Distances to Stellar Explosions. The case of Core-Collapse Supernovae

Details Distances to Stellar Explosions. The case of Core-Collapse Supernovae Distances to Stellar Explosions. The case of Core-Collapse Supernovae

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1111..565d&link_type=abstract

PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE: CEFALU 2008, Proceedings of the International Conference. AIP Conferen

Physics

3

Radiative Transfer, Scattering, Supernova Remnants, Gamma-Ray Sources, Gamma-Ray Bursts

Scientific paper

We review the usage of Type II supernovae (SNe) for distance determinations, with an emphasis on the Expanding Photosphere Method (EPM). Despite their generally high luminosity powered in a large part through ejecta/CSM interaction, Type IIn SNe are at present rather unreliable distance measuring tools. In contrast, the apparently homogeneous sample of red supergiant stars from which Type II-Plateau (II-P) SNe seem to derive make these events much more attractive. After briefly describing core-collapse SN ejecta properties, we present the EPM and the properties of the correction factors ξ that allow one to approximate the observed SN spectral energy distribution as a blackbody. We suggest that a former discrepancy with a Cepheid-based distance resulted from the use of ξ values that were systematically too small and of a time baseline extending into the recombination phase when such factors are highly sensitive to color-temperature Tc. From a large sample of non-LTE models, we find a >~20% scatter in ξ for a given Tc, making the use of analytical ξ-Tc distributions unreliable at that level. Such ξ uncertainties are visible in the scatter obtained for the distance determined from different filter combinations. However, employing tailored models to multi-epoch spectroscopic observations, one can obtain a distance with a <~10% accuracy, and differing by no more than 1% between different bandpass choices. We advocate the use of Type II-P SNe for an independent determination of the Hubble constant, and present means of alleviating the requirement for multiple high S/N spectra by selecting Type II SNe with breakout detections obtained through the GALEX Time-Domain-Survey.

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