Download Environment and the Formation of Galaxies: 30 years later: by A. Dressler (auth.), Ignacio Ferreras, Anna Pasquali (eds.) PDF

By A. Dressler (auth.), Ignacio Ferreras, Anna Pasquali (eds.)

The ebook of the morphology - density relation by means of Alan Dressler in 1980 introduced into the limelight the function performed via setting within the formation and evolution of galaxies. The symposium Environment and the Formation of Galaxies: 30 years later, used to be organised with the aim of creating the environmental effect at the evolution of galaxies and its dependence on look-back time. specific emphasis used to be put on the actual mechanisms which are answerable for reworking galaxies when they are accreted via a bunch or a cluster, together with the observable imprint left within the galaxy hello distribution.

Other significant subject matters of the symposium have been the environmental dependence of galaxy homes at z ≥ 1 and the implementation of environmental results in cosmological versions of galaxy formation and evolution.

This e-book offers the edited court cases of this stimulating meeting.

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Read or Download Environment and the Formation of Galaxies: 30 years later: Proceedings of Symposium 2 of JENAM 2010 PDF

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Weinmann et al. Fig. 2 The mean stellar mass-weighted age (left hand panel) and metallicity (right hand panel) for central galaxies (large filled circles) and for satellite galaxies (lines with errorbars) for different stellar mass bins A–E, as indicated. Results for satellites are shown as a function of halo mass. It can be seen that low mass centrals have lower metallicities than satellites, and that the metallicity for low mass satellites increases with increasing host halo mass. More details are given in [33] highly concentrated galaxies (which typically have elliptical morphologies) are not produced by environmental effects.

Blaizot, MNRAS 375, 2 (2007) 3. F. , MNRAS 376, 1425 (2007) 4. A. , A&A 509, A40C (2010) 5. C. , ApJ 697, 1842 (2009) 6. O. , A&A 439, 845 (2005) 7. C. , ApJ 580, 122 (2002) 8. V. 9C0851 P. W. Zeilinger Abstract Numerical simulations as well as optical and X-ray observations have shown that poor groups of galaxies can evolve to what is called a fossil group. Dynamical friction as the driving process leads to the coalescence of individual galaxies in ordinary poor groups, leaving behind nothing more than a central, massive elliptical galaxy supposed to contain the merger history of the whole group.

About 100 dwarfs fall in this void. The goal of the ongoing project is to obtain the evolutionary parameters of the void sample galaxies. Here we present the intermediate results of O/H determination, based mainly on the SAO 6-m telescope observations. A. O. za S. Pustilnik A. Tepliakova A. ru I. Ferreras and A. 1007/978-3-642-20285-8 4, © Springer-Verlag Berlin Heidelberg 2011 25 26 A. Kniazev et al. Fig. 1 Metallicity-Luminosity relation for 38 Lynx-Cancer void galaxies. Solid, short-dashed and dotted lines show respectively the known L–Z relations for isolated late-type galaxies [6], nearby dIs [7] and nearby dI and I galaxies from [3].

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