00020+2706 = ADS 17175
--------- Speckle observations of 85 Peg are showing considerable
theta residuals in comparison to the orbit of Hall
(1949 AJ, 54, 102). (Hrt1992b)
00061+6341 = HD 108
--------- Hutchings (1975) presented a preliminary orbit with a
period of 4.6 d, but subsequent work has cast doubt on
the reality of the orbit (Underhill 1994a). (Msn1998a)
00084+2905 = alp And
1988.6880 Separations and magnitude differences are derived by model
fitting to calibrated squared visibilities, using
measurements with the Mark III interferometer. This paper
also includes a determination of orbital elements and masses.
(MkT1992a)
00122+5337 = Bu 1026 AB
--------- An orbit for this system was published in Hrt1996a.
00173+0852 = ADS 238
--------- The measure reported in McA1982b for 1976.6220 is spurious
and has been deleted from this catalog.
1985.745 Large and irregular residuals preclude the correction of
an orbit. (Tok1985)
00177+5126 = HD 1337 (AO Cas)
--------- The classification is from the UV tomographic analysis
of Bagnuolo & Gies (1991). (Msn1998a)
00283-2020 = HR 108
1979.7730 This measure was omitted in McA1982d.
1982.7657 This autocorrelogram was remeasured; the new results
are listed here.
1989.9382 This has long been a difficult visual system, with the
two components remaining within 0".2 of each other
throughout the orbit. With this observation we have
completed a full revolution using speckle data alone,
and have derived new orbital elements which will be
published shortly.
00318+5432 = ADS 434
1972.837 550/100 + 753/100 filters (Wck1973)
00323+0657 = McA 1
--------- The Aa component of ADS 449 apparently went through
periastron some time during 1987 - 1990. (Hrt1992b)
00352-0336 = ADS 490
1979.5326 This measure was incorrectly attributed to ADS 2200 in
McA1982d.
00372+7149 = HDS 86
1997.7289 Large change in separation seen since Hipparcos epoch.
(Msn1999b)
00374-3904 = PCPC2
--------- Other IDs uncertain; based on Simbad search
using epoch-1950 coordinates 003456-392028 from Whi1991.
00386-3903 = PCPC2
--------- Other IDs uncertain; based on Simbad search
using epoch-1950 coordinates 003609-391934 from Whi1991.
Listed as possibly resolved by Whi1991.
00416+2438 = HR 178
1983.9362 According to Bnu1984, this (and presumably other) negative
results may be due to a delta m between 1.5 and 3.
00479-2921 = I 261
1989.9437 Having had only one other measure in the last 35 years,
this pair needs further observation, especially since
we appear to be near periastron at this epoch.
00528+5638 = HD 5005
--------- This is a trapezium system (Abt 1986) which lies at the
center of the cluster IC 1590 at a distance of 2.94 +/-
0.15 kpc (Guetter & Turner 1997). All four components
were observed and appeared to be single. (Msn1998a)
00561-8237 = CD-83 13
--------- Listed as possibly resolved by Whi1991.
00567+6043 = ADS 782
1975.636 Disk unresolved in H alpha emission and in H beta. (Bla1977a)
00568+6022 = ADS 784
1979.7703 Theta was incorrectly given as 308.6 in McA1982d.
--------- The measure for 1979.7730 given in McA1982d was a spurious
preliminary measure of the observation on 1979.7703,
and has been deleted from this catalog.
--------- New orbital elements for this visual multiple system,
including a combined speckle/spectroscopic orbit for
the speckle astrometric component, have been
published by Cole et al. (1992 AJ, 103, 1357). (Hrt1992b)
00573+2326 = HR 271 = eta And
--------- Errors are given as "error ellipses"; these values are
tabulated below. Columns include date (BY), major and
minor axes of the ellipse (in mas), and ellipse
orientation (in degrees). (MkT1993b)
1990.5359 0.57 0.04 107.1
1990.5687 0.12 0.02 105.8
1990.5742 0.17 0.02 105.2
1990.6125 0.43 0.05 102.7
1990.6262 0.12 0.03 98.5
1990.6426 0.09 0.02 96.9
1990.6563 0.08 0.02 93.3
1990.6591 0.06 0.01 85.7
1990.6646 0.24 0.02 81.0
1990.6673 0.06 0.02 82.2
1990.6728 0.09 0.03 100.6
1990.6837 0.61 0.09 78.9
1990.7056 0.08 0.02 92.4
1990.8233 0.08 0.02 98.0
1991.6037 0.22 0.04 105.1
1991.6557 0.10 0.02 88.5
1991.6584 0.12 0.03 98.1
1991.7077 0.10 0.03 96.5
1991.7104 0.08 0.02 99.7
1991.7132 0.05 0.01 84.4
1991.7460 0.08 0.02 84.3
1992.6413 0.19 0.03 85.5
1992.6441 0.56 0.05 96.3
01015+6921 = ADS 836
1984.9965 This autocorrelogram was remeasured; the new results
are listed here.
01024+050 = HDS 135
1997.7180 Mean motion indicates P ~ 80 yr, rho decreasing.
(Msn1999b)
01083+5459 = HR 321 = mu Cas
--------- these papers also compare their observations with
published orbits and discuss luminosities and masses of
components, helium abundances, etc. (Mcy1993, Pie1985,
Kar1986b, Hay1992)
01198-0029 = ADS 1081
1985.8430 This autocorrelogram was remeasured; the new results
are listed here.
01198-0029 = Fin 337
1982.7629 (also 1982.7657, 1983.7106) A mistake in reduction resulted in
90 degree errors for these three measures in McA1987b.
01234+5808 = ADS 1105
--------- First measured by F.W. Struve in 1836 at an angular separation
of 0".68, this system had opened to 1".2 by 1910, then steadily
closed to 0".35 at the time of the first speckle measurement in
1978. Based on a preliminary visual/speckle orbit, the pair
reached an apparent minimum separation of 0".01 in the spring of
1984.
1983.7107 This autocorrelogram was remeasured; the new results are listed
here.
01243-0655 = Bu 1163
--------- This system underwent periastron in late 1988, an event
now covered by speckle observations. (Hrt1992b)
--------- A new interferometric orbit of this very eccentric
(e = 0.94) system is in preparation. (Hrt1993)
01296+2250 = A 1910 AB
--------- An orbit for this system was published in Hrt1996a.
01376-0924 = Kui 7
1980.7179 This measure was omitted in McA1983.
1982.7657 This autocorrelogram was remeasured; the new results are listed
here.
01492+4754 = CHR 4
--------- Although this new component is indicated as Aa, we have not
firmly established whether it is associated with the A or B
component of the wide pair.
01546+2048 = bet Ari
1988.6742 Separations and magnitude differences are derived by model
fitting to calibrated squared visibilities, using
measurements with the Mark III interferometer. This paper
also includes a determination of orbital elements and masses.
(MkT1990)
02019+7054 = ADS 1598
1980.7205 This measure was incorrectly attributed to ADS 1958 in McA1983.
02038+7013 = Mlr 375
1983.0663 This autocorrelogram was remeasured; the new results are listed
here.
02039+4220 = ADS 1630
--------- See discussion in BLM1978.
02132+4414 = CHR 5
--------- The negative results obtained during 1976 - 1980 are apparently
due to a large magnitude difference.
02134+5106 = HR 645
1981.9602 Single line SB, P = 4.5 yr. Halbwachs (1981 A&AS, 44,
47) predicts a maximum separation = 0".047. (Bag1984b)
02145+6631 = HR 640
1983.9364 Composite spectrum star. Markowitz (1969 Dissertation, Ohio
State Univ.) gives classifications B9V + G0II-III, with delta m
= 0.2 magnitude. (Bnu1984)
02157+2503 = Cou 79
1985.738 Cou 79 passed periastron earlier than predicted. Now the orbit
is definitive. (Tok1985)
1986.567 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
--------- An orbit for this system was published in Hrt1996a.
02229+4129 = HD 14633
--------- Rodgers (1974) made a preliminary orbital analysis
(P =15.3 d) but the variations appear to be more
complicated than originally claimed (Bolton & Rodgers
1978). (Msn1998a)
02268+5853 = HD 14947
--------- Garmany & Stencel (1992) include this star in Per OB1.
(Msn1998a)
02290+6724 = CHR 6
--------- Heintz (1962 Veroff. Sternw. Munchen 5, 136) found a submotion
to the visual orbit of ADS 1860 AB (P = 840 yr, a = 2".27) with
a period of 52 years and an amplitude of 0".11. The component
listed here may coincide with Heintz' astrometric component.
1985.8540 This autocorrelogram was remeasured; the new results are listed
here.
02327+6127 = HD 15558
--------- Both visual components were observed and appeared to be
single. (Msn1998a)
02333+5218 = ADS 1938
1982.7604 This autocorrelogram was remeasured; the new results are listed
here.
02360+0652 = HR 753
--------- This object was misidentified as HD 61660 in McA1978c.
02366+1226 = HR 763 = McA 7
1982.7659 These three measurements of 31 Ari were based on
reprocessing 1984.7046 of archival video data. A
combined spectroscopic/speckle 1988.6554 orbital
analysis of this very close system is now in progress,
in collaboration with F.C. Fekel.
--------- This system has a small Delta m (~0.1 in the blue, 0.3
in the red) as determined from lunar occultation
measures by Africano et al. (1978). Orbits of this
system have been published by Balega & Balega (1989,
SvAL, 14, 393) and Mason (1994, Ph.D. thesis, Georgia
State Univ.; 1995, PASP, 107, 799); a further analysis
is in progress. (Hrt1996b)
02402+0436 = HDS 347
1997.7208 Mean motion indicates P ~ 90 yr, rho increasing.
(Msn1999b)
02408+6117 = HD 16429
--------- Both visual components were observed: A was resolved
(CHR 208 Aa) but B appeared to be single. Gies &
Bolton (1986) found a large scatter in radial
velocities (but could not find a suitable period), and
this suggests that at least one component may be a
spectroscopic binary. (Msn1998a)
02422+4012 = McA 8
--------- Analysis of the spectroscopic/interferometric orbit is given by
McAlister (1978 ApJ, 223, 526).
1977.0867 This measure was omitted in McA1979a.
02424+2000 = HR 793
1981.6847 Occultation binary, known to have a variable radial velocity.
(Bag1984b)
02449+1007 = HR 813
1985.745 A preliminary spectroscopic orbit with a period of 1202 days has
been published by Abt (1965 ApJS, 11, 429). (Tok1985)
02487+3107 = GJ 9102
1981.6875 HD 17433 was misidentified as Gliese 113 in Bag1984b. It is uncertain
whether this observation is of HD 17433 or of GJ 113 = HD 17382.
02518-2117 = See 21
1989.9330 This very close visual system was discovered at a
separation of 0".36 and has closed steadily for over
90 years. It is unknown at this point whether the
system is still approaching periastron or has begun
to widen. (Hrt1993)
02537+3820 = ADS 2200
--------- A measure on 1979.5326 was incorrectly attributed to ADS 2200 in
McA1982d; it actually belongs to ADS 490.
02543+5245 = HR 854
--------- Analysis of the spectroscopic/interferometric orbit is given by
McA1981c.
03023+0405 = HR 911
1975.634 Disk possible marginally resolved (0".014 +/- 0".005) at 400 and
425 nm. (Bla1977a)
1975.639 Disk possible marginally resolved at 460 nm. (Bla1977a)
03048+5330 = HR 915
1975.7815 Uncertain angle readout (Bla1977a)
--------- Analyses of the spectroscopic/interferometric orbit are given by
McA1982a and by Ppp1987.
03082+4057 = HR 936
--------- See discussion and orbital elements in Lab1974.
--------- Analysis of the spectroscopic/interferometric orbit is given by
Bonneau (1979, A&A, 80, L11).
03141+5934 = HD 19820 (CC Cas)
--------- The classification is from the tomographic analysis of
Hill et al. (1994). (Msn1998a)
03174+0739 = Hyades vB 1 = HD 20430
--------- ADS 2451 = Bu 1039 with rho = 2".2 and Delta m = 6.0
is outside detection window. (Msn1993a)
03266+2843 = CHR 9
--------- This is UX Ari, an RS CVn type binary that is not eclipsing.
The spectrum shows three components (Fekel, 1986 private
communication), two of which are identified with the 6.44-day
system described by Carlos & Popper (1971, PASP, 83, 504),
while the third is possibly the component listed here.
03272+0944 = HR 1038
1975.629 Marginally resolved at 450 nm? (Bla1977a)
03284+2248 = Bag 2 = 66 Ari
--------- Agreement is poor between this observation and the only
other measurement, by Balega (1988, private
communication). (Hrt1992b)
03311+1544 = HDS 443
1997.7181 Large change in separation seen since Hipparcos epoch.
(Msn1999b)
03327+3540 = BD+35 714 = HD 21847
1991.8989 This object is a new addition to older Hyades member
lists added by Schwan (1991 A&A, 243, 386), although
Griffin (1992 private communication) doubts that this
object is actually a cluster member. (Msn1993a)
03337+5752 = CHR 117
--------- See McA1992 for a preliminary orbital analysis of this
high-space-velocity binary. (Hrt1992b)
03378+1526 = HR 1102
--------- This star was misidentified as BD+17 0593 = SAO 93525 in the
first speckle catalogue.
03465+2415 = H 341 = CHR 12
1985.8488 Pleiades cluster member. This measure is from
reanalysis of archival data. Not listed as an SB by
Abt et al (1965 ApJ, 142, 1604), but it may show
measurable velocity variation at some phases of a
possibly eccentric orbit. (Msn1993b)
03482+2419 = H 693 = CHR 155
1991.9045 Included in the Pleiades cluster survey of Abt et al.
(1965 ApJ, 142, 1604), who did not detect variable
RV. Pearce & Hill (1975 Pub DAO, 14, 319) did notice
velocity variation at the 1% level, and Liu et al.
(1991 ApJ, 377, 141) found the system to be a SB2,
although large velocity difference may imply a closer
companion than this. (Msn1993b)
03483+2325 = HR 1172
--------- Misidentified as SAO 76125 in the first speckle catalogue.
03492+2408 = H 878 = CHR 125
1989.7067 Pleiades cluster member. Possible long-period SB
(Hoffleit 1982, Bright Star Catalogue). Frequently
unresolved, probably due to large Delta m. (Msn1993b)
03496+6318 = HR 1158 = Car 1
1995.948 Theta corrected from published value of 213 degrees,
following email message from Eric Aristidi 11/28/97.
Erratum to be published in A&A, probably 1/98.
03544-4021 = Fin 344 AB
1989.9438 This is the first observation of this system since
those of Finsen in the 1960's, and is considerably
closer than any of his results. It is known that in
some instances Finsen's rho values appeared
systematically larger than those of speckle; further
observations of this system will determine whether
such is again the case.
04007+2023 = Hyades vB 9 = BD+19 641
--------- SB with P > 7 yr according to Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
04036-3611 = CD-36 1581
--------- Listed as possibly resolved by Whi1991.
04037-1545 = A 2913
1989.9413 This system closed steadily from its discovery at
0".45 in 1915 to 0".22 in 1959; this is the first
observation in 30 years so it is unknown whether the
pair has passed through periastron.
04044+2025 = Hyades RHy 49
1996.0656 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
LP ID from Luyten et al. (1981 Proper Motion Survey with
the 48-inch Schmidt Telescope, LIX, U. Minn). Candidate
Hyades member; Reid considers definite binary. (Rei1997)
04049-3527 = CHR 224 AC
--------- Surprisingly, no record of this wide companion to the
0".8 pair I 152 is listed in the WDS, despite 17
observations spanning 90+ years since Innes' (1897,
ANac, 143, 171) discovery in 1896. Misidentification
appears ruled out, since both the Innes pair and the
new component are seen on two separate occasions.
(Hrt1996b)
04069-2200 = Hu 1363
1994.8069 Quadrant determined by speckle imaging analysis. (Hor1996)
04077+1509 = Hyades vB 11 = HD 26015
--------- ADS 2999 = STF 495 with rho = 3".8 is outside
detection window. (Msn1993a)
04077+1509 = Hyades vB 12 = HD 26015
--------- ADS 2999 = STF 495 with rho = 3".8 is outside
detection window. (Msn1993a)
04078+6220 = HD 25638 (SZ Cam)
--------- The classification is from Chocol (1980). The
discovery of a speckle companion (CHR 209 Aa) with a
period of some 60 y confirms the third body model
advocated by Mayer et al. (1994) based on the
appearance of the spectrum and variations in the time
of light curve minimum (they suggest a third body
period of 50.7 y). Another light curve solution is
given by Harries et al. (1997b). The B component (HD
25639) was also observed and appeared to be single.
Classification of the B component is from the WDS.
(Msn1998a)
04089+2912 = MWC 2376 = HD 26090
--------- ADS 3017 = Bu 1232 with predicted rho = 0".038 was
apparently somewhat closer and thus unresolvable.
Griffin et al. (1988 AJ, 96, 172) find this to be a
SB but doubt its membership in the Hyades in spite of
its inclusion by Wayman et al. (1965 Royal Obs.
Bull., 98). (Msn1993a)
04113+0532 = Hyades vB 14 = HD 26462
--------- CPM companion with rho = 124".1 is outside detection
window. An additional component was noted as
spectroscopic by Griffin et al. (1988 AJ, 96, 172).
(Msn1993a)
04119+2338 = CHR 14 = HD 284163
--------- Observed under poor seeing conditions. Griffin & Gunn
(1981 AJ, 86, 588) found a 2.4-day SB. (Msn1993a)
04120+5016 = CHR 15
--------- Van Maanen (1941 Ap.J. 94, 396) suspected this star to be a
binary, but these are the first measurements of a companion.
04136+0743 = A 1938
--------- An orbit for this system was published in Hrt1996a.
04155+2048 = Hyades RHy 119
1996.1230 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
LP ID from Luyten et al. (1981 Proper Motion Survey with
the 48-inch Schmidt Telescope, LIX, U. Minn). Candidate
Hyades member; Reid considers definite binary. (Rei1997)
04157+2049 = Hyades vB 162 = HD 26874
--------- The 55.1-day SB of Griffin & Gunn (1981 AJ, 86, 588)
is outside detection window. (Msn1993a)
04162+1648 = Hyades RHy 126
1995.8821 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
LP ID from Luyten et al. (1981 Proper Motion Survey with
the 48-inch Schmidt Telescope, LIX, U. Minn). Candidate
Hyades member; Reid considers possible binary. (Rei1997)
04176+1657 = Hyades vB 22 = HD 27130
--------- The 5.6-day SB of Griffin et al. (1985 AJ, 90, 609) is
outside detection window. (Msn1993a)
04180+1815 = Hyades vB 23 = HD 27149
--------- The 75.6-day SB of Batten & Wallerstein (1973 Pub DAO,
14, 135) is outside detection window. (Msn1993a)
04185+2135 = HR 1331 = Hyades vB 24 = McA 14
--------- Analysis of the spectroscopic/interferometric orbit of this
Hyades binary is given by McAlister (1977 ApJ, 212, 459).
1978.1490 Theta was incorrectly given as 325.5 degrees in McA1980b.
1991.8938 HR 1331 (51 Tau) is a spectroscopic binary first resolved
with speckle interferometry by McA1977. A new orbit with a
period of 11.3 years was determined by Dombrowski (1991,
Ph.D. thesis, Georgia State University). (Msn1993a)
04187+1632 = ADS 3135
1978.6183 The date of this observation was given incorrectly as 1977.6183
in McA1980b.
--------- Observed under poor seeing conditions. ADS 3135 is a SB
according to Griffin et al. (1988 AJ, 96, 172). (Msn1993a)
04198+1538 = HR 1346 = Hyades vB 28
--------- This object was misidentified as HR 1349 in McA1978c.
--------- Observed under rather poor seeing conditions. BLM1982
also report a large magnitude difference. (Msn1993a)
04209+1352 = Hyades vB 34 = HD 27483
--------- The 3.06-day SB of Northcott & Wright (1952 JRASC, 46,
11) is outside detection window. (Msn1993a)
04220+1405 = Hyades vB 38 = HD 27628
--------- The 2.14-day SB of Abt (1961 ApJS, 6, 37) is outside
detection window. (Msn1993a)
04224+1118 = J 259 = HD 286770
--------- The 3-year SB of Griffin et al. (1988 AJ, 96, 172) is
outside detection window. (Msn1993a)
04228+1504 = Hyades vB 40 = HD 27691
--------- The 255.5-year binary, ADS 3169 = STT 82 AB is outside
detection window, although part of a peak is seen at the
edge of the window at the expected position angle,
according to the orbit in the Worley & Heintz (1983 Pub.
USNO, 24, part VII) orbit catalog. A wider companion
(LDS 1166 AC, rho = 62", M = 17.8) and a 4-d SB of
Sanford (1921 ApJ, 53, 201) are also outside detection
window. (Msn1993a)
04228+1647 = Hyades vB 39 = HD 27685
--------- SB with P > 7 yr according to Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
04230+1732 = Hyades vB 41 = HD 27697
1991.8995 This is a particularly unexpected result, given the
four previous epochs at which our observations have
shown no indications of duplicity. All four of the
earler observations were reanalyzed using the same
procedures employed here, but no additional supporting
evidence of duplicity was found. If this additional
component is confirmed, vB 41 will be the second K0
giant binary that has been resolved in the Hyades (HR
1411 being the other). The common proper motion
companion at a separation of 195".5 is far outside our
window of observation, and the 530-day spectroscopic
component of Griffin & Gunn (1977 AJ, 82, 176) would
have an angular separation below the diffraction limit
of the KPNO 4-m telescope. (Msn1993a)
04234+1647 = Hyades vB 45 = HD 27749
--------- The 8.418-day SB of Abt & Levy (1985 ApJS, 59, 229) is
outside detection window. (Msn1993a)
04234+1940 = Hyades vB 43 = HD 284414
--------- The 1.617-year SB of Griffin et al. (1985 AJ, 90, 609)
is outside detection window. (Msn1993a)
04236+4226 = ADS 3172
1977.7420 The date of this observation was given incorrectly as 1978.7420
in McA1980b.
04241+1727 = Hyades vB 47 = HD 27819
--------- CPM companion with rho = 143".0 is outside detection
window. (Msn1993a)
04242+1446 = Hyades vB 50 = HD 27836
1991.8992 Noted as a possible spectroscopic binary by Griffin et
al. (1988 AJ, 96, 172), it is uncertain whether the
system we detect here is also producing the radial
velocity variation. (Msn1993a)
04245+1653 = Hyades vB 52 = HD 27859
--------- Noted as a possible SB by Griffin et al. (1988 AJ, 96,
172). (Msn1993a)
04247+0442 = Hyades vB 140 = HD 27935
--------- The 156.4-day SB of Griffin et al. (1985 AJ, 90, 609)
is outside detection window. (Msn1993a)
04254+2218 = Hyades vB 54 = HD 27934
--------- ADS 3201 = STF 9 is a multiple. STF 9 AB with rho =
339".5, STF 9 Aa with rho = 141".1 and STF 9 Bb with
rho = 106".9 are all outside detection window. (Msn1993a)
04255+1756 = Hyades vB 56 = HD 27962
--------- ADS 3206 is a multiple system. Kui 17 AB with rho =
1".5, and H 101 AB with rho = 77".2 are both outside
detection window. (Msn1993a)
04256+1557 = Fin 342
--------- Quadrant determinations made at several epochs by McAlister et
al (1988 AJ, 96, 1431) have shown that this system is best
represented by an eccentric orbit of period 6.3 years, rather
than a circular 13-year orbit.
--------- The published measure for 1988.6582 (McA1990) is spurious.
The data leading to this measure are actually the same as those
for HR 1331 (= McA 14) for the same epoch. These two stars
were observed in immediate sequence but with different
microscope objectives, and the final reductions calculated two
results from the same data set, but with different scale
factors; the HR 1331 measure for 1988.6582 is the correct
one. Reanalysis of the correct data for Fin 342 gives the
25 mas result shown here. Peterson (1992, private
communication) pointed out the inconsistency of our
originally published measure with respect to our previous
orbital analysis of this Hyades binary (McA1988). (Hrt1992b)
1977.7421 Theta was incorrectly given as 6.0 degrees in McA1980b.
1991.8967 HR 1391 (70 Tau) is another resolved spectroscopic
binary (with P = 6.28 yr) discussed by McA1988 and by
Dombrowski (1991, Ph.D. thesis, Georgia State University).
(Msn1993a)
04256+1852 = ADS 3210
1982.7579 This autocorrelogram was remeasured; the new results are listed
here.
--------- The 27.67-year binary (see Dombrowski 1991, Ph.D.
thesis, Georgia State University) ADS 3210 was
observed at a time when atmospheric seeing was rated
as poor. Also noted as a SB in Griffin et al. (1988
AJ, 96, 172). (Msn1993a)
04258+1733 = Hyades RHy 221
1996.1449 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
Candidate Hyades member; Reid considers definite binary.
(Rei1997)
04258+1800 = Hyades vB 176 = HD 27990
--------- SB with P > 15 yr according to Griffin et al. (1988
AJ, 96, 172). (Msn1993a)
04261+1531 = Hyades vB 59 = HD 28034
--------- SB with P > 7 yr according to Griffin et al. (1988
AJ, 96, 172). (Msn1993a)
04263+1538 = Hyades vB 141 = HD 28052
--------- CPM companion with rho = 134".4 is outside detection
window. Also, noted as a 14.24-year SB by Abt (1965
ApJS, 11, 429). (Msn1993a)
04263+2128 = Hyades vB 62 = HD 28033
--------- 8.55-day SB of Griffin & Gunn (1978, AJ, 83, 1114) is
outside detection window. (Msn1993a)
04264+1651 = Hyades vB 63 = HD 28068
--------- SB with P ~ 7 yr according to Griffin et al. (1985 AJ,
90, 609). (Msn1993a)
04264+2249 = Hyades vB 60 = HD 28024
--------- CPM companion with rho = 110".2 is outside detection
window. (Msn1993a)
04268+1052 = J 271 = HD 286820
1991.8990 This K dwarf is noted as a binary with a period in
excess of 16 years in Griffin et al. (1988 AJ, 96,
172), and it is likely that we have detected the
spectroscopic companion. (Msn1993a)
04271+2542 = DF Tau = HD 283654
Preliminary orbital elements give P=82 yr and total
mass 2.8 +/- 1.5 Msun (Thb1995).
04276+1927 = Hyades RHy 244
1995.6986 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
LP ID from Luyten et al. (1981 Proper Motion Survey with
the 48-inch Schmidt Telescope, LIX, U. Minn). Candidate
Hyades member; Reid considers definite binary. (Rei1997)
04286+1557 = Hyades vB 71 = McA 15
1979.698 + 1979.857 possible third component (Heg1983)
1991.8967 HR 1411 (the 1 Tau) is a long period interferometric
companion in addition to the spectroscopic component
suggested by Griffin & Gunn (1977) to have a period
of about 16 years. An estimate of Delta m = 0.76
was made by Dombrowski (1991, Ph.D. thesis, Georgia
State University). (Msn1993a)
04286+1944 = Hyades vB 69 = HD 28291
--------- The 41.66-day SB of Griffin et al. (1985 AJ, 90, 609)
is outside detection window. (Msn1993a)
04286+1553 = Hyades vB 72 = HD 28319
--------- The 140.7-day SB of Ebbighausen (1959 Pub. DAO, 11,
235) is outside detection window. (Msn1993a)
04290+1610 = Hyades vB 75 = Hu 1080
1991.8967 A new orbit for ADS 3248 with P = 40.15 yr and
Delta m = 0.65 mag was determined by Dombrowski (1991,
Ph.D. thesis, Georgia State University). (Msn1993a)
04293+1733 = Hyades vB 77 = HD 28394
--------- The 238.9-day SB of Griffin et al. (1985 AJ, 90, 609)
is outside detection window. (Msn1993a)
04303+1950 = Hyades vB 81 = HD 28483
--------- Noted as a probable SB in Griffin et al. (1988 AJ, 96,
172). (Msn1993a)
04306+1344 = Hyades vB 84 = HD 28556
--------- CPM companion with rho = 111".9 is outside detection
window with a large Delta m of 5.8. (Msn1993a)
04306+1542 = Hyades vB 83 = HD 28546
--------- CPM companion with rho = 161".8 is outside detection
window. (Msn1993a)
04306+1545 = Hyades vB 182 = HD 28545
--------- 358.4-day SB of Griffin & Gunn (1981 AJ, 86, 588) is
outside detection window. (Msn1993a)
04306+1612 = Hyades vB 82 = HD 28527
--------- This was noted as a possible binary by Peterson et al.
(1981 AJ, 86, 280). (Msn1993a)
04316+1742 = J 285 = HD 28634
--------- 2.31-year SB according to Griffin et al. (1985 AJ, 90,
609). (Msn1993a)
04325+2044 = Hyades RHy 309
1996.0902 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
LP ID from Luyten et al. (1981 Proper Motion Survey with
the 48-inch Schmidt Telescope, LIX, U. Minn). Candidate
Hyades member; Reid considers possible binary. (Rei1997)
04328+1600 = Hyades vB 91 = HD 28783 = CHR 152
1991.9021 CHR 152 is probably the spectroscopic system found
by Griffin et al. (1988 AJ, 96, 172) to have a period
in excess of 15 years. (Msn1993a)
04338+1451 = Hyades vB 95 = HD 28910
--------- 1.337-year SB according to Abt (1965 ApJS, 11, 429).
(Msn1993a)
04340+1510 = Hyades vB 96 = CHR 17
1991.9021 This rapidly moving system within the wide binary ADS
3317 is probably the spectroscopic system with P ~ 13
yr found by Griffin et al. (1988 AJ, 96, 172). (Msn1993a)
04354+1045 = Hyades RHy 346
1996.8130 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
LP ID from Luyten et al. (1981 Proper Motion Survey with
the 48-inch Schmidt Telescope, LIX, U. Minn). Candidate
Hyades member; Reid considers definite binary. (Rei1997)
04367+1155 = LDS 1181 = HD 286900
--------- ADS 3330 = LDS 1181 with rho = 29" is outside
detection window. The secondary is also very faint
(M = 16.2). (Msn1993a)
04375+1509 = Hyades vB 102 = HD 29310 = CHR 153
1991.9021 Reprocessing of archival speckle data have confirmed
this already strong detection and have shown a change
in theta of 15 deg in 2.7 yr. CHR 153 cannot be the
2-yr spectroscopic system of Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
04382-1418 = Kui 18
--------- An orbit for this system was published in Hrt1996a.
04382+1230 = Hyades vB 104 = HD 29388
--------- Two CPM companions with rho = 44".1 and rho = 119".8,
both outside detection window. (Msn1993a)
04382+1603 = Hyades vB 103 = HD 29375
--------- CPM companion with rho = 140".5 is outside detection
window. (Msn1993a)
04389+1406 = Hyades vB 106 = HD 29461
--------- SB with P ~ 10 yr according to Griffin et al. (1988
AJ, 96, 172). (Msn1993a)
04399+1940 = Hyades RHy 391
1996.0929 RHy ID and coordinates from Reid (1992 MNRAS, 257, 257).
Candidate Hyades member; Reid considers possible binary.
(Rei1997)
04399+5329 = ADS 3358
--------- The equinox-1900 position was incorrectly given as 04320+5310
in McA1982d.
--------- A new orbit for this system is in preparation. (Hrt1992b)
04404+1631 = Hyades vB 185 = CHR 154
1991.9021 The spectroscopic orbit for HD 29608 (Griffin et al.
1985 AJ, 90, 609) is that of a much closer system, not
the companion observed here and designated CHR 154.
(Msn1993a)
1993.2045 This confirms the discovery observation of this Hyades binary,
made in 1991. (Msn1993a)
04415-4328 = Anon
--------- ID as EQ 0439-4333 uncertain; based on Simbad search
using epoch-1950 coordinates 043955-433318 from Whi1991.
04416-4302 = HD 29993
--------- Listed as possibly resolved by Whi1991.
04422+2257 = HR 1497 = McA 16
1983.9337 (also 1983.9391) Occultation binary. Interferometric
observations are incompatible with the large delta m reported by
Jeffers et al (1963 Publ. Lick Obs. 21, 1). (Bnu1984)
04444+1109 = Hyades vB 111 = HD 30034
--------- Two CPM companions with rho = 74".7 and rho = 10".0,
both outside detection window. (Msn1993a)
04465+1528 = Hyades vB 142 = HD 30246
--------- Noted as a SB in Griffin et al. (1988 AJ, 96, 172).
(Msn1993a)
04465+4220 = Cou 2031
1985.740 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
04468+0901 = Hyades vB 113 = HD 30311
--------- SB with P ~ 7 yr according to Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
04468+1745 = J 328 = HD 30264
--------- Noted as a slow SB in Griffin et al. (1988 AJ, 96,
172). (Msn1993a)
04476+1816 = Hyades vB 114 = HD 30355
--------- SB with P >5 yr according to Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
04487+2106 = Hyades vB 115 = HD 284787
--------- SB with P ~ 4 yr according to Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
04492+2448 = Hyades vB 117 = HD 283882
--------- The 11.93-day SB of Griffin & Gunn (1978, AJ, 83,
1114) is outside detection window. (Msn1993a)
04504+1712 = Hyades vB 119 = HD 30676
--------- Noted as a SB in Griffin et al. (1988 AJ, 96, 172).
(Msn1993a)
04506+1505 = Hyades vB 120 = CHR 20
1991.9023 This may be the spectroscopic system found by Griffin
et al. (1988 AJ, 96, 172), but more observations are
needed to determine the orbital motion. (Msn1993a)
04508+1613 = Hyades vB 121 = HD 30738
--------- The 5.751-day SB of Griffin & Gunn (1978 AJ, 83,
1114) is outside detection window. (Msn1993a)
04512+1104 = Hyades vB 122 = Bu 883
1991.8969 A new orbit for ADS 3475 with P = 16.30 yr and Delta m
= 0.19 was determined by Dombrowski (1991, Ph.D.
thesis, Georgia State University). This star was
noted as a spectroscopic binary by Griffin et al.
(1988 AJ, 96, 172). (Msn1993a)
04518+1339 = Hyades vB 124 = Bu 552
1991.8969 A new orbit for ADS 3483 with P = 94.57 yr was
determined by Dombrowski (1991, Ph.D. thesis,
Georgia State University). The spectroscopic
system with P = 143 days of Griffin et al. (1985 AJ,
90, 609) would be too close for us to resolve by
speckle interferometry. (Msn1993a)
04541+6621 = HD 30614 (alp Cam)
--------- Fullerton (1990) presents high quality profiles that
indicate the presence of line profile variations; his
associated radial velocity measurements do not confirm
any of the periods suggested by Zeinalov & Musaev
(1986) and Musaev & Snezhko (1988). (Msn1998a)
04545-0313 = Rst 5501
1977.9196 This measure was omitted in McA1982b.
04597+1555 = Hyades vB 128 = HD 31845
--------- CPM companion with rho = 106".4 is outside detection
window. (Msn1993a)
05025+4105 = HR 1612
--------- This object was misidentified as rho Aur in McA1978c.
--------- Errors are given as "error ellipses"; these values are
tabulated below, together with filters used. Columns
include date (BY), major and minor axes of the ellipse
(in mas), ellipse orientation (in degrees), and filter
effective wavelengths (in nm). (MkT1996)
1989.7857 1.63 0.31 98.1 800,550,450
1989.7994 0.56 0.14 86.9 800,550,450
1989.8213 0.58 0.12 84.5 800,550,450
1989.8240 0.73 0.15 78.6 800,550,450
1989.8350 0.50 0.12 85.3 800,550,450
1989.9281 0.48 0.17 96.1 800,550,450
1989.9363 1.24 0.27 86.1 800,550,450
1990.7029 1.14 0.16 104.0 800,550,500
1990.8124 0.56 0.17 97.5 800,550,500
1990.8179 0.69 0.14 91.7 800,550,500
1991.7488 2.00 0.20 111.9 800,550,500
1991.7871 0.65 0.12 92.4 800,550,500
1991.8364 0.32 0.09 94.1 800,550,500
1991.9048 0.21 0.07 86.4 800,550,500
1992.0855 1.31 0.15 90.4 800,550,500
1992.0965 1.50 0.25 73.5 800,550,500
1992.7700 0.63 0.14 99.5 800,550,500
1992.7946 0.65 0.11 98.5 800,550,500
1992.7974 0.44 0.08 104.2 800,550,500
1992.8932 1.82 0.24 111.3 800,550,500
1992.9206 1.39 0.27 99.0 800,550,500
1992.9452 1.23 0.23 101.9 800,550,500
05056+2304 = Stt 97
1977.9197 This measure was omitted in McA1982b.
05057+0628 = Hyades vB 151 = HD 240629
--------- SB with P ~ 2 yr according to Griffin et al. (1988 AJ,
96, 172). (Msn1993a)
05074+1839 = ADS 3701
--------- A measure on 1977.9196 was incorrectly attributed to ADS 3701
in McA1982b; it actually belongs to ADS 4020.
05093+0950 = Hyades vB 130 = HD 33254
--------- Two CPM companions with rho = 88".6 and rho = 168".0,
both outside detection window. (Msn1993a)
05098+2802 = Hyades vB 131 = HD 33204
--------- STF A,BC = ADS 3730 with rho = 11".6 is outside
detection window. (Msn1993a)
05098+2802 = Hyades vB 132 = Bu 1047
1991.9023 ADS 3730 is a visual binary with P = 32.1 yr and a
large eccentricity (e = 0.93). Its elements are likely
to be refined by speckle observations during its
approach to periastron during the next 8 yr. The star
was noted as a spectroscopic binary by Griffin et al.
(1988 AJ, 96, 172). (Msn1993a)
05145-0812 = HR 1713
1975.631 Possible binary (450 and 656 nm). (Bla1977a)
1975.636 Possible binary (400, 500, 600, and 750 nm). (Bla1977a)
05162-1121 = CHR 225
--------- It in uncertain whether the pair resolved here is the
known G8III + A0V composite spectrum binary (Hoffleit &
Warren 1992, Bright Star Catalogue, preliminary 5th
edition). The small apparent change in theta over the
4-year span between observations does not appear
consistent with our estimated period of ~15 or so
years; however, the magnitude difference between the
components is small, so we are unable to rule out a 180
deg quadrant flip or perhaps an eccentric orbit.
(Hrt1996b)
05167+4601 = HR 1708
--------- All position angles have been reduced to equinox 2000.
--------- A relative orbit determined from all available interferometric
data is given by McAlister (1981 AJ, 86, 795). Colors and
spectral types determined by speckle photometry are given by
Bgn1988.
--------- Position angles have been reversed where necessary to agree with
the quadrant determination of Bgn1983.
--------- See discussion in Lab1974.
--------- Separations from paper And20 have been modified as described by
Merrill in Mrr1922.
1969.1348 This position angle was incorrectly published as 303.0 degrees
in Bag1977.
1978.915 (also 1978.929,1979.082) Observations on these three dates
overlap in papers Koe1979 and Koe1983, with only slight changes. Values
from Koe1983 are given here.
1984.9309 (also 1985.1062, 1985.1994) Estimates of the position angle and
angular separation are deduced from the elongation of the
central speckle peak in the autocorrelation. (Bnu1986)
--------- observations were made through narrow band filters centered at 800,
550, and 450 nm. Colors were derived from all 1988-1992 data, so are
listed at the mean epoch of 1991.9. Paper also includes a new orbit.
Finally, errors are given as "error ellipses"; these values are
tabulated below. Columns include date (BY), major and minor axes of
the ellipse (in mas), and ellipse orientation (in degrees). (MkT1994)
1988.7973 0.95 0.11 96.
1988.8000 0.42 0.03 93.3
1988.8028 0.22 0.03 85.7
1988.8055 0.15 0.02 88.2
1990.9411 0.09 0.02 86.6
1990.9548 0.13 0.05 88.6
1991.7159 0.73 0.08 124.1
1991.7214 0.37 0.06 179.6
1991.7241 0.23 0.05 156.5
1991.7871 0.07 0.01 93.7
1991.8364 0.07 0.02 91.6
1991.8665 0.04 0.01 94.5
1991.8857 0.06 0.02 88.4
1991.8939 0.10 0.05 149.3
1991.9021 0.16 0.05 77.9
1991.9733 0.10 0.03 87.6
1991.9870 0.09 0.02 77.5
1992.0006 0.50 0.07 83.0
1992.0417 0.24 0.05 73.4
1992.0445 0.09 0.02 83.8
1992.0691 0.25 0.05 74.6
1992.0855 0.22 0.02 93.5
1992.0965 0.10 0.02 78.5
1992.7399 0.33 0.05 111.1
1992.7426 0.42 0.04 118.5
1992.7454 0.21 0.06 110.6
1992.7481 0.40 0.09 121.2
1992.7508 0.62 0.08 121.3
1992.7536 0.71 0.16 103.9
1992.7563 0.76 0.12 121.9
1992.7755 0.05 0.01 105.9
1992.8357 0.19 0.02 118.1
1992.8658 0.09 0.04 78.1
1992.8658 0.14 0.04 91.8
1992.8686 0.09 0.02 69.5
1992.8686 0.14 0.07 92.9
1992.8823 0.07 0.02 88.8
1992.8932 0.11 0.02 116.4
1992.9206 0.43 0.07 98.8
1992.9452 0.15 0.03 113.0
05207+3726 = HD 34656
--------- Fullerton et al. (1991) describe profile and radial
velocity variations that suggest that this star is a
short-period, radial pulsator. Underhill (1995) also
discusses radial velocity measurements. (Msn1998a)
05244-0224 = McA 18
--------- Analysis of the spectroscopic/interferometric orbit is given by
McA1976.
--------- This measurement of the Aab,c component of eta Ori,
overlooked in the original analysis of this run, was
discovered during preparation of our paper on absolute
quadrant determinations (Bgn1992). (Hrt1992b)
1979.7709 This measure was omitted in McA1982d.
05248-5219 = I 345 AB
1989.9388 This system has also decreased in separation steadily
since the 1920's, and was last resolved visually in
1983.
05255-0033 = ADS 4020
1977.9196 This measure was incorrectly attributed to ADS 3701 in McA1982b, with
an incorrect position angle.
05271+1758 = ADS 4038 = McA 19 Aa
1982.7551 All archival data for this system were reprocessed using more
powerful algorithms than earlier available, resulting in four
new unresolved measures as well as the new 1991 measurement.
In addition, new rho and theta values have been determined for
the observations originally published from 1986.9-1988.3 (McA1989),
1988.7-1989.2 (McA1990), and 1990.3--1990.8 (Hrt1992b). (Hrt1994)
1988.2518 This date was incorrectly given as 1988.2490 in McA1989.
--------- Orbital analysis of this system is in progress; a preliminary
orbit gives a period of ~15.3 years and a semi-major axis of
0".080. (Hrt1994)
05279+3447 = HD 35652 (IU Aur)
--------- The classification is from Mammano et al. (1977), and
because the stars are are classified as B-type we have
not included this system in our distributions for the
O-stars. Harries et al. (1997b) discuss the inner
double-lined system and evidence of a near tertiary in
a 294-day orbit. The distant, fourth star was detected
both by us (on the suggestion of B. Schaeffer) and
Hipparcos (ESA 1997). (Msn1998a)
05293-2517 = HD 36239
--------- Listed as possibly resolved by Whi1991.
05294+1152 = V649 Ori
1980.95 marginal evidence for additional component with separation
0".47, pos. angle 36 or 216 deg (Bai1985b)
05297+3523 = HD 35921 (LY Aur)
--------- The classification is from Drechsel et al. (1989).
Howarth et al. (1997) give Delta m for both
spectroscopic and astrometric components. (Msn1998a)
05320-0018 = HD 36486 (del Ori)
--------- Orbital elements are also given by Levato et al.
(1988). The Aa visual pair has increased in
separation from 0".20 to 0".29 between 1979 and 1994.
The spectral classification for the C component is from
Morrell & Levato (1991). (Msn1998a)
05351+0956 = HD 36861 (lam Ori)
--------- Both A and B components were observed and appeared
to be single. The AB pair may not be physical (Lindroos
1985). The classification of the C component is from
Lindroos (1985; based on photometry). Lindroos gives a
distance of 430 pc. The classification of the B
component is from Hoffleit & Warren (1991). (Msn1998a)
05353-0523 = HD 37022 (the 1 Ori C)
--------- Stahl et al. (1996) find that the H-alpha profiles vary
with a 15.4-day cycle which they suggest is related to
the star's rotational period; photospheric line radial
velocity variations are small. All 4 of the Orion
Trapezium stars were observed with the speckle camera
(A = HD 37020; B = HD 37021; C = HD 37022; D = HD
37023) and all appeared to be single. Classifications
of the B and D components are from the WDS. The
spectral classification for the A component is from
Morrell & Levato (1991). (Msn1998a)
05353-0425 = HR 1891
1977.9197 This measure was omitted in McA1982b.
05354-0555 = HD 37043 (iot Ori)
--------- The classification is from Stickland et al. (1987).
The A component was resolved (CHR 250 Aa); the B
component was also observed but appeared to be single.
The classification of the B component is from Hoffleit
& Warren (1991). (Msn1998a)
05354-0525 = HD 37041 (the 2 Ori)
--------- The A component (CHR 249 Aa) was resolved on 3
occasions, but the distant StF 17 B component was
observed to be single. The Hipparcos results (HIP1997b)
confirm the CHR 249 Aa pair. The spectral
classification for the B component is from Morrell &
Levato (1991). The classification of the C component
is from Hoffleit et al. (1983). (Msn1998a)
05387-6903 = R 136
1980.93 results are tabulated from the combined data set only. Rms
errors from comparing data sets are 0".011 in separation,
1.6 deg in position angle, 0.28 in magnitude diff. (Peh1992)
05387-0235 = HD 37468 (sig Ori)
1977.9197 This measure was omitted in McA1982b.
--------- The AB pair has decreased in position angle from 171
deg to 125 deg between 1975 and 1994. Fullerton (1990)
describes three spectral components in the He I 5876 A
profile which suggests that one of the stars is a
double-lined spectroscopic binary (see Bolton 1974).
The classifications of the B, C, and D components are
from Hoffleit & Warren (1991), while the classification
for the E component is from Morrell & Levato (1991).
(Msn1998a)
--------- An orbit for this system was published in Hrt1996a.
05408-0157 = HD 37742 (zet Ori)
--------- Levato et al. (1988) and Fullerton (1990) also report
small radial velocity variations (< 35 km/sec). Both A
and B components were observed and both appeared to be
single. The classification of the B component is from
Hoffleit & Warren (1991). (Msn1998a)
05411+1632 = ADS 4265
1977.9197 This measure was omitted in McA1982b.
05460-3218 = HD 38666 (mu Col)
--------- Additional radial velocity measurements by Fullerton (1990)
and Pnn1993 confirm the lack of variability. (Msn1998a)
05547+1351 = HD 39680
--------- Both components were observed and appeared to be
single. (Msn1998a)
05565-2631 = B 94
1989.9362 This system was last resolved visually in 1978, and
appears to be continuing to approach periastron.
05589+1249 = ADS 4562
1980.1560 This measure was incorrectly attributed to STF 784 in McA1983.
06004-3103 = HJ 3823 AC
1997.0952 In this multiple system, our observation failed to
detect the closer pair Hu 1399 AB, where the secondary
has magnitude 9.2 and approximate separation 0".5.
(Hor1997)
06017+2224 = HR 2116 = CHR 161
1988.1703 Listed by Appleby (1980 JBAA, 139, 1139) as having
anomalous behavior. (McA1993)
1993.1967 This confirms the discovery observation, made in 1988. (Hrt1994)
06024+0939 = ADS 4617
--------- See discussion in BLM1978.
--------- A visual orbit of this system was published by Osvalds
(1964, Pub. McCormick Obs., 11, 175); a combined
speckle/spectroscopic solution is in progress. (Hrt1996b)
06098-2246 = Rst 3442
--------- An orbit for this system was published in Hrt1996a.
06149+2230 = HR 2216
1979.7709 This negative result was omitted in McA1981b.
06154-0902 = A 668
--------- An orbit for this system was published in Hrt1996a.
06171+0957 = Fin 331 Aa
--------- An orbit for this system was published in Hrt1996a.
06200-1038 = HD 44179
--------- See Mea1983 for a discussion of the observational history of
this object also known as the ``Red Rectangle''.
06212+2932 = HR 2272 = CHR 165
1993.1967 This confirms the discovery observation, made in 1988. (Hrt1994)
06256+2320 = HR 2304 = McA 26
1979.7709 This negative result was incorrectly attributed to ADS 5103 in
McA1981b.
06273+1453 = HD 45314 = CHR 251
--------- The classification is from Conti & Leep (1974). The
star was resolved (CHR 251) in the single observation
we made. (Msn1998a)
06289+2014 = ADS 5103
1975.780 Oblate correlation peak, under very poor seeing. (Bla1977a)
--------- A negative result on 1979.7709, incorrectly attributed to ADS
5103 in McA1981b, actually belongs to HR 2304.
06294-0249 = Ross 614 = Gliese 234
1986.952 combination of NS and EW 1-D IR speckle data for 1986.952 (Cpb1994)
1991.896 combination of data from 1991.894 and 1991.897 (Cpb1994)
1992.143 combination of data from 1992.141 -- 1992.146 (Cpb1994)
06374+0608 = HD 47129 (Plaskett's star)
--------- The classification is from Bagnuolo & Barry (1996).
