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Spectra of high-redshift type Ia supernovae and a comparison with their low-redshift counterparts

  • Author(s): Hook, IM
  • Howell, DA
  • Aldering, G
  • Amanullah, R
  • Burns, MS
  • Conley, A
  • Deustua, SE
  • Ellis, R
  • Fabbro, S
  • Fadeyev, V
  • Folatelli, G
  • Garavini, G
  • Gibbons, R
  • Goldhaber, G
  • Goobar, A
  • Groom, DE
  • Kim, AG
  • Knop, RA
  • Kowalski, M
  • Lidman, C
  • Nobili, S
  • Nugent, PE
  • Pain, R
  • Pennypacker, CR
  • Perlmutter, S
  • Ruiz-Lapuente, P
  • Sainton, G
  • Schaefer, BE
  • Smith, E
  • Spadafora, AL
  • Stanishev, V
  • Thomas, RC
  • Walton, NA
  • Wang, L
  • Wood-Vasey, WM
  • et al.

Published Web Location

https://doi.org/10.1086/497635
Abstract

We present spectra for 14 high-redshift (0.17 < z < 0.83) supernovae, which were discovered by the Supernova Cosmology Project as part of a campaign to measure cosmological parameters. The spectra are used to determine the redshift and classify the supernova type, essential information if the supernova are to be used for cosmological studies. Redshifts were derived either from the spectrum of the host galaxy or from the spectrum of the supernova itself. We present evidence that these supernovae are of Type Ia (SNe Ia) by matching to spectra of nearby supernovae. We find that the dates of the spectra relative to maximum light determined from this fitting process are consistent with the dates determined from the photometric light curves, and, moreover, the spectral time sequences for SNe Ia at low and high redshift are indistinguishable. We also show that the expansion velocities measured from blueshifted Ca H and K are consistent with those measured for low-redshift SNe Ia. From these first-level quantitative comparisons we find no evidence for evolution in SN Ia properties between these low- and high-redshift samples. Thus, even though our samples may not be complete, we conclude that there is a population of SNe Ia at high redshift whose spectral properties match those at low redshift. © 2005. The American Astronomical Society. All rights reserved.

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