Constraining cosmic evolution of type Ia supernovae

被引：55

作者：

Foley, Ryan J. ^{[1
]}

Filippenko, Alexei V. ^{[1
]}

Aguilera, C. ^{[2
]}

Becker, A. C. ^{[3
]}

Blondin, S. ^{[4
]}

Challis, P. ^{[4
]}

Clocchiatti, A. ^{[5
]}

Covarrubias, R. ^{[3
]}

Davis, T. M. ^{[6
]}

Garnavich, P. M. ^{[7
]}

Jha, S. W. ^{[1
,8
,9
]}

Kirshner, R. P. ^{[4
]}

Krisciunas, K. ^{[10
]}

Leibundgut, B. ^{[11
]}

Li, W. ^{[1
]}

Matheson, T. ^{[12
]}

Miceli, A. ^{[3
]}

Miknaitis, G. ^{[13
]}

Pignata, G. ^{[14
]}

Rest, A. ^{[2
,15
]}

Riess, A. G. ^{[16
,17
]}

Schmidt, B. P. ^{[18
]}

Smith, R. C. ^{[2
]}

Sollerman, J. ^{[6
,19
]}

Spyromilio, J. ^{[11
]}

Stubbs, C. W. ^{[4
,15
]}

Suntzeff, N. B. ^{[2
]}

Tonry, J. L. ^{[20
]}

Wood-Vasey, W. M.

Zenteno, A. ^{[21
]}

机构：

[1] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[2] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile

[3] Univ Washington, Dept Astron, Seattle, WA 98195 USA

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile

[6] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark

[7] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA

[8] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA

[9] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA

[10] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA

[11] European So Observ, D-85748 Garching, Germany

[12] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[13] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[14] Univ Chile, Dept Astron, Santiago, Chile

[15] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

[16] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[17] Johns Hopkins Univ, Baltimore, MD 21218 USA

[18] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo & Siding Spring Observ, Weston, ACT, Australia

[19] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden

[20] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[21] Univ Illinois, Dept Astron, Urbana, IL 61801 USA

来源：

ASTROPHYSICAL JOURNAL | 2008年 / 684卷 / 01期

基金：

美国国家科学基金会;

关键词：

cosmology : observations; distance scale; supernovae : general;

D O I：

10.1086/589612

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 similar to 0.02 mag. The variance in the composite spectra gives an estimate of the intrinsic variance in low-redshift maximum light SN spectra of similar to 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.

引用

页码：68 / 87

页数：20

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