The Cepheid Distance to NGC 1637: A Direct Comparison with the EPM Distance to SN 1999em

Details The Cepheid Distance to NGC 1637: A Direct Comparison with the EPM Distance to SN 1999em The Cepheid Distance to NGC 1637: A Direct Comparison with the EPM Distance to SN 1999em

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9155l&link_type=abstract

HST Proposal ID #9155

Computer Science

Hst Proposal Id #9155 Cosmology

Scientific paper

Opportunities to directly compare distances estimated by two primary extragalactic distance indicators are rare. The appearance of supernova 1999em, a bright, extremely well- observed type II plateau {II-P} event in the nearby SBc galaxy NGC 1637 {v = 717 km s^-1}, offers the best chance to test the consistency of the Expanding Photosphere Method {EPM} of supernova distance determination with that derived from Cepheid variable stars. Although EPM distances have been measured to 18 type II supernovae out to 180 Mpc and used to determine Hubble's constant independent of the Cepheid distance scale {H_o = 73 +/- 7 km s^-1 Mpc^-1 Schmidt et al. 1994a}, there have never been any measurements of Cepheids in a galaxy that has hosted a normal type II-P supernova, the classic variety of core-collapse event to which EPM-derived distances are most robust. We thus propose to determine the distance to NGC 1637 through the discovery and analysis of its Cepheid variable stars. Since previous distance estimates to NGC 1637 exist using the Tully-Fisher relation {d = 8.9 Mpc} and the galaxy's brightest red supergiants {d = 7.8 Mpc}, a Cepheid distance will further refine the calibration of these secondary distance indicators as well. Cycle 10 observations of NGC 1637 will also provide rare late-time light curve measurements of a type II-P supernova more than two years after explosion.

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