MODIFIED DYNAMICS (MOND) AS A DARK HALO

We propose a form for dark haloes that embodies the fundamental aspect of Milgrom's modified dynamics (MOND): the discrepancy between the vi sible mass and the Newtonian dynamical mass appears below a critical a cceleration. This is a halo having a density distribution, at least to several tens of kpc, of the form Sigma(0)/r, where Sigma(0), is a con stant of surface density which does not vary from galaxy to galaxy. To avoid rising rotation curves, such a density distribution must obviou sly steepen beyond some radius, and we have chosen the Hernquist model in which the density falls as 1/r(4) beyond a characteristic scale. W e show that, assuming that the visible (baryonic) matter is some const ant fraction of the dark matter, spiral galaxies with such haloes exhi bit a Tully-Fisher law of the observed form. In a sample of 10 spiral galaxies with well-determined extended rotation curves this halo, comb ined with the observable matter, can successfully model the observed c urves. Moreover, in the seven most luminous galaxies, the best-fitting models have about the same value of Sigma(0) and are effectively one- parameter fits as in MOND (mass-to-light of the visible disc). The one -parameter description, however, does break down for the three dwarf g alaxies in the sample with the lowest internal accelerations.