46/ 47 (10.3/11.0) Magnitudes given by Moffat et al. (1975A&AS...20...85M) 46/ 47 for this close pair (B=10.1 and 10.7 respectively; LS region A 46/ 47 chart) are consistent with LS mpg, while those in Haug 46/ 47 (1970A&AS....1...35H) (B=10.8 and 10.2) are not. I have assumed 46/ 47 that Haug (1970A&AS....1...35H) interchanged identifications for 46/ 47 these stars; that is, his stars 19-4 and 19-5 are taken to be 46/ 47 LS stars 47 and 46, respectively. 47 See 46 98 (7.5) Variations in the spectrum of this pathological Wolf-Rayet 98 star (EZ CMa) are discussed by O.C. Wilson (1948PASP...60..383W) 98 and a flux-calibrated spectrum of this star to the Lyman limit is 98 discussed in McCandliss et al., 1993ApJ...416..372M. Howarth and 98 Schmutz, 1995A&A...294..529H, reference (302), report a distance of 98 1.8kpc for this star. Willis and Stevens (1996A&A...310..577W) 98 report on ROSAT X-ray observations of this star, concluding that 98 the 0.28-keV X-ray emergent emission has a characteristic radius 98 of >1000_{sun}_. Harries, Howarth, Schulte-Ladbeck and Hillier 98 (1999MNRAS.302..499H) report that the continuum polarization of 98 this star shows long-term quasi-periodic variations in both 98 magnitude and position. 120 (11.3) Simbad attributes tabulated data (which disagrees with LS 120 mpg) to LS 120 via cross-reference of BD-08 1666. LS chart 5 120 shows two fairly bright stars (120 and 121) side-by-side. Racine 120 (1968AJ.....73..233R) remarks that this is a triple star. 166 (7.4) Gies et al., 1994ApJ...422..823G, remark that this star is a 166 spectroscopic binary with a period of 6.0173 days. The companion 166 has a mass ratio 0.23+/-0.04, and a magnitude difference 3.3+/-0.4. 349/ 422 (10.2/10.3) These stars are respectively BD-20 1896 and BD-19 1896. 349/ 422 LS cross-lists 349 as KN 25, for which Klare & Neckel 349/ 422 (1977A&AS...27..215K) and Schild et al. (1983ApJS...51..321S) both 349/ 422 report B=9.8. Simbad attributes the data in Schild et al. 349/ 422 (1983ApJS...51..321S) to LS 422, but Schild et al. 349/ 422 (1983ApJS...51..321S) cross-references KN 25 as CPD-20 2314, which 349/ 422 Simbad assigns to neither 349 or 422. I have assumed both 349/ 422 observations refer to LS 349, and that the CPD reference in Schild 349/ 422 et al. (1983ApJS...51..321S) is an error. 414 (10.3) V=9.2-9.6; P=3.12days. 418 (6.0) HR 2855=FY CMa. Long-term differential Stromgren photometry 418 carried out by Sterken, Vogt, and Mennickent (1996A&A...311..579S) 418 reveals a periodic photometric variation for this star with a 418 period of 92.7days. 422 See 349 437 (12.1) High mass X-ray binary. See Steiner et al. 437 (1984ApJ...280..688S) 518 (8.6) High radial velocity due to galactic rotation. 675 (7.7) Variability in Hipparcos photometry (max. range 0.12mag) 675 discussed by van Leeuwen et al., 1998A&AS..128..117V. 752 (11.5) Miller & McCarthy (1974AJ.....79.1294M) and Turner 752 (1977AJ.....82..805T) report B=12.1 and 11.6 respectively. Turner 752 (1977AJ.....82..805T) cross-lists this star as CD-31 5034, which 752 Simbad verifies; the finding chart appearing in Miller & McCarthy 752 (1974AJ.....79.1294M) agrees with LS chart 18. Variable? 752 LS notes emission. 840 (10.1) Havlen (1972A&A....17..413H) gives B=10.7; four other 840 references report B=10.1. Probably misidentified by Havlen 840 (1972A&A....17..413H), whose data are not included. Not crowded on 840 LS chart 17; LS notes {lambda}4686 emission. 850 (4.1) Massa et al., 1995ApJ...452..842M, have studied the wind 850 variability from this early-B supergiant. See also S.R. Colley, 850 2003Obs...123...96C. 949 (2.0) Reported as variable by L.A. Balona, 1992MNRAS.254..404B. 949 Time-resolved echelle spectroscopy of this star is reported by Reid 949 and Howarth (1996A&A...311..616R), who find a period of 8.54 hours, 949 with evidence of non-radial pulsation. van der Hucht et al., 949 1997NewA....2..245V, report a distance of 429 (-77) (+120)pc for 949 this star based on Hipparcos parallax measurements, and conclude 949 that it is located at the back of the Gum nebula. See also Schaerer 949 et al., 1997ApJ...484L.153S. Blomme et al. (Hot Star Newsletter 949 No. 77, July 2003) present radio and submillimeter observations of 949 this star and discuss structure in the outer region of its wind. 952 (9.9) Apparently misidentified in Orsatti (1992AJ....104..590O), who 952 gives B=13.0, and may be referring to LS 951. 980 (1.6) van der Hucht et al., 1997NewA....2..245V, report a distance 980 of 258 (-31) (+41) pc for this (WC8+O7.5-8 III-II) binary based on 980 Hipparcos parallax measurements, and conclude that it is a 980 foreground object before the open cluster Cr173 and the association 980 Vel OB2. Absolute visual magnitudes of -3.7 for the WC8 star and 980 -5 for the O star are derived; they conclude that the latter 980 indicates an O8.5 III star, as opposed to the O9 I that had 980 previously been assumed. This star is one of the ionizing sources 980 of the Gum nebula. See also Schaerer, et al., 1997ApJ...484L.153S, 980 who report a system mass of 29.5+/-15.9M_{sun}_, an effective 980 temperature of 34000+/-1500K for the O-star, and a luminosity of 980 logL=5.3+/-0.15 for the O-star. Eversberg et al. 980 (1999PASP..111..861E) report low-resolution, high signal-to-noise 980 ratio spectropolarimetry of this system, remarking that it has 980 the potential to represent a prototype of wind-wind interaction 980 for massive stars. 984 (10.7) Probably misidentified by Reed (1990AJ....100..737R and 1990, 984 AJ, 100, 988), whose data is not included. Appears to have a nearby 984 companion of approximately equal 984 magnitude on LS chart 21. 992 (12.9) Motch et al. (1997A&A...323..853M) classify this star as a 992 likely massive X-ray binary. 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 1995ApJ...455..590W. The two stars are separated by 2700AU, 1085 and the primary (= HD 72127A) is probably a single-line 1085 spectroscopic binary with a B8 V companion. 1111 (9.0) Adjacent to LS 1112 on LS chart 26; Klare & Neckel 1111 (1977A&AS...27..215K) may have measured both together. 1113 (5.0) Variability in Hipparcos photometry (max. range 0.06mag) 1113 discussed by van Leeuwen et al., 1998A&AS..128..117V. 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, Klare & Neckel 1129 (1977A&AS...27..215K) and Schild et al. (1983ApJS...51..321S) 1129 report B=9.3 and 8.6, respectively. KN 213 is listed as HD 74580 1129 in Klare & Neckel (1977A&AS...27..215K) and as CPD-47 2605 in 1129 Schild et al. (1983ApJS...51..321S). Simbad indicates that 1129 CPD-47 2605 and HD 74580 are the same star. LS chart 30 shows 1129 1129 as the northeast component of a double in a small cluster. Probably 1129 neither Klare & Neckel (1977A&AS...27..215K) or Schild et al. 1129 (1983ApJS...51..321S) refer to "clean" measurements of the LS star. 1135 (11.2) Corti et al. (2003A&A...405..571C) find that this star is a 1135 short-period (2.75 days) O-type binary. 