11aHD 1337 = AO Cas.  Possible apsidal motion with a 78 year period.
 20aHD 5005C = ADS 791C.  Visual companion to HD 5005, 3.9 arcminute
 20bseparation.  Delta-m(A,C) = 0.8 mag.  Component in B is 1.4 arc-
 20cseconds from A and and about 2.0 mag. fainter.
 55aBD +62 424. Located in a very faint part of MA19.
 56aHD 16429. One of the values for the radial velocity (+87.4 km/sec,
 56bone plate) given for this star (H.A. Abt 1970, Ap. J. Suppl., 19,
 56c387) has not been considered here because it is 111 km/sec larger
 56dthan the maximum velocity yielded from 14 other plates.  We suspect
 56ethe dicordant velocity refers to a nearby field F5 star (see Abt,
 56fLevy and Gandet 1972).
 69aHD 19820 = CC Cas.  Probably ellipsoidal variable (Delta-m = 0.1).
 80aHD 34078 = AE Aur = HR 1712.  Irregular variable m(v) = 5.4 - 6.1.
 80bMA50 superimposed on MA52.
 83aHD 242908.  MA 53 superimposed on MA 52.
 84aHD 242926.  MA 53 superimposed on MA 52.
 85aHD 242935.  MA 53 superimposed on MA 52.
 87aHD 35619.  In MA52 and less than 0.5 degrees away from MA56 and
 87bMA58.
 88aBD +34 1054.  MA56 superimposed on MA52.
 90aHD 35921 = LY Aur.  Orbit and light curve are preliminary.  The
 90brealtive velocity of the binary components is large (450 km/sec)
 90cas deduced from only five spectrograms.
 92aHD 36486 = Delta Ori.  Many orbits have been computed but systemic
 92bvelocities differ appreciably (+12 to +23 km/sec).  We have used
 92cMiczaika's value (1952, Zs. f. Ap., 30, 229).  Variations in
 92dbrightness (delta-m = 0.1 mag.) could be of eclipsing nature.
 95aHD 36841. Probably inside a reflection nebula near IC 434.
 97aHD 37022 = Theta(1)C Ori.  In the Orion Nebula, NGC 1976.  The lines
 97bare broad and Si IV is absent (Conti and Alschuler 1971).  Suspected
 97cvariability in the velocity might be an error; more observations
 97dseem necessary.
 99aHD 37041 = Theta(2) Ori.  In the Orion Nebula, NGC 1976.  As in
 99bTheta(1) Si IV lines are very weak.
100aHD 37043 = Iota Ori.  In the Orion Nebula, NGC 1976.
101aHD 37468 = HR 1931.  In IC 434.
105aHD 37742 = Zeta Ori.  In IC 434.
106aHD 37743.  In IC 434.  Companion to HD 37742; separation 2.7 arc-
106bseconds.
108aHD 247042 = BD +29 981.  Near a SN remnant.
111aHD 39680.  Although the star is probably of variable velocity, the
111badopted velocity is the weighted average of Lick's mean of eight
111cplates, as published in Wilson (1953), and the mean of two plates as
111dgiven in Abt and Biggs (1972) because we could not find the individ-
111eual plate velocities obtained by Lick.
121aHD 254755.  McDonald observers suspect velocity variability in this
121bstar, but no velocity range is given (C. K. Seyfert and D. M. Popper
121c1941, Ap. J. 93, 461).
127aHD 45314.  The star may be a subdwarf (Conti and Alschuler 1971).
127bIt has however been estimated that M(v) = -6.8.  (Hutchings 1970).
127cSome H lines are filled in, and according to Hutchings, H-beta shows
127da P Cygni P profile.
135aHD 46966.  In a SN remnant: D14.
136aHD 47129.  In a SN remnant: D14.
141aHD 48099.  In a SN remnant: D14; but at less than 1 degree away from
141ban unnamed region.
143aBD +0 1576.  MA93 is a very faint region associated with a brighter
143bone.
150aHD 53975.  Less than 0.5 degrees away from MA110.
153aHD 55879.  In a faint part of MA111.
155aHD 57060.  Batten (1967) suggests that the systemic velocity is
155bvariable, with a range of about 25 km/sec.  The velocity adopted
155chere is the average of the systemic velocities for the orbits com-
155dputed in 1935, 1941, and 1958 (cited by Abt and Biggs 1972).
166aHD 61827.  In a very faint H II region.
167aCD -29 4849.  Region is very faint, probably associated with this
167bstar and HD 61827.
238aHD 93161.  Visual binary quoted by Thackeray et al. (1973) as having
238bcomponents 2.0 arcseconds apart and delta-m = 0.1.  The spectral
238ctypes, according to these authors, are O6 for the Np component and
238dO5 for the Sf one.  The adopted velocity is the mean for both stars.
238eThey are both suspected of showing variable velocity; the range of
238fthe Sf component is 46 km.sec and that of the Np is hard to estimate
238gowing to the large scatter in the two measurements published for
238heach plate.
254aHD 93521.  The H and K lines have been considered as stellar in ori-
254bgin and included in the computation of the radial velocity of this
254cstar (Plaskett, J. S and Pearce, J. A. 1931, Publ. Dom. Ap. Obs.,
254d5, 1).  However, we were able to correct each of the 19 plates,
254esince the authors list the H and K line velocities separately in all
254fcases.  The effect was to increase the scatter of the individual
254gplate velocities, which strongly suggests real variations in velo-
254hcity, not suspected by Plackett and Pearce (although they did sug-
254igeat possible doubling of lines).  The star is probably a spectro-
254jscopic binary with very broad lines.
