Contents

1. Introduction

2. Strategy

2.1 UBVß Photometry

2.2 Spectroscopy

3. Format information for Catalog and Databases

4. Remarks On Individual Stars

5. References in Numerical Order

6. References in Alphabetical Order

Acknowledgements

Much of the spectroscopic data for the southern Case-Hamburg stars were checked and keypunched by Amy Beatty. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. I am grateful to the inter-library loan staff at Alma College for tracking down a number of references, and to the Office of the Provost of Alma College for support of publication costs. Special thanks are due Brian Skiff of Lowell Observatory for forwarding me coordinates and cross-identifications for a number of objects. This research was supported at various times by awards from Research Corporation and the RUI program of the National Science Foundation (AST-9731179).

1. Introduction

This project originated in the summer of 1991 when the author began compiling a cross-reference “catalog” and tabulation of published UBVß photometry for stars listed in Stephenson and Sanduleak’s Luminous Stars in the Southern Milky Way [Publ. Warner & Swasey Obs., Vol. 1, no. 1 (1971)]. This database was published in July 1993 [ApJS 87, 367 (1993)] and was subsequently expanded to include compilations of published MK classifications [ApJS 97, 189 (1995)], 4-color photometry [AAS 117, 313 (1996)], and radial velocities [AJ 113, 823 (1997)] for these objects. In mid-1997 the project was again expanded to include UBVß photometry for stars listed in the northern-hemisphere volumes of the “Case-Hamburg” surveys [ApJS 115, 271 (1998)]; MK classifications for the northern stars were similarly compiled and made electronically available to interested parties, though were not formally published. Work on the radial velocity and four-color compilations has since been discontinued, but interested readers may still obtain those (for the LS-South stars) from the author.

The “Case-Hamburg” (CH) surveys comprise a seven-volume listing of intrinsically luminous stars within about ten degrees of the plane of the Milky Way. These objects are hereafter referred to as “LS” objects. The seven volumes were published between 1959 and 1971 by the Hamburg and Warner and Swasey Observatories. Most of the LS objects are OB stars, but there are as well a number of A, F, and G supergiants and a few white dwarfs and Wolf Rayet stars. These surveys reached a limiting photographic magnitude of approximately 13.5, and were based on objective-prism surveys of dispersion 580 Angstrom per millimeter at Hydrogen-gamma. Six of the LS volumes cover the northern Milky Way:

Hardorp, J., Rohlfs, K., Slettebak, A. and Stock, J. 1959, Luminous Stars in the Northern Milky Way I. (Hamburg-Bergedorf: Hamburger Sternwarte and Warner and Swasey Observatory).

Stock, J., Nassau, J. J. and Stephenson, C. B. 1960, Luminous Stars in the Northern Milky Way II. (Hamburg-Bergedorf: Hamburger Sternwarte and Warner and Swasey Observatory).

Hardorp, J., Theile, I. and Voigt, H. H. 1964, Luminous Stars in the Northern Milky Way III. (Hamburg-Bergedorf: Hamburger Sternwarte and Warner and Swasey Observatory).

Nassau, J. J., and Stephenson, C. B. 1963, Luminous Stars in the Northern Milky Way IV. (Hamburg-Bergedorf: Hamburger Sternwarte and Warner and Swasey Observatory).

Hardorp, J., Theile, I. and Voigt, H. H. 1965, Luminous Stars in the Northern Milky Way V. (Hamburg-Bergedorf: Hamburger Sternwarte and Warner and Swasey Observatory).

Nassau, J. J., Stephenson, C. B. and MacConnell, D. J. 1965, Luminous Stars in the Northern Milky Way VI. (Hamburg-Bergedorf: Hamburger Sternwarte and Warner and Swasey Observatory).

The southern survey was published in a single volume:

Stephenson, C.B., and Sanduleak, N. 1971, Luminous Stars in the Southern Milky Way, Publ. Warner & Swasey Obs., Vol. 1, no. 1.

By the end of the year 2000 the author’s databases had grown to incorporate over 33,000 observations (lines of data) on just over 8500 CH stars drawn from 680 references. The strategy and procedures used in compiling these databases of LS-star data are detailed in section 2 below. The remainder of this introduction describes further expansion of the catalog and databases.

While engaged in the LS-stare compilations I became aware that there exist many galactic OB stars not listed in the CH surveys. There are a number of reasons for this: many OB stars lie outside the sky coverage of those volumes or reside in crowded clusters and associations, while yet others are fainter than the CH limiting magnitude.

Motivated by encouragement from various colleagues, I decided in early 2001 to undertake supplementing my database to include identifications, UBVß photometry, and MK classifications for “non CH” galactic OB stars. This work has now been brought to a reasonable first stage of completeness.

The definition of an OB star is somewhat loose. Since the original LS catalogs were based on spectroscopic criteria my initial inclination was to only incorporate as so-called “supplemental OB stars” objects known to be such on the basis of their spectra. However, I quickly came to realize that such a criteria would discriminate against many likely OB stars. Thus I decided to relax my definition to include both spectroscopically-detected OB stars and stars whose UBV-based Q-values are indicative of an early type. My working definition(s) of an OB star can be summarized as:

(i) “Apparently normal” main sequence stars down to and including temperature class B2.

(ii) “Apparently normal” stars of luminosity class I-IV down to and including temperature class B9.

(iii) If spectral information is not available, “apparently normal” stars with Q < –0.667. This Q-value corresponds to approximately type B2 on the main sequence and will catch supergiant B stars down to about temperature type B6.

To keep the work tractable and to avoid incorporating as few non-OB stars as possible, I as a rule incorporated as supplemental OB stars only objects for which photometry and/or MK-type classifications have been published, although this rule was not always rigidly followed. That is, suspected OB stars (for example, based on low-dispersion objective prism spectra or photographic photometry) are not as a rule included.

My search for supplemental OB stars went along the following general lines.

I began by examining the approximately 680 papers I had on hand that contained data for CH stars, beginning with particular ones that were expected to be rich in supplemental objects. The first of these were those papers giving photometry and classifications for objects appearing in the “Heidelberg” survey of galactic OB stars: Klare & Neckel [AAS 27, 215 (1977)]; Schild, Garrison & Hiltner [ApJS 51, 321 (1983)]; Garrison, Hiltner & Schild [ApJS 35, 111 (1976)]. While many Heidelberg (Hbg) and LS objects are in common, the Hbg catalog records some 560 early-type objects not appearing in the LS catalog. The general procedure was that as supplemental OB stars were recognized, I added them to my master catalog of LS objects. Each star is assigned an internal “Alma LS” (ALS) number, a source name, cross-references to the BD, CPD, CD, SAO, HD and HR catalogs as appropriate, 2000-epoch right ascension and declination, and galactic coordinates. ALS numbers run from 1-5132 for CH southern stars, 6001-13390 for CH northern stars, and 14001 and up for “supplemental” OB stars. (ALS numbers 5133-6000 not used.) Each supplemental star was queried on SIMBAD to locate any other published photometry or classifications; this often lead to new references to be examined, with the result that data from just over 800 individual papers now appear in my photometric and spectroscopic compilations.

After the Heidelberg objects I examined some historically “classic” papers: Hiltner’s tabulation of photometry, polarization measurements, and classifications for over 1200 O and B stars [ApJS 2, 389 (1956)], and Morgan, Code, & Whitford’s classifications for 1270 blue giants [ApJS 2, 41 (1955)] (see also Morgan, Whitford & Code [ApJ 118, 318 (1953)]). Hiltner et. al. [ApJ 157, 313 (1969)] published classifications for HR-numbered southern OB stars. Another major source of objects was Deutschman, et. al’s photometry of Celescope objects [ApJS 30, 97 (1976)]. More recently, Philip Massey and his various collaborators have uncovered numerous previously undetected OB stars in rich clusters and associations (such as Eta Car) via deep CCD photometry [AJ 105, 980 (1993); ApJ 454, 151 (1995); AJ 101, 1408 (1991); AJ 106, 1906 (1993); AJ 121, 1050 (2001)].

