The Expanding Photosphere Method (EPM): Distance Calculations to Type II-P Supernovae and a Comparison with the Standard Candle Method

Details The Expanding Photosphere Method (EPM): Distance Calculations to Type II-P Supernovae and a Comparison with the Standard Candle Method The Expanding Photosphere Method (EPM): Distance Calculations to Type II-P Supernovae and a Comparison with the Standard Candle Method

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733721e&link_type=abstract

American Astronomical Society, AAS Meeting #217, #337.21; Bulletin of the American Astronomical Society, Vol. 43, 2011

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The use of independent methods to calculate extragalactic distances is important to help constrain cosmological parameters and to provide mutual checks on the external accuracy of other distance measuring techniques. In this work we present EPM distance estimates to a group of nearby (≤150 Mpc) Type II-Plateau Supernovae (SN-IIP) that are drawn from a sample for which distances have previously been determined by Poznanski et al. (2009) using the Standardized Candle Method (SCM), an independent distance-measuring technique for SNe II-P. We use the same photometric and spectral data as was used by Poznanski et al. (2009), which enables a direct comparison between the two techniques. To calculate our EPM distances we use the dilution factors of Jones et al. (2009), which were derived from the atmosphere models of Dessart & Hillier (2005b), and employ the filter subsets {BV}, {BVI}, and {VI}. Our “best” EPM distance estimates are derived as the mean of the three individual distances. We compare the EPM and SCM distance measurements and speculate on potential causes of any discrepancies found between our study and a parallel one carried out by Olivares et al. (2010) using a different dataset (which found a 40% difference between EPM and SCM distances, in the sense that EPM distances were systematically larger). Finally, we use our sample of EPM distances to SNe II-P to estimate the Hubble constant. We are grateful for the financial support of NSF grant AST-0908886, the TABASGO Foundation, and (for DP) an Einstein Fellowship.

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