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High-Velocity Clouds
High-velocity clouds (HVCs) consist of neutral hydrogen (\HI) atvelocities incompatible with a simple model of differential galacticrotation; in practice one uses {the absolue value of} VLSR {greater orequal to} 90 km/s to define HVCs. This review describes the mainfeatures of the sky and velocity distributions, as well as the availableinformation on cloud properties, small-scale structure, velocitystructure, and observations other than in 21-cm emission. We show thatHVCs contain heavy elements and that the more prominent ones are morethan 2 kpc from the Galactic plane. We evaluate the hypotheses proposedfor their origin and reject those that account for only one or a fewHVCs. At least three different hypotheses are needed: one for theMagellanic Stream and possibly related clouds, one for the Outer ArmExtension, and one (or more) for the other HVCs. We discuss the evidencefor the accretion and the fountain model but cannot rule out either one.
| Four-colour and H-beta photometry for early type stars in three southern galactic regions
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&AS...41...85L&db_key=AST
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Datos observacionales y astrométricos
| Constelación: | Escorpio |
| Ascensión Recta: | 17h18m38.32s |
| Declinación: | -36°05'13.1" |
| Magnitud Aparente: | 8.268 |
| Distancia: | 256.41 parsecs |
| Movimiento Propio en Ascensión Recta: | -5.1 |
| Movimiento Propio en Declinación: | -13.6 |
| B-T magnitude: | 8.937 |
| V-T magnitude: | 8.324 |
Catálogos y designaciones:
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