Less synoptic but still valuable surveys for OB stars have been carried out by a number of groups. Lynga [Lund. Medd. Astron. Obs. Ser. II, 141, 1 (1964)], for example, published coordinates for some 400 putative OB stars, about 90 of which are new to my catalog. The La Plata, Argentina, group has been very active along these lines: Muzzio [AJ 79, 959 (1974)] and Orsatti [AJ 104, 590 (1992)], for example, have published surveys for OB stars, for which some follow-up photoelectric photometry has been published [Muzzio & Forte AJ 80, 1037 (1975)]. In such cases I incorporated no stars whose identification as early types would have been based only on photographic Q-values. Howard Lanning and his collaborators [PASP 85, 70 (1973); PASP 106, 38 (1994); PASP 107, 751 (1995); PASP 110, 586 (1998)] have identified 351 UV-bright objects in the galactic plane, including a number of LS stars. However, many of these are white dwarfs, planetaries, dwarf novae and the like, so I did not as a rule incorporate these objects into my catalog unless information gleaned from SIMBAD indicated that they could reasonably be construed to be OB stars; likewise for Stephenson and Sanduleak’s [ApJS 33, 459 (1977)] listing of 455 H-alpha emission stars in the Milky Way. Drilling and Bergeron [PASP 107, 846 (1995)] published a list of 234 stars as an “extension” to the CH surveys, which prompted me to include those not previously picked up even though their list probably includes some non-OB types.

Beyond “survey-type” papers, OB stars appear in a number of papers dealing with individual clusters. In some cases where stars were identified only via finding charts I was able to determine coordinates from the RealSky set of CDs; in a few cases of ambiguity or extreme nebulosity I opted not to include objects. Ultimately, every one of the approximately 650 papers in my possession that had contributed CH-star data were examined for supplemental OB stars. At this writing the number of supplemental stars stands at about 5960. All of the supplemental stars have been checked for UBVß on SIMBAD; checking for spectral classifications is now underway.

Two previous catalogs deserve mention here. Goy [AAS 26, 273 (1976)] prepared a catalog of 763 O-type stars, listing UBV photometry, polarizations, associated HII regions, and spectral types. Similarly, Garmany, Conti, and Chiosi [ApJ 263, 777 (1982)] compiled a listing of 765 O stars for which spectral types, luminosity class, and UBV photometry existed at that time. All but a handful of objects appearing in those catalogs appear in my catalog.

A difficult issue was whether or not to include as supplemental stars those objects for which Houk has given classifications in her Michigan Spectral Survey volumes. A search of those volumes revealed ~9300 stars that meet the criteria for “OB stars” given above but which I did not otherwise pick up. The majority of these are late B-type (B8-B9) giants. Given that Houk has a tendency to classify as too luminous, I opted not to include these objects.

Of the 12,235 independent objects tabulated in the CH volumes (excluding 287 duplicate entries), Reed [AJ 120, 314 (2000)] found that 10,669 are nominally of “OB” type; the present approximately 5,900 supplemental OB stars now incorporated bring the total of OB-type objects to about 16,600. Given that the number of “Case Hamburg OB-type” stars within the solar circle has been estimated at ~ 19,000 [Reed, PASP 113, 537 (2001)] we can have some hope that astronomers’ inventory of these objects is reaching a reasonable stage of completeness.

In the text that follows, references to “LS” stars should be understood to generally mean “original Case-Hamburg LS stars plus supplemental OB stars” except where obvious from context. When it is necessary to distinguish between stars listed in the Northern/Southern CH volumes, I refer to objects listed in the former (latter) as LSN (LSS) stars, respectively; otherwise, the generic label “LS” (luminous star) is used in reference to either CH or “supplemental” objects.

A few comments of a general nature are appropriate here. This catalog doubtlessly fails to include some legitimate OB stars even while it will no doubt prove to include a number of objects that it should not: the difference between a classification of B9 IV and A0 V is not great. In some cases judgment calls were made based on the source of a classification, the dispersion, etc.

2. Strategy

The primary criteria applied for incorporation of data into this compilation are originality and adherence to the UBVß and MK systems.

In a compilation of this size, complete consistency is impossible to achieve: readers interested in any particular star are urged to treat this work as a sourcebook and consult original references whenever possible.

A few remarks are in order regarding the Northern-hemisphere volumes of the CH survey. Various of the LSN volumes overlap in sky coverage, leading to duplicate entries for 138 stars. [Note: this number is given incorrectly as 135 in Reed, ApJS 115, 271 (1998). Since publication of that paper, three more duplicate entries were discovered: LS V + 55 3 (ALS 7060) = LS I +56 43 (ALS 7058), LS III + 39 1 (ALS 10932) = LS II + 39 11 (ALS 10929), and LS IV + 11 11 (ALS 10375) = LS II + 11 8 (ALS 10376)]. Note is made of these in the catalog, and care taken to assign photometry consistently to one ALS-numbered star of a duplicate pair. In addition, there is also some overlap between the LSS and LSN catalogs: 149 stars are in common. In all such cases I assign the data to the LSS-based identification number, and make note of the duplicates in the catalog. In fields where the LSS and LSN volumes overlap in sky coverage, stars in close proximity to each other may appear in either a northern volume or in the Stephenson/Sanduleak volume; particular examples in this regard are stars in the open clusters NGC 6604 and 6611. Ordering the catalog by 2000-epoch right ascension alleviates some of this confusion, but at the price of permuting the ordering of some LSS stars, whose numbers were originally assigned according as increasing 1900 right ascension.

It is also worth noting that in declination zone +54 of LSN Volume III, running numbers 1 through 15 are used twice, designating two different sets of stars. In these cases one looks to magnitudes, coordinates, and cross-identifications that appear in the original literature to establish what star is involved. Upon accounting for duplicates, the seven CH volumes contain a total of 12,235 independent objects.

FORTRAN format codes for reading the catalog and UBVß and MK databases are given in section 3 below. This is followed by detailed notes for some stars, and by a complete list of references.

2.1 UBVß Photometry

Excepting a very few values representing averaged observations, only photoelectric data reported in the original research literature have been incorporated. Care was taken to exclude any results adopted from or that derived from averaging or homogenizing data from different sources: what appears here is, as much as possible, unadulterated. V magnitudes deriving from uvby photometry have not been incorporated. A chronic problem area was the number of measurements reported for each star: while most authors state this explicitly, some give only a minimum number and others no details at all. If no information along these lines could be gleaned, the number of measurements was taken to be one.

2.2 Spectroscopy

The general precepts used in assembling the photometric compilation are retained here: only original data from references directly available to the author have been incorporated. Most classifications derive from grating, prism, or objective-prism spectra; in a few instances they derive from equivalent widths, microphotometer tracings or the like.

Two particular complications arise when dealing with spectra. The first is that notations used to designate peculiarities (uncertain classification, emission, broadening, interstellar lines, double lines, etc.) differ from source to source and continue to evolve. Within the limits imposed in producing a printable collation, I have attempted to remain faithful to original notations. The second is that there is an element of subjectivity to classification: two credible sources may legitimately assign different classifications to the same star; this is particularly so in the case of luminosity classifications where low-dispersion spectra are involved. Except for resolving obvious cases of misidentification (a star classified as both B and K, for example), no attempt has been made to scan the compilation for such differences.

An important exception was made to the “original data only” precept in compiling spectral data: the catalog of L. F. Smith [reference 301; MNRAS 138, 109 (1968)] was used in its entirety, even though not all data therein is original to her. Her paper introduced a new classification system for the Wolf-Rayet stars and included re-classification of previous material on the new system. No supplemental stars appear in this reference.

Given that a wide variety of instruments and techniques underlie these classifications, a 20-character “dispersion record” is given for those classifications taken from papers where instrumental details were given. If no details were given, the dispersion record is left blank. These records follow a format where up to three items are detailed: (1) type of instrument used, (2) dispersion in Å/mm, and (3) the wavelength at which the dispersion applies. These dispersion records incorporate a number of abbreviations as follows:

A Ångstrom

d Hydrogen delta

g Hydrogen gamma

m/A microns per Ångstrom

Cass Cassegrain spectrum

1P 1-prism

2P 2-prism

3P 3-prism

C Coude spectrum

G Grating spectrum (reflection or transmission not specified)

IT Image tube spectrum

OP Objective-prism

P Prism

RG Reflection grating

S Slit

TG Transmission grating

TP Thin prism

Examples: “126” in the dispersion record indicates that the original reference reported only a dispersion of 126 Å/mm. “OP 77g” would indicate an objective-prism spectrum of dispersion 77 Å/mm at H-gamma. “3P 36g” indicates a 3-prism spectrum of dispersion 36 Å/mm at H-gamma. “S 20” designates a slit spectrum of dispersion 20 Å/mm. The appearance of a question mark in parentheses indicates that the instrumental configuration was inferred from the original paper.

3. Format information for Catalog and Databases

The tables below detail the various columns of data in the electronically-distributed versions of the galactic OB-star catalog and the UBVß and MK databases.

The Catalog

Note that BD numbers are in the format +dd nnnn while CPD and CD numbers are in the format +dd nnnnn.

If a star does not have a given cross-identification, the entry for that column will appear blank.