We took the mass ratio from Bgn1992. (Msn1998a)
06386+0137 = HD 47432
--------- The star is a member of Mon OB2 according to Hill et
al. (1986). (Msn1998a)
06401-3919 = HD 48149
--------- The classification is from Conti & Alschuler (1971).
(Msn1998a)
06410+0954 = HD 47839 = 15 Mon = CHR 168
--------- The classification of the speckle companion (CHR 168
Aa) is from Gie1993. The spectroscopic orbit and current
periastron passage of Aa are discussed by Gie1997. The B
component was observed and appeared to be single. The
classifications of the B, C, D, and E components are
from Hoffleit & Warren (1991) who list the E component
as a close pair. (Msn1998a)
06503+2410 = Cou 768
1984.9999 The published McA1987b measure contained a 10 degree typographical
error in theta.
06573-3530 = I 65
1997.1172 Despite nearly a century of visual observations and
a grade 1 orbit in the orbit catalog of Worley & Heintz
(1983), ours is apparently the first speckle measure of
this system. (Hor1997)
07003-2207 = Fin 334 Aa
1989.9336 The system has opened slightly since the last speckle
observation in 1989.3; unfortunately it was last
observed in 1966 so it may be difficult to pin down the
time of periastron passage.
07015-0307 = HD 52533
--------- The classification is from Conti et al. (1977). (Msn1998a)
07067-1117 = ADS 5795
1980.905 This observation was incorrectly attributed to ADS 5975 in
Sta1981b (noted in Tok1982b).
07148-1529 = Bu 575 AB
1997.1226 The magnitude difference of the system is listed in
the WDS as 0.1. Our reduction does not give the same
quadrant as the latest measure in the WDS. (Hor1997)
07187-2457 = HD 57061 = 30 tau CMa = Fin 313
--------- van Leewen & van Genderen (1997) and Stickland et al.
(1997e) argue that the brighter A component of the
visual Aa binary is a triple system consisting of a
close 1.28-day eclipsing system orbiting a distant O
star (the spectroscopic binary with a period of 154.9
d). The visual Aa pair has slowly decreased in
separation from 0".19 to 0".15 between 1977 and 1994.
The classification of the D component is from Hoffleit
& Warren (1991). (Msn1998a)
07187-2434 = HD 57060 = 29 UW CMa
--------- The classification is from the UV tomographic analysis
of Bagnuolo et al. (1994). (Msn1998a)
07220-0859 = HD 57682
--------- Additional radial velocity measurements by Pnn1993
confirm the lack of variability. (Msn1998a)
07277+2127 = ADS 6089 = McA 30
--------- Fekel (1986 private communication) detected this system as a
third component in the spectrum and makes a preliminary estimate
of the period of 760 days. A combinedspectroscopic/speckle orbit
of this system has been undertaken in collaboration with Fekel.
07298+2755 = McA 31
--------- The measurement resulting from the original analysis of
this observation was rejected prior to publication. Our
reanalysis of the observation by new techniques yielded
a quite good result, however. (Hrt1992b)
07330-2820 = HD 60369
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
07398-3235 = HD 61827
--------- The classification is from Houk & Cowley (1975).
(Msn1998a)
07479+6019 = ADS 6354
--------- This system underwent periastron sooner than predicted
by the orbit of Baz1961b. (Hrt1992b)
--------- An orbit for this system was published in Hrt1996a.
07486+2309 = ADS 6378
--------- The equinox-1900 position was incorrectly given as 07526+2323
in McA1978b and McA1980b.
07528-0526 = Fin 325
--------- An orbit for this system was published in Hrt1996a.
08017+6019 = McA 33
--------- An orbit for this system was published in Hrt1996a.
08036-4000 = HD 66811 = zet Pup
--------- The distance estimate is from Reid & Howarth (1996).
Van Rensbergen et al. (1996) discuss the star's
trajectory and possible runaway status. (Msn1998a)
08095-4720 = HD 68273 = gam 2 Vel = WR 11
--------- The Hipparcos distance suggests a position in front of
the Vel OB2 association (van der Hucht et al. 1997;
Schaerer et al. 1997) at a distance of 258 +41/-31 pc;
however, the Hipparcos distances for the B stars in Vel
OB2 (Brandt et al. 1971) yield a comparable distance of
317 +/- 42 pc. This is also consistent with the
distance from the resolution of the binary by Hanbury
Brown et al. (1970) of 350 +/- 50 pc. Thus, we have
chosen to keep gam 2 Vel as a member of Vel OB2.
The classification is from van der Hucht et al.
(1997). The B component was also observed and appeared
to be single. The classifications of the B, C, and D
components are from Hoffleit & Warren (1991). (Msn1998a)
08095+3213 = ADS 6623 = CHR 190 Aa
1991.3210 This is a new component to the wide (2".8) pair STF 1187,
discovered by F.G.W. Struve in 1829.
08122+1740 = HR 3209
--------- This object was misidentified as HR 3210 in McA1978c.
08125-4616 = CHR 143 Aa
1989.9391 These measurements confirm the discovery observation
of this close companion to See 96, made in the spring
of 1989.
08138-3444 = I 193
1997.1201 A smaller annulus was used in the power spectrum fit
due to the faintness of the source. As a consequence,
the separation and position angle uncertainties may be
larger than other measures. (Hor1997)
08246-0345 = HR 3297 = CHR 172
1988.1649 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
08249-4418 = HD 71304
--------- Turner (1979) includes this star in the Vel OB1 group
at a distance of 1.8 kpc. Photometric spectral
classifications of the B and C components are from
Lindroos (1985), who also finds a distance of 2.7 kpc.
(Msn1998a)
08250-4246 = CHR 226 Aa
--------- This close companion to Rst 4888 has been observed on
three occasions, but has shown little movement over a
1.6-year period. The 1989 measurements of the Rossiter
pair have already been published (McA1990, Hrt1993).
Following discovery of the close pair in the 1990 data,
these 1989 data were rereduced, resulting in
``preconfirmation" of the new component. (Hrt1996b)
08267+2433 = A 1746 BC
--------- An orbit for this system was published in Hrt1996a.
08285-0230 = A 551 AB
--------- All speckle measures are discordant with the published
orbit of B__1953b; a new orbit is in preparation. (Hrt1992b)
08388-3352 = B 1621
1995.1160 Quadrant determined by speckle imaging analysis. (Hor1996)
08391+2000 = Praesepe KW 143 = HD 73430
1991.3239 Praesepe cluster member and occultation binary.
OCC1984a found a vector separation in April 1982 of 0".044,
which should have been resolvable by us unless the system
closed. They find magnitude differences (noted as unreliable)
of 2.5 mag at 445 nm and 0.35 mag at 750 nm, which if
correct would not have prevented us from seeing the
companion. Incorrectly noted as HD 73460 in text,
although the tabular information is correct. (Msn1993b)
08392-4025 = HD 73882
--------- Eggen (1982) assigns this star to a group associated
with the cluster IC 2395 at distance of 0.8 kpc. The
Hipparcos Catalogue (ESA 1997) contains a light curve
with a period of 1.46 d. (Msn1998a)
08398+1932 = Praesepe KW 212 = CHR 156 Da
1986.8839 No published evidence of RV variation. Noted as
occultation binary by OCC1984a. Magnitude differences of
3.1 in blue and 3.8 in red reported by OCC1989b
are consistent with our difficulty in detecting the
faint secondary. Praesepe cluster member. (Msn1993b)
08402+1921 = Praesepe KW 284 = CHR 130
1984.0607 Praesepe cluster member with anomalous occultation
behavior (Appleby 1980 JBAA, 139, 1139). This and
1986 measure are from reanalysis of archival data.
OCC1989b measured magnitude differences of 1.9 in blue
and red. (Msn1993b)
08402+1958 = Praesepe KW 265 = CHR 28 Bb
1986.8922 Praesepe cluster member with excess luminosity. This
measure is from reanalysis of archival data.
Frequently unresolved, due to large delta m. (Msn1993b)
08412+2028 = Praesepe KW 377 = Bu 585
1991.3184 Praesepe cluster member. Although the peak remains
convincing, we have been unable to confirm this
measure, perhaps due to either a variable secondary
or to the star closing within our resolution limit.
(Msn1993b)
08418+1952 = Praesepe KW 428 = HD 73974
1991.3293 Praesepe K0 giant and occultation binary. OCC1984a
found a projected separation in April 1982 of 0".018,
which could lead to a true separation below our
resolution limit. (Msn1993b)
08468+0625 = Sp 1 AB
--------- An orbit for this system was published in Hrt1996a.
08504-4205 = HD 75759
--------- The classification is from Thackeray (1966). The star
is part of a group associated with the cluster IC 2395
(Eggen 1982). (Msn1998a)
08506-4632 = HD 75821 = KX Vel
--------- The classification is from Conti et al. (1977). Part
of an eclipse was observed by Balona & Laing (1986)
(the orbital ephemeris is discussed by Mayer et al.
1997). (Msn1998a)
08540-4229 = HD 76341
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
08551-4736 = HD 76556
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
08575-5045 = HD 76968
--------- Turner (1979) includes this star in a group with the
Cepheid SW Vel which lies beyond Vel OB1 at a distance
of 2.6 kpc. (Msn1998a)
08579+3014 = ADS 7107
1986.388 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
09008+4148 = Kui 37
--------- An orbit for this system was published in Hrt1996a.
09036+4709 = ADS 7158
1975.950 This observation was made under very poor conditions and yielded
a poor set of fringes. (BLM1978)
1981.350 This observation was incorrectly attributed to Fin 347 in Tok1982a
(noted in Tok1982b).
09123+1459 = Fin 347
1981.358 This observation was incorrectly attributed to ADS 7158 in Tok1982a
(noted in Tok1982b).
1983.9371 (also 1983.9372) Interferometric observations indicate that
Finsen's 1965 orbit (see Worley & Heintz, 1983 Fourth Catalog
of Orbits of Visual Binary Stars) must be revised. (Bnu1984)
1990.9166 Residuals (4.0 deg in theta, 0".007 in rho) to the orbit of
Hrt1989 are only fair, due to a combination of large zenith
distance and close angular separation at the time of this
observation. A combined speckle/spectroscopic solution
for this double-lined binary is in progress. (Hrt1996b)
--------- A combined astrometric/spectroscopic orbit is given
in Msn1996a.
09188+3648 = HR 3690 = CHR 173 Ba
1988.1705 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
09276-0840 = HR 3748
1976.397 Unresolved in H alpha. (Bla1977a)
09278-0604 = HR 3750
1982.1683 Single line SB, P = 2.5 yr, also a known visual binary. Primary
is G2V, so companion should likely be a cooler dwarf; this seems
to be confirmed from magnitude differences observed at 7500,
5500, and 4500 Angstroms. (Bag1984b)
09320-0111 = HR 3787 = CHR 174
1988.1677 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
09337-4900 = HJ 4220
1995.1024 Quadrant determined by speckle imaging analysis. (Hor1996)
09372-5340 = See 115
1995.1024 WDS Catalog lists equal magnitudes and nearly equal
spectral types for this object. Our observations do
not unambiguously determine the quadrant in this case,
so we adopt the same quadrant as the most recent
observation listed in the WDS.
1997.1229 The magnitude difference of the system is listed in
the WDS as 0.0. Our reduction does not give the same
quadrant as the latest measure in the WDS. (Hor1997)
09398-5008 = Rst 4917
1995.1024 Quadrant determined by speckle imaging analysis. (Hor1996)
1997.1229 A smaller annulus was used in the power spectrum fit
due to the faintness of the source. As a consequence,
the separation and position angle uncertainties may be
larger than other measures. (Hor1997)
09398-1034 = HR 3846 = CHR 175
1988.1677 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
09446+6459 = HR 3859 = CHR 176
1993.2025 This confirms the discovery observation, made in 1988. (Hrt1994)
09474+1134 = HR 3880 = McA 34
1980.1538 Theta was incorrectly given as 206.6 degrees in McA1983.
09476+1126 = HR 3882
1976.397 Disk resolved (0".030 +/- 0".007 at 770 nm,
0".054 +/- 0".009 at 750 nm,
0".049 +/- 0".009 at 730 nm,
0".032 +/- 0".005 at 540 nm). (Bla1977a)
10000+2433 = CHR 145 = DH Leo
1989.2271 Three K stars are seen in spectroscopic observations of
Barden (1984 AJ, 89, 683). Fekel (1989, private
communication) has observed the third component of this
system and finds no velocity changes in excess of +/-
2km/sec from 12 spectra obtained since 1984. This new
speckle component is thought to be this third
spectroscopic component. (McA1990)
10050-5119 = Hu 1594
1995.1024 Quadrant determined by speckle imaging analysis. (Hor1996)
10083+3137 = Kui 48 AB
--------- An orbit for this system was published in Hrt1996a.
10093+2020 = ADS 7662
--------- Composite spectrum binary, classified G2III+A2V by Markowitz
(1969 Dissertation, Ohio State Univ.), who quotes delta m = 1.1.
1983.9371 (also 1983.9372) Interferometric observations are in disaccord
with the 1957 orbital elements of Baize (see Worley & Heintz,
1983 Fourth Catalog of Orbits of Visual Binary Stars). (Bnu1984)
1984.1861 (also 1984.2814, 1985.2053) The speckle interferometric
observations show that Finsen's orbit (Worley & Heintz, 1983
Fourth Catalog of Orbits of Visual Binary Stars) fails to
describe the orbital motion of this system. (Bnu1986)
10095-6841 = I 13 AB
1997.1230 Our reduction does not give the quadrant
unambiguously. We therefore adopt the quadrant
consistent with the latest measure in the WDS. (Hor1997)
10117+1321 = Hu 874
--------- An orbit for this system was published in Hrt1996a.
10120-2836 = B 194
1990.3407 Periastron passage apparently occurred about the time of
or shortly before our first speckle observation in 1989.3.
10157-5115 = HD 89137
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
10191-6441 = HJ 4306
1997.0902 The magnitude difference of the system is listed in
the WDS as 0.1. Our reduction does not give the same
quadrant as the latest measure in the WDS. (Hor1997)
10200+1951 = GJ 388 = Bag Ca
1981.2446 Flare star (M4.5Ve) known as having an unseen companion of P ~
27 yr (Reuyl, 1943 ApJ, 97, 186). Companion has been detected
only at 7500 Angstroms. The companion is expected to have a
very low mass. (Bag1984b)
10223-5945 = HD 90087
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
10238-4415 = I 208 AB
1997.1230 A smaller annulus was used in the power spectrum fit
due to the faintness of the source. As a consequence,
the separation and position angle uncertainties may be
larger than other measures. (Hor1997)
10269+1931 = Cou 292
1983.9557 (also 1983.9667) Measurements should be given low confidence.
(Bag1985)
10279+3643 = ADS 7780
--------- This object was misidentified as Ho 879 in McA1982d.
10318-6356 = HD 91452
--------- The classification is from the LSC; however, Garrison
et al. (1977) assign a type B0 Ia. (Msn1998a)
10329-4700 = HD 91504
1995.1025 WDS Catalog lists a companion at 40".3 and position
angle 163 deg. The component listed here appears to be
a new discovery. Our two observations of this object
were forty minutes apart on February 7, 1995 (UT).
1997.1176 This is the first measure of this system since the
discovery measures in 1995 of Dinescu et al. (1997, IAU
Comm. 26 Inf. Circ. 131, 1). The difference in
position angle from their last measure is 2.2 deg and
the difference in separation is 0".020. (Hor1997)
10427+0335 = ADS 7896
--------- This object was misidentified as ADS 7986 in McA1982d.
10438-5933 = CP-58 2611
--------- This object is designated as Trumpler 14 20 in the list
of Feinstein et al. (1973) and as FMM 20 in Pnn1993.
(Msn1998a)
10439-5933 = Trumpler 14 FMM 9
--------- This object is designated as Trumpler 14 9 in the list
of Feinstein et al. (1973) and as FMM 9 in Pnn1993.
(Msn1998a)
10440-5933 = HD 93129
--------- Both A and B components were observed with the speckle
camera and appeared to be single (Pnn1993). (Msn1998a)
10440-5932 = CP-58 2620
--------- This object is designated as Trumpler 14 8 in the list
of Feinstein et al. (1973) and as FMM 8 in Pnn1993.
