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The most powerful tests of stellar models come from the brightest stars inthe sky, for which complementary techniques, such as astrometry,asteroseismology, spectroscopy, and interferometry can be combined. The K2Mission is providing a unique opportunity to obtain high-precision photometrictime series for bright stars along the ecliptic. However, bright targetsrequire a large number of pixels to capture the entirety of the stellar flux,and bandwidth restrictions limit the number and brightness of stars that can beobserved. To overcome this, we have developed a new photometric technique, thatwe call halo photometry, to observe very bright stars using a limited number ofpixels. Halo photometry is simple, fast and does not require extensive pixelallocation, and will allow us to use K2 and other photometric missions, such asTESS, to observe very bright stars for asteroseismology and to search fortransiting exoplanets. We apply this method to the seven brightest stars in thePleiades open cluster. Each star exhibits variability; six of the stars showwhat are most-likely slowly pulsating B-star (SPB) pulsations, with amplitudesranging from 20 to 2000 ppm. For the star Maia, we demonstrate the utility ofcombining K2 photometry with spectroscopy and interferometry to show that it isnot a 'Maia variable', and to establish that its variability is caused byrotational modulation of a large chemical spot on a 10 d time scale.

Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades