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Shells and Dark Matter in Elliptical Galaxies

Published online by Cambridge University Press:  04 August 2017

Lars Hernquist  and
P.J. Quinn
Lars Hernquist
Affiliation:
Department of Astronomy, U.C. Berkeley
P.J. Quinn
Affiliation:
The Space Telescope Science Institute

Abstract

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A new method for probing the distribution of matter in elliptical galaxies surrounded by shell systems is described. As an illustration we have applied this technique to the giant elliptical galaxy NGC 3923. If the potential is modeled as the sum of an r1/4 law and a non–singular isothermal halo, then the best fit to the shell number and shell distribution gives a halo mass (within the shell system ~ 100h−1 kpc) ~ 40 times the mass of the elliptical and a halo core radius ~ 3 times the effective radius of the luminous material.

Type
Posters
Information
Symposium - International Astronomical Union , Volume 127: Structure and Dynamics of Elliptical Galaxies , 1987 , pp. 467 - 468
Copyright
Copyright © Reidel 1987 

References

REFERENCES

Bahcall, J.N. and Casertano, S. 1985. Astrophy. J. (Letters), 293, L7.Google Scholar
Quinn, P.J. 1984. Astroph. J., 279, 596.CrossRefGoogle Scholar
Forman, W., Jones, C., and Tucker, W. 1985. Astroph. J., 293, 102.Google Scholar
Hernquist, L. and Quinn, P.J. 1986a. Astrophy. J., submitted.Google Scholar
Hernquist, L. and Quinn, P.J. 1986b. Astrophy. J., in press.Google Scholar