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Catalog of Galactic OB Stars
B. Cameron Reed
Department of Physics
Alma College
Alma, Michigan 48801
e-mail: reed@alma.edu
(989) 463–7266
Last Update:
2 March 2011
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Contents
1.
Introduction
2.
Strategy
2.1
2.2
2.3
UBV Photometry
Spectroscopy
uvby Photometry
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, and of the WEBDA database. 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).
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1. Introduction
This project originated in the summer of 1991 when I began compiling a cross-reference
“catalog” and tabulation of published UBV 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 UBV 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 compilation has since been discontinued but interested readers may still obtain
those (for the LS-South stars) from the author. As of this writing (December 2005), 4-color
(Stromgren b-y, m1, c1) data have not been systematically searched for, but essentially all 4-color
data available from (over 1100) references compiled for the UBV and MK databases has been
incorporated. However, as 4-color and Hphotometry are often done together this should
capture much of the Stromgren photometry available for OB stars.
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 H. 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:
3
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-star 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 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, UBV photometry, MK
classifications, and some uvby photometry for “non CH” galactic OB stars.
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 criterion 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
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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 and 13391-14000 are 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.
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 [e.g., 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)] 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)] 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.
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.
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.
5
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 spectral
dispersion, etc.
In December 2006, coordinates for LS-North Volume I stars were replaced with more
accurate figures from Brian Skiff, who also pointed out a few new BD and HD cross-references.
2. Strategy
The primary criteria applied for incorporation of data into this compilation are originality
and adherence to the UBV 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.
Various of the LSN volumes overlap in sky coverage, leading to duplicate entries for 153
stars. In addition, there is also some overlap between the LSS and LSN catalogs, leading to 151
stars in common. Note is made of these duplicates in the catalog, and care taken to assign data
consistently to one star of a duplicate pair. 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.
FORTRAN format codes for reading the catalog and UBV 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
UBV 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
6
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
for 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 or Å
d
g
m/A
Cass
1P
2P
3P
C
G
IT
OP
P
RG
S
TG
Ångstrom
Hydrogen delta
Hydrogen gamma
microns per Ångstrom
Cassegrain spectrum
1-prism
2-prism
3-prism
Coude spectrum
Grating spectrum (reflection or transmission not specified)
Image tube spectrum
Objective-prism
Prism
Reflection grating
Slit
Transmission grating
7
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.
2.3
uvby Photometry
See comments in the first paragraph under Introduction above. The author’s long-term
intention is to undertake a systematic survey for uvby photometry as time permits.
8
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 UBV 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
1X
A25
1X
A8
1X
A9
1X
A9
1X
A6
1X
A6
1X
A4
1X
A10
1X
F5.1
1X
A1
1X
I2
1X
I2
1X
F4.1
1X
A1
I2
1X
I2
1X
I2
1X
F8.2
1X
F8.2
Alma LS (ALS) number
Source name
BD number
CPD number
CD number
SAO number
HD number
HR number
Notes
Magnitude (dummy value = 99.9)
Source for magnitude: V = pe, P = pg, N = none
RA hours
RA minutes
RA seconds
Sign of declination
Declination degrees
Declination minutes
Declination seconds
Galactic longitude, degrees
Galactic latitude, degrees
9
UBV Database
1X
I5
A1
1X
A25
1X
A2
A9
1X
A6
F6.2
2X
F6.2
F6.2
2X
I3
F7.3
1X
I3
A20
1X
F10.4
1X
F10.4
1X
A25
1X
A25
1X
A10
Alma LS (ALS) number
Flag for remark
Source name
DM identifier: BD, CD, or CP
DM number
HD number
V (dummy value 99.99)
B-V (dummy value 99.99)
U-B (dummy value 99.99)
Number of UBV observations
H (dummy value 99.99)
Number of Hbeta observations
Notes to photometry
2000 right ascension, hh.mmss
2000 declination, +dd.mmss
Reference
First author
Sundry notes, variable identifier, etc.
