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NGC 3992 – A Galaxy without a Massive Halo

Published online by Cambridge University Press:  04 August 2017

S. T. Gottesman ,
J. H. Hunter Jr.  and
J. R. Ball
S. T. Gottesman
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida, U. S. A.
J. H. Hunter Jr.
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida, U. S. A.
J. R. Ball
Affiliation:
Department of Astronomy, University of Florida, Gainesville, Florida, U. S. A.

Extract

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As a continuation of our earlier work (Gottesman and Hunter, 1982), we have reobserved the HI emission from the galaxy NGC 3992. We have combined all the data and produced new maps, at a significantly improved signal-to-noise ratio, of the gas density and velocity distribution with resolutions of ~ 22″ and 25 km s−1. The resultant, angle averaged, HI rotational velocity is shown in Figure 1 for the symmetric and nearly circular flows for r ≤ 3.35′ from the center (r ≤ 14.0 kpc, assuming de Vaucouleurs' (1979) distance of 14.2 mpc for NGC 3992). Shown, also, in Figure 1 is a fit to the observations provided by a Toomre disk of index n = o. No attempt was made to fit the observational data within 1′, in view of the low signal to noise.

Type
I. Kinematics of Gas and the Underlying Mass Distribution
Information
Symposium - International Astronomical Union , Volume 100: Internal Kinematics and Dynamics of Galaxies , 1983 , pp. 93 - 94
Copyright
Copyright © Reidel 1983 

References

Bahcall, J. N. and Tremaine, S. 1981, Astrophys. J., 244, 805.CrossRefGoogle Scholar
de Vaucouleurs, G. 1979, Astrophys. J., 227, 729.Google Scholar
Gottesman, S. T. and Hunter, J. H. 1982, Astrophys. J., 260, 65.CrossRefGoogle Scholar
Toomre, A. 1963, Astrophys. J., 138, 385.Google Scholar