1149 (9.2) Discordant data from Cousins & Stoy (1962RGOB...64..103C) 1149 (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. (1995A&A...303..483V) 1227 have obtained high-resolution, high signal-to-noise spectra of this 1227 star, finding evidence for varying tidal forces. 1268 (9.2) Noted as alpha-Cygni variable by Van genderen et al., 1268 1992A&A...264...88V. Variability in Hipparcos photometry (max. 1268 range 0.20mag) discussed by van Leeuwen et al., 1998A&AS..128..117V 1358 (9.9) Double on LS chart 31. 1362 (12.3) Central star of a planetary nebula; Heber et al., 1362 1988A&A...194..223h. 1376 (10.0) V=9.82-10.99 1411 (9.9) Oudmaijer et al. (1998MNRAS.300..170O) report that this Be 1411 system possesses a fast wind in excess of 1000km/s, with 1411 polarization changes across H-alpha. They conclude that the system 1411 consists of a fast polar wind from the star and a slowly 1411 expanding disk wind. 1415 (10.1) Reference (48) reports B-V=1.14 and a spectral type of B2 for 1415 this star, whereas numerous others give B-V=0.4 and O9 III. Data 1415 from (48) discarded. 1490 (11.3) V=9.60-10.80 1523 (9.6) A long-term multiwavelength spectrophotometric study of the 1523 Luminous Blue Variables (LBV's) HR Car (= LS 1523) and AG Car 1523 (= LS 2035) by Shore, Altner and Waxin (1996AJ....112.2744S) 1523 reveals them both to have luminosities on the order of 1523 10^6^L_{sun}_ with evidence of dust formation in the AG Car wind 1523 during the most recent outburst. 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 (1972PASP...84..450N) records absorption-line 1568 velocities for this star ranging from -179 to +37km/s, and 1568 concludes that it is probably a spectroscopic binary with a period 1568 of a few days. 1582/ 1583 (11.2/10.1) LS cross-lists 1583 as KN 413 [which Klare & Neckel 1582/ 1583 (1977A&AS...27..215K) lists as HD 302841] and Schild et al. 1582/ 1583 (1983ApJS...51..321S) as CPD-57 3265. Simbad concurs with this CPD 1582/ 1583 identification, and also lists 1583 as CD-57 3234, but attributes 1582/ 1583 HD 302841 to LS 1582. Both stars reside in a crowded area in 1582/ 1583 cluster IC 2581. 1583 See 1582 1627 (10.3) Colors not appropriate for a B star; U-B may be missing a 1627 negative sign in Loden (1973A&AS...10..125L). 1656/ 1657 (12.0/8.3) LS misidentifies 1656 as HD 91824; 1657 is HD 91824. Data 1656/ 1657 in Klare & Neckel (1977A&AS...27..215K) and Schild et al. 1656/ 1657 (1983ApJS...51..321S) attributed to HD 91824 is assigned to 1656/ 1657 LS 1657. LS 1657 is in NGC 3293. 1657 See 1656 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, 1958MNRAS.118..618F. 1673 However, both Feinstein & Marraco (1980PASP...92..266F) and Turner 1673 et al. (1980AJ.....85.1193T) indicate that this star is an M1 1673 supergiant with B-V=2.0. When precessed to 1875, the coordinates of 1673 LS 1673 match very closely to those of CPD-57 3506, which is star 1673 number 22 in Feast's chart, a B1 II star. I have assumed that 1673 Stephenson and Sanduleak marked the wrong star; the data given is 1673 that for number 22. 1679 (10.0) In NGC 3293. LS catalog gives no HD number for this star, but 1679 Simbad claims LS 1679 = HD 92007 = CPD-57 3526 = CD-57 3350 = 1679 Feast (1958MNRAS.118..618) no. 27 (B=9.0). Feast identifies his 1769 no. 27 (B=9.0) as CPD-57 3527 and his no. 6 (B=8.3) as HD 92007. 1769 The HD catalog gives m_pg_=9.1 for HD 92007, favoring 1769 identification with Feast no. 27, but also cross-lists this star 1769 as CPD-57 3527. Feast no. 27 has been noted as a Beta Cep variable. 1769 Comparing charts from Feast and the LS catalog shows that Feast's 1769 no. 27 is clearly LS 1679 [see also chart in Feinstein and Marraco 1769 (1980PASP...92..266F)]. Klare & Neckel (1977A&AS...27..215K) claim 1769 that HD 92007=Hbg 435; they and Schild et al. (1983ApJS...51..321S) 1769 give B 8.4 for this star; their data disregarded in view of this 1769 confusion. Data for HD 92007 in Hoffleit (1956ApJ...124...61H) 1769 likewise disregarded. I take Feast no. 27 to be LS 1679; 1679 Feast no. 6 is designated here as ALS 15752. No cross-reference 1679 information is included for either star. ALS 15751 is Feast no. 26. 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 (=LS 1689). Correctly identified in Feinstein and Marraco 1688 (1980PASP...92..266F) and Turner et al. (1980AJ.....85.1193T). 1688 Misidentified as HD 92007 in Klare & Neckel (1977A&AS...27..215K) 1689 (8.0) HD 92025. Misidentified by LS as HD 92007. 1697 (8.2) Misidentified in Vogt & Moffat (1975A&A....45..405V) as 1697 HD 92209. Brightest star in group at center of IC 2599. 1698 (12.2) Motch et al. (1997A&A...323..853M) classify this star as a 1698 likely massive X-ray binary. 1774 (10.2) FitzGerald & Mehta (1987MNRAS.228..545F) and Feinstein 1774 (1981PASP...93..202F) give an incorrect HD number (302989) for 1774 this star. 1780 (9.1) Double in LS region D chart. Drilling (1991ApJS...76.1033D) 1780 notes variability. 1801 (9.7) Simbad cross-identifies this star as HD 93026, CPD-58 2594, 1801 CD-58 3518, and as star 35 in Bochum 10. Moffat & Vogt 1801 (1975A&AS...20..125M) identifies their star 13 (B=11.4) as LS 1801, 1801 but this disagrees with the LS region D chart; star 13 lies just 1801 SW of 1801; Forte (1976A&AS...25..271F) also gives B=11.4. 1801 Feinstein (1981PASP...93..202F) identifies their star 35 (B=9.7) as 1801 HD 93026, but this also disagrees with the LS chart; their 1801 number 39 (B=11.4) would appear to be LS 1801. On the LS chart, 1801 1801 appears comparable in brightness to 1790, which has B=10.8. 1801 The LS catalog agrees with the Simbad CD cross-reference, but lists 1801 no HD number; Simbad lists only the UBV data from Feinstein 1801 (1981PASP...93..202F). I have assumed that Moffat & Vogt 1801 (1975A&AS...20..125M) mis-labeled their finding chart, and that 1801 star 39 of Feinstein (1981PASP...93..202F) is LS 1801. The data 1801 given in the compilation are for star 13 of Moffat & Vogt 1801 (1975A&AS...20..125M), star 39 of Feinstein (1981PASP...93..202F), 1801 and LS 1801 as reported by Forte (1976A&AS...25..271F). 1801 Identification as HD 93026 must be regarded as uncertain. 1811 (8.6) Note that Deutschman et al. (1976ApJS...30...97D) is 1811 discordant. 1820 (8.2) Crowded in the Tr 14/16 complex; (LS 1819 is 3 sec West/10" 1820 South). Resolved as binary (separation 0.055 arcsec, {Delta}m=0.9) 1820 by Nelan et al. (2004AJ....128..323N). 1839 (7.5) Possibly an eclipsing variable. 1849 (8.5) Morrell et al. (2001MNRAS.326...85M) report the results of 1849 high-quality orbital-element analysis for this double-lined O3V+O8V 1849 binary, deriving a semi-amplitude of 133+/-2 and 314+/-2km/s for 1849 each binary component. If the O3 component has a mass of 1849 22-25M_{sun}_, the mass of the O3 primary is derived to be 1849 52-60M_{sun}_. The inclination of the orbital plane is estimated 1849 to be 55 degrees. 