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Title:
Quantitative comparison between type Ia supernova spectra at low and high redshifts: a case study
Authors:
Garavini, G.; Folatelli, G.; Nobili, S.; Aldering, G.; Amanullah, R.; Antilogus, P.; Astier, P.; Blanc, G.; Bronder, T.; Burns, M. S.; Conley, A.; Deustua, S. E.; Doi, M.; Fabbro, S.; Fadeyev, V.; Gibbons, R.; Goldhaber, G.; Goobar, A.; Groom, D. E.; Hook, I.; Howell, D. A.; Kashikawa, N.; Kim, A. G.; Kowalski, M.; Kuznetsova, N.; Lee, B. C.; Lidman, C.; Mendez, J.; Morokuma, T.; Motohara, K.; Nugent, P. E.; Pain, R.; Perlmutter, S.; Quimby, R.; Raux, J.; Regnault, N.; Ruiz-Lapuente, P.; Sainton, G.; Schahmaneche, K.; Smith, E.; Spadafora, A. L.; Stanishev, V.; Thomas, R. C.; Walton, N. A.; Wang, L.; Wood-Vasey, W. M.; Yasuda, N.
Affiliation:
AA(Department of Physics, Stockholm University, Albanova University Center, 106 91 Stockholm, Sweden ; LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), AB(Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101, USA), AC(Department of Physics, Stockholm University, Albanova University Center, 106 91 Stockholm, Sweden ), AD(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), AE(Department of Physics, Stockholm University, Albanova University Center, 106 91 Stockholm, Sweden ), AF(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), AG(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), AH(Osservatorio Astronomico di Padova, INAF, vicolo dell'Osservatorio 5, 35122 Padova, Italy), AI(Department of Physics, University of Oxford, Nuclear & Astrophysics Laboratory, Keble Road, Oxford OX1 3RH, UK), AJ(Colorado College, 14 East Cache La Poudre St., Colorado Springs, CO 80903), AK(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, 94720-7300 CA, USA), AL(American Astronomical Society, 2000 Florida Ave, NW, Suite 400, Washington, DC, 20009 USA), AM(Institute of Astronomy, School of Science, University of Tokyo, Mitaka, Tokyo 181-0015, Japan), AN(CENTRA e Dep. de Fisica, IST, Univ. Tecnica de Lisboa), AO(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), AP(Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37240, USA), AQ(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, 94720-7300 CA, USA), AR(Department of Physics, Stockholm University, Albanova University Center, 106 91 Stockholm, Sweden ), AS(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), AT(Department of Physics, University of Oxford, Nuclear & Astrophysics Laboratory, Keble Road, Oxford OX1 3RH, UK), AU(Department of Astronomy and Astrophysics, University of Toronto, 60 St. George St., Toronto, Ontario M5S 3H8, Canada), AV(National Astronomical Observatory, Mitaka, Tokyo 181-0058, Japan), AW(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), AX(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), AY(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), AZ(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), BA(European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile), BB(Isaac Newton Group, Apartado de Correos 321, 38780 Santa Cruz de La Palma, Islas Canarias, Spain ; Department of Astronomy, University of Barcelona, Barcelona, Spain), BC(Institute of Astronomy, School of Science, University of Tokyo, Mitaka, Tokyo 181-0015, Japan), BD(Institute of Astronomy, School of Science, University of Tokyo, Mitaka, Tokyo 181-0015, Japan), BE(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), BF(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), BG(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, 94720-7300 CA, USA), BH(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), BI(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), BJ(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), BK(Department of Astronomy, University of Barcelona, Barcelona, Spain), BL(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), BM(LPNHE, CNRS-IN2P3, University of Paris VI & VII, Paris, France), BN(Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37240, USA), BO(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), BP(Department of Physics, Stockholm University, Albanova University Center, 106 91 Stockholm, Sweden ), BQ(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), BR(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK), BS(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA), BT(E. O. Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA ; Department of Physics, University of California Berkeley, Berkeley, 94720-7300 CA, USA), BU(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, 277 8582 Japan)
Publication:
Astronomy and Astrophysics, Volume 470, Issue 2, August I 2007, pp.411-424 (A&A Homepage)
Publication Date:
08/2007
Origin:
EDP Sciences
Keywords:
stars: supernovae: general, cosmology: early Universe
DOI:
10.1051/0004-6361:20065400
Bibliographic Code:
2007A&A...470..411G

Abstract

We develop a method to measure the strength of the absorption features in type Ia supernova (SN Ia) spectra and use it to make a quantitative comparisons between the spectra of type Ia supernovae at low and high redshifts. In this case study, we apply the method to 12 high-redshift (0.212 ≤ z ≤ 0.912) SNe Ia observed by the Supernova Cosmology Project. Through measurements of the strengths of these features and of the blueshift of the absorption minimum in Ca ii H&K, we show that the spectra of the high-redshift SNe Ia are quantitatively similar to spectra of nearby SNe Ia (z < 0.15). One supernova in our high redshift sample, SN 2002fd at z = 0.279, is found to have spectral characteristics that are associated with peculiar SN 1991T/SN 1999aa-like supernovae.
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