10
MK Database
I5
1X
A25
1X
A2
A9
1X
A6
1X
A8
1X
A8
1X
A8
1X
A20
1X
A20
1X
F10.4
1X
F10.4
1X
A25
1X
A25
1X
A10
Alma LS number
Source name
DM identifier: BD, CD, or CP
DM number
HD number
Temperature Class
Luminosity Class
Spectral-luminosity qualifier
Dispersion description
Remarks
2000 right ascension, hh.mmss
2000 declination, +dd.mmss
Reference
First author
Remarks/other identifications
11
uvby Database
1X
I5
A1
1X
A25
1X
A2
A9
1X
A6
F8.3
2X
F8.3
F8.3
2X
I3
1X
A20
1X
F10.4
1X
F10.4
1X
A25
1X
A25
1X
A10
Alma LS (ALS) number
Flag for remark
Source name
DM identifier: BD, CD, or CP
DM number
HD number
b-y (dummy value 99.99)
m1 (dummy value 99.99)
c1 (dummy value 99.99)
Number of uvby observations
Notes to photometry
2000 right ascension, hh.mmss
2000 declination, +dd.mmss
Reference
First author
Sundry notes, variable identifier, etc.
12
Photometric Note Codes
001 Emission
002 Double
003 Variable or suspect
004 Subdwarf
005 P Cyg star
006 WR star
007 See comments in Ref
008 Beta uncertain
009 ID uncertain
010 Beta to 0.01 only
011 Of star
012 UBV uncertain
013 Combined result
014 Crowded field
015 Brighter of pair
016 RV variable
017 DLSB
018 Combined pe/pg
019 CCD data
020 Carbon star
021 Beta Cep variable
022 4-color to 0.01 only
023 Shell star
024 A component
025 White dwarf?
026 H-alpha emission
027 Beta CMa variable
028 Transformed Tycho BV
029 B component
030 X-Ray binary
031 Transformed HST BV
032 Bessel BV filters
033 Eclipsing binary
034 Double?
035 n(UBV) not explicit
036 n(Beta) not explicit
037 n(UBV/Beta)not given
038 Double-light of both
039 Faint companion
040 He-rich
041 H-poor
042 Spectroscopic binary
043 Nebulosity
044 Multiple system
045 Beta variable
046 Cepheid
047 S Doradus variable
048 Alpha Cyg variable
049 O II strong
13
050 Hg II star
051 Mn II star
052 Si II star
053 Ap star
054 n(uvby) not explicit
055 uvby uncertain
056 Double lines?
057 AB components
058 ABC components
059 BC components
060 AC components
061 C component
062 Gamma Cas variable
063 Beta Lyrae variable
064 UBV to 0.01 only
065 D component
066 FG components
067 E component
068 V to 0.1 only
069 UBV from spectrophotometry
070 -------------------071 -------------------072 -------------------073 --------------------
14
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 mpg, 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.
140 (7.4) HD 53367. Pogodin et al. [A&A 452, 551-559 (2006)] present spectroscopic evidence
that this may be a binary system consisting of a main-sequence B0e star plus a 5 solar-mass premain-sequence secondary.
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.
640 (7.7) Boyajian et al. [PASP 119, 742-746 (2007)] report radial velocity variations for this
star due to wind variations.
15
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).
16
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; 13May2003) find that this star is a short-period
(2.75 days) O-type binary. Lajus & Niemela (arxiv:astro-ph/0601396; 18Jan2006) present an
analysis of spectra and photometry for this system, deducing that it is an eclispsing O6.5 V + B1
V 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 LSun 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).
17
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 mpg = 9.1 for HD 92007, favoring identification with Feast no. 27, but also crosslists 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.
18
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 orbitalelement 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 1765Å 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 85day 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, arguing 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 system 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 largerscale 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.
