00177+5126 = HD 1337 (AO Cas) : The classification is from the UV tomographic analysis of Bagnuolo & Gies (1991).

00528+5638 = HD 5005 : This is a trapezium system (Abt 1986) which lies at the center of the cluster IC 1590 at a distance of 2.94 +/- 0.15 kpc (Guetter & Turner 1997). All four components were observed and appeared to be single.

02268+5853 = HD 14947 : Garmany & Stencel (1992) include this star in Per OB1.

02229+4129 = HD 14633 : Rodgers (1974) made a preliminary orbital analysis (P =15.3) but the variations appear to be more complicated than originally claimed (Bolton & Rodgers 1978).

02327+6127 = HD 15558 : Both visual components were observed and appeared to be single.

02408+6117 = HD 16429 : Both visual components were observed: A was resolved (CHARA 208 Aa) but B appeared to be single. Gies & Bolton (1986) found a large scatter in radial velocities (but could not find a suitable period), and this suggests that at least one component may be a spectroscopic binary.

03141+5934 = HD 19820 (CC Cas) : The classification is from the tomographic analysis of Hill et al. (1994).

04078+6220 = HD 25638 (SZ Cam) : The classification is from Chocol (1980). The discovery of a speckle companion (CHARA 209 Aa) with a period of some 60 confirms the third body model advocated by Mayer et al. (1994) based on the appearance of the spectrum and variations in the time of light curve minimum (they suggest a third body period of 50.7). Another light curve solution is given by Harries et al. (1997b). The B component (HD 25639) was also observed and appeared to be single. Classification of the B component is from the WDS.

04541+6621 = HD 30614 ( Cam) : Fullerton (1990) presents high quality profiles that indicate the presence of line profile variations; his associated radial velocity measurements do not confirm any of the periods suggested by Zeinalov & Musaev (1986) and Musaev & Snezhko (1988).

05207+3726 = HD 34656 : Fullerton et al. (1991) describe profile and radial velocity variations that suggest that this star is a short-period, radial pulsator. Underhill (1995) also discusses radial velocity measurements.

05279+3447 = HD 35652 (IU Aur) : The classification is from Mammano et al. (1977), and because the stars are are classified as B-type we have not included this system in our distributions for the O-stars. Harries et al. (1997b) discuss the inner double-lined system and evidence of a near tertiary in a 294 orbit. The distant, fourth star was detected both by us (on the suggestion of B. Schaeffer) and Hipparcos (ESA 1997).

05297+3523 = HD 35921 (LY Aur) : The classification is from Drechsel et al. (1989). Howarth et al. (1997) give m for both spectroscopic and astrometric components.

05320-0018 = HD 36486 ( Ori) : Orbital elements are also given by Levato et al. (1988). The Aa visual pair has increased in separation from 0".20 to 0".29 between 1979 and 1994. The spectral classification for the C component is from Morrell & Levato (1991).

05351+0956 = HD 36861 ( Ori) : Both A and B components were observed and appeared to be single. The AB pair may not be physical (Lindroos 1985). The classification of the C component is from Lindroos (1985; based on photometry). Lindroos gives a distance of 430 pc. The classification of the B component is from Hoffleit & Warren (1991).

05353-0523 = HD 37022 ( Ori C) : Stahl et al. (1996) find that the H profiles vary with a 15.4 cycle which they suggest is related to the star's rotational period; photospheric line radial velocity variations are small. All 4 of the Orion Trapezium stars were observed with the speckle camera (A = HD 37020; B = HD 37021; C = HD 37022; D = HD 37023) and all appeared to be single. Classifications of the B and D components are from the WDS. The spectral classification for the A component is from Morrell & Levato (1991).

05354-0525 = HD 37041 ( Ori) : The A component (CHARA 249 Aa) was resolved on 3 occasions, but the distant StF 17 B component was observed to be single. The Hipparcos results (ESA 1997) confirm the CHARA 249 Aa pair. The spectral classification for the B component is from Morrell & Levato (1991). The classification of the C component is from Hoffleit et al. (1983).

05354-0555 = HD 37043 ( Ori) : The classification is from Stickland et al. (1987). The A component was resolved (CHARA 250 Aa); the B component was also observed but appeared to be single. The classification of the B component is from Hoffleit & Warren (1991).

