**Table 1:** Known magnetic massive OB stars and their properties. We note that for a dipole field, the magnetic field strength at the pole ( $B_{\rm pol}$ ) and the equator ( $B_{\rm eq}$ ) are related by $B_{\rm pol}=2~B_{\rm eq}$ .
Name	Spectral Type	$v\sin i$	$P_{\rm rot}$	M	Inclination	$\beta$	$B_{\rm pol}$	Reference
		(km s^-1)	(d)	( $M_{\odot}$ )	(deg.)	(deg.)	(Gauss)
$\theta^1$ Ori C	O4-6V	20	15.4	45	$\sim$ 45	42 $\pm$ 6	1100 $\pm$ 100	Donati et al. (2002)
HD 191612	Of?p	<77	538^a	$\sim$ 40	$\sim$ 45	$\sim$ 45	$\sim$ 1500	Donati et al. (2006a)
$\tau$ Sco	B0.2V	5^b	41	15	$\sim$ 70	$\sim$ 90	$\sim$ 500^c	Donati et al. (2006b)
$\xi ^1$ CMa	B0.5IV	20	<37	14			$\sim$ 500	Hubrig et al. (2006a)
$\beta$ Cep	B1IV	27	12.00	12	60 $\pm$ 10	85 $\pm$ 10	360 $\pm$ 40	Henrichs et al. (2000)
V2052 Oph	B1V	63	3.64	10	71 $\pm$ 10	35 $\pm$ 17	250 $\pm$ 190	Neiner et al. (2003b)
$\zeta$ Cas	B2IV	17	5.37	9	18 $\pm$ 4	80 $\pm$ 4	340 $\pm$ 90	Neiner et al. (2003a)
$\omega$ Ori	B2IVe	172	1.29	8	42 $\pm$ 7	50 $\pm$ 25	530 $\pm$ 200	Neiner et al. (2003c)

^a To be confirmed.
^b Mokiem et al. (2005).
^c Field more complex than dipolar.

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