(Msn1998a)
10441-5935 = HD 93160
--------- This star (component C of HD 93161) was observed with
the speckle camera and appeared to be single. (Msn1998a)
10441-5935 = HD 93161
--------- Both A and B components were observed with the speckle
camera and appeared to be single. Levato et al. (1991)
derive a single-lined spectroscopic orbit for HD 93161
but they do not indicate which component is the
binary. Howarth et al. (1997) and Penny (1996a) found
large radial velocity changes in closely spaced IUE
spectra, and Howarth et al. argue that both components
are short-period binaries. (Msn1998a)
10443-7052 = CHR 227 Ba
--------- Worley (private communication) noted that the
systematic binary star surveys of Rossiter (Rst1955)
and van den Bos missed the declination band -73 to -70
deg. This probably explains why this half-arcsecond pair
remained undiscovered until now. CHR 227 represents a new
component to the wide (63") common proper motion pair
HR 4211-12 = Dun 99 AB, discovered by J. Dunlap in 1826
(Dun1829) and last observed nearly 80 years ago (Daw1918)
A 10th magnitude C component also lies some 35" from A,
discovered by John Herschel (HJ_1847a) in 1835, but no
closer components are known. (Hrt1996b)
10444-6000 = HD 93206 = QZ Car
--------- The classifications are from Morrison & Conti (1980)
who describe this quadruple that consists of a pair of
SB1 systems (the shorter period system is also
eclipsing). Their expressed hope that speckle
interferometry might resolve the pair was not realized
in our work, but the object remains an important target
for high resolution work. (Msn1998a)
10446-5944 = HD 93205
--------- The classification is from the UV tomographic analysis
of Penny (1996b). The companion star, HD 93204 (BsO 4 B)
was also observed and appeared to be single. (Msn1998a)
10451-5941 = HD 93308 = eta Car
--------- This famous luminous blue variable is not classified as
an O star, but it is almost certainly a massive
object. The inner structure of the ejecta of this star
is described by Davidson et al. (1997). A preliminary
set of orbital elements is given by Damineli et al.
(1997) who suggest a 5.5-yr orbit with a maximum
angular separation of 0".004. The central object
appeared single in our observations. The H component
(HDE 303308) was also observed and appeared to be
single. (Msn1998a)
10453+3831 = ADS 7915 = Ho 532 AB + CHR 191 Aa
1983.4277 The Aa pair is a new component to the 0".7 pair Ho 532. This
new component was actually first resolved in 1983 (McA1987b) but it
was believed at the time that the measurement was of the known
pair (the wide component laid outside the processor "window"
of our old autocorrelator). Reprocessing of our archival video
data allowed us to resolve both components in the 1983 and 1984
data sets, although both early measurements of the Aa component
are quite weak.
10457-5924 = HD 93403
--------- The classification is from the UV tomographic analysis
of Penny (1996b). (Msn1998a)
10484+3734 = HD 93521
--------- The classification is from Hobbs et al. (1982).
Fullerton (1990) and Howarth & Reid (1993a) describe
the striking line profile variations in the spectra
apparently due to nonradial pulsations. (Msn1998a)
11047-0413 = ADS 8048
--------- Eggen's (1967 ARA&A, 5, 132) orbit for this pair of
11th magnitude M dwarfs (= A 676 BC) predicts a
separation of 0".20 and a position angle of 86 deg at
this epoch. Our measurement is in poor agreement with
this prediction. (Hrt1992b)
11049-6103 = HD 96264
--------- The classification of the B component is from Lindroos
(1985), who finds a distance of 3.5 kpc. (Msn1998a)
11053-2718 = Fin 47
--------- A new orbital analysis of this system is in progress,
some three decades after van den Bos (B__1957a)
published his solution. (Hrt1996b)
11072-5952 = HD 96670
--------- The classification and SB1 orbit are from Garcia
(1994). (Msn1998a)
11118-6042 = HD 97434
--------- The star belongs to a group behind Tr 18 (Vazquez &
Feinstein 1990) at a distance of 2.8 kpc; we designate
this as "Tr 18B" in Table 1. (Msn1998a)
11150+3735 = ADS 8102 = CHR 192 Aa
1987.2666 This is a new component to the 0".6 pair STT 232, discovered by
Otto Struve in 1843. Reprocessing of archival data (whose 1987
and 1988 measurements for the wide pair were originally published
in McA1989) has allowed us to confirm this discovery and also to note
that the system appears to be accelerating toward periastron.
11158+1318 = HR 4365
1985.1123 (also 1985.2053) This system has been observed at the limit of
resolution of a 2-m telescope, so delta m is probably < 1.
(Bnu1986)
11182+3132 = ADS 8119 = STF 1523 AB
--------- An orbital analysis of Xi UMa, including both the AB pair, the
astrometric companion, and the newly-discovered Bc companion,
has been published by Msn1995.
11182+3132 = HR 4374 = CHR 178 Bc
1988.1624 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
11182+3133 = HR 4375
--------- This object was misidentified as HR 4374 in McA1978c.
11191+3811 = HR 4380 = CHR 133
--------- Preliminary orbital elements (P = 5.12 yr) are given
in McA1993.
11210-5429 = HR 4390
1976.474 This system was observed within a few months of periastron.
(BLM1978)
11272-1539 = Hu 462
1997.1231 Our reduction does not give the quadrant
unambiguously. We therefore adopt the quadrant
consistent with the latest measure in the WDS. (Hor1997)
11304-6349 = HD 100099
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
11324+6105 = ADS 8197
1979.0369 This measure was incorrectly attributed to ADS 8249 in McA1982d.
11336-4035 = I 78
1997.1177 The magnitude difference is listed in the WDS as 0.0.
Our reduction does not give the same quadrant as the
latest measure in the WDS. (Hor1997)
11384-6312 = HD 101223
--------- Additional similar radial velocities are reported by
Thackeray & Wesselink (1965) and Humphreys (1973).
(Msn1998a)
11391-6326 = HD 101298
--------- Additional similar radial velocities are reported by
Thackeray & Wesselink (1965). (Msn1998a)
11398-6329 = HD 101413
--------- This star (BsO 7 B) is the optical companion of HD
101436 (Lindroos 1985). Both stars were observed and
appeared to be single. Additional diverse radial
velocities for HD 101413 are reported by Thackeray &
Wesselink (1965) and Conti et al. (1977). (Msn1998a)
11415+3145 = HR 4501
1984.4086 This system is known to have a variable radial velocity.
(Bnu1986)
12058-6934 = HD 105056 = GS Mus
--------- Harmanec (1987) gives a preliminary orbit with P =1.74
d and K =12.4 km/sec. The same period and its double
also appear in photometry (van Genderen et al. 1989),
so the radial velocity variations may be related to
pulsation instead of orbital motion. The radial
velocity variations are also discussed by Walborn et
al. (1980) and Levato et al. (1988). (Msn1998a)
12061+6842 = StF 3123 AB
--------- An orbit for this system was published in Hrt1996a.
12088-4023 = Anon
--------- ID as EQ 1206-4006 uncertain; based on Simbad search
using epoch-1950 coordinates 120613-400627 from Whi1991.
12165+3304 = CHR 37
--------- A spectroscopic orbit with a period of 1300 days was determined
by Christie (1936 ApJ, 83, 433). The many negative results
listed here may be due to a large or variable magnitude
difference.
12199-0040 = HR 4689 = McA 37
--------- Preliminary orbital elements based entirely on speckle
observations are given in Bag1984b.
--------- This is not the double line SB because the observed
angular separations are much larger than the 12 mas
maximum predicted by Halbwachs (1981 A&AS, 44, 47)
from the spectroscopic elements. See further
discussion in Bag1984b.
--------- A new speckle/spectroscopic orbit of the early A type
triple system eta Vir has been determined by Hrt1992a.
(Hrt1992b)
1985.2053 (also 1985.2491) These measurements agree well with
the preliminary orbit of Balega et al. (Bag1984b), who
adopted a period of 13 years. The orbit proposed by
Tokovinin (Tok1984) with P = 9.8 years fails to fit the
speckle observations. (Bnu1986)
12332+0901 = GJ 473
1990.04 Theta and rho values are averages of observations taken
in J, K, and L bands (1250/380, 2200/480, and 3400/700
nm). Magnitude difference is that at K band. (Prr1992)
12493+2733 = HR 4869 = CHR 179 Aa
1988.1654 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
12501+5506 = GD 319
--------- Magnitude difference is based on images from 1988.1736 and
1993.2054. This system is probably an optical pair. (McA1996)
12540+5558 = HR 4905
1975.383 Erroneously listed as HD 112815 in BLM1978 notes. The Yale
Bright Star Catalogue cites this star as a spectroscopic variable
with periods of 4.15 years and 0.95 days; the object is also a
photometric variable with period 5.09 days. This observation
presumably resolved the longer period system. (BLM1978)
12560-5650 = HD 112244
--------- Classification of the B component is from Lindroos
(1985), who finds a distance of 2.5 kpc. (Msn1998a)
12567-4741 = I 83
1995.1028 Quadrant determined by speckle imaging analysis. (Hor1996)
12597-0348 = CHR 39 Aa
1991.3921 This interferometric system has now completed nearly 180
deg of revolution since its discovery in 1984. A
preliminary determination of orbital elements yields a
low-eccentricity orbit with a period of 15.7 years.
Absolute quadrant determinations based on reanalysis of
earlier speckle data have ruled out a possible short-
period high-eccentricity orbit. A more complete orbital
analysis is in progress.
13003+3047 = HDS 1823
1996.4274 Very weak detection, possibly an artifact. (Msn1999b)
13031-7129 = CHR 228
--------- As was the case with CHR 227, this star falls within
the declination band missed in the surveys of Rossiter
(Rst1955) and van den Bos (B__1957a). If physical, this
0".56 pair would presumably have an extremely long period,
given the spectral type and large calculated distance of
its primary. The small change in theta seen over 2.75
years is consistent with this, implying a period of order
500 -- 600 years. The star is noted in Abt & Biggs (1972,
Bibliography of Stellar Radial Velocities, New York,
Latham Process Corp.) as having variable radial velocity;
Hoffleit & Warren (1992, Bright Star Catalogue, preliminary
5th edition) also note photometric variability of amplitude
~0.2 mag, as well as variability in the line width of H alpha
emission. (Hrt1996b)
13064+2109 = CHR 150 Aa
--------- Here is a newly discovered component to 39 Com, in
addition to the wide (1".2) pair Cou 11 AB. (Hrt1992b)
13065-6505 = HD 113659
--------- The classification is from Houk & Cowley (1975). (Msn1998a)
13081-6518 = HD 113904 = the Mus = WR 48
--------- The classification is from Houk & Cowley (1975).
Moffat & Seggewiss (1977) found evidence of orbital
motion in the WR star, but the O star appeared
stationary. We found a possible binary companion at a
separation of 0".04 which needs confirmation, but if
correct, this suggests that the system is triple,
consisting of a WR SB1 plus a distant O star. The
visual B component was observed and appeared to be
single. (Msn1998a)
13100-0532 = ADS 8801
1976.3669 This epoch was incorrectly given as 1976.3699 in McA1982b.
13100+1731 = ADS 8804
--------- A preliminary orbit for this edge-on pair indicates that one of
the F5 V stars may partially eclipse the other in early 1990.
1997.1179 The magnitude difference of the system is listed in the WDS
as 0.0. Our reduction does not give the quadrant unambiguously,
so we adopt the quadrant that gives a position angle consistent
with previous measures in the WDS. (Hor1997)
13121+2415 = HDS 1848
1997.4597 Very weak detection, possibly an artifact. (Msn1999b)
13161-6235 = HD 115071
--------- Hipparcos has shown this star to be an eclipsing binary with a
period of 1.37 d (ESA1997). Both Penny (1996a) and Howarth et
al. (1997) found evidence of line-doubling. Turner (1985)
shows that this star appears close to and has a similar distance
to the cluster Stock 16. (Msn1998a)
13164+2906 = HZ 43
--------- This system is probably an optical pair. (McA1996)
13166+1948 = HDS 1862
1988.1655 Unresolved upon initial inspection (McA93), a very weak
peak was later found which agreed well with the
Hipparcos measurement. (Msn1999b)
13175-0041 = HR 5014 = Fin 350
--------- An orbital analysis of this system is in progress. This binary is
comprised of a pair of F0V stars of near-zero delta m, so there is
considerable uncertainty as to whether the orbit is of short-period/
high-eccentricity (P~9yr, e~0.6) or long-period/low-eccentricity
(P~18yr, e~0.0). The rms residuals to the speckle observations are
slightly smaller for the long-period orbit, but mass sums (a^3/P^2)
for the two orbits differ by just 2%, insufficient to rule out either
solution on the basis of plausibility. (Hrt1994)
--------- An orbit for this system was published in Hrt1996a.
13197+4747 = ADS 8862 = CHR 193 Aa
1992.3126 This appears to be a new component to the 1".5 49-year period pair
of K/M dwarfs Hu 644. This is the only one of the current crop of
new interferometric binaries which has not yet been confirmed.
13202+1747 = A 2166
--------- An orbit for this system was published in Hrt1996a.
13304-7851 = HD 116852
--------- The classification is from Morgan et al. (1955).
Sembach & Savage (1994) suggest that the star lies at
1.3 kpc from the Galactic plane, and so we have
assigned it to the "runaway" category. (Msn1998a)
13328+3454 = ADS 8939
1986.397 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
13347-6320 = HD 117856
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
13396+1044 = ADS 8987
1980.1539 This measure was omitted in McA1983.
13529-6243 = HD 120678
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
14064-5943 = HD 122879
--------- The classification is from the LSC; however, Garrison
et al. (1977) assign a type B0 Ia. (Msn1998a)
14088+7733 = HR 5321
1984.2791 Single line SB with a period of 606 days. Halbwachs
(1981 A&AS, 44, 47) predicts an angular separation of
about 0".03 and the system appears to be at the limit
of resolution of the 6-m telescope. (Bnu1986)
14139+2906 = ADS 9174
1980.4791 This measure was omitted in McA1983.
14157+1911 = HR 5340
1975.624 Disk not clearly resolved at 600 nm but resolved
(0".018 +/- 0".004) at 450 nm. (Bla1977a)
1975.634 Disk resolved (0".018 +/- 0".005) at 500 nm. (Bla1977a)
14182-5130 = HD 124979
--------- The classification is from McConnell & Bidelman (1976).
Tobin & Kilkenny (1981) place the star at 0.7 kpc from
the Galactic plane, so we have included it in the
"runaway" group. Penny (1996a) suggests that the star
may be a double-lined binary which needs confirmation
since there are only 2 other known double-lined
binaries among the runaway stars (both B-type systems;
see Gies & Bolton 1986). (Msn1998a)
14202-6105 = HD 125206
--------- This "field" object may belong to the "CLUST 3" group
of Mel'nik & Efremov (1995). (Msn1998a)
14321+3819 = HR 5435
1975.383 Photometric variable star of tentative period 0.29 day;
also a member of a binary system with separation ~
33".4 and delta m ~ 9.27. This observation apparently
resolves the brighter primary into two stars. (BLM1978)
14323+2641 = ADS 9301
1977.1780 This measure was omitted in McA1982b.
1980.1539 This measure was omitted in McA1983.
14403+2158 = HR 5472 = McA 40
1980.4791 This measure was omitted in McA1983.
1983.3041 A spectroscopic triple system, with periods 101.6 and
3320 days. The long-period pair has covered more than
half its orbit; the orbit may be determinable. (Bag1984a)
1985.5226 This measure was found to give very large residuals to
the orbit of Barlow & Scarfe (1991 AJ, 102, 2098).
Comments in our reduction log note the measure was
marginal, and after reinspection we have determined
that this measure was spurious. (Hrt1992b)
14543-3737 = CD-37 9777
--------- Listed as possibly resolved by Whi1991, but no
separation or position angle given.
14575-2125 = ADS 9446 = H 28 BC
1987.455 Vector separations from the 1D data are combined to
1987.756 give 2D theta and rho values for these four dates.
1988.312 (Mar89)
1988.499
14587-2739 = ADS 9453
1976.474 The observed separation is much larger than that
derived from the elements given by Mourao (1965 IAU
Comm. 26, Circ. Inf. 35), which gives a period of
339.3 yr. These elements yield a total mass of 13.65
Msun, which seems too large for a pair of A5 stars.
