By G. Efstathiou (auth.), Professor Dr. Roland Wielen (eds.)
Progress in the direction of an knowing of the dynamics and interactions of galaxies has been spurred on greater than ever by means of a wealth of recent observations and numerical experiments. The Heidelberg convention 1989, the papers of that are amassed during this quantity, used to be tremendous profitable in offering a synoptic view of the sphere in all its facets: galaxy interactions within the early universe and in recent years, interactions of our galaxy and its neighbours, dynamical difficulties of elliptical and disk galaxies, teams and clusters, starburst and nuclear task caused through interactions, merger situations, and numerical experiments. Researchers and graduate scholars, experts or no longer, will locate the following a whole review of a quickly starting to be box of astronomy.
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Extra resources for Dynamics and Interactions of Galaxies: Proceedings of the International Conference, Heidelberg, 29 May – 2 June 1989
1988). 2. The rest of the figure is occupied by stars of the slowly rotating halo, which show no trend of mean rotational velocity with [Fe/H). 5. However, constructing a mean Vrot - abundance relation in this way would ignore the obvious presence of the separate disk and halo components and their overlap in abundance. Here is a brief summary of the properties of the metal weak halo ([Fe/HJ ;S -1): see Freeman (1987) for further references. 2 percent of the disk density. Its radial density distribution falls off as r- 3 .
17 is a galaxy with properties similar to those of other distant radio galaxies and the most distant galaxy known. The line-emitting gas is elongated along the radio source and a Lyman alpha halo extends by more than 100 kpc, considerably beyond the radio source. The gas is clumpy and has a turbulent velocity field , with a gradient of -2000 km/s and a half-width of -1200 km/s. The inner gas kinematics may be influenced by entrainment in the radio source. Mass estimates range from 10 9 to 10 11 Mo for the ionized gas and an upper limit of 10 12 Mo can be set on the total mass of the galaxy from the gas kinematics.
Astron. , in press. J. McCarthy The Observatories of the Carnegie Institution of Washington 1. Introduction The recent identification of large samples of faint radio sources has resulted in the discovery of a number of high luminosity galaxies at redshifts larger than 1. These objects are highly unusual in their morphological and kinematic properties. Given that there is a fairly well established connection between interactions, and possibly mergers, and nuclear activity in nearby radio sources, it seems plausible that tne high redshift radio galaxies are systems in which substantial interaction is occurring.