Top: specific angular momentum as a function of cloud mass. The trends from B18 for M 33 and from Phillips (1999) are indicated. This figure can be directly compared with B18 and with Dobbs (2008). Middle: here we show the strong M 33 clouds along with the M 51 clouds, without showing the distinctions between pro/retrograde and S/N level. While the values are lower for the M 33 clouds, the M 51 clouds follow a similar trend. Bottom: specific angular momentum as a function of cloud radius. The trend from Phillips (1999) is indicated. The cloud radii are from Colombo et al. (2014a) and the accumulation at 32 pc is due to a limit set by Colombo et al. (2014a). The fit results for M 33 and M 51 for both the high S/N and full samples are given in Table 1. The scatter about the fits is a factor 2–3 (precise values given in Table 1).