ar X iv : a st ro - p h / 99 12 14 8 v 1 8 D ec 1 99 9 Galaxy population properties in the rich clusters MS 0839 . 8 + 2938

ar X iv : a st ro - p h / 95 12 02 8 v 1 6 D ec 1 99 5 A search for distant X - ray galaxy clusters

We report on the progress of our search for serendipitous distant X-ray galaxy clusters in the ROSAT PSPC pointed observations archive. The initial aim of our work is to measure the X-ray luminosity function of clusters down to f lim = 4×10 −14 erg cm −2 s −1 and so test the claims of cluster evolution at moderate redshifts. We have R band images and spectroscopy for 45 extended sources detecte...

ar X iv : a st ro - p h / 99 12 26 8 v 1 1 4 D ec 1 99 9 The Gas Reservoir for present day Galaxies : Damped Ly α Absorption Systems

We present results from an ongoing search for galaxy counterparts of a subgroup of Quasar Absorption Line Systems called Damped Lyα Absorbers (DLAs). DLAs have several characteristics that make them essential in the process of understanding how galaxies formed in the early universe and evolved to the galaxies we see today in the local universe. Finally we compare DLAs with recent findings of a ...

ar X iv : a st ro - p h / 99 11 43 8 v 1 2 3 N ov 1 99 9 H 2 molecules and cold clouds in cooling flow clusters †

ar X iv : a st ro - p h / 98 12 16 7 v 1 9 D ec 1 99 8 LYMAN BREAK GALAXIES AT z ∼ 3 AND BEYOND

We report on the status of large surveys of photometrically selected star forming galaxies at z ∼ 3 and z ∼ 4, with particular emphasis on both the advantages and the limitations of selecting objects using the “Lyman break” technique. Current results on the luminosity functions, luminosity densities, color distribution, star formation rates, clustering properties, and the differential evolution...

ar X iv : a st ro - p h / 98 12 32 8 v 1 1 7 D ec 1 99 8 MOND in the Early Universe

I explore some consequences of Milgrom’s modified dynamics for cosmology. There appear to be two promising tests for distinguishing MOND from CDM: (1) the rate of growth of structure and (2) the baryon fraction. These should be testable with observations of clusters at high redshift and the microwave background, respectively.