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

ISBN-10: 3642202845

ISBN-13: 9783642202841

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

Other significant themes 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 provides the edited complaints of this stimulating meeting.

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Extra info for Environment and the Formation of Galaxies: 30 years later: Proceedings of Symposium 2 of JENAM 2010

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The first fully analyzed sample of 15 void galaxies demonstrated the success of our strategy [17]. With 14 detections out of 15, the HI detection rate is very high. We discovered one previously known and five previously unknown companions, while two appear to be interacting. Of these five befriended void galaxies, two are interacting in HI. All HI-detected companions have optical counterparts within the SDSS. Of the nine isolated void galaxies, many exhibit irregularities in the kinematics of their gas disks.

Lines indicate increments of 8 km s 1 . Right: position-velocity diagram along the kinematic major axis (from [17]) rotation curve. Mdyn is typically 109 –1010 Mˇ . The detected companions are more dwarfish. The void galaxy population appears to represent the extreme blue and faint tail of an otherwise normal galaxy population. There are a few characteristics which seem to set them apart, mainly concerning their HI gas content and star formation activity. 1 Magnitudes and Colors Despite their affected outer regions, our study finds that in the color-magnitude diagram the target void galaxies nicely reside at the faint end of the blue cloud of galaxies.

Very dark-grey diamonds: VGS void galaxies from the full sample. Dark-grey diamonds: control sample galaxies (from [17]) 3 Results of the VGS Survey: Current State of Affairs The first results of the Void Galaxy Survey are tantalizing and has revealed a few surprising gas configurations. With a HI mass limit of 2 107 Mˇ and column density limit of 1019 cm 2 , our HI survey provides a significantly improved view of HI in void galaxies compared to past studies [30]. Figure 2 shows one of the most surprising specimen in our survey, the polar ring void galaxy VGS12 (see Sect.

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Environment and the Formation of Galaxies: 30 years later: Proceedings of Symposium 2 of JENAM 2010 by A. Dressler (auth.), Ignacio Ferreras, Anna Pasquali (eds.)

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