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On the similarity of the statistics of high-velocity clouds and stars of the spherical component of the Galaxy
An account is given of a comparison, for the first time, ofhigh-velocity H I clouds (HVCs) with objects of the spherical subsystemof the Galaxy. The dependence of the radial velocities of the HVCs ongalactic longitude is similar to Stromberg's asymmetry. The galacticrotational velocity and the velocity dispersion of the HVCs are the sameas for the objects of the spherical subsystem (subdwarfs, RR Lyraevariables, globular clusters). Like the subdwarfs near them, the HVCs donot exhibit a concentration near the center of the Galaxy. There areelongated groups of stars, including Kapteyn's group, that are projectedonto (or are in the neighborhood of) C II, the 'Magellanic Stream', andother complexes with the same radial velocities as these HVCs. Thedistances of the majority of the stars of these groups are on the orderof 100 pc.
| The nature of the Yale Common Proper Motion groups of stars
Attention is given to a large group of approximately 90 stars, twogroups of 20-30 stars, and 12 groups of a few stars each, taken from DDOsystem image tube spectral classification and intermediate bandphotometry for the Yale Common Proper Motion groups of 180 southernstars. Spectroscopic and photometric analyses of these groups haveindicated a very scattered Pop I main sequence in their color-magnitudediagrams. Distance moduli of 5 or less were derived from the averagespectroscopic parallaxes, in keeping with the proper motion amplitude of0.1 arcsec/year. The main sequence of each group shows scatter whenplotted in an HR diagram, indicating that they are probably nothomogeneous groups of stars sharing common physical origins.
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Durbun |
| Sað Açýklýk: | 19h45m31.80s |
| Yükselim: | -49°59'50.8" |
| Görünürdeki Parlaklýk: | 8.12 |
| Uzaklýk: | 174.825 parsek |
| özdevim Sað Açýklýk: | 5.6 |
| özdevim Yükselim: | -113.7 |
| B-T magnitude: | 9.398 |
| V-T magnitude: | 8.226 |
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