05387-0236 = HD 37468 ( Ori) : The AB pair has decreased in position angle from 171 to 125 between 1975 and 1994. Fullerton (1990) describes three spectral components in the He I 5876 profile which suggests that one of the stars is a double-lined spectroscopic binary (see Bolton 1974). The classifications of the B, C, and D components are from Hoffleit & Warren (1991), while the classification for the E component is from Morrell & Levato (1991).

05408-0157 = HD 37742 ( Ori) : Levato et al. (1988) and Fullerton (1990) also report small radial velocity variations (< 35 km/sec). Both A and B components were observed and both appeared to be single. The classification of the B component is from Hoffleit & Warren (1991).

05460-3218 = HD 38666 (Mu Col) : Additional radial velocity measurements by Fullerton (1990) and Penny et al. (1993a) confirm the lack of variability.

05547+1351 = HD 39680 : Both components were observed and appeared to be single.

06273+1453 = HD 45314 : The classification is from Conti & Leep (1974). The star was resolved (CHARA 251) in the single observation we made.

06374+0608 = HD 47129 (Plaskett's star) : The classification is from Bagnuolo & Barry (1996). We took the mass ratio from Bagnuolo et al. (1992b).

06386+0137 = HD 47432 : The star is a member of Mon OB2 according to Hill et al. (1986).

06410+0954 = HD 47839 (15 Mon) : The classification of the speckle companion (CHARA 168 Aa) is from Gies et al. (1993). The spectroscopic orbit and current periastron passage of Aa are discussed by Gies et al. (1997). The B component was observed and appeared to be single. The classifications of the B, C, D, and E components are from Hoffleit & Warren (1991) who list the E component as a close pair.

06401-3919 = HD 48149 : The classification is from Conti & Alschuler (1971).

07015-0307 = HD 52533 : The classification is from Conti et al. (1977).

07187-2434 = HD 57060 (29 UW CMa) : The classification is from the UV tomographic analysis of Bagnuolo et al. (1994).

07187-2457 = HD 57061 (30 CMa) : van Leewen & van Genderen (1997) and Stickland et al. (1997e) argue that the brighter A component of the visual Aa binary is a triple system consisting of a close 1.28 eclipsing system orbiting a distant O star (the spectroscopic binary with a period of 154.9). The visual Aa pair has slowly decreased in separation from 0".19 to 0".15 between 1977 and 1994. The classification of the D component is from Hoffleit & Warren (1991).

07220-0859 = HD 57682 : Additional radial velocity measurements by Penny et al. (1993a) confirm the lack of variability.

07330-2820 = HD 60369 : The classification is from Garrison et al. (1977).

07398-3235 = HD 61827 : The classification is from Houk & Cowley (1975).

08036-4000 = HD 66811 ( Pup) : The distance estimate is from Reid & Howarth (1996). Van Rensbergen et al. (1996) discuss the star's trajectory and possible runaway status.

08095-4720 = HD 68273 ( Vel, WR 11) : The Hipparcos distance suggests a position in front of the Vel OB2 association (van der Hucht et al. 1997; Schaerer et al. 1997) at a distance of 258 +41/-31 pc; however, the Hipparcos distances for the B stars in Vel OB2 (Brandt et al. 1971) yield a comparable distance of 317 +/- 42 pc. This is also consistent with the distance from the resolution of the binary by Hanbury Brown et al. (1970) of 350 +/- 50 pc. Thus, we have chosen to keep Vel as a member of Vel OB2. The classification is from van der Hucht et al. (1997). The B component was also observed and appeared to be single. The classifications of the B, C, and D components are from Hoffleit & Warren (1991).

08249-4418 = HD 71304 : Turner (1979) includes this star in the Vel OB1 group at a distance of 1.8 kpc. Photometric spectral classifications of the B and C components are from Lindroos (1985), who also finds a distance of 2.7 kpc.

08392-4025 = HD 73882 : Eggen (1982) assigns this star to a group associated with the cluster IC 2395 at distance of 0.8 kpc. The Hipparcos Catalogue (ESA 1997) contains a light curve with a period of 1.46 d.

08504-4205 = HD 75759 : The classification is from Thackeray (1966). The star is part of a group associated with the cluster IC 2395 (Eggen 1982).

08506-4632 = HD 75821 (KX Vel) : The classification is from Conti et al. (1977). Part of an eclipse was observed by Balona & Laing (1986) (the orbital ephemeris is discussed by Mayer et al. 1997).

08540-4229 = HD 76341 : The classification is from Garrison et al. (1977).