1855 (10.0) LS erroneously cross-lists this star as RT Car. LS 1855 and 1855 RT Car are respectively numbers 15 and 16 in Feinstein et al. 1855 (1980AJ.....85..708F). 1868 (9.5) Eta Carinae. Damineli, Conti, and Lopes (1997NewA....2..107D) 1868 suggest that Eta Car may in fact be a binary system of high 1868 eccentricity. Ebbets et al. (1997ApJ...489L.161E) report that 1868 high-quality spectra of Eta Car between 1203 and 1765 Angstrom 1868 obtained with the GHRS reveal a morphology suggesting a composite 1868 of features seen in B-type supergiants in the range B2 Ia to B8 Ia, 1868 with additional lower temperature lines also seen. Davidson and 1868 Humphreys review Eta Car and its environment in an extensive paper 1868 appearing in 1997ARA&A..35....1D. Davidson et al. 1868 (1998NewA....3..241D) point out that an 85-day periodicity in the 1868 X-ray emission of Eta Car has been reported, while spectroscopic 1868 events recur with a period of 5.5 years, and suggest that if the 1868 X-rays are produced by colliding winds in a 5.5-year binary system, 1868 then the 85-day period may represent pulsation or rotation of the 1868 primary star, or conceivably the orbit of a third object. 1868 Janot Pacheco et al. (1999A&AS..137..407J) present photometric data 1868 and high-resolution, high signal-to-noise optical spectra of 1868 Eta Car, finding evidence for multiperiodic variations, 1868 specifically, frequencies of 1.29, 1.78, 3.82, and 4.51cy/day. 1868 Damineli et al. (2000ApJ...528L.101D) report confirmation of the 1868 binary nature of Eta Car, with a periodicity of 2020+/-5 days, 1868 arguning for a colliding wind binary scenario that rules out 1868 multiple shell ejection. Martin and Koppelman (2004AJ....127.2352M) 1868 present HST observations of the central star. 1869 (8.9) Resolved as binary (separation 0.015 arcsec, {Delta}m=1.0) 1869 by Nelan et al. (2004AJ....128..323N). 1870 (10.0) Resolved as binary (separation 70 arcsec, {Delta}m=1.6) by 1870 Nelan et al. (2004AJ....128..323N). 1871 (10.4) Analysis of high-resolution spectra by Freyhammer et al. 1871 (873) show this system to be a detached eclipsing binary. They 1871 classify the syatem as O9.5V+B0.3V, and estimate a distance of 1871 2.6+/-0.1kpc, an age of 2Myr, and a photometric period of 1871 1.47 days. Member of Trumpler 16. 1872 (8.6) Appears to be the northeast component of a double on LS region 1872 E chart. A larger-scale chart of this area around Eta Car is given 1872 by Feinstein, Marraco, & Muzzio (1973A&AS...12..331F). Comparing 1872 their chart to the LS chart appears to indicate that 1872 FMM 34=LS 1872; the other component of the double is HD 93343 1872 according to their chart. Both are OB stars. I designate HD 93343 1872 as ALS 16717. Simbad cross-lists LS 1872 as HD 93343. 1881 (7.6) Extensive wings on the short wavelength side of each stellar 1881 line; suspected binary. 1932 (7.2) Prinja, Massa, Howarth, and Fullerton (1998MNRAS.301..926P) 1932 report results of a 28-day IUE time-series campaign to monitor the 1932 stellar wind of this O5 giant, finding repeatability in the wind 1932 structures with a 7.1-day period. 1964 (13.1) Niemela and Gamen (2000A&A...362..973N) rerport that this 1964 object is a double-lined WN+O binary with a aperiod 1964 of 3.16415 days. 1973 (8.1) Data from (95) (B=10.8) not included. In LS theta Car 1973 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., 2018 1988A&A...194..223H. 2033 (9.4) Variability in Hipparcos photometry (max. range 0.2mag) 2033 discussed by van Leeuwen et al., 1998A&AS..128..117V. 2035 (8.2) AG Car. See 1523 above. Recorded radial velocity calculated 2035 from absorption line velocities. 2062 (10.3) HD 305757=CPD-59 2901. 2035 Klare & Neckel (1977A&AS...27..215K) reports B=11.6 whereas 2035 Lynga & Wramdemark (1973A&AS...12..365L) and Humphreys 2035 (1973A&AS....9...85H) give B=10.8. The LS chart (theta Car region) 2035 appears to agree with that in Lynga & Wramdemark 2035 (1973A&AS...12..365L); the CPD number reported in Klare & Neckel 2035 (1977A&AS...27..215K) agrees with Simbad. Probably misidentified 2035 by Klare & Neckel (1977A&AS...27..215K) whose data are not included 2138 (11.3) HD 303776; misidentified by LS as HD 96286 (=LS 2141), 2138 which 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. Johansson (1980A&AS...41...43J) lists 2234 these as two separate stars; the data reported for CPD-60 2647 2234 (adopted here) is consistent with that given for LS 2234 by 2234 Moffat & Vogt (1975A&AS...20..125M) and (93). Data reported for 2234 HD 306182 by Johansson (1980A&AS...41...43J) likely erroneous. 2244 (9.7) HD 306185=CPD-60 2671. As in LS 2234 above, Johansson 2244 (1980A&AS...41...43J) lists these as two separate stars; the data 2244 reported for CPD-60 2671 is consistent with that reported in 2244 Moffat & Vogt (1975A&AS...20..125M) and (103). Data reported by 2244 Johansson (1980A&AS...41...43J) for HD 306185 is likely erroneous; 2244 note that (103) reports CPD-60 2671 as double. 2258 (9.3) Berdnikov and Turner (1995PAZh...21..603B) report a period 2258 of 4.43 days for this Cepheid. 2364 (8.1) Probably unresolved double-lined binary. 2372 (8.4) Misidentified as HD 100277 in Bok et al. (1972AJ.....77..733B; 2372 1972 AJ 77, 775, errata in 1973 AJ 78, 1021) actually HD 100242. 2424 (7.3) As LS 949.2425 (8.8) As LS 949. 2428 (8.8) Probably misidentified by Humphreys (1973A&AS....9...85H) 2428 (B=7.4), whose data are not included. 2430 (9.9) Suspected binary. 2462 (10.2) Probably misidentified by Feinstein (1969MNRAS.143..273F) 2462 (B=8.8) whose data are not included. 2513 (10.5) Errata in Reed & Thomas (1991PASP..103.1094R); correct data 2513 given here. 2557 (10.3) The kinematics of this high velocity star are discussed by 2557 Kilkenny (1974Obs....94....4K). 2564 (11.7) As 2513. 2584 (10.6) Steiner and Diaz (1998PASP..110..276S) note this star as one 2584 of four (V617 Sgr, HD 104994, WX Cen, and V Sge) that they define 2584 as V Sagittae stars. These stars show high-ionization species (O V 2584 and N V); the emission of He II lambda 4686 is stronger than twice 2584 the strength of Hbeta. The orbital periods vary from 5 to 12hr, 2584 and the orbital light curves have shapes of either double eclipse 2584 or sine waves. The close similarities of these objects to supersoft 2584 X-ray sources is pointed out. The nature of the compact star in 2584 these system is still an open question. 2645 (11.9) Drilling (1991ApJS...76.1033D) and Wramdemark 2645 (1980A&AS...41...33W) report B=10.2 and 11.9 respectively. Drilling 2645 (1991ApJS...76.1033D) remarks that the fainter of two stars at this 2645 position was measured; his colors are not indicative of an OB star. 2645 Data from Drilling (1991ApJS...76.1033D) are not included. 