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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| A catalog of K giants at the South Galactic Pole - Broadband and DDO photometry and radial velocities
We describe a sample of K giants at the South Galactic Pole, selected toexamine the chemical and kinematical properties of stars perpendicularto the galactic plane and to measure the local column density of thedisk. We report velocities, abundances, absolute magnitudes, andbroadband BV photometry for over 500 giants.
| Local dark matter from a carefully selected sample
The precise data obtained by Flynn and Freeman (1991) on K giants at thesouth Galactic pole are used to analyze the amount of local dark matterin which the systematic effects can be modeled easily and evaluatedaccurately. The method of Bahcall (1984) is employed to solve theself-consistent equations for the distribution of dark matter. TheK-giant survey is found to provide significant evidence for disk darkmatter. Taking into account all recognized sources of error using astatistical test devised by Gould (1989, 1990), a model with no darkmatter is inconsistent with the data at the 86-percent confidence level.The best-fit P-model (in which dark matter is distributed proportionallyto known matter) has 53 percent more dark matter than visible matter.
| Spectroscopic studies of Wolf-Rayet stars. III - The WC subclass
Wolf-Rayet (W-R) stars, which are the descendants of massive O-typestars, can be subdivided into three groups depending on their spectralappearance. These groups include the nitrogen class (WN), the carbonclass (WC), and the oxygen class (WO). The present paper is concernedwith the WC stars. The assignment of WC subtypes has been based onvisual inspections of photographic plates. One of the aims of this studyis related to the quantification of the visual estimates. The measuredratios of equivalent widths and the FWHM of the 4650 A line for Galacticand LMC stars are presented, and the reclassification of some stars isproposed on this basis. In particular, it is shown that the majority ofthe LMC WC stars should logically be classified WC4 instead of WC5.Comments on individual stars are provided, and terminal velocities arediscussed. It is attempted to give a complete overview of the mostimportant spectroscopic features of the WC stars in the optical region.
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| Takýmyýldýz: | Balina |
| Sað Açýklýk: | 00h36m43.71s |
| Yükselim: | -17°47'48.4" |
| Görünürdeki Parlaklýk: | 8.335 |
| Uzaklýk: | 362.319 parsek |
| özdevim Sað Açýklýk: | 10.6 |
| özdevim Yükselim: | -32.3 |
| B-T magnitude: | 9.797 |
| V-T magnitude: | 8.456 |
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