ROTATION CURVES FROM BARYONIC INFALL - DEPENDENCE ON DISK-TO-HALO RATIO, INITIAL ANGULAR-MOMENTUM, AND CORE RADIUS, AND COMPARISON WITH DATA

Using a simple analytic model of the response of dark matter halos to the dissipative infall of the luminous material to form an exponential disk, we explore the dependence of the final rotation curves on all t he relevant parameters: the ratio F = M(b)/M of the dissipative baryon ic mass M(b) to the total galaxy mass M including dark matter; the rat io b/R of the disk exponential scale length b to the truncation radius R (beyond which infall can be neglected); the core radius r(core) of the isothermal halo in the absence of dissipation; and the dimensionle ss angular momentum parameter lambda = J\E\1/2 G-1 M-5/2 (where J and E are the total angular momentum and energy of the galaxy). We explore in particular the final rotation curves expected in the tidal torque theory of angular momentum, in which [lambda] almost-equal-to 0.05. Fo r lambda = 0.05, we find the final rotation curve to be flat when the gravitational effect of the infalling baryonic material on the dark ha lo is included and if F almost-equal-to 0.05, the value suggested by n ucleosynthesis constraints if the Hubble parameter H0 almost-equal-to 50 km s-1 Mpc-1. Also, the mass inside a ''Holmberg'' radius R(H) = 4. 5b is about half luminous and half dark as observations indicate. Thes e results are quite insensitive to r(core) provided it is sufficiently large, and are characteristic of any theory in which [lambda] almost- equal-to F. The key results are that for F almost-equal-to 0.05 the di spersion in lambda expected in the tidal torque theory, 0.02 less than or similar < lambda less than or similar 0.1, (a) leads to rotation c urves for bright galaxies whose systematics are much like those of the galaxies for which H I data are available when consistent baryonic di sk scale lengths are used throughout; and (b) the mass inside R(H) sho ws a spread of values consistent with observations except possibly for the smallest galaxies, which may have suffered significant gas loss. With this range of lambda-values, the distribution of outer rotation c urve slopes for a given maximum rotation velocity is inconsistent with the data if F is substantially larger or smaller than 0.05, or if r(c ore)/R is substantially smaller than 0.2.