19
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)] report that this object is a doublelined WN+O binary with a period 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.
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.
20
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 Cep variable. See Reed, PASP 114, 249-252 (2002).
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. See Reed, PASP 114, 249-252 (2002).
2810 (11.2) Apparently star III-1 of (152), an identification with which (107) and (140) agree,
despite their B magnitudes disagreeing with LS mpg. Crowded field in NGC 4755. (314) notes
LS 2810 as a Cep variable. See Reed, PASP 114, 249-252 (2002).
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. See Reed, PASP 114, 249-252
(2002).
2816 (9.8) Noted by (314) as a Cep 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.
21
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 Mv = –7.88 + 0.66.
3378 (11.6) Pandey & Reddy (arXiv:astro-ph/0604023v1 3Apr2006) report a detailed abundance
analysis of this cool extreme helium star.
3403 (9.7) Magnitudes given by both (27) and (45) disagree with LS mpg; 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. HD 148937. A rare Of?p star. Naze et al. [AJ 135, 1946-1957 (2008)]
report on a detailed optical and X-ray study of this star, finding low-level variability in the
Balmer and HeII 4686 lines, and a possible periodicity of 7 days in the H line.
3655 (12.0) LS magnitude favors (10); crowded on Fig. 12 of (10) and on LS chart 55.
22
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. Note that (2) refers to CPD –47 7858. Probably misidentified by (2), whose data are
not included.
3728 (11.3) (116) gives V = 9.19 for this star; (116) data not included, nor that from the Tycho
catalog (861).
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 east 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 mpg 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.
23
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)]. Largeamplitude 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 analyzed 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, 673683 (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, 404412 (1992).
4018 (7.4) Possible unresolved double-lined binary.
4080/4081 (12.5/12.1) Close pair enveloped in nebulosity.
measured together; his observation dropped.
(119) remarks that both were
4142 (11.6) HD 319718 = Pis 24-1. See Ref. 1165; at least a triple system. NE component is
O3.5 If* and SW component O4 III (f+). 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, noneclipsing 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 spectrographic 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 mpg.
4452 (11.8) The wrong star appears to be marked on the LS chart. The LS coordinates indicate a
star about 5 arcminutes north of the one marked, which is too is too bright (probably HD
316499). Data for 4452 from (45) and (124) ignored. LS 4452 appears to be Hiltner (60)
number 675.
24
4522 (7.0) HD 163899. Saio et al. [arXiv: astro-ph/0606712v1 29Jun2006] report the detection
of 48 oscillatory frequencies < 2.8 cy/day with amplitudes of a few millimagnitudes or less in
this B supergiant.
4589 (12.0) HD 164740 = Herschel 36. Arias et al. (arXiv: 1001.3892v1 [astro-ph ST]
21Jan2010 report that this object is definitely a multiple system with at least three components: a
close massive O9 V + B0.5 V binary of period 1.54 days, plus a O7.5 V star, the most luminous
member of the system, which presents RV variations with a period close to 498 days.
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 mpg = 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 system 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. See also BoschRamon et al. arXiv astro-ph/0507412v1 (18 Jul 2005). Casares et al. (arXiv astro-ph/0507549v1
22 Jul 2005 and 0507549v2 27Sep2005) propose that the compact object in this system is a black
hole. Aharonian et al. [Science 309, 746 (2005)] find evidence for gamma-ray emission > 100
GeV from this system. Aharonian et al. [arXiv: astro-ph/0508658v2 1Sep2005 and astroph/0607192v1 10Jul2006] argue that this system may be a potential TeV neutrino source and that
the high-energy gamma-rays from this source are modulated with the 3.9-day orbital period of the
binary system.
6127 [I +61 135] (7.7) Boyajian et. al. [arXiv: astro-ph/0604247v1 11Apr2006] report a detailed
radial velocity analysis of this double system.
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.
