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Kinematics of Sandage-Fouts stars in three cardinal directions
V and (B - V) for 429, 442, and 427 stars are observed in the directionsof the anticenter, Cygnus, and the NGP, respectively, and DDO colors forthose stars G0 and later. The samples observed are ones for whichSandage and Fouts (1987) have published radial velocities. W, V, and Wcomponents of space velocity are derived from DDO distances withavailable proper motions. A clear correlation was found to exist betweenthe velocity dispersions and Fe/H with the dispersions decreasing asFe/H increases to about + 0.00, where V then becomes significantlynegative. The 'thick disk' component is clearly recognized, with sigma(W) approximately equal to 36 km/sec. In the 'old thin disk' and the'young thin disk', 43 percent and 42 percent of the stars have negativeV values, respectively.
| U, V, W velocity components for the old disk using radial velocities of 1295 stars in the three cardinal Galactic directions
New radial velocities are presented for 1295 stars chosen at random nearthe three cardinal Galactic directions of l = 180 deg, b = 0; l = 90deg, b = 0 deg; and b = 90 deg, giving the distribution in U, V, and W,respectively, from the radial velocities alone. The measurements weremade with the coude spectrograph of the Mount Wilson 100 in. Hookerreflector. The purpose of the program is to set limits on the densitynormalization in the solar neighborhood of the old thin disk, the oldthick disk, and the halo. Many more high-velocity stars are present inthe unbiased sample than expected from previous estimates of thenormalization. The data suggest the density ratios in the solarneighborhood to be about 90 percent, 10 percent, and about 0.5 percentfor the thin disk, thick disk, and halo populations, respectively.
| Photoelectric V and (B-V) for McCuskey stars near the Galactic anticenter
V and (B-V) for 135 stars near the Galactic anticenter were obtained.The ultimate purpose of the study is to establish accurate colors which,in conjunction with DDO-derived spectral and luminosity classes, willenable interstellar absorption correction. Ninety-four of these starsalso have been observed by McCuskey for a stellar density analysis ofthe Galactic anticenter. The specific objective here is to establish therelationship between the presented photoelectric and McCuskey'sphotographic colors and magnitudes. Small but significant systematicdifferences exist between the two systems. These differences, ifuniversal for McCuskey's entire sample, increase his distances by about20 percent and decrease his densities by about 40 percent.
| The stellar distribution in the galactic anticenter.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1967AJ.....72.1199M&db_key=AST
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Boga |
| Sað Açýklýk: | 05h58m24.54s |
| Yükselim: | +23°09'21.2" |
| Görünürdeki Parlaklýk: | 7.599 |
| Uzaklýk: | 180.505 parsek |
| özdevim Sað Açýklýk: | -1.2 |
| özdevim Yükselim: | -23 |
| B-T magnitude: | 8.917 |
| V-T magnitude: | 7.708 |
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