08551-4736 = HD 76556 : The classification is from Garrison et al. (1977).

08575-5045 = HD 76968 : Turner (1979) includes this star in a group with the Cepheid SW Vel which lies beyond Vel OB1 at a distance of 2.6 kpc.

10157-5115 = HD 89137 : The classification is from Garrison et al. (1977).

10223-5945 = HD 90087 : The classification is from Garrison et al. (1977).

10318-6356 = HD 91452 : The classification is from the LSC; however, Garrison et al. (1977) assign a type B0 Ia.

10438-5933 = CPD-58 2611 : This object is designated as Trumpler 14 20 in the list of Feinstein et al. (1973) and as FMM 20 in Penny et al. (1993a).

10439-5933 = Tr 14 9 : This object is designated as Trumpler 14 9 in the list of Feinstein et al. (1973) and as FMM 9 in Penny et al. (1993a).

10440-5933 = HD 93129 : Both A and B components were observed with the speckle camera and appeared to be single (Penny et al. 1993a).

10440-5932 = CPD-58 2620 : This object is designated as Trumpler 14 8 in the list of Feinstein et al. (1973) and as FMM 8 in Penny et al. (1993a).

10441-5935 = HD 93160 : This star (component C of HD 93161) was observed with the speckle camera and appeared to be single.

10441-5935 = HD 93161 : Both A and B components were observed with the speckle camera and appeared to be single. Levato et al. (1991) derive a single-lined spectroscopic orbit for HD 93161 but they do not indicate which component is the binary. Howarth et al. (1997) and Penny (1996a) found large radial velocity changes in closely spaced IUE spectra, and Howarth et al. argue that both components are short-period binaries.

10444-6000 = HD 93206 (QZ Car) : The classifications are from Morrison & Conti (1980) who describe this quadruple that consists of a pair of SB1 systems (the shorter period system is also eclipsing). Their expressed hope that speckle interferometry might resolve the pair was not realized in our work, but the object remains an important target for high resolution work.

10446-5944 = HD 93205 : The classification is from the UV tomographic analysis of Penny (1996b). The companion star, HD 93204 (BsO 4 B), was also observed and appeared to be single.

10451-5941 = HD 93308 (Eta Car) : This famous luminous blue variable is not classified as an O star, but it is almost certainly a massive object. The inner structure of the ejecta of this star is described by Davidson et al. (1997). A preliminary set of orbital elements is given by Damineli et al. (1997) who suggest a 5.5 orbit with a maximum angular separation of 0".004. The central object appeared single in our observations. The H component (HDE 303308) was also observed and appeared to be single.

10457-5924 = HD 93403 : The classification is from the UV tomographic analysis of Penny (1996b).

10484+3734 = HD 93521 : The classification is from Hobbs et al. (1982). Fullerton (1990) and Howarth & Reid (1993a) describe the striking line profile variations in the spectra apparently due to nonradial pulsations.

11049-6103 = HD 96264 : The classification of the B component is from Lindroos (1985), who finds a distance of 3.5 kpc.

11072-5952 = HD 96670 : The classification and SB1 orbit are from Garcia (1994).

11118-6042 = HD 97434 : The star belongs to a group behind Tr 18 (Vazquez & Feinstein 1990) at a distance of 2.8 kpc; we designate this as "Tr 18B" in Table 1.

11304-6349 = HD 100099 : The classification is from Garrison et al. (1977).

11384-6312 = HD 101223 : Additional similar radial velocities are reported by Thackeray & Wesselink (1965) and Humphreys (1973).

11391-6326 = HD 101298 : Additional similar radial velocities are reported by Thackeray & Wesselink (1965).

11398-6329 = HD 101413 : This star (BsO 7 B) is the optical companion of HD 101436 (Lindroos 1985). Both stars were observed and appeared to be single. Additional diverse radial velocities for HD 101413 are reported by Thackeray & Wesselink (1965) and Conti et al. (1977).

12058-6934 = HD 105056 (GS Mus) : Harmanec (1987) gives a preliminary orbit with P =1.74 and K =12.4 km/sec. The same period and its double also appear in photometry (van Genderen et al. 1989), so the radial velocity variations may be related to pulsation instead of orbital motion. The radial velocity variations are also discussed by Walborn et al. (1980) and Levato et al. (1988).

12560-5650 = HD 112244 : Classification of the B component is from Lindroos (1985), who finds a distance of 2.5 kpc.

