Titlebook: Galaxy Distances and Deviations from Universal Expansion; Barry F. Madore,R. Breant Tully Book 1986 D. Reidel Publishing Company, Dordrech

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Lance W. Roberts,Susanne von Belows young objects which are considerably more metal deficient than those in either the Galaxy or the LMC. It is therefore of importance in checking metallicity effects on (young) distance indicators. However because of its great depth (~18 kpc) in the line of sight it is less suitable than the LMC for

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Kenneth Zweibel,Richard Mitchell) versus rate of decline relation for novae. In the spring of 1986 the CFH Telescope will be used to search for novae in Virgo Cluster ellipticals. It is hoped that these observations will result in an improved determination of the Hubble parameter.

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Thermosyphon Solar Energy Water Heaters,flow. Absolute calibration of the method, however, remains highly uncertain owing to the poor state of nearby galaxy distances. A coordinated ground-based and space attack on this problem, primarily involving Cepheids, holds out great promise for a measurement of the Hubble constant good to ten perc

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https://doi.org/10.1007/978-1-4613-9945-2the 21 cm line width (?υ). Using these best known extragalactic distances it is hoped to get an efficient tool for deriving distances to galaxies whose magnitudes and line widths have been measured. In addition the galaxy’s inclination (i) is needed for correcting both quantities, the magnitude for

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A Solar Hydrogen Energy System,IR) vs.log ?v. relation . in the log ?v. vs. M(IR) relation. This means that in addition to the Malmquist effect another bias must be present. A discussion of possible bias sources reveals that, in addition to type differences, the line width ?v. itself has probably influenced the sample. Indeed, a

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