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Formation and evolution of galactic spheroids by mergers

Published online by Cambridge University Press:  01 July 2007

Thorsten Naab ,
Andreas Burkert ,
Peter H. Johansson  and
Roland Jesseit
Thorsten Naab*
Affiliation:
University Observatory Munich, Scheinerstr. 1, 81679 Munich, Germany email: naab@usm.lmu
Andreas Burkert
Affiliation:
University Observatory Munich, Scheinerstr. 1, 81679 Munich, Germany email: naab@usm.lmu
Peter H. Johansson
Affiliation:
University Observatory Munich, Scheinerstr. 1, 81679 Munich, Germany email: naab@usm.lmu
Roland Jesseit
Affiliation:
University Observatory Munich, Scheinerstr. 1, 81679 Munich, Germany email: naab@usm.lmu
*
†email: naab@usm.lmu.de
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Abstract

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Galactic spheroids can form as a result of galaxy interactions and mergers of disks. Detailed analyses of the photometric properties, the intrinsic orbital structure, the line-of-sight velocity distributions and the kinemetry of simulated merger remnants, which depend critically on the geometry and the gas content of the interacting progenitors, indicate that low and intermediate mass rotating ellipticals can form from mergers of disks. The masses and metallicities of all massive ellipticals and the kinematics of some massive non-rotating ellipticals cannot be explained by binary mergers. Thus these galaxies might have formed in a different way.

Keywords

galaxies: elliptical and lenticularcDgalaxies: evolutionmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 47 - 50
Copyright
Copyright © International Astronomical Union 2008

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