Astron. Astrophys. 359, 876-886 (2000)

2. Observational data

The data for our analysis come from recent photometric observations of bright SNe Ia, consisting of the large data collections presented by Hamuy et al. (1996b) and Riess (1996, see also Riess et al. 1999). Table 1 summarizes the objects which have sufficient data, in at least the BVRI filters, to construct accurate individual filter light curves. Listed are the available filters (column 2) and the references of the SN photometry (column 3), the adopted distance modulus (column 4) and its source (column 5). The distance modulus is taken either from direct distance measurements via cepheids, surface brightness fluctuations or Tully-Fisher luminosity-line width relation or by adopting a of 65 km s^-1 Mpc^-1 for galaxies in the Hubble flow ( km s^-1). We use the host galaxy dust extinction values of Phillips et al. (1999) (column 6). The Galactic extinction given by the COBE dust maps is provided in column 7 (Schlegel et al. 1998).

Table 1. Photometry of well-observed SN Ia.
a) References:
1) Wells et al. 1994, 2) Lira et al. 1998, 3) Filippenko et al. 1992, 4) Leibundgut et al. 1993, 5) Turatto et al. 1996, 6) Suntzeff 1996, 7) Hamuy et al. 1996b, 8) Richmond et al. 1995, 9) Patat et al. 1996, 10) Meikle et al. 1996, 11) Smith et al. priv. comm., 12) Riess et al. 1999, 13) Sadakane et al. 1996, 14) Saha et al. 1999, 15) Fisher et al. 1999, 16) Hamuy et al. 1996a and references therein, 17) Suntzeff et al. 1999 and references therein, 18) Riess et al. 1996a and references therein

Not all objects have sufficient observations in all filters to guarantee that our method will work. In some cases, the light curve fits had to be restricted to a limited phase range. Only three objects (SN 1989B, SN 1991T, and SN 1994D) have a significant number of U filter observations. Our analysis does not include any JHK or ultraviolet data.

© European Southern Observatory (ESO) 2000

Online publication: July 13, 2000
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