Spatial Structures, Kinematics, and Masses of Faint Galaxies

Details Spatial Structures, Kinematics, and Masses of Faint Galaxies Spatial Structures, Kinematics, and Masses of Faint Galaxies

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.5801k&link_type=abstract

HST Proposal ID #5801

Mathematics

Logic

Hst Proposal Id #5801 Galaxies &Amp, Clusters

Scientific paper

We intend to extract detailed structural information for very faint {B <= 24^m} galaxies from two sets of 4 adjacent V, I WFPC2 images from programs GTO 5090 and 5109. Each set will span the full length available for multislit work with a single pointing of the Keck 10-m low-resolution spectrograph. Thus we can efficiently measure redshifts, emission line ratios, metallicity and age indices, and most importantly, velocity widths {as appropriate for the brightness and spectral-type} for 30 galaxies with each observation. The Keck velocity width data coupled with the HST sizes will provide an unprecedented opportunity to estimate masses, which will be used as independent parameters to probe the luminosity evolution of very faint field galaxies. The high spatial resolution in the two WFPC2 bands is essential to separate differing evolution of the bulge and disk components. In principle, the correlations among velocity width, size or surface brightness, and luminosity are sufficiently tight to untangle evolutionary versus cosmological {q_o} effects. This separation is possible because velocity width and surface brightness are not dependent on q_o, while velocity width and size should depend only weakly on evolution. Our team has extensive experience and tools for analyzing the HST images {developed as part of the Medium Deep Survey in Cycles 1-4}, and equally important, we have access to Keck to ensure acquisition of the vital spectroscopic data once the targets are identified from the archive images.

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