All Tables

Table 1: Summary of the parameters used in this work to describe the I-band light curve. The first five parameters are determined by fitting the data (see text for details). The next four parameters are determined from the first set and are the actual time and peak values of the light curve.
Table 3: List of SNe used in the Hubble diagram. $m_I^{\rm eff}$ is the peak magnitude corrected for dust extinction and for the width-luminosity relation, following Eq. (1). The quoted uncertainties do not include the redshift contribution due to peculiar velocities in the host galaxies, assumed equal to 300 km s^-1. Redshifts from Table 2 are here transformed into the CMB frame.
Table 4: Summary of $J_{\rm s}$ -band data for SN 2000fr. The quoted errors are due to statistical Poisson noise and the uncertainty in the ZP (contributing 0.01 mag). Epochs are in restframe days relative to the date of B-band maximum. The restframe I-band is obtained through cross-filter k-correction from the observed $J_{\rm s}$ -band to Bessel I-band. The uncertainties also include the contribution from k-corrections, estimated to be 0.05 mag at all epochs considered.
Table 5: Summary of IR data for SN 1999ff. Epochs are in restframe days relative to the date of the B-band maximum ( $t_{\rm max}={\rm MJD}~51494.8$ ); restframe I-band magnitudes are computed applying k-corrections to the observed J-band data published in Tonry et al. (2003). The uncertainties also include the contribution from k-corrections, estimated to be 0.05 mag at all epochs considered.
Table 6: List of the high redshift type Ia SNe used in this work. Columns are: IAU name, redshift, number of data points used in the fit, magnitude of the peak resulted from the fit (both statistical and systematic uncertainties are given) before Milky Way extinction correction, best fit template, $\chi ^2$ of the fit, Milky Way extinction in the J-band.
Table 7: $\chi ^2$ (for 2 d.o.f.) of each model to the high redshift data, without stretch correction and with systematic uncertainties added in quadrature ( $\chi ^2_a$ ), neglecting the systematic uncertainties ( $\chi ^2_b$ ), with stretch correction and adding the systematic uncertainties in quadrature ( $\chi ^2_c$ ) or neglecting them ( $\chi ^2_d$ ).
Table 8: Restframe B-I colours in magnitudes for the two high redshift SNe. The Epoch is in restframe days relative to the B-band maximum, divided by the B-band stretch.
Table 9: Restframe B-V colours in magnitudes for SN 1999ff and SN 2000fr. The Epoch is in rest frame days relative to the B-band maximum, divided by the B-band stretch.
Table 10: $\chi ^2$ computed for the 3 different models and colours for each of the supernovae and for their combination.
Table 11: $\Delta \chi ^2$ for the fit of the high redshift SNe to the templates of the two underluminous SNe relative to the best fits (which are "normal'' SN templates). n is the number of data points used in the one-parameter fit (see discussion in Sect. 4.4).
Table 2: Results of the I-band light curve fit of 42 nearby supernovae: t₁ and I₁ are the parameters for the time and amplitude fitted on the first template, t₂ and I₂ are the parameters for the time and amplitude fitted on the second template, and s_I is the stretch factor. N is the number of points used in the fit ( ${\rm d.o.f.}=N-5$ ). The data were taken from: ¹ Wells et al. (1994), ² Richmond et al. (1995), ³ Riess et al. (1999), ⁴ Hamuy et al. (1996a), ⁵ Jha (2002), ⁶ Filippenko et al. (1992b), Leibundgut et al. (1993).