2015MNRAS.451..878K

We present a systematic analysis of the rotation curves of 187 galaxies with stellar masses greater than 10¹⁰M_☉, with atomic gas masses from the GALEX Arecibo Sloan Survey (GASS) and with follow-up long-slit spectroscopy from the MMT. Our analysis focuses on stellar rotation curves derived by fitting stellar template spectra to the galaxy spectra binned along the slit. In this way, we are able to obtain accurate rotation velocity measurements for a factor of 2 more galaxies than possible with the Hα line. Galaxies with high atomic gas mass fractions are the most dark-matter-dominated galaxies in our sample and have dark matter halo density profiles that are to first order well described by Navarro-Frenk-White profiles with an average concentration parameter of 10. The inner slopes of the rotation curves correlate more strongly with stellar population age than with galaxy mass or structural parameters. At fixed stellar mass, the rotation curves of more actively star-forming galaxies have steeper inner slopes than less actively star-forming galaxies. The ratio between the galaxy specific angular momentum and the total specific angular momentum of its dark matter halo, Rj, correlates strongly with galaxy mass, structure and gas content. Low-mass, disc-dominated galaxies with atomic gas mass fractions greater than 20 per cent have median values of Rj of around 1, but massive, bulge-dominated galaxies have Rj = 0.2-0.3. We argue that these trends can be understood in a picture where gas inflows triggered by disc instabilities lead to the formation of passive, bulge-dominated galaxies with low specific angular momentum.