The blue anbd visual absolute magnitude distributions of Type IA supernovae

Details The blue anbd visual absolute magnitude distributions of Type IA supernovae The blue anbd visual absolute magnitude distributions of Type IA supernovae

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...439..558v&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 439, no. 2, p. 558-564

Astronomy and Astrophysics

Astrophysics

72

Data Reduction, Stellar Magnitude, Supernovae, Astronomical Photometry, Astronomical Spectroscopy, Color-Color Diagram, Color-Magnitude Diagram, Distance, Hubble Constant, Spectrum Analysis

Scientific paper

Tully-Fisher (TF), surface brightness fluctuation (SBF), and Hubble law distances to the parent galaxies of Type Ia supernovae (SNs Ia) are used in order to study the SN Ia blue and visual peak absolute magnitude (MB and MV) distributions. We propose two objective cuts, each of which produces a subsample with small intrinsic dispersion in M. One cut, which can be applied to either band, distinguishes between a subsample of bright events and a smaller subsample of dim events, some of which were extinquished in the parent galaxy and some of which were intrinsically subluminous. The bright events are found to be distributed with an observed dispersions of 0.3 less than or approximately = Sigmaobs less than or approximately = 0.4 about a mean absolut magnitude (M-barB or M-barV). Each of the dim SNs was spectroscopically peculiar and/or had a red B-V color; this motivates the adoption of an alternative cut that is based on B-V rather than on M. To wit, SNs Ia that are both known to have -0.25 less than B-V less than + 0.25 and not known to be spectroscopically peculiar show observational dispersion of only Sigmaobs(MB) = Sigmaobs(MV) = 0.3. Because characteristics observational errors produce Sigmaerr(M) greater than 0.2,the intrinsic dispersion among such SNs Ia is Sigmaint(M) less than or approximately = 0.2. The small observational dispersion indicates that SNs Ia, the TF relation, and SBFs all good relative distances to those galaxies that produce SNs Ia. The conflict between those who use SNs Ia in order to determine the value of the Hubble constant (H0) and those who use TF and SBF distances to determine H0 results from discrepant calibrations.

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