The Center for Astrophysics Redshift Survey: Luminosity Function and Two-Point Correlation Function

The aim of the survey is to sample a relatively large, randomly chosen volume of the Universe in order to study the large-scale distribution of galaxies using the two-point correlation function, the peculiar velocities between galaxy pairs and to provide an estimate of the galaxian luminosity function that is unaffected by density inhomogeneities and Virgo infall.

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The Center for Astrophysics Redshift Survey: Luminosity Function and Two-Point Correlation Function

Symposium - International Astronomical Union ◽

10.1017/s0074180900136502 ◽

1988 ◽

Vol 130 ◽

pp. 519-519

Author(s):

Valérie de Lapparent ◽

Margaret J. Geller ◽

John P. Huchra

Keyword(s):

Correlation Function ◽

Luminosity Function ◽

Theoretical Models ◽

Spatial Correlation Function ◽

Correlation Lengths ◽

Two Samples ◽

Derived Properties ◽

Point Correlation ◽

Point Correlation Function ◽

Redshift Survey

We compare the luminosity function and the two-point spatial correlation function for the two slices of the CfA redshift survey extension to mB(0) ≤ 15.5 [8h ≤ RA. ≤ 17h and 26.5° ≤ DEC. ≤ 38.5°], with those for the early survey limited to mB(0) ≤ 14.5 [bII ≥ 40°, and DEC. ≥ 0°]. The derived properties of the two samples agree within the errors. The parameters of the luminosity function are M* = −19.1±0.1 and α = −1.2±0.1 for the 15.5 sample, and M* = −19.3±0.1 and α = −1.1 ± 0.1 for the 14.5 sample. We use an inhomogeneity-independent method to calculate the luminosity function. The slopes of the correlation functions for the two samples are −1.5 ± 0.35, shallower than the canonical slope of −1.8. The correlation lengths are 7.5 ± 5h−1 Mpc, larger than the correlation length of 5h−1 Mpc matched to the theoretical models. Because of the 25% uncertainty in the mean density of the 15.5 sample, the correlation function is indeterminate on scales larger than ∼ 20h−1 Mpc.

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Results from a faint QSO redshift survey

Symposium - International Astronomical Union ◽

10.1017/s0074180900152192 ◽

1986 ◽

Vol 119 ◽

pp. 37-43

Author(s):

T. Shanks ◽

R. Fong ◽

B.J. Boyle ◽

B.A. Peterson

Keyword(s):

Correlation Function ◽

Luminosity Function ◽

Ultraviolet Excess ◽

Fibre Optic ◽

Complete Sample ◽

Point Correlation ◽

Point Correlation Function ◽

Redshift Survey ◽

The Universe ◽

Optic Coupler

We have used the FOCAP fibre optic coupler at the Anglo-Australian Telescope (AAT) to measure redshifts for a complete sample of ∼ 170 B ≤ 21m QSO's selected using the ultraviolet excess (UVX) criterion. We present preliminary estimates of the QSO luminosity function in discrete redshift ranges and show how these observations differentiate between models of QSO evolution. We have also investigated the clustering of QSOs in this complete sample by estimating the QSO 2-point correlation function and we use this to derive direct constraints on the homogeneity of the Universe at large scales.

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