2800/ 2802 (10.2/10.9) In NGC 4755. Comparing LS and Arp & Van Sant 2800/ 2802 (1958AJ.....63..341A) finding charts indicates that 2800 and 2802 2800/ 2802 are respectively stars G and K of Arp & Van Sant 2800/ 2802 (1958AJ.....63..341A). LS 2806 is apparently star IV-18 of 2800/ 2802 Arp & Van Sant (1958AJ.....63..341A). Balona & Koen 2800/ 2802 (1994MNRAS.267.1071B) notes LS 2800 as a beta Cep variable. 2802 See 2800 2803 (6.7) uvby colors given by Crawford et al. (1971AJ.....76..621C) for 2803 HR 4890 (= LS 2813) correspond to those of LS 2803 according to 2803 other sources; data from Crawford et al. (1971AJ.....76..621C) 2803 therefore attributed to LS 2803=HR 4887. In NGC 4755. 2810 (11.2) Apparently star III-1 of Arp & Van Sant 2810 (1958AJ.....63..341A), an identification with which Perry et al. 2810 (1976AJ.....81..632P) and Dachs & Kaiser (1984A&AS...58..411D) 2810 agree, despite their B magnitudes disagreeing with LS mpg. Crowded 2810 field in NGC 4755. Balona & Koen (1994MNRAS.267.1071B) notes 2810 LS 2810 as a beta Cep variable. 2813 (6.7) See comments for 2803. 2814 (9.2) Misidentified by Perry et al. (1976AJ.....81..632P) and 2814 Dachs & Kaiser (1984A&AS...58..411D) as star III-5 of 2814 Arp & Van Sant (1958AJ.....63..341A); actually star II-1. Possible 2814 spectroscopic binary in view of large radial velocity range. 2816 (9.8) Noted by Balona & Koen (1994MNRAS.267.1071B) as a beta Cep 2816 variable. Possible spectroscopic binary in view of large radial 2816 velocity range. 2883 (10.9) Johnston et al. (1994MNRAS.268..430J) note that LS 2883 is 2883 the binary companion of a pulsar, PSR B1259-63, one of only two 2883 binary pulsars known (at that writing) where the companion mass 2883 exceeds 3M_{sun}_. The orbital period is 1236.79 days, projected 2883 semi-major axis is 1295.98 light-seconds, and eccentricity 2883 is 0.8698. The pulsar period is 47.76ms. In a subsequent 2883 paper, these authors (1996MNRAS.279.1026J) measured the magnetic 2883 field of LS 2883 to be approximately 40mG at 45 stellar radii, the 2883 first direct measurement of the magnetic field of a Be-star disk. 2946 (9.7) Uncrowded on LS chart 46. Schild et al. (1983ApJS...51..321S) 2946 gives V=9.57, which has been assumed to be a typographical error, 2946 and changed to 8.57. Drilling (1991ApJS...76.1033D) notes uncertain 2946 photometry. 2998 (8.2) Probably misidentified by Lynga (1970IAUS...38..270L) (B=6.9), 2998 whose data are not included. 3024 (9.4) Berdnikov and Turner (1995PAZh...21..603B) report a period 3024 of 6.46 days for this Cepheid. 3114 (11.6) Only absorption-line values are used in computing the 3114 recorded radial velocity; one discordant observation discarded. 3184 (11.9) Drilling et al. (1998A&A...329.1019D) report this object, 3184 BX Cir, to be an extreme Helium star [n(H)/n(He)<0.00015], 3184 specifically, an early B-type giant with a pulsational period 3184 of 2.5 hours, T(eff)=23300K, and E(B-V)=0.27. Kilkenny et al. 3184 (1999MNRAS.310.1119K) report on over 95 hours of photometry of this 3184 object, and give a period of 0.1065784-days, and an amplitude 3184 in V of 0.03mag. 3247 (10.0) Velocity -90km/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. 3320 (10.3) Muzzio (1979AJ.....84..639M) points out that two OB stars are 3320 present at the position indicated by the LS catalog. These lie 3320 along a NS line, separated by about 34 arcsec, with the southern 3320 star (CPD-59 5864) slightly brighter (V=10.70) than the northern 3320 (CPD-59 5863; V=10.82). Klare & Neckel (1977A&AS...27..215K) 3320 evidently chose the southern star to be the LS object, whereas 3320 Drilling (1991ApJS...76.1033D) and Lynga (1968Obs....88...20L) 3320 chose the northern star. SIMBAD assigns LS 3320 to the northern 3320 star, an identification also implied by the LS chart. I have 3320 adopted the northern object to be the LS star. The southern star 3320 subsequently entered my database as ALS 19115. 3328 (8.9) (46) indicates V=9.39 and B-V=0.34; six other references give 3328 V=8.2, B-V=1.0. Simbad does not verify the HD and CD numbers quoted 3328 in LS (134959,-58 5973). Drilling (1991ApJS...76.1033D) suspects 3328 variability, Moffat & Vogt (1973A&AS...10..135M) and Muzzio 3328 (1979AJ.....84..639M) note emission. Not clearly marked on LS 3328 chart 51; crowded with LS 3327. Turner (1996AJ....111..828T) 3328 concludes that this star is a B2 Ia-O hypergiant of absolute 3328 magnitude Mv=-7.88+/-0.66. 3403 (9.7) Magnitudes given by both Kozok (1985A&AS...61..387K) and 3403 Drilling (1991ApJS...76.1033D) disagree with LS mpg; colors in 3403 Kozok (1985A&AS...61..387K) do not correspond to an OB star, so 3403 that data disregarded. Clearly marked on LS 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+/-6km/s after correction for solar 3404 motion. 3422 (11.2) Cross-listed by LS as KN 1028=CPD-55 6802, for which 3422 Klare & Neckel (1977A&AS...27..215K) gives B=11.4 and Schild et al. 3422 (1983ApJS...51..321S) B=8.9. Note that Schild et al. 3422 (1983ApJS...51..321S) refers to CPD-54 6802, which Simbad does not 3422 cross-list as an LS star. Probably misidentified in Schild et al. 3422 (1983ApJS...51..321S) whose data are not included. 3601 (10.3) Misidentified as LS 3106 by Bok et al. (1972AJ.....77..733B; 3601 1972 AJ 77, 775, errata in 1973 AJ 78, 1021) 3625 (6.2) Variability in Hipparcos photometry (max. range 0.11mag) 3625 discussed by van Leeuwen et al., 1998A&AS..128..117V. 3646 (6.8) As LS 949. 3655 (12.0) LS magnitude favors Moffat & Vogt (1975A&AS...20..155M); 3655 crowded on Fig. 12 of Moffat & Vogt (1975A&AS...20..155M) and 3655 on LS chart 55. 3672 (5.6) Rauw et al. (2001A&A...368..212R) report an analysis of an 3672 extensive set of high-resolution spectra of this massive binary, 3672 deriving a classification of O7.5I(f)+ON9.7I. The period is 3672 about 9.81 days. 3674 (12.4) LS magnitude favors FitzGerald (1987MNRAS.229..227F), who 3674 notes this star as spectral class K. Too faint to see on LS 3674 chart 55. 3690 (8.8) Klare & Neckel (1977A&AS...27..215K) and Schild et al. 3690 (1983ApJS...51..321S) give B=9.1; Kozok (1985A&AS...61..387K) gives 3690 B=7.6. Probably misidentified by Kozok (1985A&AS...61..387K), whose 3690 data are not included. 3719 (9.6) Cross listed in LS as KN 1195=CPD-47 7860, for which 3719 Klare & Neckel (1977A&AS...27..215K) gives B=9.9 and Schild et al. 3719 (1983ApJS...51..321S) B=10.5. Simbad tabulates no UBV. Note that 3719 Schild et al. (1983ApJS...51..321S) refers to CPD-47 7858. Probably 3719 misidentified by Schild et al. (1983ApJS...51..321S) whose data are 3719 not included. 3728 (11.3) LS mpg favors Dachs et al. (1982A&AS...50..261D) over 3728 Whiteoak (1963MNRAS.125..105W). 3733 (11.8) As 3728. 