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Selection criteria for targets of asteroseismic campaigns

Various dedicated satellite projects are underway or in advanced stages of planning to perform high-precision, long duration time series photometry of stars, with the purpose of using the frequencies of stellar oscillations to put new constraints on the internal structure of stars. It is known (cf. Brown et al. 1994) that the effectiveness of oscillation frequencies in constraining stellar model parameters is significantly higher if classical parameters such as effective temperature and luminosity are known with high precision. In order to optimize asteroseismic campaigns it is therefore useful to select targets from among candidates for which good spectroscopic and astrometric data already exists. This paper presents selection criteria, as well as redeterminations of stellar luminosity and reddening for stars satisfying these criteria. The aim of asteroseismology is to use the properties of the oscillations of stars to place constraints on their internal struc- ture. The frequencies of stellar oscillations can be used to de- termine parameters of stars that are either inaccessible to clas- sical observation or can not be determined with an accuracy that is sufficient for many purposes. The foremost examples of these parameters are the mass and angular momentum of stars. Currently, accurate masses of stars can only be deter- mined if they are members of close binary systems. Even for the best spectroscopic data and stellar atmospheres modelling currently available, for single stars their mass is not known to better than 20%. If one wishes to determine the mass function of stars and investigate its universality, for instance in order to investigate star formation processes, the current data are heav- ily biased to stars that have formed in binary systems, which may not reflect the variety of conditions under which stars can form and thus provide an incorrect mass function for the galaxy. As a consequence of the fact that forming stars con- tract from molecular clouds many orders of magnitude larger than their main sequence stellar radius, a substantial amount of angular momentum must be shed during the contraction. An important constraint for theories of mechanisms mediating this angular momentum loss would be the measurement of the an- gular momentum of stars for a range of masses. Also, for the post-main sequence evolution of in particular high-mass stars the loss of angular momentumduringevolution is similarly im- portant. Unfortunately spectroscopic observations have access to only the projected surface rotation velocity. The true angu- lar momentum can only be obtained through asteroseismology (Pijpers 2003).