1X

I5 Alma LS (ALS) number

1X

A25 Source name

1X

A8 BD number

1X

A9 CPD number

1X

A9 CD number

1X

A6 SAO number

1X

A6 HD number

1X

A4 HR number

1X

A10 Notes

1X

F5.1 Magnitude (dummy value = 99.9)

1X

A1 Source for magnitude: V = pe, P = pg, N = none

1X

I2 RA hours

1X

I2 RA minutes

1X

F4.1 RA seconds

1X

A1 Sign of declination

I2 Declination degrees

1X

I2 Declination minues

1X

I2 Declination seconds

1X

F8.2 Galactic longitude, degrees

1X

F8.2 Galactic latitude, degrees

UBVß Database

1X

I5 Alma LS (ALS) number

A1 Flag for remark

1X

A25 Source name

1X

A2 DM identifier: BD, CD, or CP

A9 DM number

1X

A6 HD number

F6.2 V (dummy value 99.99)

2X

F6.2 B-V (dummy value 99.99)

F6.2 U-B (dummy value 99.99)

2X

I3 Number of UBV observations

F7.3 Hß (dummy value 99.99)

1X

I3 Number of Hbeta observations

A20 Notes to photometry

1X

F10.4 2000 right ascension, hh.mmss

1X

F10.4 2000 declination, +dd.mmss

1X

A25 Reference

1X

A25 First author

1X

A10 Sundry notes, variable identifier, etc.

MK Database

I5 Alma LS number

1X

A25 Source name

1X

A2 DM identifier: BD, CD, or CP

A9 DM number

1X

A6 HD number

1X

A8 Temperature Class

1X

A8 Luminosity Class

1X

A8 Spectral-luminosity qualifier

1X

A20 Dispersion description

1X

A20 Remarks

1X

F10.4 2000 right ascension, hh.mmss

1X

F10.4 2000 declination, +dd.mmss

1X

A25 Reference

1X

A25 First author

1X

A10 Remarks/other identifications

4. Remarks On Individual Stars

Each note begins with the ALS number(s) in boldface type. For CH stars, this is followed by parentheses containing the corresponding photographic magnitude(s) given in the CH catalog, otherwise the photoelectric B magnitude. Boldface numbers in parentheses are reference numbers. KN refers to reference (1), Klare and Neckel, AAS 27, 215-247 (1977).

Identification numbers 6001 through 13390 have been assigned to the LS-North stars, in increasing order of 1950-epoch right ascension. Notes for LS-North stars follow the same format as for LS-South stars, but with addition of the original LS-North identification numbers in square brackets.

46/47 (10.3/11.0) Magnitudes given by (8) for this close pair (B = 10.1 and 10.7 respectively; LS region A chart) are consistent with LS m_pg, while those in (47) (B = 10.8 and 10.2) are not. I have assumed that (47) interchanged identifications for these stars; that is, his stars 19-4 and 19-5 are taken to be LS stars 47 and 46, respectively.

98 (7.5) Variations in the spectrum of this pathological Wolf-Rayet star (EZ CMa) are discussed by O.C. Wilson, PASP, 60, 383-384 (1948), and a flux-calibrated spectrum of this star to the Lyman limit is discussed in Mccandliss, et. al., ApJ, 416, 372-378 (1993). Howarth and Schmutz, AA, 294, 529-535 (1995), reference (302), report a distance of 1.8 kpc for this star. Willis and Stevens (AA, 310, 577-591, 1996) report on ROSAT X-ray observations of this star, concluding that the 0.28-keV X-ray emergent emission has a characteristic radius of > 1000 solar radii. Harries, Howarth, SchulteLadbeck and Hillier [MNRAS, 302, 499-511, 1999] report that the continuum polarization of this star shows long-term quasi-periodic variations in both magnitude and position.

120 (11.3) Simbad attributes tabulated data (which disagrees with LS m_pg) to LS 120 via cross-reference of BD –08 1666. LS chart 5 shows two fairly bright stars (120 and 121) side-by-side. (40) remarks that this is a triple star.

166 (7.4) Gies, et. al., ApJ, 422, 823 (1994) remark that this star is a spectroscopic binary with a period of 6.0173 days. The companion 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 –19 1896. LS cross-lists 349 as KN 25, for which (1) and (2) both report B = 9.8. Simbad attributes the data in (2) to LS 422, but (2) cross-references KN 25 as CPD –20 2314, which Simbad assigns to neither 349 or 422. I have assumed both observations refer to LS 349, and that the CPD 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 carried out by Sterken, Vogt, and Mennickent (AA, 311, 579-586, 1996) reveals a periodic photometric variation for this star with a period of 92.7 days.

437 (12.1) High mass X-ray binary. See (877)

518 (8.6) High radial velocity due to galactic rotation.

675 (7.7) Variability in Hipparcos photometry (max. range 0.12 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

752 (11.5) (41) and (51) report B = 12.1 and 11.6 respectively. (51) cross-lists this star as CD –31 5034, which Simbad verifies; the finding chart appearing in (41) agrees with LS chart 18. Variable? LS notes emission.

840 (10.1) (63) gives B = 10.7; four other references report B = 10.1. Probably misidentified by (63), whose data are not included. Not crowded on LS chart 17; LS notes 4686 emission.

850 (4.1) Massa, et. al., ApJ, 452, 842-862 (1995) have studied the wind variability from this early-B supergiant. See also S. R. Colley, Observatory, 123, 96-97 (2003).

949 (2.0) Reported as variable by L.A. Balona, MNRAS, 254, 404-412 (1992). Time-resolved echelle spectroscopy of this star is reported by Reid and Howarth (AA, 311, 616-630, 1996), who find a period of 8.54 hours, with evidence of non-radial pulsation. vanderHucht, et. al., New Astronomy 2, 245-250 (1997), report a distance of 429 (–77) (+120) pc for this star based on Hipparcos parallax measurements, and conclude that it is located at the back of the Gum nebula. See also Schaerer, et. al., ApJ 484, L153 (1997). Blomme, et. al. (Hot Star Newsletter no. 77, July 2003) present radio and submillimeter observations of this star and discuss structure in the outer region of its wind.

952 (9.9) Apparently misidentified in (181), who gives B = 13.0, and may be referring to LS 951.

980 (1.6) vanderHucht, et. al., New Astronomy 2, 245-250 (1997), report a distance of 258 (–31) (+41) pc for this (WC8 + O7.5-8 III-II) binary based on Hipparcos parallax measurements, and conclude that it is a foreground object before the open cluster Cr173 and the association Vel OB2. Absolute visual magnitudes of –3.7 for the WC8 star and –5 for the O star are derived; they conclude that the latter indicates an O8.5 III star, as opposed to the O9 I that had previously been assumed. This star is one of the ionizing sources of the Gum nebula. See also Schaerer, et. al., ApJ 484, L153 (1997), who report a system mass of 29.5 +/- 15.9 solar masses, an effective temperature of 34000 +/- 1500 K for the O-star, and a luminosity of log L = 5.3 +/- 0.15 for the O-star. Eversberg, et. al. [PASP 111, 861-870 (1999)] report low-resolution, high signal-to-noise ratio spectropolarimetry of this system, remarking that it has the potential to represent a prototype of wind-wind interaction for massive stars.

984 (10.7) Probably misidentified by (11), whose data is not included. Appears to have a nearby companion of approximately equal magnitude on LS chart 21.

992 (12.9) Motch, et. al. [AA 323, 853-875 (1997)] classify this star as a likely massive X-ray binary.

1085 (5.1) An analysis of the interstellar lines in the spectrum of this B3 III + B3 V binary is reported by Wallerstein, Vanture and Jenkins, ApJ, 455, 590-597 (1995). The two stars are separated by 2700 AU, and the primary (= HD 72127A) is probably a 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 together.

1113 (5.0) Variability in Hipparcos photometry (max. range 0.06 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

1129 (10.6) Cross-listed by LS as KN 213 and CD –47 4273; LS gives no HD listing. Simbad cross-lists LS 1129 as CD –47 4273 and CPD –47 2607 and also gives no HD listing. For KN 213, (1) and (2) report B = 9.3 and 8.6, respectively. KN 213 is listed as HD 74580 in (1), and as CPD –47 2605 in (2). Simbad indicates that CPD –47 2605 and HD 74580 are the same star. LS chart 30 shows 1129 as the northeast component of a double in a small cluster. Probably neither (1) or (2) refer to “clean" measurements of the LS star.

1135 (11.2) Corti, et. al. (arxiv:astro-ph/0305226; 13 May 2003) find that this star is a short-period (2.75 days) O-type binary.

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 Vela X-1 X-ray source. Vankerkwijk, et. al., AA 303, 483-496 (1995) have obtained high-resolution, high signal-to-noise spectra of this star, finding evidence for varying tidal forces.