3745 (7.0) Note that B-V from Sherwood & Dachs (1976A&A....48..187S) is 3745 about equal to the negative of other B-V values; no change to that 3745 data has been made herein. 3765 (7.3) As LS 949. 3785 (6.6) LS chart 60 indicates a rather faint star; probably intended 3785 to 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 3791 HD 326305. Finding charts show this star to be about 1.25arcminutes 3791 south and 2 seconds esat of a brighter object. Apparently the 3791 fainter, southernmost object is LS 3791 (HD 326305, V=10.01) and 3791 the brighter one is KN 1221 (HD 152042, V=8.28). The latter, 3791 brighter, star is designated as number 16055 in this database. 3794 (8.8) HD 152076. (111, 117, 122, 126) give B=8.7, while Dachs et al. 3794 (1982A&AS...50..261D) gives B=11.2. Dachs et al. 3794 (1982A&AS...50..261D) remarks that LS cross-reference the wrong 3794 HD star (152076), and that they measured the star marked on the 3794 LS chart 60 some 2 minutes north of 152076. LS mpg suggests that 3794 Stephenson and Sanduleak had HD 152076 in mind. Data from Dachs et 3794 al. (1982A&AS...50..261D) are not included. 3804 (8.6) Noted as possibly variable by Bok et al. (1966MNRAS.131..247B) 3810 (6.9) Luhrs (1997PASP..109..504L) has derived a colliding-wind model 3810 for this WC7+O6 binary system. Struve (1944ApJ...100..384S) gives a 3810 period of 8.82 days for this system. 3828 (6.0) As LS 949. See also S.R. Colley, 2003Obs...123...96C. 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 (1995A&A...303..766S). Large-amplitude 3918 variations are present, indicating that this hydrogen-deficient, 3918 N-rich star is on its way to becoming a WN star. 3926 (9.6) Kozok (1985A&AS...61..387K) gives B=10.4, and Drilling 3926 (1991ApJS...76.1033D) B=7.9. On LS chart 67, 3926 appears about as 3926 bright as LS 4044, for which many references agree B=8.4. 3982 (6.6) WN. LS 3982 is the primary of a triple system. 3992 (11.7) Machado et al. (2001A&A...368L..29M) have analysed Halpha and 3992 Hbeta line profiles of this peculiar supergiant, concluding that it 3992 may be close to the LBV phase, but it is also possible that it 3992 could be a B[e] supergiant. Miroshnichenko et al. [Ref 852; 3992 2003A&A...406..673M] report high-resolution optical spectroscopy of 3992 this object, concluding that this system is a B+F binary with an 3992 orbital period of on the order of 6 months whose orbital plane is 3992 viewed nearly edge-on. These authors deduce a distance of 3992 1.5+/-0.5kpc, and suggest that this system represents an advanced 3992 evolutionary stage of beta Lyrae type binary. 3995 (6.8) As LS 949; discovered to be an eclipsing binary 3995 by L.A. Balona, 1992MNRAS.254..404B. 4018 (7.4) Possible unresolved double-lined binary. 4080/ 4081 (12.5/12.1) Close pair enveloped in nebulosity. Neckel 4080/ 4081 (1978A&A....69...51N) remarks that both were measured together; his 4080/ 4081 observation dropped. 4081 See 4080 4142 (11.6) Reddened; double on LS chart 64. 4200 (11.7) Close double with LS 4199 on LS chart 67. 4225/ 4226 (6.0/10.7) Radial-velocity, optical and UV light curves for this 4225/ 4226 hot, massive, non-eclispsing binary in the open cluster NGC 6383 4225/ 4226 have been solved simultaneously by Pachoulakis 4225/ 4226 (1996MNRAS.280..153P), who concludes the pair to be an O6V+O7V 4225/ 4226 pair with masses and radii of 32 and 9.6 solar, respectively, with 4225/ 4226 the slightly more massive primary hotter (42500K) than the 4225/ 4226 secondary (35000K). Mass loss rates are estimated at 4225/ 4226 3.0x10^-6^M_{sun}/yr from each star. 4226 See 4225 4275 (11.2) A spectographic investigation by Niemela et al. 4275 (1995RMxAA..31...45N) reveals this star to be an O6+WN binary 4275 system with an orbital period of 12.595 days. 4293 (11.3) Presumed to be star 3 in Ruprecht 127 in Moffat & Vogt 4293 (1975A&AS...20..155M), not star 2. Crowded field on LS chart 64. 4352 (9.4) Drilling (1991ApJS...76.1033D) claims that this star is not 4352 CPD-28 13519; but Simbad concurs with the CPD identification. 4352 Colors reported in Drilling (1991ApJS...76.1033D) are not those of 4352 an OB star. 4420 (12.2) B magnitudes reported by Kozok (1985A&AS...61..387K) and 4420 Dachs et al. (1982A&AS...50..261D) fall equidistant from LS mpg. 4825 (11.5) Ryans et al. (1997ApJ...490..267R) report high-resolution 4825 spectroscopic observations of this star, concluding it to be a 4825 young supergiant lying on the far side of the galaxy at a distance 4825 of 21+/-5kpc. Multiple interstellar components are observed. 4893 (10.2) In NGC 6604. Confusion seems to exist between this star, 4893 BD-12 4979, and LS IV-12 22 (= BD-12 4978; ALS 9474.) The 4893 photographic magnitudes are respectively 10.2 and 11.2, with 4893, 4893 the brighter of the two, about 23 arcsec south and 2 seconds east 4893 of 9474. Stars 3 and 4 of Moffat & Vogt (1975A&AS...20..155M) 4893 appear to be 4893 and 9474, respectively. Data for Hiltner & 4893 Johnson (1956ApJ...124..367H), Hiltner (1956ApJS....2..389H), 4893 Hiltner & Iriarte (1955ApJ...122..185H) ascribed in those 4893 references to 4893 are assigned here to the fainter star, 9474. 4893 Reference Kozok (1985A&AS...61..387K), which reports B=10.8, may 4893 have measured both together. Note that 4893=LS IV-12 23, ALS 9475. 4910 (10.9) In NGC 6611. Hiltner & Johnson (1956ApJ...124..367H) reports 4910 V=10.1, B-V=0.8; four other references give V=9.6, B-V=0.85. 4910 Drilling (1991ApJS...76.1033D) suspects this crowded star may be 4910 variable. I have assumed that Hiltner & Johnson 4910 (1956ApJ...124..367H) is referring to LS 4905, also mpg=10.9. 4919 (9.7) Variable? 4954 (9.5) See remarks for 1268. Variability in Hipparcos photometry 4954 (max. range 0.31mag) discussed by van Leeuwen et al., 4954 1998A&AS..128..117V. 4956 (9.5) Robberto and Herbst (1998ApJ...498..400R) present high spatial 4956 resolution images of thermal emission from the nebula surrounding 4956 this luminous blue variable. They estimate a distance of 1.2kpc; 4956 the dust emission has a bipolar structure. See also remarks 4956 for 1268. Variability in Hipparcos photometry (max. range 0.19mag) 4956 discussed by van Leeuwen et al., 1998A&AS..128..117V. 5039 (11.4) Marti, Paredes, and Ribo (1998A&A...338L..71M) report this 5039 system to be a radio-loud, massive X-ray binary. See also LS 7373 5039 below. Paredes, Marti, Ribo, and Massi (2000Sci...288.2340P) claim 5039 that this systrem is a high-energy gamma-ray emitter, and Ribo et 5039 al. (2002A&A...384..954R) claim that this system is a runaway 5039 microquasar with a velocity component perpendicular to the galactic 5039 plane of larger than 100km/s. 6312 (11.7) [I +64 34] Ignace et al. (Hot Star Newsletter No. 77, July 6312 2003) present an analysis of the X-ray spectrum of this system. 