ar X iv : a st ro - p h / 01 07 53 7 v 2 6 S ep 2 00 2 POWER SPECTRA FOR GALAXY SHAPE CORRELATIONS

ar X iv : a st ro - p h / 01 07 53 7 v 1 2 7 Ju l 2 00 1 POWER SPECTRA FOR GALAXY SHAPE CORRELATIONS

It has recently been argued that the observed ellipticities of galaxies may be determined at least in part by the primordial tidal gravitational field in which the galaxy formed. Long-range correlations in the tidal field could thus lead to an ellipticity-ellipticity correlation for widely separated galaxies. I present results of a calculation of the angular power spectrum of intrinsic galaxy s...

ar X iv : a st ro - p h / 01 05 53 8 v 1 3 0 M ay 2 00 1 Circumnuclear stellar population , morphology and environment of Seyfert 2 galaxies : an evolutionary scenario

We investigate the relation between the characteristics of the circumnuclear stellar population and both the galaxy morphology and the presence of close companions for a sample of 35 Seyfert 2 nuclei. Fifteen galaxies present unambiguous signatures of recent episodes of star formation within ≈300 pc from the Jansky Fellow Gemini Fellow

ar X iv : a st ro - p h / 01 11 13 6 v 1 7 N ov 2 00 1 1 Active Optics in Modern , Large Optical Telescopes

ar X iv : a st ro - p h / 00 01 29 6 v 1 1 7 Ja n 20 00 H 2 emission as a diagnostic of physical processes in starforming galaxies By Paul

Observations and interpretation of extragalactic rotational and rovibrational H2 emission are reviewed. Direct observations of H2 lines do not trace bulk H2 mass, but excitation rate. As such, the H2 lines are unique diagnostics, if the excitation mechanism can be determined, which generally requires high-quality spectroscopy and suitable additional data. The diagnostic power of the H2 lines is...

ar X iv : a st ro - p h / 01 09 04 0 v 1 4 S ep 2 00 1 Clusters of Galaxies - Keys to Cosmology

Various cosmological applications of galaxy clusters are presented. Clusters are used to determine the baryon fraction, dark matter distribution and the matter density Ωm of the universe. They also contain a wealth of information about structure formation and evolution on different scales: large-scale structure, cluster formation and also galaxy formation via the interaction of cluster galaxies...