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We investigate the use of spiral arm pitch angles as a probe of disk galaxymass profiles. We confirm our previous result that spiral arm pitch angles (P)are well correlated with the rate of shear (S) in disk galaxy rotation curves.We use this correlation to argue that imaging data alone can provide a powerfulprobe of galactic mass distributions out to large look-back times. We then usea sample of 13 galaxies, with Spitzer 3.6-$\mu$m imaging data and observedH$\alpha$ rotation curves, to demonstrate how an inferred shear rate coupledwith a bulge-disk decomposition model and a Tully-Fisher-derived velocitynormalization can be used to place constraints on a galaxy's baryon fractionand dark matter halo profile. Finally we show that there appears to be a trend(albeit a weak correlation) between spiral arm pitch angle and haloconcentration. We discuss implications for the suggested link betweensupermassive black hole (SMBH) mass and dark halo concentration, using pitchangle as a proxy for SMBH mass.

astrophysical journal/the astrophysical journal

Constraining dark matter halo profiles and galaxy formation models using  spiral arm morphology. II. Dark and stellar mass concentrations for 13 nearby  face-on galaxies