317aHD 101223.  Magnitude and color index from Humphreys (1973).
317bThackeray, A. D. and Wesselink, A. J. (M.N.R.A.S., 131, 121 1965)
317cgive m(v) = 8.68 and B-V = 0.17.
363aHD 135240 = Delta Cir.  The adopted velocity is the average of the
363bsystemic velocities resulting from two solutions from the orbital
363celements.  The solutions correspond to different epochs and the
363dvalues of v(0) are quite similar (+9.2 and +4.8).  Apsidal motion
363eand/or variable systemic velocity is suspected.
384aHD 149757.  Published radial velocities are very discordant:
384bVictoria, +31 (2 plates); Yerkes, -35(5); Lick, -20(4); Canberra,
384c-1 (3).  Variability is suspected only by the observers of the
384dlatter observatory, but the velocity range deduced from their
384eresults is only 22 km/sec.
386aHD 150136 = HR 6187.  Visual multiple system companion to
386bHD 150135 (CGO 385).
393a150958.  Radial velocity given here is from the absorption lines
393bonly; the velocity from the emission lines is -39 km/sec.
400aHD 151804.  The adopted velocity refers to the absorption lines
400bonly.  Conti and Alschuler (1971) find H-beta with P Cygni profile,
400cand it has been noted that O III lambda 3760 also shows such struc-
400dture and suggested that all absorption lines arise from an expand-
400eing shell (Struve 1944).  According to Struve, emission line velo-
400fcity is +52.0 km/sec.
407aHD 152218.  Double line spectroscopic binary with tentative v(0)
407bvalue by Struve (1944).
413aHD 152248.  Provisional orbit by Struve (1944), very uncertain.  The
413bstrength of the lines of the components is almost equal, but the
413cstrongest one always appears to be blue-shifted relative to the
413dweaker component.
422aHD 152408.  Classified as a typical P Cygni-type object by Struve
422b(1944).  We list the absorption-line velocity average of three inde-
422cpendent observations (8 plates).  Emission-line velocity according
422dto Struve is +12.3 (5 plates).  Hutchings (1968) notes that the at-
422emosphere of this star is expanding rapidly, and that the measure-
422fment of large negative radial velocity is due to this fact, since
422gthe strongest spectral lines are highly blue-shifted.
466aHD 163800.  Considered of variable velocity, although no velocity
466brange is given (Neubauer 1943).  From the probable error given by
466cthe latter the range must be about 56 km/sec, assuming the varia-
466dbility is due to circular orbital motions.
483aHD 167264.  In a very faint H II region, possibly MA365.
485aHD 167659.  Less than 1 degree away from MA359.  Conti Alschuler
485b(1971) note a very weak Si IV line on the spectrum of this star.
486aBD -12 4964.  MA361 superimposed on MA362.
488aBD -12 4979.  In the faint part of MA361 superimposed on MA362.
490aHD 167971.  MA361 superimposed on MA362.
491aBD -12 4984.  MA361 superimposed on MA362.
497aHD 168112.  MA361 superimposed on MA362.
513aBD -12 5039.  In region MA 361.
516aHD 169755.  A close companion in the spectrograph slit was mentioned
516b(Neubauer 1943).
517aBD -8 4617.  Less than 0.5 degrees away from MA381.
518aHD 170452.  Neubauer (1943) notes that the spectrum of this star is
518bcomposite.
522aHD 171198.  Declared of variable velocity by Neubauer (1943).  He
522bdoes not list the individual plate velocities or give velocity
522crange, but we estimate that the latter is about 350 km/sec.  More
522dobservations are clearly needed for this star.
523aBD -8 4634.  Less than 1 degree away from MA385.
540aBD +24 3866.  Less than 0.5 degrees away from MA406.
546aHD 188001 = 9 Sge = HR 7574.  It has been considered that the star's
546bradial velocity may vary from -6 to +34 km/sec with a long period
546c(Underhill, A. B. 1958, Pub. Dom. Ap. Obs., 11, 143).  The star has
546dan expanding atmosphere and its spectrum shows emission lines with
546ewidely different wavelength shifts (Hutchings 1970).
552aHD 190429 = AGC 13312AB.  Visual binary with components 2.0 arcsec-
552bonds apart.  The radial velocity of each component has been measured
552cindependently several times.  Both stars show velocity variability
552dwith range 63 km/sec (component A) and 121 km/sec (component B).
552eThe heliocentric velocity listed here is the weighted average of the
552fadopted velocity for each star (-16 km/sec for A and -6 km/sec for
552gB); the weight is the ratio of the number of plates to the velocity
552hrange.
584aHD 194280.  Less than 0.5 degrees away from MA526.
585aHD 194334.  Less than 0.5 degrees away from MA529.
587aHD 229234.  Belongs to NGC 6913 but its identification is ambiguous.
587bWe used the velocity by Abt, Levy and Gandet (1972) to compute the
587cadopted velocity.
619aHD 202124.  Less than 1 degree away from MA614.
631aHD 210839.  In a broken H II region (S 134) within a reflection
631bnebula.
638aHD 214023.  In a very faint part of MA636.
641aHD 214680 = 10 Lac + HR 8622.  Short term irregular variations in
641bthe observed radial velocity have been found.  These variations
641ccould be smoothed out in long-exposure plates (Grygar, J. 1964,
641dB.A.N., 17, 305).  The amplitude of the variations is 15 km/sec.
641eLess than 1 degree away from a very faint unnamed H II region.
644aHD 216532.  In a very faint part of MA 649.