All Tables

Table 1: The low redshift spectra analyzed in this study. The dates correspond to the epoch relative to maximum luminosity in the B-band. Many of these spectra are available in the SUSPECT archive as well as their listed publications.
Table 2: The photometric properties of the low-z spectra analyzed in this study. The published photometry from these objects was re-fit to determine the magnitudes and lightcurve shape parameters shown here. SN 1991M did not have published photometry in B-band, so the parameters for this object were not determined. The SNLS models did not fit the sub-luminous SN 1991bg with any accuracy; the values given here for this unusual object are from Altavilla et al. (2004). The precision of the derived values for the unusual SN 2000cx are also in doubt and were not used in any of the analysis in this paper. Uncertainties in each quantity are given in brackets.
Table 3: Wavelength regions for the SNeIa features defined by F04.
Table 4: A quantitative comparison of the spectroscopic features in high-z supernovae (as measured with EW and CaII H&K ejection velocities) and the mean trends exhibited for these quantities by local SNe Ia. These results show that there are no significant differences between distant SNLS objects and nearby SNe, with the exception of EW{MgII}.
Table 5: Comparison of SNe Ia spectral features in different host types at low and high-z. The values given are the mean and error in the mean of the residuals from the low-z trend.
Table 7: SNLS identifications and derived properties for SNe candidates observed from Nov. 2004 to May 2006.
Table 6: Observed properties and instrument settings for SNLS SNe candidates observed from November 2004 to May 2006. The magnitudes and "percentage increase'' are estimated from the lightcurves and correspond to the date of spectroscopy.
Table A.1: Equivalent width and ejection velocity results for the published high redshift SNe Ia observed by the SNLS at the Gemini telescopes. This set includes all of the SNLS objects (reduced by the author) that were confirmed as Type Ia SNe (a confidence index of 3 or higher) and were subject to less than 65% contamination from their host galaxies. The blank spaces (" $\cdots$ '') indicate where a measurement had to be removed due to inadequate wavelength coverage. The uncertainties in the EW results include measurement errors, errors from any possible variance in the pseudo-continuum, and the uncertainty from the host galaxy contamination correction.