Mathematics – Logic
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........13s&link_type=abstract
Thesis (PH.D.)--DARTMOUTH COLLEGE, 1995.Source: Dissertation Abstracts International, Volume: 56-07, Section: B, page: 3807.
Mathematics
Logic
2
Scientific paper
The distribution and peculiar motions of galaxies in the main ridge of the Perseus-Pisces Supercluster (PPS) are investigated. This region is the densest section of the PPS and is composed mainly of three concentrations of galaxies, the cluster Abell 262 and the NGC 507 and NGC 383 groups. Both a redshift survey and I-band Tully -Fisher (TF) distance measurements were used to study the three-dimensional structure of the supercluster. The redshift survey consisting of 724 galaxies shows that the core of A262 within 0.5^circ is indeed virialized. However, the 'clumpy' nature of the distribution of galaxies in the main ridge suggests that the supercluster is relatively young dynamically, with galaxies still accreting onto major galaxy concentrations. The morphological segregation of galaxies is seen both in the plane of the sky and in redshift space, indicating an asymmetric infall of spirals into the cluster core and providing evidence that the clusters are not yet fully evolved. The TF distances were obtained from I-band surface photometry and HI 21cm linewidth observations for 57 galaxies. The main ridge can be characterized as a filament, with galaxies infalling from both sides. The observed infall pattern, after correcting for the non-homogeneous Malmquist effect and differences in the sample, could have an amplitude up to 1000 km rm s^{-1}. However, the sizes of the errors are comparable with the magnitudes of the peculiar velocities; thus the observed infall is not statistically significant. We showed that the use of wrong TF slope leads to unphysically large peculiar velocities. We also demonstrated that it was necessary to apply a different treatment and separate TF relation to set of galaxies which are morphologically and intrinsically different. The TF analysis also revealed the clumpy nature of the galaxy distribution in the ridge, which agrees with the results of the redshift survey. Although the overall picture seems to support the hierarchical CDM model in which small-scale structures form and then coalesce into a supercluster, the observational and systematic errors are too large to allow confirmation of the existence of the observed infall velocities.
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