(BLM1978)
15039+4739 = ADS 9494
1975.383 The fainter component is a W UMa variable and a SB.
The visual binary has been observed here. (BLM1978)
15073+1827 = ADS 9505
1986.384 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
15088-4517 = HR 5626
1976.471 The observed separation is significantly different from the
value derived from van den Bos' (1962 J. Obsers. 45, 55)
preliminary elements. (BLM1978)
15121+1858 = HR 5654
1986.4500 Delta m = 2 at 550 nm and 3 - 3.5 at 700 nm. (Bla87)
15123-1947 = B 2351 Aa
--------- This system has crude Delta m estimates from lunar
occultation of about 1.3 magnitudes in both red and blue
(OCC1979e). Orbits of this system have been published by
Heintz (Hei1982c) and later by Mason (1994, Ph.D. thesis,
Georgia State Univ.; 1995, PASP, 107, 799); a further
analysis is in progress. (Hrt1996b)
15169-6057 = HD 135240 (Delta Cir)
--------- This "field" object may belong to the "Pis 20" group
of Mel'nik & Efremov (1995). The secondary
classification is an estimate from Stickland et al.
(1993b). The Hipparcos Catalogue (ESA1997) contains
an eclipsing light curve. Classification of the B
component of the optical pair is from Lindroos (1985).
Lindroos also finds a distance of 750 pc to this
system. (Msn1998a)
15182+3139 = U CrB
1983.3123 Lippincott's (1983 A.J. 88,542) recent improved parallax of
0".0041 practically rules out direct observation of the
companion that is perturbing the orbital motion of this SB.
(Bag1984a)
15188-6030 = HD 135591 = 45 Cir
--------- This "field" object may belong to the "Pis 20" group of
Mel'nik & Efremov (1995). Classifications of the B and
C components are from Lindroos (1985); the C component
classification is photometric. Lindroos finds a
distance of 1.0 kpc. (Msn1998a)
15245+3723 = ADS 9626 = CHR 181 Aa
1993.1976 This confirms the discovery observation, made in 1988 (Hrt1994).
15278+2906 = HR 5747
1973.22 (also 1973.45) See discussion and orbital elements in Lab1974.
1975.383 (also 1975.455) The observations presented here are of poor
quality but the results are consistent with those of Labeyrie
et al. and McAlister. (BLM1978)
1980.4682 See preliminary elements and discussion in Bag1984b.
1983.3206 A peculiar SB with a 10.5-year period. (Bag1984a)
1984.1867 (also other observations through 1985.2440) The
speckle interferometric observations are in good
agreement with both Balega et al. (1984 A&AS, 57, 31),
and Tokovinin (1984 SvAL, 10, 121) orbits; radial
velocity measurements are strongly needed to improve
the spectroscopic orbit of this system. (Bnu1986)
15318+4053 = ADS 9688
1921.400 This observation is highly uncertain.
1985.2002 (also 1985.2494) These two measurements are not precise because
this interferometric binary is only marginally resolved with a
2-m telescope. Estimates of rho and theta are deduced from the
elongation of the central peak in the autocorrelation. (Bnu1986)
15351-4110 = HR 5776
1976.471 Heintz (1956 Astr. Nachr., 283, 145) reports that this orbit is
not well known. (BLM1978)
15360+5438 = HR 5818 = CHR 47
--------- Apparently a spurious binary (9 attempted confirmations,
1986.41 - 1992.31). (McA1993)
15416+1941 = ADS 9744
1973.22 (also 1973.45) These measurements agree with the published
orbit of van den Bos (1967 J. Obs, 13, 119). (Lab1974)
1980.4791 This measure was omitted in McA1983.
1986.388 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. It is now possible to make the final choice between
two orbits of van den Bos (1963) in favor of the circular orbit
and to perform small but necessary corrections to the orbit.
(Tok1985)
15420+0028 = ADS 9747
1986.395 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
15447+1716 = HR 5858 = CHR 49
--------- Apparently a spurious binary (10 attempted confirmations,
1986.41 - 1992.31). (McA1993)
15465+0721 = HR 5868
--------- This object was misidentified as HR 5863 in McA1978c.
15513-0305 = CHR 51
--------- This peak was overlooked in the original analysis of our
speckle data, but rediscovered during work on our
quadrant determination paper. (Hrt1992b)
16003-2237 = HR 5953
1973.22 (also 1973.45) The new component here appears to have a much
longer period than the 20-day single line SB reported by van
Hoof et al. (1963 ApJ, 137, 824). (Lab1974)
1981.4767 (also other observations through 1981.4929) Companion
discovered by intensity interferometry (Hanbury Brown et al.,
1974, MNRAS, 167, 121). Delta m in the visible is about 2.
(Bag1984b)
1993.415 observations with MAPPIT on 3.9m AAT; maximum separation of
apertures was 3.3m. Paper gives orbit. (Bed1993)
--------- An orbit for this system was published in Hrt1996a.
16033+3638 = HR 5983
1983.3070 A type dF9 + A0 SB with a 108 day period. A visual companion
with delta m ~ 2 magnitudes is suspected, but further
confirmation is required. (Bag1984a)
1984.2792 Halbwachs (1981 A&AS, 44, 47) predicts an angular
separation of about 0".02. Analysis of the
interferometric measurements combined with the
spectroscopic orbit shows that the interferometric
binary is probably not the spectroscopic system. (Bnu1986)
16035-5747 = HD 143474
--------- This star was misidentified as ADS 9870 = HD 143456 in the
first speckle catalogue.
1976.474 Visual observations of this system extend over more than two
periods, but this separation is significantly different from
that derived from van den Bos' (B__1961b) elements. (BLM1978)
1994.5216 Our measure is plotted with orbital data from the WDS
catalogue in Figure 2. (Hor1996)
16057-0617 = Fin 384 Aa
1990.3494 Residuals from the orbit of Baize (1992 A&AS, 92, 31)
are (-4.5 deg, 0".003).
16059+1041 = HDS 2273
1991.3273 This observation confirms the Hipparcos solution at a
similar epoch (1991.25). An elongated secondary peak
yielded an inaccurate value for rho, however. (Msn1999b)
1996.3240 An elongated secondary peak yielded an inaccurate value
for rho. (Msn1999b)
16079+1425 = ADS 9931
1983.7151 This autocorrelogram was remeasured; the new results are listed
here.
16085-1006 = ADS 9932
1980.4791 This measure was omitted in McA1983.
16119+3626 = HR 6046
1983.3098 Very poor atmospheric conditions. (Bag1984a)
16146-1832 = HR 6053
--------- A measure on 1980.7255 was incorrectly attributed to HR 6053 in
McA1983; that measure, with a factor of two correction in the
separation, actually belongs to HR 6560.
16212-2536 = HR 6084
1976.471 These measurements cannot be that of the SB system observed by
Struve et al. (1961 ApJ, 133, 509) but probably relates to the
more distant companion observed by Nather et al (1974 PASP,
86, 116) at a lunar occultation. The system is also a
photometric variable. (BLM1978)
16238+6142 = CHR 138
--------- This measure confirms the discovery of the Aa component
of ADS 10052 by McAlister et al. (McA1989). (Hrt1992b)
16245-3734 = B 868
1991.3926 This system may have made a very close periastron passage
between the times of our 1989.3 observation (rho = 0".039)
and this one, although unfortunately the system was not
observed in 1990.
16254+3724 = HR 6123 = CHR 55
--------- Preliminary orbital elements (P = 32.75 yr) are given
in McA1993.
16273-2442 = ROX 21
1986.4 0.45 - 0.18 flux ratio in J band (Sim87)
1986.4 1.00 - 0.35 flux ratio in H band (Sim87)
16303+2129 = HR 6148
--------- A measure on 1980.4820 was incorrectly attributed to HR 6148 in
McA1983; it actually belongs to HD 163640.
1975.6273 SB, companion is red. (Bla1977a)
1983.3043 Only the asymmetry of the ACF peak indicate that the star is
double. The system has been resolved in the red (Bla1977a) with
the 200-inch telescope. (Bag1984a)
--------- Single line SB; all positive observations have been made in the
red spectral range (wavelength > 6000 Angstroms) so delta m
probably is >3 in the visible. (Bnu1986)
16341+4227 = HR 6168
--------- This object was misidentified as tau Her in McA1978c. The observation
on 1976.2963 which was reported in McA1978c as yielding a negative
result does indeed show duplicity, as was correctly reported in
McA1978b. The negative result reported in McA1978c for 1976.2991 is
spurious.
1972.28 (also 1973.45) Two of the three observations yielded fringes in
the Fourier transform which were quite different; this is
difficult to reconcile with the 50-year period estimated from
Kepler's law. (Lab1974)
1977.1781 This is a previously unpublished photographic measure.
1977.3284 Theta was incorrectly given as 5.7 degrees in McA1982b; the correct
value was published in McA1989.
1983.3098 Very poor atmospheric conditions. (Bag1984a)
16364-4252 = HD 149404
--------- The classification is from the UV tomographic analysis
of Penny (1996b). (Msn1998a)
16372-1034 = HD 149757 = zet Oph
--------- The line profile variations of this nonradial pulsator
are most recently described in Kambe et al. (1997).
Van Rensbergen et al. (1996) discuss the runaway
trajectory of the star. (Msn1998a)
16391-3713 = Fin 340 AB
1991.3926 From its discovery in 1954 through the mid-1960's, this
system closed from 0".14 to 0".10 and increased in theta
from 147 deg to 172 deg. It is impossible to determine
from this single speckle measure whether the pair has gone
through periastron and flipped quadrant, but this should
become obvious within the next couple of observations.
16406+0412 = HR 6194 = CHR 56
--------- Apparently a spurious binary (9 attempted confirmations,
1986.41 - 1992.31). (McA1993)
16413-4846 = HD 150135
--------- This star (the C component of HD 150135) was observed
and appeared to be single. (Msn1998a)
16416+2655 = HR 6213 = CHR 57
--------- Apparently a spurious binary (9 attempted confirmations,
1986.41 - 1992.31). (McA1993)
16438-5330 = Fin 251 AB
1990.3467 CHR 147 Aa, the close third component to this system
1990.3495 discovered in 1989.3, was unfortunately not confirmed in
1991.3926 these observations.
16450+2928 = Cou 490
1983.3125 Very poor atmospheric conditions. (Bag1984a)
16453+5647 = HR 6237 = McA 44
1983.3099 Elongated ACF peak suggests that the object may be double with
theta ~ 104 degrees, rho ~ 0".024. HR 6237 is in fact a 1386
day SB. (Bag1984a)
16466-4705 = HD 150958
--------- Leep (1978) suggests that this star is a single-lined
binary with a period of approximately 5 d. (Msn1998a)
16500-4137 = HD 151564
--------- The classification is from Schild et al. (1969);
however, Garrison et al. (1977) assign a type B0.5 V.
(Msn1998a)
16528-4147 = HD 152003
--------- Constant radial velocity is also found by Levato et al.
(1988). (Msn1998a)
16540-4143 = HD 152218
--------- The classification is from the UV tomographic analysis
of Penny et al. (Pnn1993). A new orbit by Stickland et
al. (1997b) yields a period of 5.604 d. (Msn1998a)
16541-4147 = HD 152233
--------- This O star is the F component of the multiple system.
The A component is HD 152234 which is a B0.5Ia star
(Hoffleit & Warren 1991). The AB system is a 0".5
binary which was observed and resolved 3 times. (Msn1998a)
16542-4151 = HD 152249
--------- We found a possible binary companion at a separation of
0".06 which needs confirmation. (Msn1998a)
16542-4150 = HD 152248
--------- The classification is from the UV tomographic analysis
of Penny (1996b). The Aa component (CHR 252) was
resolved in 2 of 4 observations. (Msn1998a)
16543-4149 = HD 152270 (WR 79)
--------- The classification is from Seggewiss (1974). (Msn1998a)
16546-4125 = HD 152333
--------- The classification is from Schild et al. (1969). (Msn1998a)
16549-4031 = HD 152405
--------- Raboud (1996) finds the star to be a radial velocity
variable. (Msn1998a)
16550-4109 = HD 152408
--------- Classification of the B component is from Lindroos
(1985). (Msn1998a)
16551-4459 = HD 152386
--------- This Of star is assigned to the field in the LSC, but
Turner (1979) argues that it belongs to an anonymous OB
association related to the Cepheid, KQ Sco. (Msn1998a)
16551-4205 = HD 152424
--------- Fullerton (1990) finds radial velocity variations that
suggest an orbit with a period greater than a month.
Levato et al. (1988) also find radial velocity
variations. (Msn1998a)
16562-4040 = HD 152623
--------- Fullerton (1990) discovered the short-period
spectroscopic variation, and subsequently Wiemker
(1992) showed that the spectral variations are best
explained by the superposition of a stronger stationary
component and a moving component. Thus, the speckle
resolution of this system (CHR 210) makes clear that
this is (at least) a triple consisting of a
short-period SB1 and a distant O star. The Hipparcos
results (ESA1997) confirm the CHR 210 pair. (Msn1998a)
16563-4030 = HD 152622
--------- The classification is from Garrison et al. (1977).
(Msn1998a)
16568-2309 = ADS 10265
1983.4282 The original McA1987b observation contained a small typo.
16569-4031 = HD 152723
--------- This new binary is designated CHR 254 Aa. Fullerton
(1990) suggests that the A component is a single-lined
spectroscopic binary with a period of about 12 d and a
semiamplitude of approximately 15 km/sec.
Classifications of the B, C, and D components are from
Lindroos (1985). Lindroos finds a distance of 2.0
kpc. (Msn1998a)
16584+3943 = Cou 1289
1986.395 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
17039-3751 = HD 153919 = 4U1700-377 = V884 Sco
--------- This is a massive X-ray binary with a neutron star
companion. The ellipsoidal variation is portrayed in a
recent Hipparcos light curve (ESA 1997). (Msn1998a)
17065-3527 = HD 154368
--------- This "field" object may belong to the "CLUST 4 " group
of Mel'nik & Efremov (1995). An ellipsoidal variation
is present in the Hipparcos data (ESA 1997) with an
unusually long period of 16.11 d. (Msn1998a)
17081+3555 = ADS 10360
1980.4766 This measure was omitted in McA1983.
17082-3500 = HD 154643
--------- This "field" object may belong to the "CLUST 4 " group
of Mel'nik & Efremov (1995). The classification is from
Garrison et al. (1977). (Msn1998a)
17095+4047 = HR 6388 = McA 45
--------- The equinox-1900 position was incorrectly given as 17093+4054
in McA1983.
17121+4545 = Kui 79
--------- An orbit for this system was published in Hrt1996a.
17146+1423 = CHR 139
--------- Radial velocity measures by Smith (1988 private communication)
for alp Her A since 1984 have shown an increase in velocity by
about 11 km/sec during a three-year interval, then an apparent
turnover in velocity during the fourth year. This suggests a
component with a period of the order of a decade; it now appears
that this system may have at least five physical components.
17150+2450 = HR 6410
1983.3180 Measurements were made with the 20-power objective, hence the
accuracy is low. (Bag1984a)
17162+0211 = HR 6412 = CHR 61
--------- Apparently a spurious binary (14 attempted
confirmations, 1986.41 - 1992.31). (McA1993)
17173-3533 = HD 156134
--------- The classification is from McConnell & Bidelman (1976).
(Msn1998a)
17175-2746 = HD 156212
--------- Levato et al. (1988) find the radial velocities to be
"probably variable", but since the total range in 11
measurements is 33 km/sec we assign it to the "C"
category. (Msn1998a)
17200-0801 = CHR 151 Aa
--------- This newly-discovered pair was unresolved in our earlier
survey for duplicity among high-velocity stars (Lu_1987).
Abt & Biggs (1972, Bibliography of Stellar Radial Velocities)
list a single radial velocity of -89.3 km/s for this object,
published in 1950. Additional observations, both by speckle
and by spectroscopy, are needed for confirmation of its
duplicity and its high velocity. (Hrt1992b)
17207-5625 = Fin 255 AB
1990.3497 This observation finally confirms the discovery of this
system by Finsen, made in 1931!
17215+2845 = HR 6466 = CHR 194 Aa
1991.3247 This is a new close companion to the 0".7 pair Kui 80. The primary
of this system is listed in the preliminary version of the fifth
edition of the Bright Star Catalogue (Hoffleit & Warren 1992) as a
G0III spectroscopic binary.
17217+3958 = HR 6469 = McA 47
--------- A new combined spectroscopic/interferometric orbital solution has been
published by Scarfe et al. (Scf1994). (Hrt1994)
17240-0921 = Rst 3972
--------- An orbit for this system was published in Hrt1996a.
17241+3834 = ADS 10531
1985.741 The residuals of these measurements (as well as those of
McAlister) are irregular and do not permit the correction of an
orbit. (Tok1985)
17292-3132 = HD 158186
--------- The classification is from Garrison et al. (1977).
