Computer Science
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........28h&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF TORONTO (CANADA), 1995.Source: Dissertation Abstracts International, Volume: 57-04, Section: B, pa
Computer Science
3
Scientific paper
The clustering of faint galaxies is studied using two complementary approaches: the angular (2-D) correlation function and the spatial (3-D) correlation function. The two-point angular correlation function, omega( theta), is constructed from a catalog of 13,000 objects in 24 fields distributed over an area 2 degrees square and complete to a limit of R = 23.5. The amplitude and slope of our correlation function on arcminute scales are in broad agreement with recent CCD results in the literature and decreases with depth. No evidence is found for a flattening of the slope of the correlation function away from delta ~ 0.8. Using the redshift distribution from the recent I-band selected Canada-France Redshift Survey (CFRS) and the observed omega(theta) , Limber's equation is reliably inverted to derive the correlation length beyond the local Universe: r _0 = 1.86 +/- 0.43{rm h}^ {-1} Mpc (q_0 = 0.5) at a redshift z = 0.48. An analogous 3-D approach is used to study the evolution of the correlation length with epoch for the 591 objects in the CFRS that have secure redshifts. The projected correlation function, omega(r_ {p}), which is unaffected by distortions in redshift space, is determined and fit to a power-law in xi(r) in three redshift bins between z = 0.2 and z = 1.0. The measured values of the correlation length in each bin are: r_0(z_{ rm med} = 0.34) = 1.67 +/- 0.19{rm h}^{-1} Mpc, r_0(z _{rm med} = 0.63) = 1.14 +/- 0.12{rm h}^{-1} Mpc, r_0(z_{rm med} = 0.85) = 1.05 +/- 0.18{rm h}^ {-1} Mpc. Results from the 2-D and 3 -D approaches are shown to be in general agreement. Thus, it is argued that the evolutionary parameter epsilon lies between 0 and 2, that is, that the correlation function, xi(r) grows with epoch at a rate (1+z)^{-3} to (1+z)^{-5}. Clustering as a function of colour is studied by dividing the CFRS into blue and red sub-samples. The blue and red sub-samples are found to cluster similarly at high redshifts while the blue galaxies cluster more weakly at low redshift. The implications of these new results are discussed in the context of our understanding of the nature of the faint galaxy population.
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