1268 (9.2) Noted as -Cygni variable by Vangenderen, et. al., AA, 264, 88-104 (1992). Variability in Hipparcos photometry (max. range 0.20 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

1358 (9.9) Double on LS chart 31.

1362 (12.3) Central star of a planetary nebula; Heber., et. al., AA, 194, 223-229 (1988)

1376 (10.0) V = 9.82 – 10.99

1411 (9.9) Oudmaijer, et. al. [MNRAS 300, 170-182 (1998)] report that this Be system possesses a fast wind in excess of 1000 km/sec, with polarization changes across H-alpha. They conclude that the system consists of a fast polar wind from the star and a slowly expanding disk wind.

1415 (10.1) Reference (48) reports B–V = 1.14 and a spectral type of B2 for this star, whereas numerous others give B–V ~ 0.4 and ~ O9 III. Data from (48) discarded.

1490 (11.3) V = 9.60 – 10.80.

1523 (9.6) A long-term multiwavelength spectrophotometric study of the Luminous Blue Variables (LBV's) HR Car (= LS 1523) and AG Car (= LS 2035) by Shore, Altner and Waxin (AJ, 112, 2744, 1996) reveals them both to have luminosities on the order of 10⁶ L_Sun with evidence of dust formation in the AG car wind during the most recent outburst.

1568 (10.1) Mean RV and standard deviation computed from four measures reported by Feast, et. al., who note emission in various hydrogen lines. Niemela (PASP, 84, 450, 1972) records absorption-line velocities for this star ranging from –179 to +37 km/s, and concludes that it is probably a spectroscopic binary with a period of a few days.

1582/1583 (11.2/10.1) LS cross-lists 1583 as KN 413 [which (1) lists as HD 302841] and (2) as CPD –57 3265. Simbad concurs with this CPD identification, and also lists 1583 as CD –57 3234, but attributes HD 302841 to LS 1582. Both stars reside in a crowded area in cluster IC 2581.

1627 (10.3) Colors not appropriate for a B star; U-B may be missing a negative sign in (96).

1656/1657 (12.0/8.3) LS misidentifies 1656 as HD 91824; 1657 is HD 91824. Data in (1) and (2) attributed to HD 91824 is assigned to LS 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 number 21 in the finding chart of Feast, MNRAS, 118, 618 (1958). However, both (30) and (31) indicate that this star is an M1 supergiant with B–V = 2.0. When precessed to 1875, the coordinates of LS 1673 match very closely to those of CPD –57 3506, which is star number 22 in Feast's chart, a B1 II star. I have assumed that Stephenson and Sanduleak marked the wrong star; the data given is that for number 22.

1679 (10.0) In NGC 3293. LS catalog gives no HD number for this star, but Simbad claims LS 1679 = HD 92007 = CPD –57 3526 = CD –57 3350 = Feast (344) no. 27 (B = 9.0). Feast identifies his no. 27 (B = 9.0) as CPD –57 3527 and his no. 6 (B = 8.3) as HD 92007. The HD catalog gives m_pg = 9.1 for HD 92007, favoring identification with Feast no. 27, but also cross-lists this star as CPD –57 3527. Feast no. 27 has been noted as a Beta Cep variable. Comparing charts from Feast and the LS catalog shows that Feast’s no. 27 is clearly LS 1679 [see also chart in Feinstein and Marraco (30)]. Klare & Neckel (1) claim that HD 92007 = Hbg 435; they and (2) give B ~ 8.4 for this star; their data disregarded in view of this confusion. Data for HD 92007 in (283) likewise disregarded. I take Feast no. 27 to be LS 1679; Feast no. 6 is designated here as ALS 15752. No cross-reference 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 ( = LS 1689). Correctly identified in (30) and (31). Misidentified as HD 92007 in (1).

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 center of IC 2599.

1698 (12.2) Motch, et. al. [AA 323, 853-875 (1997)] classify this star as a likely massive X-ray binary.

1774 (10.2) (149) and (171) give an incorrect HD number (302989) for this star.

1780 (9.1) Double in LS region D chart. (45) notes variability.

1801 (9.7) Simbad cross-identifies this star as HD 93026, CPD –58 2594, CD –58 3518, and as star 35 in Bochum 10. (9) identifies their star 13 (B = 11.4) as LS 1801, but this disagrees with the LS region D chart; star 13 lies just SW of 1801; (89) also gives B = 11.4. (171) identifies their star 35 (B = 9.7) as HD 93026, but this also disagrees with the LS chart; their number 39 (B = 11.4) would appear to be LS 1801. On the LS chart, 1801 appears comparable in brightness to 1790, which has B = 10.8. The LS catalog agrees with the Simbad CD cross-reference, but lists no HD number; Simbad lists only the UBV data from (171). I have assumed that (9) mis-labeled their finding chart, and that star 39 of (171) is LS 1801. The data given in the compilation are for star 13 of (9), star 39 of (171), and LS 1801 as reported by (89). Identification as HD 93026 must be regarded as uncertain.

1811 (8.6) Note that (61) is discordant.

1820 (8.2) Crowded in the Tr 14/16 complex; (LS 1819 is 3 sec West/10" South). Resolved as binary (separation 0.055 arcsec, m = 0.9) by Nelan, et. al. [AJ 128, 323 (2004)].

1839 (7.5) Possibly an eclipsing variable.

1849 (8.5) Morrell et al. [MNRAS, 326, 85-94 (2001)] report the results of high-quality orbital-element analysis for this double-lined O3 V + O8 V binary, deriving a semi-amplitude of 133 +/- 2 and 314 +/- 2 km/sec for each binary component. If the O3 component has a mass of 22-25 M(Sun), the mass of the O3 primary is derived to be 52-60 M(Sun). The inclination of the orbital plane is estimated to be 55 degrees.

1855 (10.0) LS erroneously cross-lists this star as RT Car. LS 1855 and RT Car are respectively numbers 15 and 16 in (32).

1868 (9.5) Eta Carinae. Damineli, Conti, and Lopes [New Astronomy, 2, 107-117 (1997)] suggest that Eta Car may in fact be a binary system of high eccentricity. Ebbets, et. al. [ApJ 489, L161-L164 (1997)] report that high-quality spectra of Eta Car between 1203 and 1765 Angstrom obtained with the GHRS reveal a morphology suggesting a composite of features seen in B-type supergiants in the range B2 Ia to B8 Ia, with additional lower temperature lines also seen. Davidson and Humphreys review Eta Car and its environment in an extensive paper appearing in ARAA 35, 1-32 (1997). Davidson, et. al., [New Astron., 3, 241-245 (1998)] point out that an 85-day periodicity in the X-ray emission of Eta Car has been reported, while spectroscopic events recur with a period of 5.5 years, and suggest that if the X-rays are produced by colliding winds in a 5.5-year binary system, then the 85-day period may represent pulsation or rotation of the primary star, or conceivably the orbit of a third object. JanotPacheco, et. al. [A&A, 137, 407-418 (1999)] present photometric data and high-resolution, high signal-to-noise optical spectra of Eta Car, finding evidence for multiperiodic variations, specifically, frequencies of 1.29, 1.78, 3.82, and 4.51 cy/day. Damineli, et. al. [ApJ, 528, L101-L104 (2000)] report confirmation of the binary nature of Eta Car, with a periodicity of 2020 +/- 5 days, arguning for a colliding wind binary scenario that rules out multiple shell ejection. Martin and Koppelman [AJ 127, 2352-2361 (2004)] present HST observations of the central star.

1869 (8.9) Resolved as binary (separation 0.015 arcsec, m = 1.0) by Nelan, et. al. [AJ 128, 323 (2004)].

1870 (10.0) Resolved as binary (separation 70 arcsec, m = 1.6) by Nelan, et. al. [AJ 128, 323 (2004)].

1871 (10.4) Analysis of high-resolution spectra by Freyhammer, et. al. (873) show this system to be a detached eclipsing binary. They classify the syatem as O9.5 V + B0.3 V, and estimate a distance of 2.6 +/- 0.1 kpc, an age of ~ 2 Myr, and a photometric period of 1.47 days. Member of Trumpler 16.

1872 (8.6) Appears to be the northeast component of a double on LS region E chart. A larger-scale chart of this area around Eta Car is given by Feinstein, Marraco, & Muzzio (94). Comparing their chart to the LS chart appears to indicate that FMM 34 = LS 1872; the other component of the double is HD 93343 according to their chart. Both are OB stars. I designate HD 93343 as ALS 16717. Simbad cross-lists LS 1872 as HD 93343.

1881 (7.6) Extensive wings on the short wavelength side of each stellar line; suspected binary.

