46 (10.3/11.0) Magnitudes given by (8) for this close pair (B = 10.1 and
/  47 10.7 respectively; LS region A chart) are consistent with LS mpg,
   47 while those in (47) (B = 10.8 and 10.2) are not. I have assumed that
   47 (47) interchanged identifications for these stars; that is, his stars
   47 19-4 and 19-5 have been taken to be LS stars 47 and 46, respectively.
   98 (7.5) Variations in the spectrum of this Wolf-Rayet star are
   98 discussed by O.C. Wilson, PASP, 60, 383-384 (1948)
   98 (=1948PASP...60.383W), and a flux-calibrated spectrum of this star to
   98 the Lyman limit is discussed in Mccandliss, et. al., ApJ, 416,
   98 372-378 (1993) (1993ApJ...416..372M). Howarth and Schmutz, AA, 294,
   98 529-535 (1995) (1995A&A...294..529H), reference no. (302), report a
   98 distance of 1.8 kpc for this star. Willis and Stevens (AA, 310,
   98 577-591, 1996) (1996A&A...310..577W) report on ROSAT X-ray
   98 observations of this star, concluding that the 0.28-keV X-ray
   98 emergent emission has a characteristic radius of > 1000 solar radii.
  120 (11.3) Simbad attributes tabulated data (which disagrees with LS mpg)
  120 to LS 120 via cross-reference of BD -08 1666. LS chart 5 shows two
  120 fairly bright stars (120 and 121) side-by-side. (40) remarks that
  120 this is a triple star.
  166 (7.4) Gies, et. al., ApJ, 422, 823 (1994) (=1994ApJ...422..823G)
  166 remark that this star is a spectroscopic binary with a period of
  166 6.0173 days. The companion has a mass ratio 0.23 + 0.04, and a
  166 magnitude difference 3.3 + 0.4.
  349 (10.2/10.3) These stars are respectively BD -20 1896 and -19 1896. LS
/ 422 cross-lists 349 as KN 25, for which (1) and (2) both report B = 9.8.
  422 Simbad attributes the data in (2) to LS 422, but (2) cross-references
  422 KN 25 as CPD -20 2314, which Simbad assigns to neither 349 or 422. I
  422 have assumed both observations refer to LS 349, and that the CPD
  422 reference in (2) is an error.
  414 (10.3) V= 9.2 - 9.6; P = 3.12 days.
  418 (6.0) HR 2855 = FY CMa. Long-term differential Stromgren photometry
  418 carried out by Sterken, Vogt, and Mennickent (AA, 311, 579-586, 1996)
  418 (1996A&A...311..579S) reveals a periodic photometric variation for
  418 this star with a period of 92.7.
  518 (8.6) High radial velocity due to galactic rotation.
  752 (11.5) (41) and (51) report B = 12.1 and 11.6 respectively. (51)
  752 cross-lists this star as CD -31 5034, which Simbad verifies; the
  752 finding chart appearing in (41) agrees with LS chart 18. Variable? LS
  752 notes emission.
  840 (10.1) (63) gives B = 10.7; four other references report B = 10.1.
  840 Probably misidentified by (63), whose data are not included. Not
  840 crowded on LS chart 17; LS notes l4686 emission.
  850 (4.1) Massa, et. al., ApJ, 452, 842-862 (1995) (=1995ApJ...452..842M)
  850 have studied the wind variability from this early-B supergiant.
  949 (2.0) Reported as variable by L.A. Balona, MNRAS, 254, 404-412, 1992.
  949 (=1992MNRAS.254..404B) Time-resolved echelle spectroscopy of this
  949 star is reported by Reid and Howarth (AA, 311, 616-630, 1996)
  949 (=1996A&A...311..616R), who find a period of 8.54 hours.
  952 (9.9) Apparently misidentified in (181), who gives B = 13.0, and may
  952 be referring to LS 951.
  984 (10.7) Probably misidentified by (11), whose data is not included.
  984 Appears to have a nearby companion of approximately equal magnitude
  984 on LS chart 21.
