1. Combined photometry. Photometric parallax was corrected for duplicity by assuming that both stars obey the adopted color-absolute magnitude relations and the magnitude difference is as given in the IDS or other source. 2. The VRI photometry was taken from Weis (1991a) wherein additional information may be found. 3. Several additional observations were made when the star was significant- ly brighter and bluer than this, presumably during flare events. 4. As noted in Weis (1991a), Vyssotsky identified Vys. 352 as AC 37:460, but AC 37:460 is located at 0h 17m 22s, 36d 12.9m (1950) and is not red. The coordinates given by Vyssotsky are near AC 37:400 and AC 37:401. Of the two, AC 37:400 is a bit redder and is more easily misprinted as AC 37:460, so it is assumed that Vys. 352 = AC 37:400. 5. Observations taken from Weis (1988). 6. GQ And 7. Previously unpublished observations have been combined with data taken from Weis (1988). 8. The star AC 38:1183,located 165" west of Vys. 359, is almost certainly not physically associated with Vys. 359, as noted in Weis (1991a) wherein photometry for AC 38:1183 may be found. 9. Companion 7"/295 deg has V/V-R/R-I = 13.30/0.59/0.52 and is evidently optical. Vys. 87 = FF And. 10. 34"/239 deg from A. 11. V388 Cas 12. Companion 35"/92 deg has V/B-V/V-R/R-I = 13.06/2.63/2.33/1.61 and is obviously a reddened background star. 13. B-V and U-B colors are anomalously blue. Comparison with the observations of Ianna (1979) suggests the possibility that my observation was made during a flare event. 14. The fainter star is Vys. 56 for which Vyssotsky gives an annual motion of 0.123" in 344 deg. The brighter star is BD 46:2014 with motion in the S.A.O. Catalog of 0.102" in 337 deg. This is almost certainly a physical pair. 15. Almost certainly a companion to Gamma Ceti, 740" distant, with which it shares a common proper motion and trigonometric parallax. 16. VX Ari 17. An additional companion noted in Ann. Toulouse 15, 63 is evidently optical. See Weis (1991a). 18. Previously unpublished observations have been combined with data taken Weis (1991a) wherein additional information may be found. 19. Observations taken from Weis and Upgren (1982), Upgren, et al. (1985), and Weis and Hanson (1988). 20. A second observation gave V/B-V/V-R/R-I = 12.78/1.39/1.21/1.10. It is not clear whether these brighter and bluer values are due to a flare event or to scattered light from the primary star. 21. Observations taken from Upgren and Weis (1977). 22. Observations taken from Upgren and Weis (1977) and Weis and Upgren (1982). 23. Previously unpublished observations have been combined with data taken from Weis and Upgren (1982). 24. Observations taken from Upgren, et al.(1985). 25. Photometry for Vys. 453 published by Eggen (1974) evidently pertains to some other star. Vys. 453 and BD 18:684, 100" distant, share a common proper motion according to Luyten (1980) and have similar radial velocities according to Griffin, et al (1988). 26. Previously unpublished observations have been combined with data taken from Upgren and Weis (1977). 27. Observations taken from Weis and Upgren (1982). 28. The observation may have been slightly contaminated by an optical comp- anion about 6"/10 deg with Delta(R) = 3 mag. 29. Previously unpublished observations have been combined with data taken from Weis (1986, 1987). 30. Another star 68"/95 deg has V/B-V/V-R/R-I = 11.96/1.62/0.87/0.63 and is evidently a slightly reddened background star. 31. The photometry indicates that this star is not a normal dwarf. 32. The binary G 193-8AB lies 20.8 arcmin south of Vys. 11 with very nearly the same motion. Combined photometry for G 193-8 gives V/V-R/R-I = 14.65/1.24/1.04 which yields a distance modulus 1.5 mag. larger than that of Vys. 11. Thus it seems unlikely that Vys. 11 and G 193-8 are phys- ically related. 33. Observations taken from Weis (1991b). 34. Companion 12"/35 deg has V/B-V/V-R/R-I = 12.38/0.49/0.17/0.20 and is evidently optical. 35. Companion noted by Worley (1962) is evidently optical. See Weis (1991a). 36. Both Eggen (1974) and Upgren and Kerridge (1973) mistakenly observed BD 33:1504 which is about 5 arcmin southwest of Vys. 16. 37. VV Lyn. Observed range in V magnitude was 0.12 mag. 38. Peculiar colors. 39. Previously unpublished observations have been combined with data taken from Weis (1987). 40. Previously unpublished observations have been combined with data taken from Weis (1986). 41. WX UMa 42. Companion 20"/275 deg has V/V-R/R-I = 13.53/0.80/0.59 and is evidently optical. 43. This is BD -17:3337. These measures have the eastern star slightly brighter and bluer than the western star. This is the reverse of what is given by Eggen (1974) and Bessell (1990), but is in agreement with Weistrop (1977). 44. SZ UMa 45. FI Vir 46. AB is 4"/30 deg. Delta(R) about 4 mag. 47. Companion is optical. See Weis (1991a). 48. BF CVn 49. DT Vir 50. The star AC -21:56726, located 160" southwest of Vys 683, is probably not physically associated with Vys 683, as noted in Weis (1991a), wherein photometry for AC -21:56726 may be found. 