1932 (7.2) Prinja, Massa, Howarth, and Fullerton [MNRAS, 301, 926-934 (1998)] report results of a 28-day IUE time-series campaign to monitor the stellar wind of this O5 giant, finding repeatability in the wind structures with a 7.1-day period.

1964 (13.1) Niemela and Gamen [AA 362, 973-977 (2000)] rerport that this object is a double-lined WN+O binary with a aperiod of 3.16415 days.

1973 (8.1) Data from (95) (B=10.8) not included. In LS  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, 223-229 (1988)

2033 (9.4) Variability in Hipparcos photometry (max. range 0.2 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

2035 (8.2) AG Car. See 1523 above. Recorded radial velocity calculated from absorption line velocities.

2062 (10.3) HD 305757 = CPD –59 2901. (1) reports B = 11.6 whereas (83) and (85) give B = 10.8. The LS chart ( Car region) appears to agree with that in (83); the CPD number reported in (1) agrees with Simbad. Probably misidentified by (1), whose data are not included.

2138 (11.3) HD 303776; misidentified by LS as HD 96286 ( = LS 2141), 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. (160) lists these as two separate stars; the data reported for CPD –60 2647 (adopted here) is consistent with that given for LS 2234 by (9) and (93). Data reported for HD 306182 by (160) likely erroneous.

2244 (9.7) HD 306185 = CPD –60 2671. As in LS 2234 above, (160) lists these as two separate stars; the data reported for CPD –60 2671 is consistent with that reported in (9) and (103). Data reported by (160) for HD 306185 is likely erroneous; note that (103) reports CPD –60 2671 as double.

2258 (9.3) Berdnikov and Turner, Ast. Lett., 21, 603-632 (1995) 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 included.

2430 (9.9) Suspected binary.

2462 (10.2) Probably misidentified by (84) (B=8.8) whose data are not included.

2513 (10.5) Errata in (34); correct data given here.

2557 (10.3) The kinematics of this high velocity star are discussed by Kilkenny (Observatory, 94, 4, 1974).

2564 (11.7) As 2513.

2584 (10.6) Steiner and Diaz (PASP, 110, 276-282 1998) note this star as one of four (V617 Sgr, HD 104994, WX Cen, and V Sge) that they define as V Sagittae stars. These stars show high-ionization species (O v and N v); the emission of He II lambda 4686 is stronger than twice the strength of H beta. The orbital periods vary from 5 to 12 hr, and the orbital light curves have shapes of either double eclipse or sine waves. The close similarities of these objects to supersoft X-ray sources is pointed out. The nature of the compact star in these system is still an open question.

2645 (11.9) (45) and (82) report B = 10.2 and 11.9 respectively. (45) remarks that the fainter of two stars at this position was measured; his colors are not indicative of an OB star. Data from (45) are not included.

2800/2802 (10.2/10.9) In NGC 4755. Comparing LS and (152) finding charts indicates that 2800 and 2802 are respectively stars G and K of (152). LS 2806 is apparently star IV-18 of (152). (314) notes LS 2800 as a ß variable.

2803 (6.7) uvby colors given by (66) for HR 4890 (= LS 2813) correspond to those of LS 2803 according to other sources; data from (66) therefore attributed to LS 2803 = HR 4887. In NGC 4755.

2810 (11.2) Apparently star III-1 of (152), an identification with which (107) and (140) agree, despite their B magnitudes disagreeing with LS m_pg. Crowded field in NGC 4755. (314) notes LS 2810 as a ß variable.

2813 (6.7) See comments for 2803.

2814 (9.2) Misidentified by (107) and (140) as star III-5 of (152); actually star II-1. Possible spectroscopic binary in view of large radial velocity range.

2816 (9.8) Noted by (314) as a ß variable. Possible spectroscopic binary in view of large radial velocity range.

2883 (10.9) Johnston, et. al. (MNRAS, 268, 430-436, 1995) note that LS 2883 is the binary companion of a pulsar, PSR B1259–63, one of only two binary pulsars known (at that writing) where the companion mass exceeds 3 solar masses. The orbital period is 1236.79 days, projected semi-major axis 1295.98 light-seconds, and eccentricity 0.8698. The pulsar period is 47.76 ms. In a subsequent paper, these authors (MNRAS, 279, 1026-1036, 1996) measured the magnetic field of LS 2883 to be approximately 40 mG at 45 stellar radii, the first direct measurement of the magnetic field of a Be-star disk.

2946 (9.7) Uncrowded on LS chart 46. (2)gives V = 9.57, which has been assumed to be a typographical error, and changed to 8.57. (45) notes uncertain photometry.

2998 (8.2) Probably misidentified by (158) (B = 6.9), whose data are not included.

3024 (9.4) Berdnikov and Turner, Ast. Lett., 21, 603-632 (1995) report a period of 6.46 days for this Cepheid.

3114 (11.6) Only absorption-line values are used in computing the recorded radial velocity; one discordant observation discarded.

3184 (11.9) Drilling, et. al. [AA 329, 1019-1027 (1998)] report this object, BX Cir, to be an extreme Helium star [n(H)/n(He) < 0.00015], specifically, an early B-type giant with a pulsational period of 2.5 hours, T(eff) = 23300 K, and E(B-V) = 0.27. Kilkenny, at. al. [MNRAS, 310, 1119-1127 (1999)] report on over 95 hours of photometry of this object, and give a period of ~ 0.1065784 days, and an amplitude in V of ~ 0.03 mag.

3247 (10.0) Velocity –90 km/s when corrected for solar motion and galactic rotation. Very similar to HD 119069 in terms of longitude, spectral type, radial velocity and distance.

3320 (10.3) Muzzio (36) points out that two OB stars are present at the position indicated by the LS catalog. These lie along a NS line, separated by about 34 arcsec, with the southern star (CPD –59 5864) slightly brighter (V = 10.70) than the northern (CPD –59 5863; V = 10.82). Klare and Neckel (1) evidently chose the southern star to be the LS object, whereas Drilling (45) and Lynga (323) chose the northern star. SIMBAD assigns LS 3320 to the northern star, an identification also implied by the LS chart. I have adopted the northern object to be the LS star. The southern star subsequently entered my database as ALS 19115.

3328 (8.9) (46) indicates V = 9.39 and B-V = 0.34; six other references give V = 8.2, B–V = 1.0. Simbad does not verify the HD and CD numbers quoted in LS (134959, –58 5973). (45) suspects variability, (7) and (36) note emission. Not clearly marked on LS chart 51; crowded with LS 3327. Turner, AJ, 111, 828-833 (1995) concludes that this star is a B2 Ia-O hypergiant of absolute magnitude M_v = –7.88 + 0.66.

3403 (9.7) Magnitudes given by both (27) and (45) disagree with LS m_pg; colors in (27) do not correspond to an OB star, so that data disregarded. Clearly marked on LS chart 48.

3404 (11.7) This star, along with 3405, 3420, 3421, 3424, 3429, 3430, 3432, and 3433 are all members of the Norma group. Mean radial velocity for the system is –36 + 6 km/s after correction for solar motion.

3422 (11.2) Cross-listed by LS as KN 1028 = CPD –55 6802, for which (1) gives B = 11.4 and (2) B = 8.9. Note that (2) refers to CPD –54 6802, which Simbad does not cross-list as an LS star. Probably misidentified in (2), whose data are not included.

3601 (10.3) Misidentified as LS 3106 by (4).

3625 (6.2) Variability in Hipparcos photometry (max. range 0.11 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

3646 (6.8) As LS 949.

3655 (12.0) LS magnitude favors (10); crowded on Fig. 12 of (10) and on LS chart 55.

3672 (5.6) Rauw, et. al. (871) report an analysis of an extensive set of high-resolution spectra of this massive binary, deriving a classification of O7.5I(f) + ON9.7I. The period is about 9.81 days.

3674 (12.4) LS magnitude favors (183), who notes this star as spectral 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 misidentified by (27), whose data are not included.

3719 (9.6) Cross listed in LS as KN 1195 = CPD –47 7860, for which (1) gives B = 9.9 and (2) B = 10.5. Simbad tabulates no UBV. Note that (2) refers to CPD –47 7858. Probably misidentified by (2), whose data are not included.

3728 (11.3) LS m_pg favors (124) over (116).

3733 (11.8) As 3728.

3745 (7.0) Note that B-V from (115) is about equal to the negative of other B-V values; no change to that data has been made herein.

3765 (7.3) As LS 949.

