Other
Scientific paper
Jun 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991phdt........15w&link_type=abstract
Ph.D. Thesis California Univ., Berkeley.
Other
58
Calibrating, Charge Coupled Devices, Galactic Clusters, Photometry, Red Shift, Spiral Galaxies, Velocity Distribution, Astronomical Observatories, Imaging Techniques, Magnitude, Statistical Analysis, Universe
Scientific paper
Tau band CCD photometric data for a sample of over 500 spiral galaxies is presented. These data were obtained from CCD images acquired at the Lick Observatory 40 inch Nickel Telescope. All of the galaxies in the sample have quality 21 cm (HI) redshift and linewidth data, which I have obtained from the published literature. I use the CCD photometric and HI data for a subsample of 156 cluster galaxies to study the properties of the luminosity-rotation velocity ('Tully-Fisher') relation for spirals. I show how the imaging character of the CCD photometry permits the definition of highly accurate total apparent magnitudes and ellipticites for the galaxies, which in turn lead to a Tully-Fisher relation with small scatter (sigma approximately equals 0.30 mag). My analysis also produces a calibration of the Tully-Fisher relation. This calibration entails zeropointing the Tully-Fisher relation at the distance of the Coma cluster, and measuring the expansion rate of the Universe in units of velocity/(distance to Coma). I apply the calibrated Tully-Fisher relation to another subsample of 330 field galaxies in the Perseus-Pisces Supercluster region. My results indicate that the highly overdense filament, or 'main ridge', of the Perseus-Pisces concentration is moving toward the Local Group with a peculiar velocity of amplitude approximately 350 km s-1. I note that this motion, in combination with other streaming motions previously detected in the local Universe, argues for the presence of a very long wavelength component of the peculiar velocity field. I place great emphasis on the critical role played by statistical biases in the analysis of Tully-Fisher data sets. I distinguish, and examine in quantitative detail, two kinds of bias: one which affects predicted apparent magnitudes when galaxy distances are given by a physical model, such as the redshift-distance relationship; and another which affects redshift-independent distances inferred directly from the Tully-Fisher data. My analysis leads to accurate mathematical formulae for bias correction. I apply these formulae to the data in both my calibration of the Tully-Fisher relation, and my study of peculiar velocities in Perseus-Pisces.
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