Bars and Dark Matter Halo Cores

Abstract

Self-consistent bars that form in galaxies embedded within cuspy halos are unable to flatten the cusp. Short bars form in models with quasi-flat rotation curves. They lose angular momentum to the halo through dynamical friction, but the continuous concentration of mass within the disk as the bar grows actually compresses the halo further, overwhelming any density reduction due to the modest angular momentum transfer to the halo. Thus the Weinberg-Katz proposed solution to the non-existence of the predicted cuspy halos from CDM simulations would seem to be unworkable. I also find that the concerns over the performance of N-body codes raised by these authors do not apply to the methods used here.

Latex 11 pages (uses emulateapj.sty), 8 figures, revised version to appear ApJ, very minor changes

References in corpus (2)

• Measurement of fast bars in a sample of early-type barred galaxies
• Dark matter within high surface brightness spiral galaxies

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