! +====================+ ! | PED OUTPUT PRODUCT | ! +====================+ ! ! /data/frodo1/aroman/work/6554.prop ! Generated by PREPROCESSOR, version 7.0.1e ! Date: Tue Mar 04 12:43:50 EST 1997 Proposal_Information Title: Extragalactic Globular Cluster Systems Proposal_Category: GO Scientific_Category: STELLAR POPULATIONS Cycle: 6 Investigators PI_Name: Jean Brodie PI_Institution: Lick Observatory, University of California CoI_Name: John Huchra CoI_Institution: Smithsonian Astrophysical Observatory Contact: Y CoI_Name: Duncan Forbes CoI_Institution: Lick Observatory, University of California Contact: N CoI_Name: Kenneth Freeman CoI_Institution: Mount Stromlo and Siding Springs Observatory Contact: N CoI_Name: Carl Grillmair CoI_Institution: Lick Observatory, University of California Contact: N Abstract: We propose to use WFPC2 imaging data to compile catalogues of globular clusters (GCs) for 6 galaxies: NGC 524, 1023, 3311, 4365, 4494 and 7619, which cover a range in galaxy luminosity, morphological type, environment, GC specific frequency and GC mean metallicity. The primary scientific aims of this program are: 1) To study the GC systems of galaxies of various types and in different environments (e.g. isolated/centrally located within rich/poor clusters of galaxies) to explore possible correlations of GC properties (colors, metallicities, kinematics) with parent galaxy properties (luminosity, morphology, environment, specific frequency, merger history). 2) To derive globular cluster luminosity functions (GCLFs) for program galaxies and determine the extent to which the luminosity of the peak in the function is universal. The peak luminosity will be used as a standard candle for distance determinations relevant to estimations of H_0. Surface brightness fluctuation (SBF) measurements exist for all but one of the target galaxies and will provide a calibration of the GCLF distances. A major objective is to obtain accurate identifications (magnitudes, colors and positions) of GCs for follow-up spectroscopy with the Keck telescope for abundances and kinematics. Spectroscopy will be feasible down to V=24 which will allow the most complete study to date of GC systems beyond the Local Group. Questions Observing_Description: We propose to obtain images at two pointings for each galaxy, the central region and a region offset by 2' from the central pointing. We wish to observe in two filters (F555W and F814W) at each pointing. Both image size and V-I colors will be used to discriminate against background galaxies and V--I colors will provide an estimate of metallicity for those GCs too faint (24