Abstract
Following the failure of the main experiment on board the Wide-Field Infrared Explorer satellite (WIRE), the on-board star camera was used as the first space-based asteroseismology experiment. From May 1999 through November 2006, well over 200 targets were observed for periods ranging up to 40+ days. The typical noise level (measured at a frequency of 10 mHz) of these observations was <5 ppm for a 3rd magnitude star. More than 35 Beta Cep and SPB stars have been observed with WIRE, and analysis has been ongoing for some time. New oscillation modes have been observed for targets such as Beta Cru (Cuypers et al. 2002), Kappa Sco (Cuypers et al. 2004), and Lambda Sco (Bruntt & Buzasi 2006). Lambda Sco in particular comprises two B type stars in a wide orbit (P = 1083 d), and one of these components has a low mass companion (P = 5.95 d). After subtracting the Beta Cep pulsation Bruntt & Buzasi (2006) could clearly see the primary and secondary eclipses in the close system. From their preliminary light curve analysis they constrained the mass and radius of the component stars. Until now, however, the majority of the B stars observed with WIRE have not been analyzed. Here we begin this process, presenting light curves and power spectra, and reporting frequencies and amplitudes for the B stars in the WIRE collection.