13065-6505 = HD 113659 : The classification is from Houk & Cowley (1975).

13081-6518 = HD 113904 ( Mus, WR 48) : The classification is from Houk & Cowley (1975). Moffat & Seggewiss (1977) found evidence of orbital motion in the WR star, but the O star appeared stationary. We found a possible binary companion at a separation of 0".04 which needs confirmation, but if correct, this suggests that the system is triple, consisting of a WR SB1 plus a distant O star. The visual B component was observed and appeared to be single.

13161-6235 = HD 115071 : Hipparcos has shown this star to be an eclipsing binary with a period of 1.37 (ESA 1997). Both Penny (1996a) and Howarth et al. (1997) found evidence of line-doubling. Turner (1985) shows that this star appears close to and has a similar distance to the cluster Stock 16.

13304-7851 = HD 116852 : The classification is from Morgan et al. (1955). Sembach & Savage (1994) suggest that the star lies at 1.3 kpc from the Galactic plane, and so we have assigned it to the "runaway" category.

13347-6320 = HD 117856 : The classification is from Garrison et al. (1977).

13529-6243 = HD 120678 : The classification is from Garrison et al. (1977).

14064-5943 = HD 122879 : The classification is from the LSC; however, Garrison et al. (1977) assign a type B0 Ia.

14182-5130 = HD 124979 : The classification is from McConnell & Bidelman (1976). Tobin & Kilkenny (1981) place the star at 0.7 kpc from the Galactic plane, so we have included it in the "runaway" group. Penny (1996a) suggests that the star may be a double-lined binary which needs confirmation since there are only 2 other known double-lined binaries among the runaway stars (both B-type systems; see Gies & Bolton 1986).

14202-6105 = HD 125206 : This "field" object may belong to the "CLUST 3" group of Mel'nik & Efremov (1995).

15169-6057 = HD 135240 ( Cir) : This "field" object may belong to the "Pis 20" group of Mel'nik & Efremov (1995). The secondary classification is an estimate from Stickland et al. (1993b). The Hipparcos Catalogue (ESA 1997) contains an eclipsing light curve. Classification of the B component of the optical pair is from Lindroos (1985). Lindroos also finds a distance of 750 pc to this system.

15188-6030 = HD 135591 (45 Cir) : This "field" object may belong to the "Pis 20" group of Mel'nik & Efremov (1995). Classifications of the B and C components are from Lindroos (1985); the C component classification is photometric. Lindroos finds a distance of 1.0 kpc.

16364-4252 = HD 149404 : The classification is from the UV tomographic analysis of Penny (1996b).

16372-1034 = HD 149757 ( Oph) : The line profile variations of this nonradial pulsator are most recently described in Kambe et al. (1997). Van Rensbergen et al. (1996) discuss the runaway trajectory of the star.

16413-4846 = HD 150136 : This star (the C component of HD 150135) was observed and appeared to be single.

16466-4705 = HD 150958 : Leep (1978) suggests that this star is a single-lined binary with a period of approximately 5 d.

16500-4137 = HD 151564 : The classification is from Schild et al. (1969); however, Garrison et al. (1977) assign a type B0.5 V.

16528-4147 = HD 152003 : Constant radial velocity is also found by Levato et al. (1988).

16540-4143 = HD 152218 : The classification is from the UV tomographic analysis of Penny et al. (1993b). A new orbit by Stickland et al. (1997b) yields a period of 5.604.

16541-4147 = HD 152233 : This O star is the F component of the multiple system. The A component is HD 152234 which is a B0.5Ia star (Hoffleit & Warren 1991). The AB system is a 0".5 binary which was observed and resolved 3 times.

16542-4150 = HD 152248 : The classification is from the UV tomographic analysis of Penny (1996b). The Aa component (CHARA 252) was resolved in 2 of 4 observations.

16542-4151 = HD 152249 : We found a possible binary companion at a separation of 0".06 which needs confirmation.

16543-4149 = HD 152270 (WR 79) : The classification is from Seggewiss (1974).

16546-4125 = HD 152333 : The classification is from Schild et al. (1969).

16549-4031 = HD 152405 : Raboud (1996) finds the star to be a radial velocity variable.

16550-4109 = HD 152408 : Classification of the B component is from Lindroos (1985).

16551-4459 = HD 152386 : This Of star is assigned to the field in the LSC, but Turner (1979) argues that it belongs to an anonymous OB association related to the Cepheid, KQ Sco.