An eclipsing light curve is presented in the Hipparcos
Catalogue (ESA 1997) for a period of 8.77 d. (Msn1998a)
17314+0244 = ADS 10607
1978.6174 This epoch was incorrectly given as 1977.6174 in McA1981b.
17317-2616 = CHR 229
--------- Possible confirmation of this pair may be found in
Hoffleit & Warren (1992, Bright Star Catalogue,
preliminary 5th edition), who note the following:
``Duplicity reported from grazing occultation
observations of 1991 Sep 15. Estimated magnitude of
comparison 8.6, separation several tenths of an
arcsecond in position angle 160 deg (all rough
estimates)". (Hrt1996b)
17335+5734 = HR 6560
1980.7255 This measure was incorrectly attributed to HR 6053 in McA1983,
with an additional factor of two error in the separation.
17347-3235 = HD 159176
--------- Our single observation appears to indicate a single
star, so we cannot confirm the reported Iso 5 Aa pair.
Nor did we detect the new Hipparcos Aa,D pair,
presumably because of the large magnitude difference
(Delta Hp = 3.2). Classifications of the B and C
components are from Lindroos (1985). Lindroos also
notes a wider "X" component (V = 10.8, separation =
25", photometric classification = B5 IV) which he
claims is physical. This component is not mentioned in
the WDS. Lindroos finds a distance of 1.8 kpc. (Msn1998a)
17349+1234 = HR 6556
--------- This object was incorrectly identified as HD 159571 in Bag1984b.
17368-2058 = ADS 10657
1985.4843 This autocorrelogram was remeasured; the new results are listed
here.
17375+2419 = HR 6571 = CHR 63
--------- Preliminary orbital elements (P = 11.02 yr) are given
in McA1993.
17461+0532 = IC 4665 K 62 = CHR 157
1991.3275 An 18.92-day period orbit in Batten et al. (1989,
Eighth Catalogue of the Orbital Elements of
Spectroscopic Binary Systems, Pub. DAO, 17)
apparently refers to a closer comonent. Membership of
this star in the cluster IC 4665 is in question: Abt
et al. (1964 ApJ, 139, 1139) list it as a member,
Sanders & van Altena (1972 A&A, 17, 193) as a
non-member. (Msn1993b)
17490+3704 = Cou 1145
1981.333 This observation was incorrectly attributed to Cou 1445 in
Tok1982a (noted in Tok1982b).
17491+5047 = HR 6656 = CHR 65
--------- Apparently a spurious binary (10 attempted confirmations,
1986.41 - 1992.31). (McA1993)
17543+1108 = Fin 381
--------- An orbit for this system was published in Hrt1996a.
17564+1820 = McA 49
1980.4820 This measure was incorrectly attributed to HR 6148 in McA1983.
17572+2400 = HR 6697
1983.3072 A close pair of solar-type stars, probable period 940 days;
astrometric binary (Bag1984a)
--------- Culver et al. (1980 BAAS 12, 250) report this to be a
spectroscopic binary with a period of 2.6 years. (Bla87)
--------- Determination of these two old measures resulted from new
reduction techniques developed over the past year; these
data were reanalysed for a joint spectroscopic/speckle
anaylsis of this system, now in preparation. (Hrt1992b)
--------- All our CCD speckle data for this close system have been
reprocessed and examined. In addition, we have listed 7
negative measures dating from observations made at the KPNO
2.1-m in the 1970's. A combined spectroscopic/interferometric
orbit is now in preparation by McAlister et al. (Hrt1994)
17584+0427 = +04 3562 = Kui 84
--------- A measurement published in McA1987b dating from 1985.4872 was misidentified
as being of Kui 84; the measurement actually was of Kui 89
(WDS 18594-1250). In addition, an observation of Kui 84 dating from
1988.6655 (theta = 270.6 deg, rho = 0".134) was published in McA1990.
These data have been reprocessed, and we now believe the 1988.6655
measurement was spurious. (Hrt1994)
17595-3601 = HD 163758
--------- Leep (1978) also finds a constant radial velocity.
(Msn1998a)
18019-1906 = HD 164438
--------- We found a possible binary companion at a separation
of 0".05 which needs confirmation. The classification
is from Garrison et al. (1977). (Msn1998a)
18050-2935 = HR 6742
1976.477 This is a Cepheid variable with a companion at a distance of
48". This measurement resolves the variable star. (BLM1978)
18052-2424 = HD 165052
--------- The classification is from Morrison & Conti (1978).
(Msn1998a)
18060-1412 = HD 165319
--------- The classification and distance are from Crampton &
Fisher (1974). (Msn1998a)
18075+2846 = HR 6779 = omi Her
1981.373 Result needs further confirmation. Delta m = 0.85? (Tok1980)
18093-2359 = HD 165921 = V3903 Sgr
--------- The classification and orbit are from Niemela &
Morrison (1988). (Msn1998a)
18117+3327 = ADS 11149
1979.3601 Theta was incorrectly given as 42.4 degrees in McA1982d.
1980.4768 Rho was incorrectly given as 0".091 in McA1983.
18152-2023 = HD 167263 = 16 Sgr = CHR 255
--------- This new binary is designated CHR 255 Aa. Garmany et
al. (1980) observed a smoothly varying velocity
indicating that the A component is probably a
single-lined binary with a period of 11 d. Lindroos
(1985) provided the classification of the B component
and determines a distance of 1.2 kpc. (Msn1998a)
18168-1631 = HD 167633
--------- Additional radial velocities are reported by Crampton &
Fisher (1974). The star appears within the boundaries
and at the same distance of Ser OB1 in the LSC. (Msn1998a)
18170-1858 = HD 167659
--------- The 3 speckle observations all indicate a single star,
so we cannot confirm the existence of a companion found
by lunar occultation (OCC1980c). (Msn1998a)
18175-1828 = HD 167771
--------- The classification of the close spectroscopic pair is
from Morrison & Conti (1978), and that of the B
component of the optical pair is from Lindroos (1985).
Lindroos also gives a distance of 2.0 kpc. (Msn1998a)
18181-1215 = HD 167971
--------- Leitherer et al. (1987) argue that this is a triple
system consisting of a close eclipsing pair and a
brighter, distant O star; the spectral classification
presumably applies to the latter star. (Msn1998a)
18186-1838 = Bu 639 AB
1994.5191 Quadrant determined by speckle imaging analysis (Hor1996)
18197-4542 = CHR 148
1989.3068 HD 167954 is a SBLM1978, with P = 120 days (Bopp et al.
1970 MNRAS, 147, 355). With rho = 0".031, the speckle
pair is probably not the SB. (McA1990)
18211+7244 = HR 6927 = chi Dra
--------- See discussion and orbital elements in Lab1974.
--------- Analyses of the spectroscopic/interferometric orbit are given
by McAlister (McA1980c) and by Tomkin et al. (Tom1987).
18255-1241 = HD 169515 = RY Sct
--------- This massive binary and its surrounding gas torus are
described by Gehrz et al. (1995). A light curve from
Hipparcos is now available (ESA 1997). The system mass
and the nature of the secondary are still controversial
(Skulskii 1992; Skulskii & West 1993; Golovatyi &
Skul'skii 1992). We found a possible binary companion
at a separation of 0".2 which needs confirmation.
(Msn1998a)
18259+1458 = HR 6906 = CHR 70
--------- Apparently a spurious binary (10 attempted confirmations,
1985.84 - 1992.31). (McA1993)
18261+0046 = ADS 11339
1980.4794 This measure was incorrectly attributed to ADS 11524 in McA1983.
18280+0612 = HR 6928 = CHR 71
--------- Preliminary orbital elements (P = 11.12 yr) are given
in McA1993.
18301+0404 = CHR 72
1985.8424 This autocorrelogram was remeasured; the new results are listed
here.
18323-1439 = CHR 73
1989.3041 Due to a typographical error, this measurement was
incorrectly attributed to 18444+3937 = CHR 77 in
McA1990. (Hrt1996b)
18340+5221 = ADS 11468
1975.533 This appears to be part of a triple system. The elements given
by Wilson (WRH1950) and by Baize (Baz1958c) are different,
possibly due to the long period of the system. This separation
is less than that derived from either ephemeris but it and the
position angle are closer to Baize's values. (BLM1978)
18383+0850 = ADS 11524
--------- A measure on 1980.4794, incorrectly attributed to ADS 11524 in
McA1983, actually belongs to ADS 11339.
18410+2450 = ADS 11574
1986.4502 RA given incorrectly as 19 hrs in Bla87.
18413+3018 = ADS 11579
1993.2059 Improved fit to observation in Hrt1994.
18444+3937 = CHR 77 Ca
--------- See note for 18323-1439 = CHR 73. (Hrt1996b)
18455+0530 = ADS 11640
--------- This quadruple system is comprised of two close (0".14) pairs of
similar position angle, discovered by Finsen with his eyepiece
interferometer. Our 1982 observations (McA1987b) were made at a lower
magnification and included all four stars in the field. The
resulting overlapping autocorrelation peaks precluded us from
measuring the Aab or Bab pairs directly, but did permit the
measurement of the AB, Aa-Bb, and Ab-Ba configurations. In
later observations made at higher magnification we observed the
A and B components separately, enabling the measurement of Aab
and Bab but not AB.
--------- Listed in the first speckle catalogue as STF 2375 AB,CD.
18455+0530 = Fin 332 Aab
--------- Listed in the first speckle catalogue as Fin 332 AB.
1980.4794 This measure was omitted in McA1983.
18455+0530 = Fin 332 Bab
--------- Listed in the first speckle catalogue as Fin 332 CD.
18492+2503 = HR 7091 = CHR 79
--------- Apparently a spurious binary (7 attempted confirmations,
1986.89 - 1992.31). (McA1993)
18530-0935 = HR 7110 = CHR 81
--------- Apparently a spurious binary (8 attempted confirmations,
1987.76 - 1992.45). (McA1993)
18582-2025 = HD 175876
--------- Classification of the B component is from Lindroos
(1985), who also gives a distance of 1.9 kpc to the
system. (Msn1998a)
18594-1250 = HR 7166 = Kui 89
1985.4872 This measurement was incorrectly attributed to Kui 84
(WDS 17584+0427) in McA1987b.
19026-2953 = HdO 150 AB
1994.5246 Our measure is plotted with orbital data from the WDS
catalogue in Figure 3. (Hor1996)
19081+2142 = CHR 83
--------- Discovered in a reanalysis of data for Bagnuolo et al.
(Bgn1992), this measure predates our "discovery" observation
by more than one year. (Hrt1992b)
19091+3436 = CHR 84
1985.5232 This autocorrelogram was remeasured; the new results are listed
here.
19126+1651 = ADS 12160
--------- This object was misidentified as HD 179558 in McA1983.
19141+6707 = HDS 2722
1997.7281 Mean motion indicates P ~ 80 yr, rho decreasing.
(Msn1999b)
19155-2515 = ADS 12214
1982.5056 This autocorrelogram was remeasured; the new results are listed
here.
19164+1433 = HR 7307 = CHR 85 Aa
--------- Preliminary orbital elements (P = 8.95 yr) are given
in McA1993.
19180+2012 = Cou 321
1986.394 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
19243+2032 = HDS 2752
1997.7200 Mean motion indicates P ~ 80 yr, rho increasing.
(Msn1999b)
19244+1656 = HDS 2753
1996.5425 Very weak detection (Hipparcos found Delta m \geq 3.8).
(Msn1999b)
19246+5014 = CH Cyg
1983.4904 Speckle interferometry can clarify the geometry of this
symbiotic star: adopting a 5750 day period, eccentricity = 0,
and 100-pc distance, and assuming the total mass of the system
is small (Wallerstein, 1983 PASP, 95, 564), we obtain rho ~
0".07. Joint speckle interferometric observations with Bonneau
and Foy on the 6-meter telescope in October 1981 also failed to
disclose the companion. (Bag1984a)
19253-2431 = Fin 327
1991.3928 With 15 years of speckle data on this system we are
finally able to attempt to improve upon Finsen's (Fin1965b)
orbital elements. We apparently view the pair at a nearly
90 deg inclination and since the delta m for the components
is near zero there is considerable ambiguity between a high-
eccentricity short-period orbit and a low-eccentricity
long-period one. A new orbital analysis is now in
preparation, including reanalysis of earlier speckle
data in order to derive absolute quadrants and possibly
resolve this ambiguity. (Hrt1993)
19254+2455 = HR 7386 = CHR 86
--------- Apparently a spurious binary (5 attempted confirmations,
1986.89 - 1991.90). (McA1993)
19303+5639 = ADS 12552
1980.7257 This measure was omitted in McA1983.
19307+2758 = McA 55
--------- See discussion of colors and magnitudes of this
composite spectrum system in Bon80a.
1977.4816 This object was incorrectly attributed to the system
ADS 12540 = STF 43 in McA1979b.
1980.7173 This measure was omitted in McA1983.
1983.4904 The distant companion reported by McAlister & Hendry
(McA1982b) would be located beyond the 0".371 ACF window.
(Bag1984a)
19394+3009 = HR 7478 = McA 57
--------- Analysis of the spectroscopic/interferometric orbit is given by
McAlister (McA1982a).
1980.7173 Theta and rho were incorrectly given as 77.1 degrees and 0".036,
respectively, in McA1983.
--------- Errors are given as "error ellipses"; these values are
tabulated below. Columns include date (BY), major and
minor axes of the ellipse (in mas), and ellipse
orientation (in degrees). (MkT1992c)
1989.4053 3.6 0.14 100.5
1989.5312 4.8 0.76 81.6
1989.6022 10.8 0.64 81.3
1989.6050 5.8 0.43 77.1
1989.6160 1.04 0.16 74.8
1989.6242 1.15 0.117 75.5
1989.6351 1.58 0.159 75.2
1989.6812 0.45 0.049 92.3
1989.6867 2.65 0.31 84.5
1989.6894 1.47 0.137 85.7
1989.7031 5.5 0.6 85.0
1989.7852 6.1 0.44 76.8
1989.7962 4.8 0.35 70.9
1990.4758 2.3 0.19 85.5
1990.4839 1.68 0.39 91.1
1990.5111 0.135 0.041 112.4
1990.5139 0.181 0.046 94.8
1990.5167 0.40 0.114 93.3
1990.5195 0.29 0.079 86.9
1990.5304 0.109 0.040 87.6
1990.5359 0.116 0.038 89.2
1990.5388 0.55 0.067 76.1
1990.5687 0.25 0.055 85.7
1990.5714 0.141 0.042 84.1
1990.5741 0.28 0.069 93.8
1990.5768 0.178 0.061 96.5
1990.5822 0.29 0.064 97.0
1990.5931 2.2 0.36 95.3
1990.6099 0.63 0.116 69.5
1990.6260 0.40 0.091 93.0
1990.6343 0.96 0.121 82.1
1990.6371 1.17 0.23 76.7
1990.6452 0.158 0.028 80.3
1990.6535 0.42 0.034 75.3
1990.8255 1.03 0.079 72.4
1991.4696 0.71 0.120 100.4
1991.5490 0.25 0.044 80.6
1991.5870 0.23 0.051 95.8
1991.5898 0.25 0.038 91.9
19412+1349 = HR 7486
1980.7256 This measure was incorrectly attributed to ADS 12973 in
McA1983.
19419+4015 = Kui 94
--------- An orbit for this system was published in Hrt1996a.
19474+1832 = HR 7536
1975.629 Disk unresolved but possible binary. (Bla1977a)
19489+1908 = ADS 12973
--------- A measure on 1980.7256 was incorrectly attributed to
ADS 12973 in McA1983; it actually belongs to HR 7486.
1975.553 This is part of a triple system. Finsen's (1937 Union
Obs. Circ 4, 359) observations covered two periods and
yield a separation close to this one. (BLM1978)
19524+1840 = HD 188001 = 9 Sge
--------- Aslanov et al. (1984), Underhill (1995), and especially
Underhill & Matthews (1995) discuss a possible 78-day
orbital period for this system. Another period, 32.5
d, was found in photometric and radial velocity
measurements by Aslanov & Barannikov (1992). However,
because of the considerable scatter in the measurements
plus evidence for wind related line profile variations
(Fullerton 1990), we tentatively place the star in the
"SB1?" category. (Msn1998a)
19525+0100 = HR 7570 = eta Aql
1975.402 Oblate correlation peak. (Bla1977a)
19553-0644 = StF 2597
--------- An orbit for this system was published in Hrt1996a.
19584+3512 = HDE 226868 = Cyg X-1 = V1357 Cyg
--------- This is a massive X-ray binary with a probable black
hole companion (Gies & Bolton 1982). (Msn1998a)
19599-0957 = Ho 276
--------- An orbit for this system was published in Hrt1996a.
