Colors and magnitudes on the (U,B, V) system are given for 228 visual binaries for which orbits are available. Mso photometry of additional, physical companions to 26 systems have been obtained with the 200-in. and 100-in. reflectors. The components of most of the orbital systems differ by less than one or two tenths of a magnitude and the mean masses and luminosities are discussed. For several systems con- taining K- and M-type dwarfs, and for late-type, common proper motion companions to several other systems, (V,R,I) photometry has been obtained with the 100-in. and 60-in. reflectors and an RCA 7102 multiplier. A calibration of the (Mv,R - I) relation yields good photometric parallaxes for these systems. New orbits have been computed for 43 systems (ADS 148, 713, 864, 999, 1833, 2630, 3520, 4153, 4971, 5949, 7131, 8166, 8337, 8344, 8635, 8680, 8954, 9094, 9185, 9264, 9380, 9397, 9441, 9689,10158, 10871, 11842,12911, 12961,14412, 14424,15267, 16436, 16836,17178, HD2885, HD20121, HD27019, HD104747, HD194433, HD20644, 1 Gem and + ) with an IBM 7090. The individual systems are discussed in Sec. II. The presence of two, discrete M-L relations is confirmed. One (called the Hyades M-L relation), which is valid for the Hyades-Pleiades stars, is linear in the (M ,logm) plane with a slope of from MB= -2 mag. to +10 mag.; the other (called the sun-Sirus M-L relation), valid for the remaining objects, contains no stars brighter than about Mv +2 mag. and has a slope of . Neither of these slopes agree with the relation 8, obtained from the available stellar model computations. The stars falling on the Hyades M-L relation are apparently all as young, or younger, than the Hyades cluster and have galactic orbits similar to the Hyades and Pleiades clusters; these objects have never been outside a galactic belt about 2 kpc wide. The objects falling on the sun-Sirius M-L relation are a mixture of objects older than the Hyades and they have galactic oribts that carry them outside the 2 kpc wide belt populated by the Hyades-Pleiades stars.
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O. J. Eggen (1965) studied this question.