 1085 (5.1) An analysis of the interstellar lines in the spectrum of this
 1085 B3 III + B3 V binary is reported by Wallerstein, Vanture and Jenkins,
 1085 ApJ, 455, 590-597 (1995) (1995ApJ...455..590W). The two stars are
 1085 separated by 2700 AU, and the primary (= HD 72127A) is probably a
 1085 single-line spectroscopic binary with a B8 V companion.
 1111 (9.0) Adjacent to LS 1112 on LS chart 26; (1) may have measured both
 1111 together.
 1129 (10.6) Cross-listed by LS as KN 213 and CD -47 4273; LS gives no HD
 1129 listing. Simbad cross-lists LS 1129 as CD -47 4273 and CPD -47 2607
 1129 and also gives no HD listing. For KN 213, (1) and (2) report B = 9.3
 1129 and 8.6, respectively. KN 213 is listed as HD 74580 in (1), and as
 1129 CPD -47 2605 in (2). Simbad indicates that CPD -47 2605 and HD 74580
 1129 are the same star. LS chart 30 shows 1129 as the northeast component
 1129 of a double in a small cluster. Probably neither (1) or (2) refer to
 1129 "clean" measurements of the LS star.
 1149 (9.2) Discordant data from (168) (B=8.5) discarded.
 1227 (7.8) HD 77581 = GP Vel; this star is the optical counterpart of the
 1227 Vela X-1 X-ray source. Vankerkwijk, et. al., AA ,303, 483-496 (1995)
 1227 (1995A&A...303..483V) have obtained high-resolution, high
 1227 signal-to-noise spectra of this star, finding evidence for varying
 1227 tidal forces. 1268 (9.2) Noted as a-Cygni variable by Vangenderen,
 1227 et. al., AA, 264, 88-104 (1992) (1992A&A..264...88V).
 1358 (9.9) Double on LS chart 31.
 1362 (12.3) Central star of a planetary nebula; Heber., et. al., AA, 194,
 1362 223-229 (1988) (1988A&A...194..223H).
 1376 (10.0) V = 9.82 - 10.99
 1415 (10.1) Reference (48) reports B-V = 1.14 and a spectral type of B2
 1415 for this star, whereas numerous others give B-V ~ 0.4 and ~ O9 III.
 1415 Data from (48) discarded.
 1490 (11.3) V = 9.60 - 10.80
 1568 (10.1) Mean RV and standard deviation computed from four measures
 1568 reported by Feast, et. al., who note emission in various hydrogen
 1568 lines. Niemela (PASP, 84, 450, 1972) (1972PASP...84..450N) records
 1568 absorption-line velocities for this star ranging from -179 to +37
 1568 km/s, and concludes that it is probably a spectroscopic binary with a
 1568 period of a few days.
 1582 (11.2/10.1) LS cross-lists 1583 as KN 413, which (1) lists as HD
/1583 302841 and (2) as CPD -57 3265. Simbad concurs with this CPD
 1583 identification, and also lists 1583 as CD -57 3234, but attributes HD
 1583 302841 to LS 1582. Both stars reside in a crowded area in cluster IC
 1583 2581.
 1627 (10.3) Colors not appropriate for a B star; U-B may be missing a
 1627 negative sign in (96).
 1656 (12.0/8.3) LS misidentifies 1656 as HD 91824; 1657 is HD 91824. Data
/1657 in (1) and (2) attributed to HD 91824 is therefore assigned to LS
 1657 1657. LS 1657 is in NGC 3293.
 1670 (10.0) Lines broad and indications of doubling.
 1673 (9.1) In NGC 3293. Stephenson and Sanduleak indicate this star as
 1673 number 21 in the finding chart of Feast, MNRAS, 118, 618 (1958)
 1673 (1958MNRAS.118..618F). However, both (30) and (31) indicate that this
 1673 star is an M1 supergiant with B-V = 2.0. When precessed to 1875, the
 1673 coordinates of LS 1673 match very closely to those of CPD -57 3506,
 1673 which is star number 22 in Feast's chart, a B1 II star. I have
 1673 assumed that Stephenson and Sanduleak marked the wrong star; the data
 1673 given is that for number 22.
  679 (10.0) In NGC 3293. LS catalog gives no HD number for this star, but
  679 Simbad claims LS 1679 = HD 92007 = CPD -57 3527 = CD -57 3351. The HD
  679 catalog gives, for 92007, mpg = 9.1 and the same CPD number. B
  679 magnitudes reported by (1) and (2) for HD 92007 (8.4) are apparently
  679 too bright to be the LS star, and have been disregarded. (30) claims
  679 that 92007 and -57 3527 are separate (but nearby) stars in NGC 3293;
  679 his star number 27 (B = 9.0), which he claims to be CPD -57 3527, is
  679 clearly LS 1679 in the LS charts; similarly for (31). I suspect that
  679 92007 and CPD -57 3527 are different objects, and take star 27 in
  679 (30) and (31) to be LS 1679.
 1682 (10.0) Spectra show some signs of line doubling.
 1683 (10.6) Indications of line doubling; probably a binary.
 1688 (8.8) HD 92044. Also in NGC 3293; misidentified by LS as HD 92025.
 1688 Correctly identified in (30) and (31).
 1689 (8.0) HD 92025. Misidentified by LS as HD 92007.
 1697 (8.2) Misidentified in (14) as HD 92209. Brightest star in group at
 1697 center of IC 2599.
 1774 (10.2) (149) and (171) give an incorrect HD number (302989) for this
 1774 star.
 1780 (9.1) HD 305439. Double in LS region D chart. (45) notes variability.
 1801 (9.7) Simbad cross-identifies this star as HD 93026, CPD -58 2594, CD
 1801 -58 3518, and as star 35 in Bochum 10. (9) identifies their star 13
 1801 (B = 11.4) as LS 1801, but this disagrees with the LS region D chart;
 1801 star 13 lies just SW of 1801; (89) also gives B = 11.4. (171)
 1801 identifies their star 35 (B = 9.7) as HD 93026, but this also
 1801 disagrees with the LS chart; their number 39 (B = 11.4) would appear
 1801 to be LS 1801. On the LS chart, 1801 appears comparable in brightness
 1801 to 1790, which has B = 10.8. The LS catalog agrees with the Simbad CD
 1801 cross-reference, but lists no HD number; Simbad lists only the UBV
 1801 data from (171). I have assumed that (9) mis-labeled their finding
 1801 chart, and that star 39 of (171) is LS 1801. The data given in the
 1801 compilation are for star 13 of (9), star 39 of (171), and LS 1801 as
 1801 reported by (89). Identification as HD 93026 must be regarded as
 1801 uncertain.
 1811 (8.6) Note that (61) is discordant.
 1820 (8.2) HD 93128. Some observers give B = 7.2 and others B = 10.0 for
 1820 this crowded star (LS 1819 is 3 sec West/10" South).
 1839 (7.5) Possibly an eclipsing variable.
 1855 (10.0) LS erroneously cross-lists this star as RT Car. LS 1855 and RT
 1855 Car are respectively numbers 15 and 16 in (32).
 1872 (8.6) Appears double on LS region E chart.
 1872
 1881 (7.6) Extensive wings on the short wavelength side of each stellar
 1881 line; suspected binary.
 1973 (8.1) Data from (95) (B=10.8) not included. In LS h Car region chart.
 2008 (10.3) Cross-referenced by Simbad as both CPD -58 2840 and 2839.
 2018 (11.6) Central star of a planetary nebula; Heber., et. al., AA, 194,
 2018 223-229 (1988) (=1988A&A...194..223H).
 2035 (8.2) Recorded radial velocity calculated from absorption line
 2035 velocities.
 2062 (10.3) HD 305757 = CPD -59 2901. (1) reports B = 11.6 whereas (83)
 2062 and (85) give B = 10.8. The LS chart (h Car region) appears to agree
 2062 with that in (83); the CPD number reported in (1) agrees with Simbad.
 2062 Probably misidentified by (1), whose data are not included.
 2138 (11.3) HD 303776; misidentified by LS as HD 96286 ( = LS 2141), which
 2138 is 2 degrees away.
 2183 (7.8) As LS 949.
 2212 (7.7) As LS 949; possible unresolved binary.
 2234 (9.5) HD 306183 = CPD -60 2647. (160) lists these as two separate
 2234 stars; the data reported for CPD -60 2647 (adopted here) is
 2234 consistent with that given for LS 2234 by (9) and (93). Data reported
 2234 for HD 306182 by (160) likely erroneous.
 2244 (9.7) HD 306185 = CPD -60 2671. As in LS 2234 above, (160) lists
 2244 these as two separate stars; the data reported for CPD -60 2671 is
 2244 consistent with that reported in (9) and (103). Data reported by
 2244 (160) for HD 306185 is likely erroneous; note that (103) reports CPD
 2244 -60 2671 as double.
 2258 (9.3) Berdnikov and Turner, Ast. Lett., 21, 603-632 (1995)
 2258 (=1995AstL...21..603B) report a period of 4.43 days for this Cepheid.
 2364 (8.1) Probably unresolved double-lined binary.
 2372 (8.4) Misidentified as HD 100277 in (4); actually HD 100242.
 2424 (7.3) As LS 949.
 2425 (8.8) As LS 949.
 2428 (8.8) Probably misidentified by (85) (B=7.4), whose data are not
 2428 included.
 2430 (9.9) Suspected binary.
 2462 (10.2) Probably misidentified by (84) (B=8.8) whose data are not
 2462 included.
 2513 (10.5) Errata in (34); correct data given here.
 2557 (10.3) The kinematics of this high velocity star are discussed by
 2557 Kilkenny (Observatory, 94, 4, 1974) (1974Obs....94....4K).
 2564 (11.7) As 2513.
 2645 (11.9) (45) and (82) report B = 10.2 and 11.9 respectively. (45)
 2645 remarks that the fainter of two stars at this position was measured;
 2645 his colors are not indicative of an OB star. Data from (45) are not
 2645 included.
 2800 (10.2/10.9) In NGC 4755. Comparing LS and (152) finding charts
/2802 indicates that 2800 and 2802 are respectively stars G and K of (152),
 2802 whereas Simbad, (140) and (107) indicate G = 2802. Simbad further
 2802 suggests LS 2806 = H of (152). I have taken G = 2800 and K = 2802. LS
 2802 2806 is apparently star IV-18 of (152). (314) notes LS 2800 as a b
 2802 Cep variable.
 2803 (6.7) uvby colors given by (66) for HR 4890 (= LS 2813) correspond to
 2803 those of LS 2803 according to other sources; data from (66) therefore
 2803 attributed to LS 2803 = HR 4887. In NGC 4755.
 2810 (11.2) Apparently star III-1 of (152), an identification with which
 2810 (107) and (140) agree, despite their B magnitudes disagreeing with LS
 2810 mpg. Crowded field in NGC 4755. Cross-referenced by Simbad as CPD -59
 2810 4549. (314) notes LS 2810 as a b Cep variable.
 2813 (6.7) See comments for 2803.
 2814 (9.2) Misidentified by (107) and (140) as star III-5 of (152);
 2814 actually star II-1. Simbad mistakenly attributes data for star II-3
 2814 from (107) to LS 2814, and data from II-1 of (107) to LS 2815. In NGC
 2814 4755. Possible spectroscopic binary in view of large radial velocity
 2814 range.
 2816 (9.8) Noted by (314) as a b Cep variable. Possible spectroscopic
 2816 binary in view of large radial velocity range.
 2883 (10.9) Johnston, et. al. (MNRAS, 268, 430-436, 1995)
 2883 (=1995MNRAS.268..430J) note that LS 2883 is the binary companion of a
 2883 pulsar, PSR B1259-63, one of only two binary pulsars known (at that
 2883 writing) where the companion mass exceeds 3 solar masses. The orbital
 2883 period is 1236.79 days, projected semi-major axis 1295.98
 2883 light-seconds, and eccentricity 0.8698. The pulsar period is 47.76
 2883 ms. In a subsequent paper, these authors (MNRAS, 279, 1026-1036,
 2883 1996) (=1996MNRAS.279.1026J) measured the magnetic field of LS 2883
 2883 to be approximately 40 mG at 45 stellar radii, the first direct
 2883 measurement of the magnetic field of a Be-star disk.
 2946 (9.7) Uncrowded on LS chart 46. Typographical error in (2)? (45)
 2946 notes uncertain photometry.
 2998 (8.2) Probably misidentified by (158) (B = 6.9), whose data are not
 2998 included.
 3024 (9.4) Berdnikov and Turner, Ast. Lett., 21, 603-632 (1995)
 3024 (=1995AstL...21..603B) report a period of 6.46 days for this Cepheid.
 3114 (11.6) Only absorption-line values are used in computing the recorded
 3114 radial velocity; one discordant observation discarded.
 3231 (6.0) HX Lup.
 3247 (10.0) Velocity -90 km/s when corrected for solar motion and galactic
 3247 rotation. Very similar to HD 119069 in terms of longitude, spectral
 3247 type, radial velocity and distance.
 3328 (8.9) (46) indicates V = 9.39 and B-V = 0.34; six other references
 3328 give V = 8.2, B-V = 1.0. Simbad does not verify the HD and CD numbers
 3328 quoted in LS (134959, -58 5973). (45) suspects variability, (7) and
 3328 (36) note emission. Not clearly marked on LS chart 51; crowded with
 3328 3327. Turner, AJ, 111, 828-833 (1995) (1995AJ....111.828T) concludes
 3328 that this star is a B2 Ia-O hypergiant of absolute magnitude Mv =
 3328 -7.88 + 0.66.
 3331 (5.0) Delta Circinus.
 3403 (9.7) Magnitudes given by both (27) and (45) disagree with LS mpg;
 3403 colors in (27) do not correspond to an OB star. Clearly marked on LS
 3403 chart 48.
 3404 (11.7) This star, along with 3405, 3420, 3421, 3424, 3429, 3430,
 3404 3432, and 3433 are all members of the Norma group. Mean radial
 3404 velocity for the system is -36 + 6 km/s after correction for solar
 3404 motion.
 3422 (11.2) Cross-listed by LS as KN 1028 = CPD -55 6802, for which (1)
 3422 gives B = 11.4 and (2) B = 8.9. Note that (2) refers to CPD -54 6802,
 3422 which Simbad does not cross-list as an LS star. Probably
 3422 misidentified in (2), whose data are not included.
 3601 (10.3) Misidentified as LS 3106 by (4).
 3646 (6.8) As LS 949.
 3655 (12.0) LS magnitude favors (10); crowded on Fig. 12 of (10) and on LS
 3655 chart 55.
 3674 (12.4) LS magnitude favors (183), who notes this star as spectral
 3674 class K. Too faint to see on LS chart 55.
 3690 (8.8) (1) and (2) give B = 9.1; (27) gives B = 7.6. Probably
 3690 misidentified by (27), whose data are not included.
 3719 (9.6) Cross listed in LS as KN 1195 = CPD -47 7860, for which (1)
 3719 gives B = 9.9 and (2) B = 10.5. Simbad tabulates no UBV. Note that
 3719 (2) refers to CPD -47 7858. Probably misidentified by (2), whose data
 3719 are not included.
 3728 (11.3) LS mpg favors (124).
 3733 (11.8) As 3728.
 3745 (7.0) Note that B-V from (115) is about equal to the negative of
 3745 other B-V values.
 3765 (7.3) As LS 949.
 3785 (6.6) LS chart 60 indicates a rather faint star; probably intended to
 3785 be the bright star just northeast of that marked.
 3791 (9.3) Cross-listed as KN 1221 and HD 152042 by LS; by Simbad as HD
 3791 326305. (1), (2), and (122) give B = 8.3, and (111) and (117) B =
 3791 10.2. LS chart 60 designates 3791 as the south-western, fainter
 3791 member of a close pair, favoring identification as HD 326305
 3791 according to coordinates given in Simbad.
