Erratum: ``A Search for Environmental Effects on Type Ia Supernovae'' [Astron. J. 120, 1479 (2000)]

Details Erratum: ``A Search for Environmental Effects on Type Ia Supernovae'' [Astron. J. 120, 1479 (2000)] Erratum: ``A Search for Environmental Effects on Type Ia Supernovae'' [Astron. J. 120, 1479 (2000)]

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aj....122.3506h&link_type=abstract

The Astronomical Journal, Volume 122, Issue 6, pp. 3506-3507.

Astronomy and Astrophysics

Astronomy

1

Errata, Addenda, Cosmology: Distance Scale, Stars: Supernovae: General

Scientific paper

Ken Nomoto, Chiaki Kobayashi, and Hideyuki Umeda have brought to our attention that the [O/H] abundances for the three spiral galaxies listed in Astron. J. 120, 1479 (2000) were incorrect. The problem was due to the fact that the log(O/H) values adopted for these galaxies corresponded to number ratios and the assumed solar value, log(O/H)solar=-1.93+/-0.07, corresponded to mass ratio. With the correct solar value for number ratio, log(O/H)solar=-3.13+/-0.07 (N. Grevesse, A. Noels, & A. J. Sauval, in ASP Conf. Ser. 99, Cosmic Abundances, ed. S. S. Holt & G. Sonneborn [San Francisco: ASP], 117 [1996]), the [O/H] abundances for the three spirals increase by 1.2 dex. The correct abundances are given in the new Table 3. Figure 1 replaces the Astron. J. 120, 1479 (2000). The main difference is that the metallicity-decline rate relation previously reported for Type Ia supernovae has disappeared. This result is now consistent with the study of the supernova properties as a function of the radial distance from their host galaxy centers (V. D. Ivanov, M. Hamuy, & P. A. Pinto, Astron. J. 120, 1479 (2000) [2000]), which suggests that the supernova diversity is not related to the metallicity of their progenitors. We also mentioned that our observations posed problems to the ``strong wind'' models of H. Umeda, K. Nomoto, C. Kobayashi, I. Hachisu, & M. Kato (Astron. J. 120, 1479 (2000) [1999]), which predict the absence of Type Ia supernovae in environments with [Fe/H]<=-1.0. The reason was that the host galaxy of SN 1972E, NGC 5253, had [O/H]=-1.93. With the revised metallicities we now obtain [O/H]=-0.73 for such galaxy, thus removing the conflict with the models.

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