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The velocity dispersion in the disk of the S0 galaxy NGC 1553
Kormendy, J.
AA(Dominion Astrophysical Observatory, Victoria, British Columbia, Canada; Observatorio Interamericano de Cerro Tololo, La Serena, Chile; Kitt Peak National Observatory, Tucson, AZ)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 286, Nov. 1, 1984, p. 116-131. (ApJ Homepage)
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NASA/STI Keywords:
Angular Velocity, Galactic Rotation, Radii, Spiral Galaxies, Stellar Rotation, Velocity Distribution, Astronomical Photometry, Axes Of Rotation, Disk Galaxies, Galactic Structure
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Stellar rotation velocities and velocity dispersions have been measured along the major, minor, and mean axes of the normal SA(lens)0 galaxy NGC 1553. These are used to study the kinematics and dynamics of the disk as a function of radius. The lens is very hot. A significant fraction of the orbits in the inner part of the lens may be retrograde. The large excursions of stars dilute any radial gradients in disk properties, and phase-mix away any small-scale structure. The velocity dispersion appears to be large enough for stability against spiral and other structure in the absence of gas. If NGC 1553 is representative, S0 galaxies may lack spiral structure partly because they are too hot.

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