ar X iv : a st ro - p h / 01 08 43 1 v 2 1 5 N ov 2 00 1 Did the Universe Reionize at Redshift Six ?

ar X iv : a st ro - p h / 03 08 07 9 v 1 5 A ug 2 00 3 THE 2 MS CHANDRA DEEP FIELD - NORTH

The 2 Ms Chandra Deep Field-North survey provides the deepest view of the Universe in the 0.5–8.0 keV X-ray band. In this brief review we investigate the diversity of X-ray selected sources and focus on the constraints placed on AGNs (including binary AGNs) in high-redshift submm galaxies.

ar X iv : a st ro - p h / 03 11 08 9 v 1 4 N ov 2 00 3 Hot Gas in the Local Group and Low - Redshift Intergalactic Medium

There is increasing observational evidence that hot, highly ionized interstellar and intergalactic gas plays a significant role in the evolution of galaxies in the local universe. The primary spectral diagnostics of the warm-hot interstellar/intergalactic medium are ultraviolet and X-ray absorption lines of Ovi and Ovii. In this paper, I summarize some of the recent highlights of spectroscopic ...

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 / 06 11 43 8 v 1 1 4 N ov 2 00 6 Lack of cooling flow clusters at z > 0 . 5

The goal of this work is to study the incidence rate of “cooling flows” in the high redshift clusters using Chandra observations of z > 0.5 objects from a new large, X-ray selected catalog [1]. We find that only a very small fraction of high-z objects have cuspy X-ray brightness profiles, which is a characteristic feature of the cooling flow clusters at z ∼ 0. The observed lack of cooling flows...

ar X iv : a st ro - p h / 98 11 01 5 v 1 2 N ov 1 99 8 The large – scale distribution of galaxies in the Shapley Concentration

We present the results of a galaxy redshift survey in the central region of the Shapley Concentration. Our total sample contains ∼ 2000 radial velocities of galaxies both in the clusters and in the inter-cluster field. We reconstruct the density profile of this supercluster, calculate its overdensity and total mass. Moreover we detect a massive structure behind the Shapley Concentration, at ∼ 3...