16551-4205 = HD 152424 : Fullerton (1990) finds radial velocity variations that suggest an orbit with a period greater than a month. Levato et al. (1988) also find radial velocity variations.

16562-4040 = HD 152623 : Fullerton (1990) discovered the short-period spectroscopic variation, and subsequently Wiemker (1992) showed that the spectral variations are best explained by the superposition of a stronger stationary component and a moving component. Thus, the speckle resolution of this system (CHARA 210) makes clear that this is (at least) a triple consisting of a short-period SB1 and a distant O star. The Hipparcos results (ESA 1997) confirm the CHARA 210 pair.

16563-4030 = HD 152622 : The classification is from Garrison et al. (1977).

16569-4031 = HD 152723 : This new binary is designated CHARA 254 Aa. Fullerton (1990) suggests that the A component is a single-lined spectroscopic binary with a period of about 12 and a semiamplitude of approximately 15 km/sec. Classifications of the B, C, and D components are from Lindroos (1985). Lindroos finds a distance of 2.0 kpc.

17039-3751 = HD 153919 (4U1700-377, V884 Sco) : This is a massive X-ray binary with a neutron star companion. The ellipsoidal variation is portrayed in a recent Hipparcos light curve (ESA 1997).

17065-3527 = HD 154368 : This "field" object may belong to the "CLUST 4 " group of Mel'nik & Efremov (1995). An ellipsoidal variation is present in the Hipparcos data (ESA 1997) with an unusually long period of 16.11.

17082-3500 = HD 154643 : This "field" object may belong to the "CLUST 4 " group of Mel'nik & Efremov (1995). The classification is from Garrison et al. (1977).

17173-3533 = HD 156134 : The classification is from McConnell & Bidelman (1976).

17175-2746 = HD 156212 : Levato et al. (1988) find the radial velocities to be "probably variable", but since the total range in 11 measurements is 33 km/sec we assign it to the "C" category.

17292-3132 = HD 158186 : The classification is from Garrison et al. (1977). An eclipsing light curve is presented in the Hipparcos Catalogue (ESA 1997) for a period of 8.77 d.

17347-3235 = HD 159176 : Our single observation appears to indicate a single star, so we cannot confirm the reported Iso 5 Aa pair. Nor did we detect the new Hipparcos Aa,D pair, presumably because of the large magnitude difference (H = 3.2). Classifications of the B and C components are from Lindroos (1985). Lindroos also notes a wider "X" component (V = 10.8, separation = 25", photometric classification = B5 IV) which he claims is physical. This component is not mentioned in the WDS. Lindroos finds a distance of 1.8 kpc.

17595-3601 = HD 163758 : Leep (1978) also finds a constant radial velocity.

18019-1906 = HD 164438 : We found a possible binary companion at a separation of 0".05 which needs confirmation. The classification is from Garrison et al. (1977).

18052-2424 = HD 165052 : The classification is from Morrison & Conti (1978).

18060-1412 = HD 165319 : The classification and distance are from Crampton & Fisher (1974).

18093-2359 = HD 165921 (V3903 Sgr) : The classification and orbit are from Niemela & Morrison (1988).

18152-2023 = HD 167263 (16 Sgr) : This new binary is designated CHARA 255 Aa. Garmany et al. (1980) observed a smoothly varying velocity indicating that the A component is probably a single-lined binary with a period of 11 d. Lindroos (1985) provided the classification of the B component and determines a distance of 1.2 kpc.

18170-1858 = HD 167659 : The 3 speckle observations all indicate a single star, so we cannot confirm the existence of a companion found by lunar occultation (Radick & Lien 1980).

18168-1631 = HD 167633 : Additional radial velocities are reported by Crampton & Fisher (1974). The star appears within the boundaries and at the same distance of Ser OB1 in the LSC.

18175-1828 = HD 167771 : The classification of the close spectroscopic pair is from Morrison & Conti (1978), and that of the B component of the optical pair is from Lindroos (1985). Lindroos also gives a distance of 2.0 kpc.

18181-1215 = HD 167971 : Leitherer et al. (1987) argue that this is a triple system consisting of a close eclipsing pair and a brighter, distant O star; the spectral classification presumably applies to the latter star.

18255-1241 = HD 169515 (RY Sct) : This massive binary and its surrounding gas torus are described by Gehrz et al. (1995). A light curve from Hipparcos is now available (ESA 1997). The system mass and the nature of the secondary are still controversial (Skulskii 1992; Skulskii & West 1993; Golovatyi & Skul'skii 1992). We found a possible binary companion at a separation of 0".2 which needs confirmation.

