**Table 3:** Physical parameters of the programme stars (values for $\xi ^1$ CMa from Morel et al. 2006).
	$\xi ^1$ CMa	$\tau$ Sco	$\theta$ Car
Spectral type	B0.7 IV	B0.2 V	B0.2 V
$T_{\rm eff}$ (K)	27 500 $\pm$ 1000	31 500 $\pm$ 1000	31 000 $\pm$ 1000
$\log g$ (cm s^-2)	3.75 $\pm$ 0.15	4.05 $\pm$ 0.15	4.20 $\pm$ 0.20
$\xi$ (km s^-1)	6 $\pm$ 2	2 $\pm$ 2	12 $\pm$ 4
$v \sin i$ (km s^-1)	10 $\pm$ 2^a	8 $\pm$ 2	113 $\pm$ 8

^a This value is an upper limit, as the spectral lines are significantly
broadened by pulsations in this $\beta$ Cephei variable.

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