Dark matter in the universe : Varenna on Lake Como, Villa Monastero, 25 July-4 August 1995 / edited by S. Bonometto, J.R. Primack, and A. Provenzale.

Includes bibliographical references.

Print version record.

Title Page; Indice; Introductory note; Gruppo fotografico dei partecipanti al Corso fuori testo; Status of cosmological parameters: Omega_0 approx 0.3 vs. Omega = 1; Introduction; Models with mostly cold dark matter; Age of the Universe t_0; Hubble parameter H_0; A) Relative-distance methods; B) Fundamental-physical approaches; Correcting for Virgocentric infall; Cosmological constant Lambda, and t_0 again; Measuring Omega_0; Very-large-scale measurements; Large-scale measurements; Measurements on scales of a few Mpc; Estimates on galaxy halo scales; Clusters.

Cluster baryons vs. big-bang nucleosynthesisCluster morphology; Cluster evolution; Early structure formation; Neutrino mass; Conclusions; OBSERVATIONAL DATA; Galaxy redshift surveys; Introduction; Redshift surveys; The Las Campanas Redshift Survey; The beginning of the end?; Beyond the LCRS; Peculiar motions and the Tully-Fisher relation; Introduction; Newtonian theory of small perturbations; The case for large-scale motions; The CMB dipole; Motions at the Local Supercluster scale; The Great Attractor; Bulk flows; The Tully-Fisher relation; Scaling laws; Extinction and the TF relation.

Optical and radio velocity widthsThe scatter in the TF relation; Importance of the TF template relation; Results for a cluster sample; An all-sky field spiral sample; Galaxy redshift surveys: caveat emptor; Introduction; Catalogs: tricks and pitfalls; Nearby-galaxy catalogs; Optical catalog; IRAS galaxy surveys; The density field based on redshift catalogs; Morphological and luminosity segregation; The Pisces-Perseus Supercluster; Not a random volume; Measures of clustering; Morphological segregation; Substructure in clusters: Abell 2634; Hidden galaxies; Conclusion.

CMBR observations: spectrumIntroduction; Spectrum observations prior to COBE; COBE mission; DIRBE measurements; FIRAS measurements; Comparison of FIRAS with other data; Possible distortions; Summary; CMBR observations: anisotropy; Introduction; History; The COBE DMR; DMR data analysis. Sparse matrix; Correlated noise in the DMR maps; Scaling to large maps; DMR results; Galactic interference; Power spectrum; Comparison to large-scale structure; Future CMB work; Galaxy number counts; Introduction; Modelling the number counts; Luminosity evolution models.

The redshift distributions of faint field galaxiesCould we fit the counts in a q_0 = 0.5 Universe model?; Conclusion; Cosmological adventures in the Lyman forest; Introduction; A Lyman-alpha database; The b-N_(HI) distributions: the temperature of the Lyman-alpha clouds; The HI column density distribution; The redshift distribution; The measure of the ultraviolet background from the proximity effect; Clustering properties of the Lyman-alpha clouds; Simulations; ADVANCED STATISTICAL ESTIMATORS; Cosmic velocity fields; Introduction; Gravitational instability; Measuring peculiar velocities.

Physics and astrophysics came to dark matter through many different routes, finally accepting it, but often with some distaste. It has been noticed that the existence of dark matter is yet another displacement of humans from the centre of the Universe: not only do our planet and our sun have no central position in the Universe, not only are humans just animals (although with a 'specialized' central nervous system), but even the material of which we are made is only a marginal component of the cosmic substance! If this is the right attitude to take, scientists feeling distaste for dark matter a.

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