25
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 longterm 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. Koenigsberger et al. [arXiv: astro-ph/0608226v1 10Aug2006] propose that puzzling
periodicities in this system may be explained by tidal interactions driving oscillations in a Bsupergiant star.
6698 [I +63 161] (10.6) Close (9”) pair, both blue. Huestamendia et. al. (1167) give the
companion as (V. BV, UB) = 10.79, 0.40, -0.41) on the basis of one measurement.
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 measured 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.
7206 [I + 58 80] (8.4) De Becker et al. [arXiv:0909.0643v1, 3 Sep2009] report a study of He II
4686 and H-beta line profile variability in this star and in ALS 7289 and 7398. Their
interpretation involves large-scale corotating structures modulating the profile of lines produced
in a strong stellar wind; there is no clear evidence for binarity.
7218 [I +52 3] (7.6) Boyajian et al. [ApJ 621, 978-984 (2005)] classify this star as a runaway
radial-velocity variable that is a possible single-line spectroscopic binary with a period close to 1
month.
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. See also 7206 above.
26
7373 [I +61 303] (11.4) Microquasar; see 5029 above. 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 analysis 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. Albert, et al. [Science 312, 1771-1773 (2006)] report on variable very-high energy ( > 100
GeV) gamma-ray emission from this system. Chernyakova et al. [MNRAS 372, 1585-1592
(2006)] find evidence for a variable X-ray spectral index of this system, which they argue can be
explained if the compact object is a rotation-powered pulsar.
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.
7398 [I +56 63] (9.3) See 7206 above.
7499 [I +60 267] (7.1) Hillwig et. al. (1135) give the components of this triple system as O7.5
V((f)), O7.5 V((f)) and O6.5 III((f)).
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 eclipsing binary consisting of two B-stars with a period of 1.21008 days and with
light curves of the  Lyrae type. The magnitude given here is that reported by them as the
system’s maximum brightness.
27
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) Eclipsing 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.
8475 [VI –02 3] (7.2)  Orionis E. Hesser et al. [ApJ 216, L31-L33 (1977)] found a period of
1.91 days for this magnetic, Helium-rich star. Oksala and Townsend [arXiv:astro-ph/0511454v1
15Nov2005] present new UBVRI observations of this star, finding that the magnetosphere has
remained stable over three decades but that the rotation period may be slightly longer than that
reported by Hesser et al.

8488 [VI –01 3] (7.1) An analysis of the spectral energy distribution of this star is presented in
Krticka, et al. [arXiv astro-ph/0509716v1 23Sep2005].
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.
8951 [VI +14 7] (6.2) Boyajian et al. [PASP 119, 742-746 (2007)] report that this star may be a
long-period (months) spectroscopic binary, but that velocity variations may be due to changes in
a circumstellar disk.
8983 [VI + 05 6] (7.5) HD 46149; binary. Degroote et al. [arXiv:1006.3139v1 16 Jun2010]
report evidence for pulsations in this star.
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.
28
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.
9922 [IV –01 7] (8.4) Lorenz et al. [MNRAS 360, 915-920 (2005)] present a spectroscopic and
photometric analysis of this eclipsing binary system. Period 1.364 days. The primary and
secondary masses are 10.1 and 5.3 solar masses. The secondary may be of type B4 IV, but
appears oversized and overluminous for such a mass.
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.
10588 [II +27 19] (12.6) D. G. Turner (Private Communication, September 2007) reports that
this star exhibits a light curve with a period of 1.85 days, possibly a large amplitude (0.3 mag in
V) slowly pulsating B star or a Beta Lyrae system, and that the spectrum looks like a normal B3
V star.
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 timeseries 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).
10885 [II +35 54] (8.1) HD 191612. Donati et al. [arXiv:astro-ph/0510395v1 13Oct2005] report
the discovery of a strong magnetic field (~-1.5kG polar strength) in this star. Howarth et al.
