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The Kinematics in the Cores of Low Surface Brightness Galaxies

Published online by Cambridge University Press:  26 May 2016

R. A. Swaters ,
M. A. W. Verheijen ,
M. A. Bershady  and
D. R. Andersen
R. A. Swaters
Affiliation:
Johns Hopkins University, 3400 N. Charles St., Baltimore MD 21218, U.S.A.; and Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, U.S.A.
M. A. W. Verheijen
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
M. A. Bershady
Affiliation:
Astronomy Department, University of Wisconsin - Madison, 475 N. Charter St., Madison, WI 53706, U.S.A.
D. R. Andersen
Affiliation:
Max Planck Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany

Abstract

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Systematic effects on HI and Hα long-slit observations make a measurement of the inner slope of the dark matter density distribution difficult to determine. Halos with constant density cores and ones with r–1 profiles both appear consistent with the data, although constant density cores generally provide better fits. High-resolution, two-dimensional velocity fields remove most of the systematic effects, yet as a result of noncircular and random motions the inner slopes still cannot be accurately measured. Halo concentration parameters provide a more useful test of cosmological models because they are more tightly constrained by observations. the concentration parameters for LSB galaxies appear consistent with, but on the low end of the distribution predicted by CDM.

Type
Part 3: Central Density Cusps, Thin Disks, and Dark Halo Substructure
Information
Symposium - International Astronomical Union , Volume 220: Dark Matter in Galaxies , 2004 , pp. 77 - 84
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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