6388 (7.4) [I +56 13] and 6389 (7.4) [I +56 14] are members of a 6388 quadruple trapezium system in NGC 281. I take ALS (6388, 6389, 6388 16471, 19498)=HD 5005 (D,A,B,C). If a reference does not 6388 discriminate between components, I attribute the data to ALS 6389. 6389 (7.4) [I +56 14]. See 6388. 6407 (2.1) [I +60 133] Gamma Cas. Miroshnichenko et al. 6407 (2002PASP..114.1226M) report a study of high-resolution spectra of 6407 this bright Be star. They find two components in the emission-line 6407 profile variations, a long-term one and a periodic one. The 6407 periodic one has a period of 205 days; they conclude this be 6407 related to orbital motion in a binary system. The long-term 6407 variations represent changes in the peak intensities and radial 6407 velocities of the spectral lines on a timescale of a few years. 6517 (12.4) [I +65 10] High mass X-ray binary. Liu et al. 6517 (1998ChA&A..22..463L) find evidence for an HII region around the 6517 neutron star in this system. 6704 (9.9) [I +62 181] Bern and Virdefors (1972A&AS....6..117B) report 6704 U-B=+0.39, while Hiltner (1956ApJS....2..389H) gives U-B=-0.41. 6704 I have assumed that the former dropped the negative sign. 6730 (10.3) [I +60 179] Mayer (1964AcMPh...1...25M) indicates that he 6730 measured LSN I +60 180 (= ALS 6734), but cross-references 6730 BD +60 322, which the LSN catalog gives as LS I +60 179. The stars 6730 are of nearly equal photographic magnitude, with I +60 180 lying 6730 19 arcminutes north and 19 seconds of time west of I +60 179. 6754 (10.7) [I +62 185] Lutz and Lutz (1972AJ.....77..376L) report 6754 (V, B-V)=(11.36, 0.64) for this star, in conflict with Hiltner's 6754 result. Hiltner's result is favored in view of its agreement 6754 (B=10.72) with the photographic magnitude. The Digitized Sky Survey 6754 shows a star about 1mag fainter and 2-3 minutes east of 6754; the 6754 Lutz's may have measuered this star by mistake. 6757 (12.2) [I +61 235] Motch et al. (1997A&A...323..853M) classify this 6757 star as a likely massive X-ray binary. 6855 (10.6) [I +62 198] Bern and Virdefors (1972A&AS....6..117B) claim 6855 this star (BD +62 332) to be an M0 star with V=8.98, B-V=1.95. It 6855 is assumed that this is a misidentification. 6978 (12.3) [I +69 5] Eclipsing binary of the W UMa type; V=12.30-13.60; 6978 P=0.5005 days. 7289 (8.8) [I +61 286] Polcaro et al. (Hot Star Newsletter No. 75, 7289 Feb.-Mar. 2003) report substantial Halpha variability for this star 7373 (11.4) [I +61 303] The X-ray spectrum of this binary system is 7373 discussed by Leahy et al., 1997ApJ...475..823. Quasi-simultaneous 7373 H-alpha and radio observations are discussed by Zamanov et al., 7373 1996Ap&SS.243..269Z. Peracaula et al (1997A&A...328..283P) report 7373 that 6-cm radio ``microflares'' from this system exhibit a period 7373 of 1.4 hours; they tentatively attribute these flares to secondary 7373 luminosity-driven shocks. Marti et al. (1998A&A...329..951M) report 7373 on deep 6-cm VLA observations of this object in an unsuccessful 7373 effort to search for extended radio emission. Strickman et al. 7373 (1998ApJ...497..419S) present the results of a multiwavelength 7373 monitoring campaign targeting the gamma-ray source 2CG 135+1 in an 7373 attempt to confirm the association of this object with LSI +61 303, 7373 but their signal-to-noise ratio was insufficient to establish a 7373 spectral or intensity correlation of the high-energy emission with 7373 simultaneous radio, optical, and infrared emission of LSI +61 303. 7373 Apparao (2000A&A...356..972A) found that the ratio of the 7373 equivalent width of the blue wing to that of the red wing of the 7373 H-alpha line shows an orbital variation, attributed to obscuration 7373 caused by the post-shock gas of a shock produced by the supersonic 7373 orbital motion of the secondary through the gas disk of the Be 7373 star. A study of long-term optical spectral observations is 7373 reported by Liu et al. (2000A&A...359..646L). Zamanov et al. 7373 (1999A&A...351..543Z) report an anlysis of the H-alpha spectrum of 7373 this system, detecting the same 26.5-day period as found at radio 7373 wavelengths, and finding that the peak separation of the H-alpha 7373 emission line seems also to vary over a time scale of 1600 days, a 7373 result they attribute to variations in the mass loss rate of the Be 7373 star and/or density variability in the circumstellar disk. Massi et 7373 al. (2004A&A...414L...1M) provide evidence for precessing 7373 relativistic radio jets in this system. Mirabel et al. 7373 (2004A&A...422L..29M) argue that this star is a runaway microquasar 7373 with velocity 27+/-6km/s. 7374 (8.2) [I +61 304] V. McSwain (Hot Star Newsletter No. 76, May 2003) 7374 reports orbital elements for this spectroscopic binary system, and 7374 suggests that this system plus LS I +61 303 (7373 above) probably 7374 belong to a sub-cluster within the Cas OB6 association. 7504 (7.0) [I +68 17] Cepheid SU Cas. Moffet and Barnes 7504 (1980ApJS...44..427M) give V=5.74-6.18 and P=1.949 days. 7513 (12.1) [I +56 74] This star has been designated as variable 7513 ZZ Per, but Haug (1970A&AS....1...35H) reports variability 7513 doubtful. 7724 (5.4) [I +59 187] Hiltner (1956ApJS....2..389H) gives B-V=-0.43; 7724 the negative sign is presumed to be a typographical error. 8023 (11.3) [V +44 17] Motch et al. (1997A&A...323..853M) classify this 8023 star as a likely massive X-ray binary. 8221 (8.4) [V +42 24] SX Aur. Chambliss and Leung (1979ApJ...228..828C) 8221 report this system to be a semidetached eclispsing binary 8221 consisting of two B-stars with a period of 1.21008 days and with 8221 light curves of the beta Lyrae type. The magnitude given here is 8221 that reported by them as the system's maximum brightness. 8306 (11.0) [V +33 25] Simbad attributes Hiltner's (1956ApJS....2..389H) 8306 photometry (V, B-V, U-B)=(10.64, 0.31, -0.62) to both this star 8306 and ALS 8308 [V +33 27]. The coordinates given by Hiltner 8306 (his no. 446) better match those for 8306. 8308 (11.5) [V +33 27] See 8306 above. 8415 (12.5) [V + 34 46] Imbedded in nebulosity in Sharpless 237. The LSN 8415 catalog assigns the same BD number, +34 1074, to ALS 8415 and 8417 8415 [V +34 46 and V +34 47]. On the basis of the photographic 8415 magnitudes I take BD +34 1074=ALS 8417. 8416 (11.2) [V +34 45] Imbedded in nebulosity in Sharpless 237. 8417 (11.7) [V +34 47] Imbedded in nebulosity in Sharpless 237. See 8415 8422 (4.9) [V +32 8] Eclispsing variable V1016 Ori. Vitrichenko, 8422 Klochkova, and Plachinda (1998PAZh...24..352V) report a 8422 radial-velocity analysis for this system, determining masses and 8422 radii of (10.2, 3.2) and (2.55, 1.8) for the two components, and a 8422 radius of 3.6 for the dust shell around the secondary component. 