[arXiv:astro-ph/0707.0594v1 4Jul2007 report on extensive optical spectroscopy of this object,
establishing a double-line binary orbit of P = 1542 days and e = 0.45, and conclude that the
29
system is consistent with a ~O8 giant with a ~B1 main-sequence secondary. The Balmer and He I
lines show trongly variable emission which is highly reporoduclible on a well-determined 538day period.]
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.
30
11371 [II + 38 90] (12.5) WR 143. Based on near-IR spectroscopy and photometry of this
system, Varricat et al. [arXiv:astro-ph/0510152v1 5Oct2005] report strong indications of the
presence of a companion, probably an early-type (< B2.5) Be star.
11422 [III +41 36] (12.7) Cyg OB2 9. Naze et al. [AA 483, 543-546 (2008)] report evidence for a
2.355-year comnpanion to this object. An orbital solution is reported by Naze et al.
[arXiv:1006.2917v1 15 Jun2010].
11423 [III + 41 37] (9.9) Cyg OB2 8A. Blomme et al. [arXiv:1006.3540v1 17 Jun 2010] report
an analysis of the non-thermal radio emission from this binary system, finding phase-locked
variability in the radio fluxes. They also present an updated x-ray light curve; the radio and x-ray
light curves are anticorrelated.
11429 [III + 43 90] (11.5) Gvaramadze & Bomans [AA 485, L29-L32 (2008)] suggest that this
runaway star is a blue starggler formed via a close encounter between two tight massive binaries
in the core of Cyg OB2.]
11626 [III +47 20] (6.1) Percy et al. [PASP, 120, 311-316 (2008)] report differential uvbyUBV
photometry of this star for a period of over 2500 days, finding peak-to-peak amplitude of about
0.15 mag in each filter. Variability was not periodic, but there are characteristic timescales of 20
days, and, occasionally, 50 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
abundance 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.
12112 [III +52 24] (12.3) Sarkar et al. [arXiv:astro-ph/0707.0595v1 4Jul2007; ref (1185)] report
on high-resolution spectroscopy (R ~ 52000) of this optical counterpart to the high-velocity (-148
km/s) hot post-AGB star IRAS 22023+5249. Nebular parameters suggest that the central star
may be evolving into a compact, young PN.]
12143 [III +54 16] (10.0) Negueruela et al. (875) present an analysis of X-ray and highresolution optical spectroscopy of this 9.5-day massive X-ray binary. Blay et al.
[arXiv:0806.4103v1 25 Jun 2008] discuss the unexpected finding of a slow, dense wind from
this object, rare for a O9.5 V star.
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.
31
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-type supergiant.
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.
14744 [HD 60848] (6.6) Boyajian et al. [PASP 119, 742-746 (2007)] report radial velocity
variations for this star possibly related to nonradial pulsations.
14760 [MCW 176; HD 14633] (7.3) Boyajian et al. [ApJ 621, 978-984 (2005)] classify this star
as a runaway single-line spectroscopic binary with a period of 15.4 days.
14781 [HD 36695] (5.2) Terrell et al. [arXiv astro-ph/0610202v1 6Oct2006] present new radial
velocities and interstellar reddening measurements of thie detached, short-period (1.48 days)
eclipsing binary, estimating it as a B1 V + B4.5 V system.
14788 [1 Ori C] (5.2) Wade et al. [arXiv astro-ph/0601623v1 26Jan2006] comfirm the
presence of a globally-ordered kG-stength magnetic field in the photosphere of this star. 
14804 [HD 54879] (7.6) Boyajian et al. [PASP 119, 742-746 (2007)] report H-alpha emission for
this star that may originate from a binary companion.
14805 [HD 57061; Tau CMa] (5.3) van Leeuwen and van Genderen [AA 327, 1070-1076
(1997)] analyzed 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.
