Confrontation of MOdified Newtonian Dynamics with the rotation curves of early-type disc galaxies

We extend the MOdified Newtonian Dynamics (MOND) analysis to a sample of 17 high surface brightness, early-type disc galaxies with rotation curves derived from a combination of 21-cm H i line observations and optical spectroscopic data. A number of these galaxies have asymptotic rotation velocities between 250 and 350 km s−1 making them among the most massive systems (in terms of baryonic mass) considered in the context of MOND. We find that the general MOND prediction for such galaxies – a rotation curve which gradually declines to the asymptotic value – is confirmed, and in most cases the MOND rotation curve, determined from the mean radial light and gas distribution, agrees in detail with the observed rotation curve. In the few cases where MOND appears not to work well, the discrepancies can generally be understood in terms of various observational errors – such as incorrect orientation angles and/or distances – or of unmodelled physical effects – such as non-circular motions. The implied mass-to-light ratios for the stellar disc and bulge constrain the MOND interpolating function; the form recently suggested by Zhao & Famaey yields more sensible values than the one traditionally used in MOND determinations of galaxy rotation curves.