Erratum: ``The Hubble Higher z Supernova Search: Supernovae to z ~ 1.6 and Constraints on Type Ia Progenitor Models'' (ApJ, 613, 200 [2004])

Details Erratum: ``The Hubble Higher z Supernova Search: Supernovae to z ~ 1.6 and Constraints on Type Ia Progenitor Models'' (ApJ, 613, 200 [2004]) Erratum: ``The Hubble Higher z Supernova Search: Supernovae to z ~ 1.6 and Constraints on Type Ia Progenitor Models'' (ApJ, 613, 200 [2004])

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...635.1370s&link_type=abstract

The Astrophysical Journal, Volume 635, Issue 2, pp. 1370-1372.

Astronomy and Astrophysics

Astronomy

13

Errata, Addenda

Scientific paper

We have found an error in our rate calculation, modest in size, due to a computational error in the volume of shells with radius z. This error was ~20% in size; after fixing it, we get the new results described here.
We have recalculated the maximum likelihood values for each of the tested models, and the results are very encouraging. In the narrow Gaussian model, the maximum likelihood value for the mean delay time of SNe Ia has decreased, but remains large, with τ=3.4 Gyr (see Fig. E1). In the revised Table 3 we show the maximum likelihood values of τ for each tested model. We also show the range in τ that contains 95% of the most likely values for τ.
The updated version of Figure 12 given here shows the Bayesian probability distributions for each of the tested models. As can be seen, e-folding models still prefer long folding times, of at least 1 Gyr but with a preference for folding times greater than 2-3 Gyr. However, these models predict that SNe Ia are just as likely to be prompt (<1 Gyr delays) as they are to have long, 10 Gyr delay times. Such models produce poorer fits to the observed redshift distributions than the Gaussian models, primarily because they require a higher fraction of SNe Ia at very high redshifts (z>~1.4) than were observed (see revised Fig. 14 given here). It is still the case that we find our narrow Gaussian model gives the best fit to the observations, now with a mean of 3.4 Gyr. This still implies that SNe Ia stem from single degenerate systems with low-mass companion stars.
Finally, there is a typographical error in the expression of the volume shown in the manuscript. The volume at redshift z is V(z)=(4π/3)[Dp(z)]3=(4π/3)(1+z)-3[DL(z)]3, where Dp(z) is the proper motion distance, and DL(z) is the luminosity distance to redshift z. The correct form of the equation has always been used in the calculations.
We thank Francisco Forster, Christian Wolfe, and Philipp Podsiadlowski of Oxford University for pointing out these errors in the manuscript.

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