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Formulas, derived by Arellano Ferro and Mendoza in Paper I (1993), tocalculate Mv, log g, and (Fe/H) were applied to a group of 73A, F, and G stars of high galactic latitude previously classified assupergiant stars. The only star that showed, from data on hand, to beluminous, slightly iron deficient, and out of the galactic plane was BLTelescopii. The remainder of the sample either present controversialresults or are definitively giant or dwarf stars misclassified assupergiants. Thus, if luminous, young stars indeed exist out of thegalactic plane, they are extremely rare.
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An empirical calibration of the Stromgren uvby-beta photometric systemfor the A, F, and early G supergiants is being derived. This paperexplains the observational program and the photometric reductiontechniques used and presents a catalog of new Stromgren photometry forover 600 A, F, and G supergiants.
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Datos observacionales y astrométricos
| Constelación: | Indio |
| Ascensión Recta: | 21h20m21.83s |
| Declinación: | -47°17'53.5" |
| Magnitud Aparente: | 8.962 |
| Distancia: | 518.135 parsecs |
| Movimiento Propio en Ascensión Recta: | 28.5 |
| Movimiento Propio en Declinación: | -26 |
| B-T magnitude: | 9.452 |
| V-T magnitude: | 9.003 |
Catálogos y designaciones:
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