Determination of the Extragalactic Distance Scale. III. M101. Recovery of 8 Lost Epochs after Safing. Repeat for HOPR#118

Details Determination of the Extragalactic Distance Scale. III. M101. Recovery of 8 Lost Epochs after Safing. Repeat for HOPR#118 Determination of the Extragalactic Distance Scale. III. M101. Recovery of 8 Lost Epochs after Safing. Repeat for HOPR#118

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992hst..prop.5010m&link_type=abstract

HST Proposal ID #5010

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #5010 Galaxies &Amp, Clusters

Scientific paper

Many fundamental problems in cosmology and astrophysics remain unsettled because the value of the expansion rate is uncertain to a factor of two. HST will provide the opportunity to break this impasse. We propose a program which in combination with other GTO and GO work should lead to a measurement of Ho to 10 % accuracy. Our main goal is the observation of Cepheids in two dozen fields in 20 nearby galaxies, for the purpose of calibrating the infrared Tully-Fisher relation as well as other secondary distance indicators, including the Planetary Nebula Luminosity Function, the Globular Cluster Luminosity Function, the Luminosity Variance method, supernovae, and the Faber-Jackson relation. Much of this work must wait for the availability of WFPC2; so our limited goals for Cycles 2 and 3 are: (a) to learn how to find Cepheids and measure their periods and amplitudes from WFC images, (b) to complete the determination of a reliable distance to M81 (and thus to furnish an important calibrator for four of the secondary distance indicators listed above), (c) to discover Cepheids in two radially different (and chemically distinct) fields in the giant spiral galaxy M101. The primary purpose here is to perform an end-to-end test of our method of determining reddening and metallicity independent distances.

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