8468 (9.8) [V + 26 5] Wang and Gies (1998PASP..110.1310W8) present 8468 radial velocity measurements of this X-ray transient system, 8468 A0535+26. Observational errors are too large to claim detection of 8468 the Be star orbital motion, but they set a semiamplitude limit 8468 of <10.6km/s. 8751 (7.4) [V +20 19] Garnier et al. (1971A&A....14..408G) report 8751 U-B=-0.39 for this star, whereas a number of other sources report 8751 U-B=-0.88 or -0.89. The Garnier et al. (1971A&A....14..408G) value 8751 is assumed to be a misprint, and is taken as -0.89. 8847 (9.3) [V + 22 43] Hiltner (1956ApJS....2..389H) notes very strong 8847 H and K lines. 9377 (11.6) [IV +06 2] Jeffery (1998MNRAS.294..391J) reports a spectral 9377 analysis of this high-gravity extreme helium star, determining 9377 Teff=31000K (making it the hottest high-gravity extreme helium 9377 star yet studied), and logg=4.05. LS IV + 6 2 lies close to the 9377 boundary of the helium star pulsation instability finger near Teff 9377 similar to 27000K. Available data indicate that the radial 9377 velocity is variable, but give no indication of amplitude or 9377 period. 9474 (11.2) [IV -12 22] See 4893 above. 9517 (10.2) [IV -11 14] WC7+OB binary; Hiltner (1945ApJ...102..492H) 9517 gives a period of 29.6 days and a semi-amplitude of 165km/s for 9517 the WC star. 9960 (99.9) [IV +07 6] Long-period (262 days) binary RZ Oph. Forbes and 9960 Scarfe (1984PASP...96..737F) report UBV photometry with V varying 9960 between 9.85 and 10.64. 10301 (8.1) [II + 18 4] Chentsov (2004AstL...30..325C) argues that this 10301 star is a white hypergiant. 10308 (10.4) [II +12 7] Hiltner (1956ApJS....2..389H) gives U-B=-0.25, 10308 but Hiltner & Iriarte (1955ApJ...122..185H) give U-B=+0.25. The 10308 former would appear more for a B1 supergiant; the latter is 10308 changed to -0.25. 10539 (6.9) [II +29 15)] V1507 Cyg. Berdyugin and Tarasov 10539 (1998PAZh...24..139B) report an analysis of UBVRI polarimetric 10539 observations of this interacting binary system, concluding that 10539 linear polarization arises from light scattering in a shell 10539 surrounding the unseen secondary component. The orbital 10539 inclination is estimated at 46.4+/-2.1 degrees. 10571 (5.4) [III + 40 2] V380 Cyg. Popper and Guinan 10571 (1998PASP..110..572P) discuss spectroscopic observations of this 10571 binary system with a B1.5 II-III primary. 10591 (6.3) [II +24 22] Hiltner (1956ApJS....2..389H) identifies this 10591 star, his no. 844, as BD +24 3914=HD 187983. According to SIMBAD, 10591 HD 187982 and HD 187983 are the same object. The LSN catalog 10591 misidentifies this star as HR 7593; it is actually HR 7573. 10594 (12.0) [II +27 21] Turner (1980ApJ...235..146T) misidentifies this 10594 star as HD 332918, which is actually LS-North II +27 20 10594 (= ALS 10592), a 10-th magnitude F6 supergiant. 10601 (5.3) [III +46 1] Fernie (1961ApJ...134..850K) reports B-V=-1.15 10601 for this star, apparently an error. His data is not included. 10601 Israelian et al. (2000MNRAS.316..407I) report on a spectral 10601 time-series analysis of this runaway binary supergiant O star, 10601 finding radial velocity variations with a possible quasi-period of 10601 6.4 days as well as night-to-night variations in the position and 10601 strength of central emission reversal of the H-alpha profile. 10603 (5.5) [III +47 1] Wehinger and Hidajat (1973AJ.....78..401W) 10603 misidentify this star as BD +47 2919 and as V819 Cyg. It is 10603 BD +47 2939; V819 Cyg is actually LS-North III +47 2 (= ALS 10614) 10712 (11.4) [IV -12 111] Arkhipova et al. (2002AstL...28..257A) claim 10712 that this star is a protoplanetary nebula with irregular 10712 variability on a timescale of 1 day with 10712 delta(V, B, U)=(0.3, 0.3, 0.4). 10896 (9.2) [II +36 22] BD +36 3914=HD 228053. Hiltner 10896 (1956ApJS....2..389H) misidentifies this star, his no. 880, as 10896 HD 228052. See also 10898 below. 10898 (9.9) [III +45 3] BD +44 3365=HD 191781. Hiltner 10898 (1956ApJS....2..389H) misidentifies this star, his no. 881, as 10898 HD 228053. See also 10896 above. 10924 (10.0) [II +20 19] FG Sge. Arkhipova et al. (1998PAZh...24..427A; 10924 1998PAZh...24..431A) report UBV and spectroscopic observations of 10924 this system, while Tatarnikov and Yudin (1998PAZh...24..359T) 10924 present a model for the dust shell around this star. 10934 (8.7) [II +38 11] Ignace et al. (Hot Star Newsletter no. 77, 10934 July 2003) report an analysis of the wind outflow of this WR star. 10968 (10.8) [II +32 19] Hiltner (1956ApJS....2..389H) gives U-B=+0.33 10968 for this star, apparently too red for a B0 star, whereas Lutz and 10968 Lutz (1972AJ.....77..376L) give U-B=-0.44. Hiltner's value is 10968 presumed to be a typographical error, and is taken here as -0.33. 11089 (9.7) [II +37 46] WN7+OB binary; Hiltner (1951ApJ...113..317H) 11089 gives a period of 10.6 days and a semi-amplitude of 240km/s for 11089 the WN7 star. 11114 (5.9) [II +40 15] W.P. McKibben et al. (1998PASP..110..900M) report 11114 radial velocity measurements and a single-lined spectroscopic 11114 orbit for the O-type star HD 193322A, which they show to be a 11114 311-day binary system that has a distant third companion in a 11114 31-year orbit. HD 193322B appears to be an unresolved 11114 spectroscopic binary. Thus HD 193322, the central object in the 11114 open cluster Collinder 419, is a multiple system that contains at 11114 least five stars. 11163 (8.7) [II +38 42] Munch (1950ApJ...112..266M) presented one of the 11163 first detailed analyses of this WN5+O6 V-III eclipsing binary 11163 system. Marchenko et al. (1997ApJ...485..826M) report on high 11163 signal-to-noise optical spectroscopy and simultaneous narrowband 11163 continuum photometry of this system. Antokhin et al. 11163 (1997Ap&SS.254..111A) discuss the velocity law in the extended 11163 photosphere of the WN5 star. Keeping (1946PASP...58..245K) 11163 gives orbital elements. 11192 (6.8) [III +43 7] Marchenko, et. al. (Hot Star Newsletter No. 77, 11192 July 2003) present an analysis of high-quality spectra of this 11192 colliding-wind WR+O binary system. The system has high 11192 eccentricity (0.881+/-0.005), a period of 2899 days, and orbital 11192 inclination 50+/-15 degrees. 11209 (11.0) [II + 36 65] Marchenko, Moffat, and Eenens 11209 (1998PASP..110.1416M) report an analysis of radial velocity 11209 measurements of this (WN5o + O5 III-V) 21.7-day binary system. The 11209 WR lines show phase-locked variability; the masses are estimated 11209 as 36-54M_{sun}_ for the WR star and 26-33M_{sun}_ for the O star 11209 for a system inclination of 68 degrees. Ivanov, Valchev, Georgiev, 11209 Barba, and Iliev (1999RMxAA..35...25I) obtained 123 11209 high-resolution CCD spectra of this system over 40 nights, and 11209 give a refined period of 21.6878+/-0.0001days. 11334 (10.8) [II +37 92] Walborn and Howarth (670) remark that this star 11334 is a single-lined spectroscopic binary with a period of 4.8 days. 11703 (7.5) [III +55 5] Hiltner (1956ApJS....2..389H) reports B=10.22 for 11703 this star, while Simonson (1968ApJ...154..923S) gives B=7.68. The 11703 latter is favored in view of the LS catalog photographic 11703 magnitude; Hiltner's data are assumed to be a misidentification 11703 and are disregarded. 