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Structure of merger remnants. I - Bulgeless progenitorsThe study examines mergers of identical galaxies consisting of self-gravitating disks and halos in the context of the suggestion that such events may form elliptical galaxies. It is shown that the luminous remnants of such mergers do indeed share many common properties with observed ellipticals. Specifically, the end states of the simulations considered rotate slowly in regions of relatively high surface density, having typical values of less than about 0.2 there. Morphologically, the remnants display a variety of structures, including shells and loops comprising loosely bound material and boxy and disky isophotes. The luminous matter is well-fitted by ellipsoidal generalizations of Hernquists's (1990, 1992) model for elliptical galaxies, implying that the surface brightness profiles are essentially de Vaucouleurs-like over a large radial interval. It is proposed that mergers of pure stellar disks do not represent an attractive mechanism for the production of massive elliptical galaxies.
Document ID
19930032434
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hernquist, Lars
(California Univ. Santa Cruz, United States)
Date Acquired
August 15, 2013
Publication Date
December 1, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 400
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A16431
Funding Number(s)
CONTRACT_GRANT: NAGW-2422
CONTRACT_GRANT: NSF AST-90-18526
Distribution Limits
Public
Copyright
Other

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