3785 (6.6) LS chart 60 indicates a rather faint star; probably intended 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 HD 326305. Finding charts show this star to be about 1.25 arcminutes south and 2 seconds esat of a brighter object. Apparently the fainter, southernmost object is LS 3791 (HD 326305, V ~ 10.1) and the brighter one is KN 1221 (HS 152042, V ~ 8.3). The latter, brighter, star is designated as number 16055 in this database.

3794 (8.8) HD 152076. (111, 117, 122, 126) give B = 8.7, while (124) gives B = 11.2. (124) remarks that LS cross-reference the wrong HD star (152076), and that they measured the star marked on the LS chart 60 some 2 minutes north of 152076. LS m_pg suggests that Stephenson and Sanduleak had HD 152076 in mind. Data from (124) are not included.

3804 (8.6) Noted as possibly variable by (122).

3810 (6.9) Luhrs [PASP 109, 504-513 (1977)] has derived a colliding-wind model for this WC7 + O6 binary system. Struve [ApJ 100, 384-387 (1944)] gives a period of 8.82 days for this system.

3828 (6.0) As LS 949. See also S. R. Colley, Observatory, 123, 96-97 (2003).

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 star spanning 10 years has been reported by Sterken, Stahl, Wolf, Szeifert and Jones [AA 303, 766-772 (1995)]. Large-amplitude variations are present, indicating that this 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 appears about as 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. [AA 368, L29-L33 (2001)] have analysed Halpha and Hbeta line profiles of this peculiar supergiant, concluding that it may be close to the LBV phase, but it is also possible that it could be a B[e] supergiant. Miroshnichenko, et. al. [Ref 852; AA 406, 673-683 (2003)] report high-resolution optical spectroscopy of this object, concluding that this system is a B+F binary with an orbital period of on the order of 6 months whose orbital plane is viewed nearly edge-on. These authors deduce a distance of 1.5 +/- 0.5 kpc, and suggest that this system represents an advanced evolutionary stage of beta Lyrae type binary.

3995 (6.8) As LS 949; discovered to be an eclipsing binary by L.A. Balona, MNRAS, 254, 404-412 (1992).

4018 (7.4) Possible unresolved double-lined binary.

4080/4081 (12.5/12.1) Close pair enveloped in nebulosity. (119) remarks that 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.

4225/4226 (6.0/10.7) Radial-velocity, optical and UV light curves for this hot, massive, non-eclispsing binary in the open cluster NGC 6383 have been solved simultaneously by Pachoulakis [MNRAS 280, 153-166 (1996)], who concludes the pair to be an O6 V + O7 V pair with masses and radii of 32 and 9.6 solar, respectively, with the slightly more massive primary hotter (42500 K) than the secondary (35000 K). Mass loss rates are estimated at 3.0 x 10^-6 solar masses per year from each star.

4275 (11.2) A spectographic investigation by Niemela, et. al. [Rev. Mex. Astron. Astrofis., 31, 45-49 (1995)] reveals this star to be an O6 + WN binary system with an orbital period of 12.595 days.

4293 (11.3) Presumed to be star 3 in Ruprecht 127 in (10), not star 2. Crowded field on LS chart 64.

4352 (9.4) (45) claims that this star is not CPD –28 13519; but Simbad concurs with the CPD identification. Colors reported in (45) are not those of an OB star.

4420 (12.2) B magnitudes reported by (27) and (124) fall equidistant from LS m_pg.

4825 (11.5) Ryans, et. al. [ApJ 490, 267-272 (1997)] report high-resolution spectroscopic observations of this star, concluding it to be a young supergiant lying on the far side of the galaxy at a distance of 21 +/- 5 kpc. Multiple interstellar components are observed.

4893 (10.2) In NGC 6604. Confusion seems to exist between this star, BD –12 4979, and LS IV –12 22 (= BD –12 4978; ALS 9474.) The photographic magnitudes are respectively 10.2 and 11.2, with 4893, the brighter of the two, about 23 arcsec south and 2 seconds east of 9474. Stars 3 and 4 of (10) appear to be 4893 and 9474, respectively. Data for (39, 60, 161) ascribed in those references to 4893 are assigned here to the fainter star, 9474. Reference (27), which reports B = 10.8, may have measured both together. Note that 4893 = LS IV –12 23, ALS 9475.

4910 (10.9) In NGC 6611. (39) reports V = 10.1, B-V = 0.8; four other references give V = 9.6, B-V = 0.85. (45) suspects this crowded star may be variable. I have assumed that (39) is referring to LS 4905, also m_pg = 10.9.

4919 (9.7) Variable?

4954 (9.5) See remarks for 1268. Variability in Hipparcos photometry (max. range 0.31 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

4956 (9.5) Robberto and Herbst [ApJ, 498, 400-412 (1998)] present high spatial resolution images of thermal emission from the nebula surrounding this luminous blue variable. They estimate a distance of 1.2 kpc; the dust emission has a bipolar structure. See also remarks for 1268. Variability in Hipparcos photometry (max. range 0.19 mag) discussed by van Leeuwen, et. al., AAS 128, 117-129 (1998).

5039 (11.4) Marti, Paredes, and Ribo, [AA 338, L71-L74 (1998)] report this system to be a radio-loud, massive X-ray binary. See also LS 7373 below. Paredes, Marti, Ribo, and Massi [Science 238, 2340-2342 (2000)] claim that this systrem is a high-energy gamma-ray emitter, and Ribo, et. al. [AA, 384, 954-964 (2002)] claim that this system is a runaway microquasar with a velocity component perpendicular to the galactic plane of larger than 100 km/s.

6312 [I +64 34] (11.7) Ignace, et. al. (Hot Star Newsletter no. 77, July 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 quadruple trapezium system in NGC 281. I take ALS (6388, 6389, 16471, 19498) = HD 5005 (D,A,B,C). If a reference does not discriminate between components, I attribute the data to ALS 6389.

6407 (2.1) [I +60 133] Gamma Cas. Miroshnichenko, et. al. [PASP 114, 1226-1233 (2002)] report a study of high-resolution spectra of this bright Be star. They find two components in the emission-line profile variations, a long-term one and a periodic one. The periodic one has a period of 205 days; they conclude this be related to orbital motion in a binary system. The long-term variations represent changes in the peak intensities and radial velocities of the spectral lines on a timescale of a few years.

6517 [I +65 10] (12.4) High mass X-ray binary. Liu, et. al. [Chinese Astronomy and Astrophysics 22, 463-468 (1998)] find evidence for an HII region around the neutron star in this system.

6704 [I +62 181] (9.9) Bern and Virdefors (392) report U–B = +0.39, while Hiltner (60) gives U–B = –0.41. I have assumed that the former dropped the negative sign.

6730 [I +60 179] (10.3) Mayer (376) indicates that he measured LSN I +60 180 (= ALS 6734), but cross-references BD +60 322, which the LSN catalog gives as LS I +60 179. The stars are of nearly equal photographic magnitude, with I +60 180 lying 19 arcminutes north and 19 seconds of time west of I +60 179.

6754 [I +62 185] (10.7) Lutz and Lutz (382) report (V, B–V) = (11.36, 0.64) for this star, in conflict with Hiltner's result. Hiltner's result is favored in view of its agreement (B = 10.72) with the photographic magnitude. The Digitized Sky Survey shows a star about 1 mag. fainter and 2–3 minutes east of 6754; the Lutz's may have measuered this star by mistake.

6757 [I +61 235] (12.2) Motch, et. al. [AA 323, 853-875 (1997)] classify this star as a likely massive X-ray binary.

6855 [I +62 198] (10.6) Bern and Virdefors (392) claim this star (BD +62 332) to be an M0 star with V = 8.98, B–V = 1.95. It is assumed that this is a misidentification.

6978 [I +69 5] (12.3) Eclipsing binary of the W UMa type; V = 12.30 – 13.60; P = 0.5005 days.

7289 [I +61 286] (8.8) Polcaro, et. al. (Hot Star Newsletter No. 75, Feb.-Mar. 2003) report substantial H-alpha variability for this star.

