Large-Scale Structure from the ESP & REFLEX Surveys
(and a glimpse to the future: the VIRMOS survey)
21 October 1999
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Table of Contents
Large-Scale Structure from the ESP & REFLEX Surveys (and a glimpse to the future: the VIRMOS survey)
Outline
Location of ESP, REFLEX and other major redshift surveys
The ESO Slice Project (ESP)
ESP: technique
ESP: strategy and results
ESP: results
ESP: luminosity function
ESP LF: faint-end population
ESP LF: comparison to other surveys
ESP: galaxy mean density
ESP local void: consequence for number counts
ESP local void: consistency with all-sky redshift surveys
ESP: two-point correlation properties
ESP x(s): comparison to other surveys
ESP: power spectrum
ESP P(k): consistency with x(s)
ESP P(k): comparison to other surveys
Using clusters to map very large scales: the REFLEX survey
The REFLEX cluster survey
REFLEX: Lx vs redshift
REFLEX: spatial distribution
REFLEX: cluster-cluster correlation function
REFLEX: clustering of clusters vs. galaxies
REFLEX: dependence of correlation length ro on Lx and on mean separation
REFLEX: Power Spectrum
REFLEX P(k): comparison with Abell and APM cluster samples
REFLEX P(k): increasing the Fourier volume. More power at small k's ?
REFLEX P(k): pushing the sample to the extreme: 1000 h-1 side box
REFLEX P(k): comparison to (linear) models
The Future: the VIRMOS Project (quick overview)
VIMOS/NIRMOS layout
VIMOS: MOS capabilities
VIRMOS project status
Author:
Luigi Guzzo
Email:
guzzo@merate.mi.astro.it