Abstract
Hot subdwarfs comprise typically 50 per cent of faint blue star surveys at high galactic latitude (e.g. the Palomar-Green (PG) survey: Green, Schmidt & Liebert 1986; the Edinburgh-Cape (EC) survey: Stobie et al. 1996a, Kilkenny et al. 1996a). In contrast to the PG survey, the EC survey has found that a large fraction (~ 15 per cent) of its hot subdwarf sample is comprised of sdB stars showing the Can K line. This implies that the hot subdwarf has a relatively luminous companion of spectral type F or G.
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