, A. C.; Blondin, S.; Challis, P.; Clocchiatti, A.; Covarrubias, R.; Davis, T. M.; Garnavich, P. M.; Jha, S. W.; Kirshner, R. P.; Krisciunas, K.; Leibundgut, B.; Li, W.; Matheson, T.; Miceli, A.; Miknaitis, G.; Pignata, G.; Rest, A.; Riess, A. G.; Schmidt, B. P.; Smith, R. C.; Sollerman, J.; Spyromilio, J.; Stubbs, C. W.; Suntzeff, N. B.; Tonry, J. L.; Wood-Vasey, W. M.; Zenteno, A.
Affiliation:
AA(Department of Astronomy, University of California, Berkeley, CA 94720-3411 .), AB(Department of Astronomy, University of California, Berkeley, CA 94720-3411 .), AC(Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile.), 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 Washington, Seattle, WA 98195-1580.), AI(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen Ø, Denmark.), AJ(Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.), AK(Department of Astronomy, University of California, Berkeley, CA 94720-3411 .; Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Center, Menlo Park, CA 94025.; Department of Physics and Astronomy, Rutgers, the State University of New Jersey, Piscataway, NJ 08854.), AL(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AM(Department of Physics, Texas A&M University, College Station, TX 77843-4242.), 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(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AR(Fermilab, Batavia, IL 60510-0500.), AS(Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile.), AT(Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile.; Department of Physics, Harvard University, Cambridge, MA 02138.), AU(Space Telescope Science Institute, Baltimore, MD 21218.; Johns Hopkins University, Baltimore, MD 21218.), AV(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek, PO 2611, Australia.), AW(Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile.), AX(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen Ø, Denmark.; Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden.), AY(European Southern Observatory, D-85748 Garching, Germany.), AZ(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.; Department of Physics, Harvard University, Cambridge, MA 02138.), BA(Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile.; Department of Physics, Texas A&M University, College Station, TX 77843-4242.), BB(Institute for Astronomy, University of Hawaii, Honolulu, HI 96822.), BC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), BD(Department of Astronomy, University of Illinois, Urbana, IL 61801.)
Publication:
The Astrophysical Journal, Volume 684, Issue 1, pp. 68-87. (ApJ Homepage)
Publication Date:
09/2008
Origin:
UCP
ApJ Keywords:
Cosmology: Observations, Cosmology: Distance Scale, Stars: Supernovae: General
DOI:
10.1086/589612
Bibliographic Code:
2008ApJ...684...68F

Abstract

We present a large-scale effort of creating composite spectra of high-redshift SNe Ia and comparing them to low-redshift counterparts in an attempt to understand possible cosmic evolution of SNe Ia, which has major implications for studies of dark energy. Through the ESSENCE project, we have obtained 107 spectra of 88 high-redshift SNe Ia with excellent light-curve information. In addition, we have obtained 397 spectra of low-redshift SNe Ia through a multiple-decade effort at the Lick and Keck Observatories, and we have used 45 UV spectra obtained by HST and IUE. The low-redshift spectra act as a control sample when comparing to the ESSENCE spectra. In all instances, the ESSENCE and Lick composite spectra appear very similar. The addition of galaxy light to the Lick composite spectra allows an excellent match of the overall SED with the ESSENCE composite spectra, indicating that the high-redshift SNe are more contaminated with host galaxy light than their low-redshift counterparts. This is caused by observing objects at all redshifts with similar angular slit widths, which corresponds to different projected physical distances. After correcting for the galaxy light contamination, a few marginally significant differences in the spectra remain. We have estimated the systematic errors when using current spectral templates for K-corrections to be ~0.02 mag. The variance in the composite spectra gives an estimate of the intrinsic variance in low-redshift maximum light SN spectra of ~3% relative flux in the optical and growing toward the UV. The difference between the maximum light low- and high-redshift spectra constrains the evolution of SN spectral features between our samples to be <10% relative flux in the rest-frame optical. Currently, galaxy contamination and the small samples of rest-frame UV spectra at low and high redshifts are the limiting factors for future studies.
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