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A mass estimate for the companion to the 'Cartwheel' galaxy
The velocity and the velocity dispersion of the elliptical companion tothe ring galaxy known as the 'Cartwheel' are measured. The velocityconfirms the suggestion by Fosbury and Hawarden (1977) that thiscompanion galaxy was the interloper responsible for the ring structure.The mass inferred from the dispersion is only 5-10% of the mass of theCartwheel itself as determined from the kinematics of the ring. It ispointed out that this low mass is not sufficient to account for theobserved ring by the collisionless kinematic model of Lynds and Toomre(1976). It is thought likely, however, that whereas the underlyingmechanism is an encounter of the kind suggested by Lynds and Toomre, thering is brightened by the star formation induced.
| Spectral and Luminosity Classification of the Bright Sequence Stars in the C Regions.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1955ApJ...121...32N&db_key=AST
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Observation and Astrometry data
| Constellation: | ヘルクレス座 |
| Right ascension: | 17h04m32.54s |
| Declination: | +14°46'42.6" |
| Apparent magnitude: | 9.745 |
| Proper motion RA: | 13.9 |
| Proper motion Dec: | -3.2 |
| B-T magnitude: | 11.173 |
| V-T magnitude: | 9.863 |
Catalogs and designations:
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INHABITED SKY
