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Delayed Galaxies

Published online by Cambridge University Press:  01 June 2007

Curtis Struck ,
Mark Hancock ,
Beverly J. Smith ,
Phillip N. Appleton ,
Vassilis Charmandaris  and
Mark Giroux
Curtis Struck
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames IA 50011, email: curt@iastate.edu
Mark Hancock
Affiliation:
Department of Physics, Astronomy, and Geology, East Tennessee State University, Johnson City TN 37614
Beverly J. Smith
Affiliation:
Department of Physics, Astronomy, and Geology, East Tennessee State University, Johnson City TN 37614
Phillip N. Appleton
Affiliation:
Spitzer Science Center, California Institute of Technology, Pasadena CA 91125
Vassilis Charmandaris
Affiliation:
Department of Physics, University of Crete, Heraklion Greece 71003
Mark Giroux
Affiliation:
Department of Physics, Astronomy, and Geology, East Tennessee State University, Johnson City TN 37614
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Abstract

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We can define Delayed Galaxies as a class of rare galaxies that maintained the bulk of their gas for most of the age of the universe following the initial formation of their disks, with little or no star formation. Invisible galaxies and Malin 1 type low-surface-brightness galaxies qualify as class members. Rare examples among interacting galaxies show that collisions can restart the stalled evolution of such galaxies, and suggest that other members of the Delayed class can be found among interacting systems with vigorous current star formation.

Keywords

galaxies: interactinggalaxies: evolutiongalaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S244: Dark Galaxies and Lost Baryons , June 2007 , pp. 231 - 234
Copyright
Copyright © International Astronomical Union 2008

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