14819 [HD 149438; Tau Sco] (2.6) Donati et al. [arXiv astro-ph/0606156v1 7 Jun2006] report
the discovery of a medium-strength (~ 0.5 kG) magnetic field on this star, making it the thirdhottest magnetic star known. A rotational modulation with a period of 41 days is evident. The
magnetic structure is unusually complex for a hot star, with significant power in sphericalharmonic modes of degree up to 5.
14820 [HD 149757; Zeta Oph] (2.6) Villamariz & Herrero [arXiv astro-ph/0507400v1
18Jul2005] speculate that this high rotational velocity runaway star may be the product of the
evolution of a close binary system.
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.
32
14973 [HD 110432] (5.6) An analysis of time-serial echelle data for this hard, variable X-ray
source is discussed in Smith & Balona [arXiv astro-ph/05090946v1; 5 Sep2005 and v2
24Nov05].
15012 [HD 136504;  Lup] (3.2) Uytterhoeven, et al. [arXiv astro-ph/0507376v1; 15 Jul 2005]
report this star as a double-lined spectroscopic binary with orbital period 4.5597 days and
eccentricity 0.277. A third body is present. The secondary is a  Cep variable.
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) Sana (Hot Star Newsletter no. 76, May 2003) reports highresolution optical spectroscopy of this binary system (P = 2.44 days), inferring type O9 III + B1
III, and suggesting that the system may be an eclipsing binary. In a later paper, Sana et al. [arXiv
astro-ph/0509542v1 19Sep2005] present a detailed, high-resolution study of this system, arguing
for classifications O9 V + B1-1.5 V. Sana et al. further analyze the wind interaction in this
system in [arXiv astro-ph/0510822v1 29Oct2005].
16044 [CD –42 11721] (12.7) Fernandes et al. [MNRAS 377, 1343-1362 (2007)] discuss an
analysis of high-resolution spectroscopy of this emission-line object, deriving an effective
temperature of 14000 K, a radius of 17.3 solar radii and a luminosity of 104 solar. They advocate
that this star may be a post-main sequence object, although a pre-main sequence nature cannot be
ruled out due to uncertain distance.
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 singleline 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 identifications 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
33
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)
analyze 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).
18901 (12.2) [LSE 44] Friedman et al. arXiv:astro-ph/0510593v1 (19 Oct 2005) report on an
analysis of column densities of interstellar D I, O I, N I, and H2 toward this subdwarf O star
made with FUSE.
18954 (11.6) HD 321589. Skiff (private communication) speculates that this star might be the
nucleus of a PN.
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 that the object is instead an intermediate polar.
19606 [WR 146] (13.2) High-resolution radio observations of this colliding-wind binary system
are discussed by O’Connor et al. [arXiv:astro-ph/0509231v1 8 Sep 2005].
19652 [MWC 297] (14.3) Acke et al. [arXiv:0804.1212v1 [astro-ph] 8 Apr 2008] present an
analysis of H, K, and N-band interferometric spectrograms of this object, revealing a compact
circumstaller cloud.
20155 (21.1) In Westerlund 1. Koumpia and Bonans [Proc. IAU Symp. 272, 1-2 (2010);
arXiv:1009.4709v1] report thi system to be a semi-detavhed DLSB; B0.5Ia+ and OB types.
20195 (13.2) McCuskey (Ref. 1085, star 22-29) misidentifies this star as LS V + 22 6; his star
22-43 is the LS star (ALS 8589).
21078 (18.5) Ref. (1236) reports a heliocentric radial velocity of +708 +/- 15 km/s, galactically
unbound.
21092 [Cyg OB2-17] (12.6) Stroud et al. [arXiv:1002.0707v1 [astro-ph.SR] 3 Feb 2010] report
that this system is a massive eclipsing double-lined spectroscopic binary with components O7Ia
+ O9 I.
34
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26.
27.
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32.
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35.
36.
37.
38.
39.
40.
41.
42.
43.
44.
45.
46.
47.
48.
49.
50.
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