Table 2: Characteristics of the B stars in the sample of Lamers et al. (1997) depicted in Fig. 5. The "observed'' absolute magnitude $M_V^{\rm H}$ is calculated from the Hipparcos parallax $\pi _{\rm H}$ (in mas), and is corrected for interstellar extinction and the presence of spectroscopic companions. The predicted absolute magnitude $M_V^{\rm SK}$ is derived from the spectral type according to the calibration of Schmidt-Kaler et al. (1982), if necessary through interpolation (note that they have a special section for Be stars). $v \sin i$ is in km s-1.
HD Sp. type $\pi_{\rm H} \pm \sigma_{\pi_{\rm H}}$ $M_V^{\rm H}$ $M_V^{\rm SK}$ $v \sin i$   HD Sp. type $\pi_{\rm H} \pm \sigma_{\pi_{\rm H}}$ $M_V^{\rm H}$ $M_V^{\rm SK}$ $v \sin i$
22951 B0.5V1) $3.53 \pm 0.88$ -3.0 -3.6 301)   37490 B2IIIe2) $2.01 \pm 0.94$ -4.4 -4.0 1602)
34503 B5III2) $5.88 \pm 0.77$ -2.7 -2.2 252)   143275 B0.2IV4) $8.12 \pm 0.88$ -3.3 -4.5 1484)
35468 B2III2) $13.42 \pm 0.98$ -2.8 -3.9 502)   144217 B0.5IV-V5) $6.15 \pm 1.12$ -3.9 -3.9 905)
36822 B0III3) $3.31 \pm 0.77$ -3.1 -5.1 503)   149438 B0V4) $7.59 \pm 0.78$ -3.1 -4.0 104)
References: 1) Andrievsky et al. (1999); 2) Hauck & Slettebak (1989); 3) Levato (1975);
4) Brown & Verschueren (1997); 5) Holmgren et al. (1997).

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