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Elliptical Galaxies
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Dwarf Galaxies
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The Evolution of Galaxies
Galaxies have a history: distant galaxies, formed early in the life of the universe, differ from the nearby ones. This book addresses the modeling of galaxy evolution from their cosmological formation to their presently observable structures, presenting the state of the art in the field.
The Resolved Stellar Populations of M 32
We present the deepest optical CMD to date of M 32, obtained from HST ACS/HRC images. The dominant feature is the RC, whose CMD location suggests a mean age between 8 and 10 Gyr for [Fe/H] = -0.2 in M 32. We detect for the first time the RGB and AGB bumps in M 32 which constrain its mean age to be 5-10 Gyr old at 2' from the center. Bright AGB stars indicate the presence of intermediate-age populations. A detected blue component of stars may indicate for the first time the presence of a young stellar population of ~0.5 Gyr in our M 32 field. However, it is likely that the younger stars of this blue plume belong to M 31 rather than to M 32. The fainter stars populating the blue plume indicate the presence of stars not younger than 1 Gyr and/or blue straggler stars in M 32.
Structure and Dynamics of Elliptical Galaxies
IAU Symposium 127 was held in Princeton on May 28-31, 1986, at the Institute for Advanced Study. There were 150 participants from 19 countries. This was the first IAU Symposium devoted exclusively to elliptical galaxies. The last decade has been a period of exceptionally rapid progress regard ing our understanding of elliptical galaxies, driven on the observational side by a wealth of new photometric and spectroscopic data, and on the theoretical side by the recognition that ellipticals are slowly rotating triaxial systems, instead of rotationally flattened bodies. The 30 invited speakers reviewed all aspects of this progress, its consequences, and the major outstanding problems. Nearly 80 p...
Galactic Bulges
This book consists of invited reviews on Galactic Bulges written by experts in the field. A central point of the book is that, while in the standard picture of galaxy formation a significant amount of the baryonic mass is expected to reside in classical bulges, the question what is the fraction of galaxies with no classical bulges in the local Universe has remained open. The most spectacular example of a galaxy with no significant classical bulge is the Milky Way. The reviews of this book attempt to clarify the role of the various types of bulges during the mass build-up of galaxies, based on morphology, kinematics and stellar populations and connecting their properties at low and high redshifts. The observed properties are compared with the predictions of the theoretical models, accounting for the many physical processes leading to the central mass concentration and their destruction in galaxies. This book serves as an entry point for PhD students and non-specialists and as a reference work for researchers in the field.
3D-Spectroscopy of Dense Stellar Populations
Globular clusters are gravitationally bound collections of hundreds of thousands of stars that are almost as old as the Universe itself. Although they have been studied for hundreds of years, their formation and evolution is not yet fully understood. We want to fi nd answers to some of the major questions by investing a large amount of observing time with MUSE, the upcoming 2nd generation instrument for ESOś Very Large Telescope. In this thesis I discuss the current state of research on globular clusters as well as the possibilities of this new instrument. Numerical methods for the analysis of MUSE data are presented, including a comprehensive library of synthetic spectra that has been created just for this purpose. The application of these methods to both synthetic and real data is discussed with particular emphasis on a "dry run" that has been conducted for MUSE. Finally, a potential program for the observation of globular clusters is presented.