12008 (7.6) [III +59 11] G. Catanzaro (Hot Star Newsletter No. 76, 12008 May 2003) reports an abundanace analysis of this system, finding 12008 that Fe, Ni, and Zn are underabundant. 12072 (9.1) [III + 54 8] Abt et al. (1970ApJ...161..477A) report that 12072 this star is a spectroscopic binary with a period of 111.6 days. 12072 See Walborn (1971ApJ...164L..67W). 12096 (5.3) [III +57 20] Harries et al. (1998MNRAS.295..386H) report new 12096 spectroscopic observations of this O+O binary (= LZ Cep). They 12096 find LZ Cep to be a semi-detached system with the secondary star 12096 filling its Roche lobe, and report a distance modulus of 12096 9.6+/-0.2, which is slightly smaller than the distance modulus 12096 to Cep OB2 (=9.9). The reddening of LZ Cep is also at the lower 12096 end of the cluster range, suggesting that the binary is located on 12096 the near side of the cluster. 12143 (10.0) [III +54 16] Negueruela, et. al. (2001A&A...371.1056N) 12143 present an analysis of X-ray and high-resolution optical 12143 spectroscopy of this 9.5-day massive X-ray binary. 12230 (9.2) [III +55 28] Barbier, et. al. (1973A&A....27..421B) give 12230 U-B=+0.19 for this star, far too red for a B2 giant. This is 12230 assumed to be an error, and is not incorporated in the database. 12324 (12.8) [III +56 42] NX Cep. Miller & Wachmann (1973RA......8..367M) 12324 give this star as spectral type F2. 12858 (10.7) [III +62 39] Hiltner (1956ApJS....2..389H) cross-references 12858 this star (his no. 1205) as BD +61 2472. However, it is clear from 12858 SIMBAD that BD +61 2472=LS I +61 12=SAO 20695=ALS 13012, an 12858 identification which has been confirmed by precessing the BD 12858 coordinates. However, Hiltner's 1900 coordinates for his no. 1205, 12858 when precessed to 1950, conform pretty closely to 12858 LS III +62 39=ALS 12858. I have assumed that Hiltner did measure 12858 12858, and wrote down the wrong BD number. 13175 (9.5) [I +62 23] Negueruela (Hot Star Newsletter No. 77, July 2003) 13175 reports observations of this triple system. The faintest member 13175 (BD +62 2296B) is a WN4 star, while the brightest component 13175 (BD +62 2296) appears to be a normal B2.5 Ia star, and the third 13175 visual component, BD +62 2296C, is a B0 III star. 13277 (7.1) [I +60 56] Fischer and Morrison (2001PASP..113..821F) discuss 13277 spectrum variability of this A-typer supergiant. 14805 (5.3) HD 57061; Tau CMa. van Leeuwen and van Genderen 14805 (1997A&A...327.1070V) analysed Hipparcos data for this 14805 double-O-type system, showing that it also contains a massive 14805 close binary of period 1.282 days. This system contains both the 14805 longest period spectroscopic binary and the shortest period 14805 eclipsing binary known for O-type stars. 14499 (7.0) [HD 163181] Josephs et al. (2001PASP..113..957J) give orbital 14499 elements for this massive interacting binary, V453 Sco. 14499 P=12 days, mass function=9M_{sun}_. 14834 (6.4) [HD 199140] Beta-Cephei star BW Vul. Percy, Velocci, and 14834 Sterken (2003PASP..115..626P)] find that nonevolutionary period 14834 changes in this star are not the result of random cycle-to-cycle 14834 fluctuations as they are in several cooler types of pulsating 14834 variables. 15036 (5.3) [HD 151804] A summary of a study of wind and photospheric 15036 variability of this star appears in S.R. Colley, 15036 2003Obs...123...96C. 15089 (8.6) [HD 172324] High velocity star: v=-115km/s; see Bonsack & 15089 Greenstein (1956PASP...68..249B). 15197 (10.0) Resolved as binary (separation 0.077 arcsec, {Delta}m=2.4) 15197 by Nelan et al. (2004AJ....128..323N). 15205 (10.7) Resolved as binary (separation 0.352 arcsec, {Delta}m=2.8) 15205 by Nelan et al. (2004AJ....128..323N). 15757 (8.5) [CPD-41 7742] H. Sana (Hot Star Newsletter No. 76, May 2003) 15757 reports high-resolution optical spectroscopy of this binary system 15757 (P=2.44 days), infering type O9 III + B1 III, and suggesting that 15757 the system may be an eclipsing binary. 16331 (10.0) Two CPD numbers appear to be assigned to this star: -57 2777 16331 (= HD 302583) and -57 2759. The coordinates and magnitudes listed 16331 in Simbad are virtually identical. Star 316 in Denoyelle 16331 (1977A&AS...27..343D). 16388 (5.0) [3 Vul] Dukes et al. (2003AJ....126..370D) report an analysis 16388 of differential uvby photometry of this star obtained over 7 16388 years. This system is a multiperiodic 53-Per type single-line 16388 spectroscopic binary showing both line profile and light 16388 variations, with three modes. The primary and secondary masses are 16388 estimated as 4.16 and 0.65 to 1.1M_{sun}_, and the age of the 16388 system is estimated as 25 million years. The orbital period is 16388 close to 1 year, and the pulsation period close to 1 day. 16471 See 6388 above. 16717 (9.8) HD 93343. See LS 1872 above. Photometry in Feinstein 16717 (1969MNRAS.143..273F). 17186 (9.3) Confusion exists in the literature concerning BD 17186 indentifications for this star and ALS17381. I assign 17186 ALS 17186 = Van den Berg (1966AJ.....71..990V) star 92a, and 17186 ALS 17381 = Van den Berg 92b. Racine (1968AJ.....73..233R) 17186 respectively identifies these stars as BD-11 1763 and BD-11 1761, 17186 whereas Herbst, Racine and Warner (1978ApJ...223..471H) reverse 17186 these identifications. SIMBAD follows the Herbst et. al. 17186 identifications, which would appear to make sense if the lower 17186 BD number corresponds to the westernmost star (finding chart in 17186 Racine). SIMBAD apparently errs in assigning BD-11 1762 to 17186 star 92c: this BD number is about 6 arcminutes north of this tight 17186 grouping of three stars. 17381 (9.0) See 17186 above. 18544 (13.8) Paardekooper et al. (2003A&A...404L..29P) report brightness 18544 variations of 0.2 magnitudes on a time scale of hours for this 18544 WO4 + O5((f))) colliding-wind binary. 18773 (16.9) [V635 Cas] High-mass X-ray binary 4U 0115+634. Negueruela et 18773 al. (872) analyse photometry and high SNR spectroscopy for this 18773 system. The distance is estimated as 7-8kpc and the binary period 18773 is 24.3 days. 18894 (9.1) [HD 138503] IT Lib. Eclipsing binary (2 B-stars) about 1kpc 18894 above the galactic plane. See Martin, 2003PASP..115...49M. 19498 See 6388 above. 19605 (16.0) Optical counterpart to X-ray pulsar 1WGAJ1958.2+3232. 19605 Suggested to be a B0 Ve star by Israel et al. 19605 (1999A&A...345L...1I), but Negueruela et al. (2000A&A...354L..29N) 19605 find this classification untenable and suggest the object is 19605 instead an intermediate polar.