51. Noted as SB in Upgren and Caruso (1988). 52. AB is 3"/90 deg. Delta(R) about 2 mag. 53. A is the 6th mag. star BD 7:2690 about 8.1 arcmin distant. 54. Can not identify the supposed companion noted by Worley (1962). 55. Another star 145"/164 deg with V/B-V/U-B/V-R/R-I = 10.71/1.32/1.48/0.66/ 0.50 is evidently not a dwarf. 56. V 1054 Oph. One component noted as SB in Stauffer and Hartmann (1986). 57. Possibly variable. Observed sigma(V) = 0.06 mag. in three measures. 58. Companion to 26 Dra about 12.3 arcmin distant. 59. AB is 3"/90 deg. Delta(R) about 4 mag. 60. Previously unpublished observations have been combined with data taken from Weis (1984). 61. V 774 Her 62. V 1285 Aql. Observations taken from Weis (1987). Noted as SB2 in Marcy, et al.(1987). 63. BDS 9858. Components B and C are optical. See Weis (1991a). 64. Observations taken from Weis (1984). 65. One additional observation gave V/B-V/V-R/R-I = 13.75/1.67/1.43/1.17. Each of the other ten observations did not differ significantly from one another. 66. The entry for BD 19:4261 in Luyten's NLTT Catalog gives the coordinates of BD 19:4262 and the color and motion of Vys. 198. BD 19:4261 and BD 19:4262 are not red, and neither star is Vys. 198. 67. V 1396 Cyg. Component A is SB2. See Fekel, et al.(1978). 68. Star 112"/310 deg has V/B-V/V-R/R-I = 13.06/1.70/1.00/0.74. 69. DO Cep 70. FL Aqr 71. FK Aqr. This component is SB2. See Herbig and Moorhead (1965). The photometric parallax was corrected for the SB2 assuming a magnitude dif- ference of 0.7 mag. 72. EV Lac. These measures agree well with those of Eggen (1968b) and of Stauffer and Hartmann (1986). Bluer and somewhat brighter measures reported by Iriarte (1971), Mumford (1956), Nikonov, et al (1957) and Eggen (1968a) were probably contaminated by light from an optical companion which was less than 8" from Vys. 852 during the period 1960- 1975. 73. EQ Peg 74. Companion 13"/190 deg has V/B-V/V-R/R-I = 13.48/2.24/1.46/0.92 and is evidently a reddened background star. 75. SZ Crt 76. HK Aqr 77. BD 42:1899 is located 109'/272 deg from Vys. 881 and has a similar proper motion. The photometry V/B-V/V-R/R-I = 8.76/0.93/0.48/0.36 is also similar to Vys. 881. However the Yale Parallax Catalog gives parallaxes for Vys. 881 and BD 42:1899 to be 0.0564" +/- 0.0051" and 0.0389" +/- 0.0088", respectively, and Adams & Joy (1923) give radial velocities of -25.4 km/s and +58.9 km/s, respectively, so the two stars are evidently not a physical pair. 78. Possibly physically associated with BD 66:34 (= ADS 433), more than 5 deg northeast of Vys. 364 but with very similar parallax, proper motion and radial velocity. 79. As noted in Weis (1991a) the difference in photometric distance modulus is about 1.2 mag., and there may be significant relative motion. Until definitive kinematic evidence is at hand, it would be prudent to allow for the possibility that this pair may not be physical. 80. Possibly physically associated with the 7th magnitude G star, DM -26:16415 located nearly 10 arcmin north of Vys. 340 but with similar proper motion. 81. These measures agree with several other determinations. The V given by Bessell (1990) appears too bright by 0.5 mag. 82. These measures agree with several other determinations. The V given by Eggen (1974) is too faint by 0.3 mag. 83. These measures agree with those of Epps (1972) and Mumford (1956). The observations of Eggen (1974) are very discordant and may be of the wrong star. 84. The observation of Figueras, et al. (1990) is very discordant and is evidently of the wrong star since they note the B component 27" distant when, in fact, the B component in only 5" distant. 85. Figueras, et al. (1990) observed BD 38:2052, not Vys. 549. 86. These measures agree with those of Bessell (1990) and Laing (1989). The V given by Rossello, et al. (1985) is too faint by 0.2 mag. 87. The observations of Upgren and Lu (1986) are discordant. There appears to be significant systematic errors in their V magnitudes for stars with 13h < R.A. < 16h 30m. 88. These measures agree with several other determinations. The V given by Rossello, et al. (1985) is too faint by 0.45 mag. 89. The observation of Eggen (1968a) is very discordant and may pertain to BD -1:3313, a brighter, redder star about 10 arcmin east of Vys. 759. 90. These measures agree with several other determinations. The observation of Upgren and Kerridge (1973) is very discordant. 91. These measures agree with those of Laing (1989) and Upgren and Lu (1986). The observation of Ianna and Whitman (1984) is discordant. 92. These measures agree with those of Stauffer and Hartmann (1986). Eggen (1968a) evidently observed the wrong star. 93. These measures agree with those of Harrington, et al. (1985). The V given by Upgren and Lu (1986) appears too bright by 0.5 mag. 94. These measures agree with several other determinations. The V given by Bessell (1990) appears too bright by 0.3 mag. 95. BC noted at the telescope. Approx. 4"/60 deg with Delta(R) = 2 or 3 mag.