All Tables

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 $B_{\rm pol}=2~B_{\rm eq}$ .
Table 2: Properties of program stars in this survey with the integration limits used to determine the magnetic-field strength. Rotational velocities are taken from the Bright Star Catalogue (Hoffleit & Jaschek 1991, O stars), Abt et al. (2002, B stars) and Abt & Morrell (1995, A stars), unless indicated otherwise. Spectral types are from Walborn (1972,1973) and Walborn & Fitzpatrick (1990). Selection criteria are UV-line variability (UV), nitrogen abundance anomalies (N, Gies & Lambert 1992), detection in X-rays by ROSAT (Berghöfer et al. 1996, X), and known $\beta$ Cep-type pulsator (var).
Table 3: Summary of the results of the data analysis. The columns denote, respectively: sequence number of the observation, date of observation, Heliocentric Julian date, measured longitudinal component of magnetic field strength (integrated over the stellar disk) with 1 $\sigma$ errors, velocity of the minimum, and first moment of the Stokes I line profile, both with 1 $\sigma$ errors, for all observed targets arranged in the same order as in Table 2.