 3794 (8.8) HD 152076. (111, 117, 122, 126) give B = 8.7, (124) B = 11.2.
 3794 (124) remarks that LS cross-reference the wrong HD star (152076), and
 3794 that they measured the star marked on the LS chart 60 some 2 minutes
 3794 north of 152076. LS mpg suggests that Stephenson and Sanduleak had HD
 3794 152076 in mind. Data from (124) are not included.
 3804 (8.6) Noted as possibly variable by (122).
 3828 (6.0) As LS 949.
 3829 (6.7) As LS 949.
 3850 (6.7) Short period (0.61470 days) velocity changes.
 3854 (7.0) Blended with LS 3853 on LS chart T.
 3899 (6.8) As LS 949.
 3918 (9.8) Visual and uvby photometry and spectroscopy for this P-Cygni
 3918 star spanning 10 years has been reported by Sterken, Stahl, Wolf,
 3918 Szeifert and Jones [AA 303, 766-772 (1995) (=1995A&A...303..766S)].
 3918 Large-amplitude variations are present, indicating that this
 3918 hydrogen-deficient, N-rich star is on its way to becoming a WN star.
 3926 (9.6) (27) gives B = 10.4, and (45) B = 7.9. On LS chart 67, 3926
 3926 appears about as bright as LS 4044, for which many references agree B
 3926 = 8.4.
 3982 (6.6) WN star; HR 6392. Bright Star Catalog indicates this star as
 3982 V915 Sco, with DV = 0.15. LS 3982 is the primary of a triple system.
 3995 (6.8) As LS 949; discovered to be an eclipsing binary by L.A. Balona,
 3995 MNRAS, 254, 404-412 (1992) (=1992MNRAS.254..404B).
 4018 (7.4) Possible unresolved double-lined binary.
 4080 (12.5/12.1) Close pair enveloped in nebulosity. (119) remarks that
 4080 both were measured together; his observation dropped.
 4142 (11.6) Reddened; double on LS chart 64.
 4200 (11.7) Close double with LS 4199 on LS chart 67.
 4275 (11.2) A spectographic investigation by Niemela, et. al. [Rev. Mex.
 4275 Astron. Astrofis., 31, 45-49 (1995) (=1995RMxAA..31...45N)] reveals
 4275 this star to be an O6 + WN binary system with an orbital period of
 4275 12.595 days.
 4293 (11.3) Presumed to be star 3 in Ruprecht 127 in (10), not star 2.
 4293 Crowded field on LS chart 64.
 4352 (9.4) (45) claims that this star is not CPD -28 13519; but Simbad
 4352 concurs with the CPD identification. Colors reported in (45) are not
 4352 those of an OB star.
 4420 (12.2) B magnitudes reported by (27) and (124) fall equidistant from
 4420 LS mpg.
 4893 (10.2) (10) reports B = 10.4, (27) B = 10.8, and (39), (60), and
 4893 (161) B = 11.1. LS mpg favors (10), whose finding chart appears to
 4893 agree with LS region Y chart. (39, 60, 161) may have measured star
 4893 number 4 of (10) (V = 10.40), immediately adjacent to LS 4893.
 4910 (10.9) In NGC 6611. (39) reports V = 10.1, B-V = 0.8; four other
 4910 references give V = 9.6, B-V = 0.85. (45) suspects this crowded star
 4910 may be variable. I have assumed that (39) is referring to LS 4905,
 4910 also mpg = 10.9.
 4919 (9.7)  Variable?
 4954  (9.5)  See remarks for 1268.
 4956 (9.5)  See remarks for 1268.
 5077 (8.0)  Catacylsmic binary; V = 9.5 - 13.6.  Herbig, et. al. (ApJ,
 5077 141, 617, 1965) have carried out a detailed spectroscopic analysis;
 5077 Simon (AA, 309, 775-776, 1996) reports possible period changes based
 5077 on observations spanning 31 years.