Abstract
Type Ia supernovae (SNs Ia), produced by the thermonuclear explosion of white dwarf (WD) stars, are used here to derive extragalactic distances and an estimate of the Hubble constant from their emission signatures at late phases (nebular SN Ia method, NSM). The method, first developed in Ruiz-Lapuente & Lucy, makes use here of an improved modeling of the forbidden line emission at late phases. Hydrodynamic models of the explosion of WDs of different masses, both sub-Chandrasekhar and Chandrasekhar, provide the basis for comparison with observations. It is shown that it is possible to probe the overall density structure of the ejecta and the mass of the exploding WD by the effect that the electron density profile has in shaping the forbidden line emission of the iron ions, and that a robust diagnostic of the mass of the exploding WD can be obtained. Cosmic distance scale can thus be related to basic diagnostics of excitation of iron lines. Once the most adequate model is selected, comparison of the predicted line emission at these phases with the observed spectra gives an internal estimate of both the reddening and the distance to the SNs Ia. The results presented here favor denser models than those corresponding to sub-Chandrasekhar explosions. From a sample of seven SNs Ia in Leo, Virgo, Fornax, and beyond, a value of the Hubble constant H0 = 68 ± 6 (statistical) ±7 (systematic) km s-1 Mpc-1 is derived. The depth of the Virgo cluster is found to be large, ranging from 13 to 23 Mpc at least. If NGC 4526 traces well the core of the Virgo Cluster, then the latter is located at 16 ± 2 Mpc. The galaxy NGC 3267 in Leo appears to be located at 9.8 ± 1.5 Mpc.
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