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Stroemgren photometry of F- and G-type stars brighter than V = 9.6. I. UVBY photometry
Within the framework of a large photometric observing program, designedto investigate the Galaxy's structure and evolution, Hβ photometryis being made for about 9000 stars. As a by-product, supplementary uvbyphotometry has been made. The results are presented in a cataloguecontaining 6924 uvby observations of 6190 stars, all south ofδ=+38deg. The overall internal rms errors of one observation(transformed to the standard system) of a program star in the interval6.5
| Stromgren photometry of three double mode high amplitude Beta Scuti stars
uvby-beta photoelectric photometric observations of the threedouble-mode high-amplitude Beta-Scuti stars AE UMa, RV Ari and BP Pegare presented. Periodogram analyses are performed using the FourierTransform Method. In all three stars the power spectra are complex, anda large number of frequencies are identified. For each star, all thesefrequencies are shown to be harmonics or combinations of two mainfrequencies nu1 and nu2 corresponding to the fundamental and firstradial pulsation modes, respectively. Intrinsic b - y, m1, and c1 valuesare derived and the physical parameters of these stars are determined.
| A photometric and spectrographic study of BP Pegasi
Photometric (uvby beta) and spectrographic observations of the dwarfCepheid BP Peg are discussed. The observations are used to derive areddening value of E(b-y) = 0.067 m. An effective temperature of 7470 K,a mean surface gravity, log g = 3.85, and a Fe/H abundance ratio of -0.08 are obtained. Pulsation theory and stellar model sequences yieldM(bol) = 1.4 m, mass = 1.85 solar masses, and age = 1.3 X 10 to the 9thyrs. Also, the radial-velocity data show a mean radial velocity of - 30km/s and a total velocity range of 36 km/s.
| The fourth meridian catalog of Besancon Observatory
The catalog presented gives differential meridian positions for 670F-type stars between plus 15 and plus 45 deg declination. The positionsare reduced to the equinox of 1950.0 without proper motions; 333 FK4stars were used as reference stars. A minimum of three and an average offive transits of each program star were observed photoelectrically usinga Gautier transit circle and a Hog grid. The internal accuracy ofindividual measurements is shown to range from 0.013 sec in rightascension and 0.30 arcsec in declination for brighter stars under betterobserving conditions to 0.020 sec in right ascension and 0.38 arcsec indeclination for fainter stars under worse conditions. The standarderrors were applied to compute weighted mean positions, mean epochs, andunweighted means for the program stars. Mean corrections for 283 FK4stars are also provided.
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