Titlebook: Looking Deep in the Southern Sky; Proceedings of the E Raffaella Morganti,Warrick J. Couch Conference proceedings 1999 Springer-Verlag Berl

的事物

GUILE

Obloquy

Neuralgia

CRUE

ESO Imaging Survey made to address this problem by carrying out a public imaging survey to produce targets for the first year of operation of the VLT. Here the goals, strategy and preliminary results of this effort are presented. Current plans to greatly expand the imaging facilities of ESO in the short and long-term

CAJ

Cosmological Tests from the New Surveys (i) the importance of understanding selection effects in catalogues and matching Northern and Southern surveys; (ii) the 2dF galaxy redshift survey of 250,000 galaxies (iii) the proposed 6dF redshift and peculiar velocity survey of near-infrared galaxies (iv) radio sources and the X-Ray Background

NAVEN

Mapping the Dark Matter with Weak Gravitational Lensing dark matter distribution in the Universe. Concentrating on those aspects which require deep wide-field imaging surveys, I will describe the basic principles of weak lensing and discuss its future application (a) to determine the statistical properties of the dark matter halos of individual galaxies

无孔

Weak Lensing with MEGACAM and the VLTts will be dedicated to surveys. In this proceeding, we show how we can use MEGACAM+VIRMOS to map the mass distribution on large scales. Simulated projected mass density maps show that mass reconstruction from lensing inversion can recover the input power spectrum using MEGACAM images. The mass reco

有机体

Gravitational Lensing in the 2dF Galaxy Redshift Survey Boyle 1997). As such it will provide a great deal of information about the galaxy population (.., luminosity function, clustering properties) in the local (∹..∹ ≃ 0.1) universe. However, the spectral information obtained will not provide any direct information about the mass of the survey galaxies.

impaction

A Weak Gravitational Lensing Cluster Surveyhe mass of the clusters is determined via weak gravitational lensing, and correlated with the X-ray and optical properties. This direct probe of the cluster mass distribution will constrain the dynamical and thermodynamical state and evolution of the cluster population.