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Title:
Using Line Profiles to Test the Fraternity of Type Ia Supernovae at High and Low Redshifts
Authors:
Blondin, Stéphane; Dessart, Luc; Leibundgut, Bruno; Branch, David; Höflich, Peter; Tonry, John L.; Matheson, Thomas; Foley, Ryan J.; Chornock, Ryan; Filippenko, Alexei V.; Sollerman, Jesper; Spyromilio, Jason; Kirshner, Robert P.; Wood-Vasey, W. Michael; Clocchiatti, Alejandro; Aguilera, Claudio; Barris, Brian; Becker, Andrew C.; Challis, Peter; Covarrubias, Ricardo; Davis, Tamara M.; Garnavich, Peter; Hicken, Malcolm; Jha, Saurabh; Krisciunas, Kevin; Li, Weidong; Miceli, Anthony; Miknaitis, Gajus; Pignata, Giuliano; Prieto, Jose Luis; Rest, Armin; Riess, Adam G.; Salvo, Maria Elena; Schmidt, Brian P.; Smith, R. Chris; Stubbs, Christopher W.; Suntzeff, Nicholas B.
Affiliation:
AA(European Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching D-85748, Germany; , , .), AB(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; .), AC(European Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching D-85748, Germany; , , .), AD(Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019; .), AE(Department of Astronomy, University of Texas, Austin, TX 78681; .), AF(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; , .), AG(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719-4933 .), AH(Department of Astronomy, University of California, Berkeley, CA 94720-3411 , , , , .), AI(Department of Astronomy, University of California, Berkeley, CA 94720-3411 , , , , .), AJ(Department of Astronomy, University of California, Berkeley, CA 94720-3411 , , , , .), AK(Stockholm Observatory, AlbaNova, SE-106 91 Stockholm, Sweden; .), AL(European Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching D-85748, Germany; , , .), AM(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; , , , , .), AN(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; , , , , .), AO(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile; .), AP(Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile; , , , .), AQ(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; , .), AR(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 , , .), AS(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; , , , , .), AT(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 , , .), AU(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Cotter Road, Weston Creek, ACT 2611, Australia; , , .), AV(Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556-5670 , .), AW(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; , , , , .; Department of Physics, Harvard University, 17 Oxford Street, Cambridge, MA 02138.), AX(Department of Astronomy, University of California, Berkeley, CA 94720-3411 , , , , .), AY(Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556-5670 , .), AZ(Department of Astronomy, University of California, Berkeley, CA 94720-3411 , , , , .), BA(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 , , .), BB(Department of Physics, University of Washington, Box 351560, Seattle, WA 98195-1560 .), BC(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile; .), BD(Department of Astronomy, Ohio State University, 4055 McPherson Laboratory, 140 West 18th Avenue, Columbus, OH 43210; .), BE(Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile; , , , .), BF(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; .), BG(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Cotter Road, Weston Creek, ACT 2611, Australia; , , .), BH(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Cotter Road, Weston Creek, ACT 2611, Australia; , , .), BI(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile; .), BJ(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; , , , , .; Department of Physics, Harvard University, 17 Oxford Street, Cambridge, MA 02138.), BK(Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile; .)
Publication:
The Astronomical Journal, Volume 131, Issue 3, pp. 1648-1666. (AJ Homepage)
Publication Date:
03/2006
Origin:
UCP
AJ Keywords:
Cosmology: Observations, Line: Formation, Line: Profiles, Stars: Supernovae: General
DOI:
10.1086/498724
Bibliographic Code:
2006AJ....131.1648B

Abstract

Using archival data of low-redshift (z<0.01 Center for Astrophysics and SUSPECT databases) Type Ia supernovae (SNe Ia) and recent observations of high-redshift (0.16<z<0.64) SNe Ia, we study the ``uniformity'' of the spectroscopic properties of nearby and distant SNe Ia. We find no difference in the measurements we describe here. In this paper we base our analysis solely on line-profile morphology, focusing on measurements of the velocity location of maximum absorption (vabs) and peak emission (vpeak). Our measurement technique makes it easier to compare low and high signal-to-noise ratio observations. We also quantify the associated sources of error, assessing the effect of line blending with assistance from the parameterized code SYNOW. We find that the evolution of vabs and vpeak for our sample lines (Ca II λ3945, Si II λ6355, and S II λλ5454, 5640) is similar for both the low- and high-redshift samples. We find that vabs for the weak S II λλ5454, 5640 lines and vpeak for S II λ5454 can be used to identify fast-declining [Δm15(B)>1.7] SNe Ia, which are also subluminous. In addition, we give the first direct evidence in two high-z SN Ia spectra of a double-absorption feature in Ca II λ3945, an event also observed, although infrequently, in low-redshift SN Ia spectra (6 out of 22 SNe Ia in our local sample). Moreover, echoing the recent studies of Dessart & Hillier in the context of Type II supernovae (SNe II), we see similar P Cygni line profiles in our large sample of SN Ia spectra. First, the magnitude of the velocity location at maximum profile absorption may underestimate that at the continuum photosphere, as observed, for example, in the optically thinner line S II λ5640. Second, we report for the first time the unambiguous and systematic intrinsic blueshift of peak emission of optical P Cygni line profiles in SN Ia spectra, by as much as 8000 km s-1. All the high-z SNe Ia analyzed in this paper were discovered and followed up by the ESSENCE collaboration and are now publicly available.

Based in part on observations obtained at the Cerro Tololo Inter-American Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation (NSF); the European Southern Observatory, Chile (ESO program 170.A-0519) the Gemini Observatory, which is operated by AURA under a cooperative agreement with the NSF on behalf of the Gemini partnership (the NSF [United States], the Particle Physics and Astronomy Research Council [United Kingdom], the National Research Council [Canada], CONICYT [Chile], the Australian Research Council [Australia], CNPq [Brazil], and CONICET [Argentina]) (programs GN-2002B-Q-14, GN-2003B-Q-11, and GS-2003B-Q-11) the Magellan Telescopes at Las Campanas Observatory; the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona; and the F. L. Whipple Observatory, which is operated by the Smithsonian Astrophysical Observatory. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.


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