18582-2025 = HD 175876 : Classification of the B component is from Lindroos (1985), who also gives a distance of 1.9 kpc to the system.

19524+1840 = HD 188001 (9 Sge) : Aslanov et al. (1984), Underhill (1995), and especially Underhill & Matthews (1995) discuss a possible 78 orbital period for this system. Another period, 32.5, was found in photometric and radial velocity measurements by Aslanov & Barannikov (1992). However, because of the considerable scatter in the measurements plus evidence for wind related line profile variations (Fullerton 1990), we tentatively place the star in the "SB1?" category.

19584+3512 = HDE 226868 (Cyg X-1, V1357 Cyg) : This is a massive X-ray binary with a probable black hole companion (Gies & Bolton 1982).

20035+3602 = HD 190429 : The Aa component (McA 59) has been resolved in only 4 of 11 observations, and the positions are discrepant (the large errors presumably result from a large magnitude difference). The B and C components were also observed and appeared to be single. The classification of the B and C components are from Hoffleit et al. (1983).

20060+3547 = HD 190918 (WR 133) : The classification is from Wilson (1949). The classification of the B, D, and F components are from Hoffleit et al. (1983).

20074+3543 = HD 191201 : The classification and orbit are from Burkholder et al. (1997).

20126+4016 = HD 192281 : Barannikov (1993) suggests a possible, low amplitude orbit with a period of 5.5, but we have placed the star in the "C" category based on the constancy found by Gies & Bolton (1986).

20181+4044 = HD 193322 : The estimated period of the speckle binary orbit (CHARA 96 Aa) is 31. The orbit quality rating in Table 1 is our own. The system is currently unresolved with the Mt. Wilson Hooker telescope, but we continue to observe this target. The brighter star of the speckle pair is also a 311, single-lined spectroscopic binary (McKibben et al. 1997). The classifications of the C and D components are from Hoffleit & Warren (1991).

20189+3817 = HD 193443 : The classification is from Conti et al. (1977) and refers to the combined AB pair.

20205+4351 = HD 193793 (WR 140) : The classification is from Smith (1968).

20306+4419 = HD 195592 : The star is close to and probably associated with WR 140.

20521+3439 = HD 198846 (Y Cyg) : The classification is from Burkholder et al. (1997). This eclipsing binary is one of two known double-lined spectroscopic binaries which are a runaway objects based on a large absolute value of systemic velocity (Gies & Bolton 1986).

21079+3324 = HD 201345 : Aslanov et al. (1984) discuss the radial velocities and the possibility of a low mass companion.

21185+4357 = HD 203064 (68 Cyg) : Reports of small radial velocity variability (Alduseva et al. 1982; Hanni & Pelt 1988; Zeinalov et al. 1987; Musaev & Snezhko 1988) probably reflect the presence of line profile variations (Fullerton 1990).

21290+5844 = HD 204827 : The classification is from Garmany & Stencel (1992). The Hipparcos results (ESA 1997) confirm the CHARA 211 Aa pair.

21384+5658 = HD 206183 : The classification is from Garmany & Stencel (1992).

21390+5729 = HD 206267 : The classification and orbit are from Burkholder et al. (1997). Stickland (1995) found that the spectral line variations result from one close binary (with weak secondary lines) and a stationary component, a conclusion later confirmed by Burkholder et al. (1997). The speckle resolution of the system (CHARA 212 Aa) clearly supports the view that this is an SB2 plus a distant O star companion. The C and D components were also observed and appeared to be single. The classifications of the C and D components are from Hoffleit & Warren (1991).

21477+5942 = HD 207538 : The classification is from Conti et al. (1977).

22021+5800 = HD 209481 (LZ Cep) : The classification is from Conti & Alschuler (1971). Radial velocity and light curve solutions are given by Harries et al. (1997b).

22115+5925 = HD 210839 (Lambda Cep) : Radial velocities are also discussed by Gies & Bolton (1986) and Underhill (1995).

22469+5805 = HD 215835 (DH Cep) : The classification is from the UV tomographic analysis of Penny et al. (1997).

23111+5304 = HD 218915 : Aslanov et al. (1984) discuss the radial velocities and the possibility of a low mass companion. We found a possible binary companion at a separation of 0".08 which needs confirmation.