All Figures

Figure 1: Observed and theoretical profiles for the Si III line at 4552 Å in HD 206165. The former is represented by a histogram whilst the theoretical profiles assume an isotropic Gaussian velocity (dashed line) and a radial-tangential model with (dotted line). Note that both theoretical approaches lead to a good fit with observation particularly in the core of the line, however the radially tangential profile requires a larger macroturblent velocity.

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In the text

Figure 2: Estimates of macroturbulent ( upper figure) and projected rotational velocities ( lower figure) plotted against effective temperature. The Galactic supergiants are represented by squares and the SMC targets by circles. For the projected rotational velocities, the linear least squares fit (excluding Sk 191) is shown as a solid line, whilst the dashed line would represent the rotational velocity assuming a random distribution of projection angles.

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In the text

Figure 3: Predictions of the evolution of the rotational velocity of two models with metallicities appropriate to our Galaxy (Meynet & Maeder 2003; initial masses: 20  - narrow solid line, 40  - narrow dashed line) and two models representative of the SMC (Meynet & Maeder 2004; 30  - thick solid line, 40  - thick dashed line). All models had an initial rotational velocity of 300 km s-1. Also shown are the estimated projected rotational velocities for our Galactic (filled squares) and SMC (filled circles) samples. The SMC target Sk 191 is represented by a filled circle enclosed in a diamond, for clarity. The dotted line represents our estimated mean rotational velocity for both samples, excluding Sk 191 and corrected assuming a random inclination angle.

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In the text

	Figure 4: Projected rotational velocities plotted against nitrogen abundances for the SMC targets. The cross (+) is for the target, AzV 487, for which only an upper limit for the nitrogen abundance could be estimated.
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In the text