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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
| Note on the nature of HD 179315
MK classification and UBVRI photometry is carried out to determinewhether the HD 179315 star is a cepheid or an ellipsoidal binary. Thespectral type proved to be G1Ib, classifying the star as a seven-daycepheid. This is supported by UBVRI data, from which is derived E(B-V) =0.48 plus or minus 0.03 on the Parsons-Bell color excess scale. The staris distinctly cooler than most seven-day cepheids, and is probably closeto the red edge of the instability strip, which may account for its lowamplitude of 0.3 magnitudes.
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Besorolás csoportokba:
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Pozíciós és asztrometriai adatok
| Csillagkép: | Vízöntő |
| Rektaszcenzió: | 19h11m15.37s |
| Deklináció: | +04°11'27.9" |
| Vizuális fényesség: | 7.488 |
| Távolság: | 118.343 parszek |
| RA sajátmozgás: | 16.6 |
| Dec sajátmozgás: | -7.2 |
| B-T magnitude: | 8.347 |
| V-T magnitude: | 7.559 |
Katalógusok és elnevezések:
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