7373 [I +61 303] (11.4) The X-ray spectrum of this binary system is discussed by Leahy, et. al., ApJ 475, 823-828 (1997). Quasi-simultaneous H-alpha and radio observations are discussed by Zamanov, et. al., ApSpSci 243, 269-274 (1996). Peracaula, et. al . [AA 328, 283-289 (1997)] report that 6-cm radio “microflares” from this system exhibit a period of 1.4 hours; they tentatively attribute these flares to secondary luminosity-driven shocks. Marti, et. al. [AA 329, 951-956 (1998)] report on deep 6-cm VLA observations of this object in an unsuccessful effort to search for extended radio emission. Strickman, et. al. [ApJ 497, 419-430 (1998)] present the results of a multiwavelength monitoring campaign targeting the gamma-ray source 2CG 135+1 in an attempt to confirm the association of this object with LSI +61 303, but their signal-to-noise ratio was insufficient to establish a spectral or intensity correlation of the high-energy emission with simultaneous radio, optical, and infrared emission of LSI +61 303. Apparao [AA 356, 972-974 (2000)] found that the ratio of the equivalent width of the blue wing to that of the red wing of the H-alpha line shows an orbital variation, attributed to obscuration caused by the post-shock gas of a shock produced by the supersonic orbital motion of the secondary through the gas disk of the Be star. A study of long-term optical spectral observations is reported by Liu, et. al. [AA 359, 646-650 (2000)]. Zamanov, et. al. [AA 351, 543-550 (1999)] report an anlysis of the H-alpha spectrum of this system, detecting the same 26.5-day period as found at radio wavelengths, and finding that the peak separation of the H-alpha emission line seems also to vary over a time scale of 1600 days, a result they attribute to variations in the mass loss rate of the Be star and/or density variability in the circumstellar disk. Massi, et. al. [AA 414, L1-L4 (2004)] provide evidence for precessing relativistic radio jets in this system. Mirabel, et. al [AA 422, L29-L32 (2004)] argue that this star is a runaway microquasar with velocity 27 +/- 6 km/s.

7374 [I +61 304] (8.2) V. McSwain (Hot Star Newsletter no. 76, May 2003) reports orbital elements for this spectroscopic binary system, and suggests that this system plus LS I +61 303 (7373 above) probably belong to a sub-cluster within the Cas OB6 association.

7504 [I +68 17] (7.0) Cepheid SU Cas. Moffet and Barnes (ApJS, 44, 427, 1980) give V = 5.74 – 6.18 and P = 1.949 days.

7513 [I +56 74] (12.1) This star has been designated as variable ZZ Per, but Haug (47) reports variability doubtful.

7724 [I +59 187] (5.4) Hiltner (60) gives B–V = –0.43; the negative sign is presumed to be a typographical error.

8023 [V +44 17] (11.3) Motch, et. al. [AA 323, 853-875 (1997)] classify this star as a likely massive X-ray binary.

8221 [V +42 24] (8.4) SX Aur. Chambliss and Leung (429) report this system to be a semidetached eclispsing binary consisting of two B-stars with a period of 1.21008 days and with light curves of the ß Lyrae type. The magnitude given here is that reported by them as the system’s maximum brightness.

8306 [V +33 25] (11.0) Simbad attributes Hiltner's (60) photometry (V, B–V, U–B) = (10.64, 0.31, -0.62) to both this star and ALS 8308 [V +33 27]. The coordinates given by Hiltner (his no. 446) better match those for 8306.

8308 [V +33 27] (11.5) See 8306 above.

8415 [V + 34 46] (12.5) Imbedded in nebulosity in Sharpless 237. The LSN catalog assigns the same BD number, +34 1074, to ALS 8415 and 8417 [V +34 46 and V +34 47]. On the basis of the photographic magnitudes I take BD +34 1074 = ALS 8417.

8416 [V +34 45] (11.2) Imbedded in nebulosity in Sharpless 237.

8417 [V +34 47] (11.7) Imbedded in nebulosity in Sharpless 237. See 8415.

8422 [V +32 8] (4.9) Eclispsing variable V1016 Ori. Vitrichenko, Klochkova, and Plachinda [Astr. Lett., 24, 296-302 (1998)] report a radial-velocity analysis for this system, determining masses and radii of (10.2, 3.2) and (2.55, 1.8) for the two components, and a radius of 3.6 for the dust shell around the secondary component.

8468 [V + 26 5] (9.8) Wang and Gies [PASP 110, 1310-1314 (1998)] present radial velocity measurements of this X-ray transient system, A0535+26. Observational errors are too large to claim detection of the Be star orbital motion, but they set a semiamplitude limit of < 10.6 km/sec.

8751 [V +20 19] (7.4) Garnier, et. al. (453) report U–B = –0.39 for this star, whereas a number of other sources report U–B = –0.88 or –0.89. The Garnier, et. al. value is assumed to be a misprint, and is taken as –0.89.

8847 [V + 22 43] (9.3) Hiltner (60) notes very strong H and K lines.

9377 [IV +06 2] (11.6) Jeffery [MNRAS, 294, 391-398 (1998)] reports a spectral analysis of this high-gravity extreme helium star, determining Teff = 31000 K (making it the hottest high-gravity extreme helium star yet studied), and log g = 4.05. LS IV + 6 2 lies close to the boundary of the helium star pulsation instability finger near T-eff similar to 27000 K. Available data indicate that the radial velocity is variable, but give no indication of amplitude or period.

9474 [IV -12 22] (11.2) See 4893 above.

9517 [IV –11 14] (10.2) WC7+OB binary; Hiltner [ApJ 102, 492-495 (1945)] gives a period of 29.6 days and a semi-amplitude of 165 km/sec for the WC star.

9960 [IV +07 6] (99.9) Long-period (262 days) binary RZ Oph. Forbes and Scarfe [PASP 96, 737 (1984)] report UBV photometry with V varying between 9.85 and 10.64.

10301 [II + 18 4] (8.1) Chentsov [Ast. Lett. 30, 325-331] argues that this star is a white hypergiant.

10308 [II +12 7] (10.4) Hiltner (60) gives U–B = –0.25, but Hiltner & Iriarte (161) give U–B = +0.25. The former would appear more for a B1 supergiant; the latter is changed to -0.25.

10539 [II +29 15)] (6.9) V1507 Cyg. Berdyugin and Tarasov [Ast. Lett. 24, 111-115 (1998)] report an analysis of UBVRI polarimetric observations of this interacting binary system, concluding that linear polarization arises from light scattering in a shell surrounding the unseen secondary component. The orbital inclination is estimated at 46.4 +/- 2.1 degrees.

10571 [III + 40 2] (5.4) V380 Cyg. Popper and Guinan [PASP, 110, 572-579 (1998)] discuss spectroscopic observations of this binary system with a B1.5 II-III primary.

10591 [II +24 22] (6.3) Hiltner (60) identifies this star, his no. 844, as BD +24 3914 = HD 187983. According to SIMBAD, HD 187982 and HD 187983 are the same object. The LSN catalog misidentifies this star as HR 7593; it is actually HR 7573.

10594 [II +27 21] (12.0) Turner (518) misidentifies this star as HD 332918, which is actually LS-North II +27 20 (= ALS 10592), a 10-th magnitude F6 supergiant.

10601 [III +46 1] (5.3) Fernie (46) reports B–V = –1.15 for this star, apparently an error. His data is not included. Israelian, et. al. [MNRAS, 316, 407-417 (2000)] report on a spectral time-series analysis of this runaway binary supergiant O star, finding radial velocity variations with a possible quasi-period of 6.4 days as well as night-to-night variations in the position and strength of central emission reversal of the H-alpha profile.

10603 [III +47 1] (5.5) Wehinger and Hidajat (525) misidentify this star as BD +47 2919 and as V819 Cyg. It is BD +47 2939; V819 Cyg is actually LS-North III +47 2 (= ALS 10614).

10712 [IV –12 111] (11.4) Arkhipova, et. al. [Ast. Lett., 28, 257-260 (2002)] claim that this star is a protoplanetary nebula with irregular variability on a timescale of ~ 1 day with delta(V, B, U) ~ (0.3, 0.3, 0.4).

10896 [II +36 22] (9.2) BD +36 3914 = HD 228053. Hiltner (60) misidentifies this star, his no. 880, as HD 228052. See also 10898 below.

10898 [III +45 3] (9.9) BD +44 3365 = HD 191781. Hiltner (60) misidentifies this star, his no. 881, as HD 228053. See also 10896 above.

10924 [II +20 19] (10.0) FG Sge. Arkhipova, et. al. [Ast. Lett., 24, 361-364 (1998); Ast. Lett., 24, 365-371 (1998)] report UBV and spectroscopic observations of this system, while Tatarnikov and Yudin [Ast. Lett., 24, 303-308 (1998)] present a model for the dust shell around this star.

10934 [II +38 11] (8.7) Ignace, et. al. (Hot Star Newsletter no. 77, July 2003) report an analysis of the wind outflow of this WR star.

10968 [II +32 19] (10.8) Hiltner (60) gives U–B = +0.33 for this star, apparently too red for a B0 star, whereas Lutz and Lutz (382) give U–B = –0.44. Hiltner's value is presumed to be a typographical error, and is taken here as –0.33.

11089 [II +37 46] (9.7) WN7+OB binary; Hiltner [ApJ 113, 317-319 (1951)] gives a period of 10.6 days and a semi-amplitude of 240 km/sec for the WN7 star.

