Constraining Cosmic Evolution of Type Ia Supernovae

doi:10.1086/589612

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Ryan J. Foley et al. 2008 ApJ 684 68 doi:10.1086/589612

Constraining Cosmic Evolution of Type Ia Supernovae

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Ryan J. Foley¹, Alexei V. Filippenko¹, C. Aguilera², A. C. Becker³, S. Blondin⁴, P. Challis⁴, A. Clocchiatti⁵, R. Covarrubias³, T. M. Davis⁶, P. M. Garnavich⁷, S. W. Jha^1,8,9, R. P. Kirshner⁴, K. Krisciunas¹⁰, B. Leibundgut¹¹, W. Li¹, T. Matheson¹², A. Miceli³, G. Miknaitis¹³, G. Pignata¹⁴, A. Rest^2,15, A. G. Riess^16,17, B. P. Schmidt¹⁸, R. C. Smith², J. Sollerman^6,19, J. Spyromilio¹¹, C. W. Stubbs^4,15, N. B. Suntzeff^2,10, J. L. Tonry²⁰, W. M. Wood-Vasey⁴ and A. Zenteno²¹

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rfoley@astro.berkeley.edu

¹ Department of Astronomy, University of California, Berkeley, CA 94720-3411
² Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile
³ Department of Astronomy, University of Washington, Seattle, WA 98195-1580
⁴ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138
⁵ Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile
⁶ Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen Ø, Denmark
⁷ Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670
⁸ Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Center, Menlo Park, CA 94025
⁹ Department of Physics and Astronomy, Rutgers, the State University of New Jersey, Piscataway, NJ 08854
¹⁰ Department of Physics, Texas A&M University, College Station, TX 77843-4242
¹¹ European Southern Observatory, D-85748 Garching, Germany
¹² National Optical Astronomy Observatory, Tucson, AZ 85719-4933
¹³ Fermilab, Batavia, IL 60510-0500
¹⁴ Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile
¹⁵ Department of Physics, Harvard University, Cambridge, MA 02138
¹⁶ Space Telescope Science Institute, Baltimore, MD 21218
¹⁷ Johns Hopkins University, Baltimore, MD 21218
¹⁸ Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek, PO 2611, Australia
¹⁹ Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden
²⁰ Institute for Astronomy, University of Hawaii, Honolulu, HI 96822
²¹ Department of Astronomy, University of Illinois, Urbana, IL 61801

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Abstract References Cited By

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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