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Title: Galaxy clustering and dynamics from redshift surveys
Author: Hale-Sutton, Duncan
ISNI:       0000 0001 3524 3908
Awarding Body: Durham University
Current Institution: Durham University
Date of Award: 1990
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The clustering and dynamical properties of the 368 galaxies in the redshift surveys of Metcalfe et al. (1989) and Parker et al. (1986) are investigated. These galaxies were selected from ten high galactic latitude fields complete to a magnitude limit of m(b(_J))<17(^m). These complement the five similarly selected fields in the survey of Peterson et al. (1986) and so the overall clustering and dynamical properties of all three samples are discussed. Initial studies of the distribution of galaxies in the survey of Peterson et al. were carried out by Bean (1983). This thesis extends that earlier work by examining the conclusions of Bean in the larger volume of the new surveys considered here. It is found that, whilst the combined estimate of the line-of-sight peculiar motions in the three samples together is in reasonable accord with that found previously, the range of peculiar motions in the individual samples is larger than previously anticipated. The rms pair-wise velocity (w(^2))(^1/2) is found to be (w(^2)(^1/2)=(600±140)kms(^-1) in the Metcalfe et al. survey as compared to (w(^2))(^1/2)=(0±240)kms(^-1) and w(w(^2))(^1/2)=(190± 90)(^-1) in the Parker et al. and Peterson et al. samples, respectively. These estimates of the motions of galaxies at spatial scales of ~1h(^-1) Mpc (H(_o)=100kms(^-1) Mpc(^-1)) together with measures of the clustering provide constraints on the mean mass density of the Universe through the Cosmic Virial Theorem. It is found that the mean mass density parameter for the three samples considered as a whole is Ω(_o)=0.18±0.09, on the assumption that galaxies trace the mass distribution, and this constraint is similar to that obtained previously mainly because of the larger range of peculiar motions found. The clustering distribution of the galaxies in the new samples was investigated on spatial scales ranging from a few up to -l00h(^-1) Mpc. It was found from the number-redshift and number-magnitude counts that these samples were fairly homogeneous at the largest scales and in good agreement with previous results from the Peterson et al. catalogue. Thus using these samples to estimate the mean clustering properties of galaxies, it was found, from the two-point correlation function ~5(s), that the galaxies in the new samples appear to exhibit a preferred clustering length at -2h(^-1) Mpc and this confirms the 'shoulder ' detected in the correlation function of the Peterson et al. data by Bean (1983). On the basis that this shoulder is a real spatial feature (and not caused by peculiar motions) the mean clustering length of galaxies in the three samples is r(_o) =(6.6±0.5)h(^-1) Mpc in the range 2
Supervisor: Not available Sponsor: Not available
Qualification Name: Thesis (Ph.D.) Qualification Level: Doctoral
EThOS ID:  DOI: Not available
Keywords: Astrophysics