11114 [II +40 15] (5.9) W. P. McKibben, et. al., PASP 110, 900-905 (1998) report radial velocity measurements and a single-lined spectroscopic orbit for the O-type star HD 193322A, which they show to be a 311-day binary system that has a distant third companion in a 31-year orbit. HD 193322B appears to be an unresolved spectroscopic binary. Thus HD 193322, the central object in the open cluster Collinder 419, is a multiple system that contains at least five stars.

11163 [II +38 42] (8.7) Munch [ApJ 112, 266-288 (1950)] presented one of the first detailed analyses of this WN5 + O6 V-III eclipsing binary system. Marchenko, et. al., ApJ 485, 826-838 (1997) report on high signal-to-noise optical spectroscopy and simultaneous narrowband continuum photometry of this system. Antokhin, et. al. [ApSpSci 254, 111-131 (1997)] discuss the velocity law in the extended photosphere of the WN5 star. Keeping [PASP 58, 236-237 (1946)] gives orbital elements.

11192 [III +43 7] (6.8) Marchenko, et. al. (Hot Star Newsletter no. 77, July 2003) present an analysis of high-quality spectra of this colliding-wind WR+O binary system. The system has high eccentricity (0.881 +/- 0.005), a period of 2899 days, and orbital inclination 50 +/- 15 degrees.

11209 [II + 36 65] (11.0). Marchenko, Moffat, and Eenens [PASP 110, 1416-1422 (1998)] report an analysis of radial velocity measurements of this (WN5o + O5 III-V) 21.7-day binary system. The WR lines show phase-locked variability; the masses are estimated as 36-54 solar masses for the WR star and 26-33 solar masses for the O star for a system inclination of 68 degrees. Ivanov, Valchev, Georgiev, Barba, and Iliev [RMxAA, 35, 25-29 (1999)] obtained 123 high-resolution CCD spectra of this system over 40 nights, and give a refined period of 21.6878 +/- 0.0001 days.

11334 [II +37 92] (10.8) Walborn and Howarth (670) remark that this star is a single-lined spectroscopic binary with a period of 4.8 days.

11703 [III +55 5] (7.5) Hiltner (60) reports B = 10.22 for this star, while Simonson (555) gives B = 7.68. The latter is favored in view of the LS catalog photographic magnitude; Hiltner’s data are assumed to be a misidentification and are disregarded.

12008 [III +59 11] (7.6) G. Catanzaro (Hot Star Newsletter no. 76, May 2003) reports an abundanace analysis of this system, finding that Fe, Ni, and Zn are underabundant.

12072 [III + 54 8] (9.1) Abt et. al. [ApJ, 161, 477 (1970)] report that this star is a spectroscopic binary with a period of 111.6 days. See (669).

12096 [III +57 20] (5.3) Harries, et. al., MNRAS 295, 386-396 (1998) report new spectroscopic observations of this O+O binary (= LZ Cep). They find LZ Cep to be a semi-detached system with the secondary star filling its Roche lobe, and report a distance modulus of 9.6 +/- 0.2, which is slightly smaller than the distance modulus to Cep OB2 (= 9.9). The reddening of LZ Cep is also at the lower end of the cluster range, suggesting that the binary is located on the near side of the cluster.

12143 [III +54 16] (10.0) Negueruela, et. al. (875) present an analysis of X-ray and high-resolution optical spectroscopy of this 9.5-day massive X-ray binary.

12230 [III +55 28] (9.2) Barbier, et. al. (385) give U–B = +0.19 for this star, far too red for a B2 giant. This is assumed to be an error, and is not incorporated in the database.

12324 [III +56 42] (12.8) NX Cep. Miller & Wachmann [Ricerche Astron. 8, 367 (1973)] give this star as spectral type F2.

12858 [III +62 39] (10.7) Hiltner (60) cross-references this star (his no. 1205) as BD +61 2472. However, it is clear from SIMBAD that BD +61 2472 = LS I +61 12 = SAO 20695 = ALS 13012, an identification which has been confirmed by precessing the BD coordinates. However, Hiltner’s 1900 coordinates for his no. 1205, when precessed to 1950, conform pretty closely to LS III +62 39 = ALS 12858. I have assumed that Hiltner did measure 12858, and wrote down the wrong BD number.

13175 [I +62 23] (9.5) Negueruela (Hot Star Newsletter no. 77, July 2003) reports observations of this triple system. The faintest member (BD +62 2296B) is a WN4 star, while the brightest component (BD +62 2296) appears to be a normal B2.5 Ia star, and the third visual component, BD +62 2296C, is a B0 III star.

13277 [I +60 56] (7.1) Fischer and Morrison, PASP 113, 821-828 (2001) discuss spectrum variability of this A-typer supergiant.

14805 (5.3) HD 57061; Tau CMa. van Leeuwen and van Genderen [AA 327, 1070-1076 (1997)] analysed Hipparcos data for this double-O-type system, showing that it also contains a massive close binary of period 1.282 days. This system contains both the longest period spectroscopic binary and the shortest period eclipsing binary known for O-type stars.

14499 [HD 163181] (7.0) Josephs, et. al. [PASP, 113, 957-963 (2001)] give orbital elements for this massive interacting binary, V453 Sco. P ~12 days, mass function ~ 9 solar masses.

14834 [HD 199140] (6.4) Beta-Cephei star BW Vul. Percy, Velocci, and Sterken [PASP 115, 626-627 (2003)] find that nonevolutionary period changes in this star are not the result of random cycle-to-cycle fluctuations as they are in several cooler types of pulsating variables.

15036 [HD 151804] (5.3) A summary of a study of wind and photospheric variability of this star appears in S. R. Colley, Observatory, 123, 96-97 (2003).

15089 [HD 172324] (8.6) High velocity star: v = -115 km/sec; see Bonsack & Greenstein (PASP, 68, 249 (1956)]

15197 (10.0) Resolved as binary (separation 0.077 arcsec, m = 2.4) by Nelan, et. al. [AJ 128, 323 (2004)].

15205 (10.7) Resolved as binary (separation 0.352 arcsec, m = 2.8) by Nelan, et. al. [AJ 128, 323 (2004)].

15757 [CPD –41 7742] (8.5) H. Sana (Hot Star Newsletter no. 76, May 2003) reports high-resolution optical spectroscopy of this binary system (P = 2.44 days), infering type O9 III + B1 III, and suggesting that the system may be an eclipsing binary.

16331 (10.0) Two CPD numbers appear to be assigned to this star: -57 2777 (= HD 302583) and –57 2759. The coordinates and magnitudes listed in Simbad are virtually identical. Star 316 in (48).

16388 [3 Vul] (5.0) Dukes, et. al. [AJ 126, 370-384 (2003)] report an analysis of differential uvby photometry of this star obtained over 7 years. This system is a multiperiodic 53-Per type single-line spectroscopic binary showing both line profile and light variations, with three modes. The primary and secondary masses are estimated as 4.16 and 0.65 to 1.1 solar masses, and the age of the system is estimated as 25 million years. The orbital period is 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 (84).

17186 (9.3) Confusion exists in the literature concerning BD indentifications for this star and ALS17381. I assign ALS 17186 = VandenBerg (1966, AJ 71, 990) star 92a, and ALS 17381 = VandenBerg 92b. Racine (40) respectively identifies these stars as BD –11 1763 and –11 1761, whereas Herbst, Racine and Warner (55) reverse these identifications. SIMBAD follows the Herbst et. al. identifications, which would appear to make sense if the lower BD number corresponds to the westernmost star (finding chart in Racine). SIMBAD apparently errs in assigning BD –11 1762 to star 92c: this BD number is about 6 arcminutes north of this tight grouping of three stars.

17381 (9.0) See 17186 above.

18544 (13.8) Paardekooper, et. al. [AA 404, L29-L32 (2003)] report brightness variations of 0.2 magnitudes on a time scale of hours for this WO4 + O5((f))) colliding-wind binary.

18773 (16.9) [V635 Cas] High-mass X-ray binary 4U 0115+634. Negueruela, et. al. (872) analyse photometry and high SNR spectroscopy for this system. The distance is estimated as 7-8 kpc and the binary period is 24.3 days.

18894 (9.1) [HD 138503] IT Lib. Eclipsing binary (2 B-stars) about 1 kpc above the galactic plane. See Martin, PASP 115, 49-58 (2003).

19498 See 6388 above.

19605 (16.0) Optical counterpart to X-ray pulsar 1WGAJ1958.2+3232. Suggested to be a B0 Ve star by Israel, et. al. (887), but Negueruela, et. al. [AA 354, L29-L32 (2000)] find this classification untenable and suggest the object is instead an intermediate polar.

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