20035+3602 = HD 190429
--------- The Aa component (McA 59) has been resolved in only 4
of 11 observations, and the positions are discrepant
(the large errors presumably result from a large
magnitude difference). The B and C components were
also observed and appeared to be single. The
classification of the B and C components are from
Hoffleit et al. (1983). (Msn1998a)
20060+3547 = HD 190918 = WR 133
--------- The classification is from Wilson (1949). The
classification of the B, D, and F components are from
Hoffleit et al. (1983). (Msn1998a)
20074+3543 = HD 191201
--------- The classification and orbit are from Burkholder et
al. (1997). (Msn1998a)
20126+4016 = HD 192281
--------- Barannikov (1993) suggests a possible, low amplitude
orbit with a period of 5.5 d, but we have placed the
star in the "C" category based on the constancy found
by Gies & Bolton (1986). (Msn1998a)
20137+4644 = HR 7735
1983.4905 A spectroscopic, eclipsing, astrometric, and
interferometric binary. Our ACFs, however, do not
resolve the system with much confidence (theta ~168
deg, rho ~0".029). (Bag1984a)
20140+5557 = BD+55 2347
1984.778 This object, first resolved here, was suspected to be
an astrometric binary with period about 11 years and
semiamplitude about 0".1 by A.A. Voltchkov. The
observed orbital motion is not incompatible with the
astrometric data. (Tok1985)
20158+2749 = HR 7744 = CHR 94 Aa
1991.8932 These two observations confirm the discovery
measurement of this close component, made in 1985 (McA1987b),
and indicate considerable motion during this interval.
20161+3854 = HR 7752 = CHR 95
--------- Apparently a spurious binary (6 attempted confirmations,
1985.84 - 1991.89). (McA1993)
20178+3802 = HR 7763
1975.636 Disk unresolved in H alpha emission but resolved
(0".020 +/- 0".008) in H beta emission. (Bla1977a)
1976.402 Disk resolved (0".022 +/- 0".006) in H beta emission.
(Bla1977a)
20181+4044 = ADS 13672 = CHR 96 Aa
1985.8396 These new observations were found from reprocessing of
1988.6630 unpublished archival data. We are currently
1989.7061 undertaking a duplicity survey of all bright (V<8)
galactic O stars; this is one of four new binaries
found by us so far in this survey. This system is also
a known spectroscopic binary, and we are reanalyzing
archival radial velocity data in an attempt to derive
masses via a combined interferometric/spectroscopic
orbit (see Gies et al. 1993 AJ 106, 2072 for a similar
combined solution of the O star 15 Mon).
--------- The estimated period of the speckle binary orbit (CHR
96 Aa) is 31 y. The orbit quality rating in Table 1 is
our own. The system is currently unresolved with the
Mt. Wilson Hooker telescope, but we continue to
observe this target. The brighter star of the speckle
pair is also a 311-day, single-lined spectroscopic
binary (McKibben et al. 1997). The classifications of
the C and D components are from Hoffleit & Warren
(1991). (Msn1998a)
20189+3817 = HD 193443
--------- The classification is from Conti et al. (1977) and
refers to the combined AB pair. (Msn1998a)
20205+4351 = HD 193793 = WR 140
--------- The classification is from Smith (1968). (Msn1998a)
20210-1447 = HR 7776
--------- An orbit based upon spectroscopic, occultation, and
interferometric observations is given by Evans & Fekel
(1979 ApJ, 228, 497).
20254-2840 = CHR 97
--------- The correspondence of this component with the 377.6-day
spectroscopic system reported by Bopp et al. (1970 MNRAS,
147, 355) can only be established by further
observation.
1983.4258 This autocorrelogram was remeasured; the new results
are listed here.
20273-1813 = HR 7814 = CHR 184 Aa
1992.4579 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
20289-1749 = SHJ 323 AB
1994.5246 Quadrant determined by speckle imaging analysis. (Hor1996)
20306+4419 = HD 195592
--------- The star is close to and probably associated with WR
140. (Msn1998a)
20311+1548 = ADS 13944
--------- A measure on 1980.7257, incorrectly attributed to ADS 13944
in McA1983, actually belongs to ADS 14761.
1980.4771 Theta was incorrectly given as 313.7 degrees in McA1983.
1980.7257 This measure was incorrectly attributed to HR 8059 in
McA1983.
1986.578 The separation of this partially resolved pair was
calculated under the assumption of zero or otherwise
known magnitude difference. (Tok1985)
20339+3515 = HR 7866
1980.7257 This measure was omitted in McA1983.
20375+1436 = ADS 14073
1975.545 (also 1975.956) The elements quoted by Finsen (1938
Union Obs. Circ. 4, 461) and Couteau (1962 J. Obs,
45, 39) each give theta and rho greater than those
observed. (BLM1978)
20393-1457 = Hu 200 AB
1994.5193 Our measure is plotted with orbital data from the WDS
catalogue in Figure 4. (Hor1996)
20406-2639 = HR 7902 = CHR 186
1992.4552 Reported by Andersen et al. (1985) as SB2, with 13
RVs measured by Beavers & Eitter (1986). (McA1993)
20462+3358 = ADS 14274 = CHR 100 Aa
1991.8987 This finally confirms the discovery observation of this
component, made in 1983 (McA1987b). A number of unresolved
observations of this very close system, dating from
1979 to 1981, were published in Hrt1984.
20474+3629 = ADS 14296 = McA 63
1986.567 The separation of this partially resolved pair was calculated
under the assumption of zero or otherwise known magnitude
difference. (Tok1985)
--------- Orbital analysis of lam Cyg is in preparation; a
preliminary orbit gives a period of 11.8 years and a
semi-major axis of 0".049. (Hrt1994)
20474+3629 = STT 413
1980.7284 This measure was omitted in McA1983.
20477+3917 = ADS 14314
--------- This observation was listed in Bla1977a under its correct GC number,
but misidentified as ADS 14394.
20478+0601 = HR 7953
1985.521 This system has an estimated delta m of 3.6 magnitudes; the
secondary probably lies just outside the observed window in this
CFHT observation.
20521+3439 = HD 198846 = Y Cyg
--------- The classification is from Burkholder et al. (1997).
This eclipsing binary is one of two known double-lined
spectroscopic binaries which are a runaway objects
based on a large absolute value of systemic velocity
(Gies & Bolton 1986). (Msn1998a)
20531-1134 = HR 7994 = CHR 101
--------- Apparently a spurious binary (8 attempted confirmations,
1985.84 - 1992.45). (McA1993)
20538+5919 = ADS 14412
1979.7699 Theta and rho were incorrectly given as 178.6 degrees and
0".106, respectively, in McA1982d.
1980.7257 This measure was omitted in McA1983.
20572+4110 = HDS 2986
1989.7114 This system looks triple. This measurement concerns
the close binary. (Msn1999b)
21002+0731 = Kui 102
--------- An observation in Tok1982a (1981.370, 48.1 degrees, 0".377) was
reduced improperly, so has been removed (noted in Tok1982b).
21019+2340 = Cou 128
--------- This object was misidentified as HR 8059 in McA1980b.
21041-0549 = McA 66
--------- A measure on 1980.7257 was incorrectly attributed to HR
8059 in McA1983; it actually belongs to ADS 13944.
21044-1951 = Fin 328
--------- This system has a Delta m of about 1.7 +/- 0.7 magnitudes,
as determined from lunar occultation measures by Evans &
Edwards (OCC1983a). Orbits of this system have been published
recently by Zulevic (1993, Circ. Inf. No. 119, 1993) and Mason
(1994, Ph.D. thesis, Georgia State Univ.; 1995, PASP,
107, 799); further analysis is in progress. (Hrt1996b)
21079+3324 = HD 201345
--------- Aslanov et al. (1984) discuss the radial velocities
and the possibility of a low mass companion. (Msn1998a)
21118+6000 = McA 67
1983.4341 (also 1983.7100, 1984.7118) These three
autocorrelograms were remeasured; the new results are
listed here.
21135+1559 = ADS 14761
1979.7700 This measure is an average of a power spectrum and an
autocorrelogram measure, listed separately in McA1982d.
1980.7257 This measure was incorrectly attributed to ADS 13944 in McA1983.
21145+1001 = ADS 14773 = Stt 535 AB
--------- A combined spectroscopic/speckle orbit of this system has been
undertaken in collaboration with F.C. Fekel. (Hrt1994)
21158+0515 = HR 8131
--------- The equinox-1900 coordinates of this star are
incorrectly given as 21158+0430 in the first speckle
catalogue.
--------- A measure on 1980.4853 was incorrectly attributed to HR
8131 in McA1983; it actually belongs to ADS 14893.
--------- Errors are given as "error ellipses"; these values are
tabulated below, together with filters used. Columns include
date (BY), major and minor axes of the ellipse (in mas),
ellipse orientation (in degrees), and filter effective
wavelengths (in nm). (MkT1992b)
1989.4493 1.94 0.081 90.9 800,550,450
1989.4628 0.45 0.049 104.5 800,550,450
1989.4712 1.23 0.095 90.8 800,550,450
1989.4766 3.19 0.16 94.7 800,550,450
1989.5177 3.84 0.57 80.6 800,550,450
1989.5313 3.69 2.24 114.8 800,550,450
1989.6021 2.51 0.48 106.5 800,550,450
1989.6050 1.39 0.36 88.9 800,550,450
1989.6159 0.99 0.18 88.6 800,550
1989.6349 0.45 0.22 78.1 800,550
1989.6430 1.13 0.22 108.2 800,550,450
1989.6540 2.86 0.10 99.4 800,550
1989.7060 2.06 0.24 85.5 800,550,450
1989.7854 4.10 1.65 74.4 800,550,450
1989.7934 3.04 0.63 75.4 800,550,450
1989.7961 1.39 0.38 77.9 800,550,450
1989.8373 0.94 0.091 69.9 800,550
1989.8482 0.73 0.085 76.1 800,550,450
1990.4840 1.35 0.22 103.7 800,550,500
1990.4896 4.72 0.74 93.2 800,550,500
1990.5743 0.15 0.042 86.4 800,550,500
1990.5770 0.33 0.080 88.8 800,550,500
1990.5824 0.26 0.059 94.9 800,550,500
1990.6536 0.19 0.041 82.4 800,550,500
1990.6616 0.41 0.079 86.3 800,550,500
1990.6644 0.29 0.054 85.8 800,550,500
1990.6698 0.20 0.050 96.2 800,550,500
1990.6727 0.66 0.086 81.4 800,550,500
1990.7054 0.34 0.081 81.4 800,550,500
21185+4357 = HD 203064 = 68 Cyg
--------- Reports of small radial velocity variability (Alduseva
et al. 1982; Hanni & Pelt 1988; Zeinalov et al. 1987;
Musaev & Snezhko 1988) probably reflect the presence of
line profile variations (Fullerton 1990). (Msn1998a)
21187+1134 = ADS 14839
1986.395 (also 1986.565) The separation of this difficult partially
resolved pair was calculated under the assumption that delta V
= 1.2 magnitude, but the large number of measurements makes the
result reliable. The strange character of the observed motion
(Tokovinin, 1986 Astron. Circ. No. 1415) is confirmed. (Tok1985)
21192+5837 = ADS 14864
1981.6869 This companion could be the blue component of the VV
Cep system M1Ib ep + B2V (Cowley, 1969 PASP, 81,
297). (Bag1984b)
21214+1021 = ADS 14893
1980.4853 This measure was incorrectly identified with HR 8131 =
alp Equ in McA1983.
21288+7034 = HR 8238
1971.48 Estimated delta m ~ 3 - 4. Attempts by Couteau (1973
private communication) to observe the companion
visually were unsuccessful, supporting this large
magnitude difference. Some anisotropic features in the
Fourier transform may indicate other companions or
circumstellar matter. (Lab1974)
1975.545 (also 1975.956) This is the primary of the system bet Cep
and is believed to be a binary of period ~ 50 yr.
There is also evidence of radial velocity variations.
Labeyrie et al (Lab1974) noted anisotropic features in the
power spectrum which might indicate other companions,
but such features were not observed in the power
spectrum derived from these observations. (BLM1978)
21290+5844 = HDS 3058
--------- The classification is from Garmany & Stencel (1992).
The Hipparcos results (ESA1997) confirm the CHR 211
Aa pair. (Msn1998a)
1994.7001 Very weak detection, possibly an artifact. (Msn1999b)
21329+4959 = HR 8246 = CHR 102
--------- Preliminary orbital elements (P = 9.68 yr) are given
in McA1993.
21353+2812 = HR 8257 = CHR 103
--------- Apparently a spurious binary (7 attempted confirmations,
1985.84 - 1991.90). (McA1993)
21377-0751 = HR 8264 = McA 68
--------- This object was misidentified as HR 8265 in McA1978c.
21384+5658 = HD 206183
--------- The classification is from Garmany & Stencel (1992).
(Msn1998a)
21387+2530 = HR 8274 = CHR 104
--------- Apparently a spurious binary (6 attempted
confirmations, 1985.84 - 1991.90). (McA1993)
21390+5729 = HD 206267 = CHR 212
--------- The classification and orbit are from Burkholder et al.
(1997). Stickland (1995) found that the spectral line
variations result from one close binary (with weak
secondary lines) and a stationary component, a
conclusion later confirmed by Burkholder et al.
(1997). The speckle resolution of the system (CHR
212 Aa) clearly supports the view that this is an SB2
plus a distant O star companion. The C and D
components were also observed and appeared to be
single. The classifications of the C and D components
are from Hoffleit & Warren (1991). (Msn1998a)
21400+0911 = CHR 105
--------- Lacy & Popper (1984 ApJ, 281, 268) discovered a
previously unknown companion to the eclipsing binary EE
Peg through its effects on radial velocity and times of
primary eclipse. Their third component, with a period
of 1464 days and a mass ratio of roughly 5 - 12, would
be expected to exhibit a separation from the primary of
approximately 0".03. It thus seems likely that the
object listed here is yet another long-period member of
this system.
21477+5942 = HD 207538
--------- The classification is from Conti et al. (1977).
(Msn1998a)
22021+5800 = HD 209481 = LZ Cep
--------- The classification is from Conti & Alschuler (1971).
Radial velocity and light curve solutions are given
by Harries et al. (1997b). (Msn1998a)
22037+6437 = McA 69
--------- Analysis of the spectroscopic/interferometric orbit is
given by McAlister (McA1980a).
22115+5925 = HD 210839 = lam Cep
--------- Radial velocities are also discussed by Gies & Bolton
(1986) and Underhill (1995). (Msn1998a)
22116-3428 = CHR 230 Aa
--------- This new component to the visual pair Bu 769 has moved
through more than 4 deg in about 10 months, implying a
period of order 60 -- 70 years. The wide pair has shown
essentially no change since its discovery by Burnham in
1879 (Bu_1887), on the other hand. (Hrt1996b)
22156-4121 = HR 8486 = CHR 187
1992.4554 Abt & Biggs (1972, Bibliography of Stellar Radial
Velocities) note variable RV. (McA1993)
22181-0014 = HR 8507 = CHR 107
--------- Apparently a spurious binary (9 attempted confirmations,
1985.84 - 1991.90). (McA1993)
22241-0451 = ADS 15902
1976.6164 This epoch was incorrectly given as 1976.6146 in McA1982b.
22274+3949 = HR 8553 = CHR 109
--------- Apparently a spurious binary (5 attempted confirmations,
1987.76 - 1991.90). (McA1993)
22300+3234 = HR 8574 = CHR 110
--------- Apparently a spurious binary (6 attempted confirmations,
1985.84 - 1991.90). (McA1993)
22357+5312 = ADS 16098
1985.8481 This autocorrelogram was remeasured; the new results are listed
here.
22361+7252 = ADS 16111
1984.7042 This autocorrelogram was remeasured; the new results are listed
here.
22373+6913 = CHR 113
--------- This confirms the 1983 discovery of this system by
McAlister et al. (McA1987b). (Hrt1992b)
22385-1519 = GJ 866
--------- Adopted magnitude differences are as follows (Lei1990):
0.20 +/- 0.13 mag 845 nm
0.63 +/- 0.08 mag 1250 nm
0.63 +/- 0.06 mag 1650 nm
0.63 +/- 0.06 mag 2250 nm
0.63 +/- 0.10 mag 3800 nm
0.55 +/- 0.36 mag 4800 nm
Paper also derives orbital elements and masses (Lei1990).
22387+4418 = Ho 295
--------- An orbit for this system was published in Hrt1996a.
22408-0333 = HR 8629
--------- The equinox-1900 position was incorrectly given as 22356+0404
in McA1978b.
22469+5805 = HD 215835 = DH Cep
--------- The classification is from the UV tomographic analysis
of Penny et al. (1997). (Msn1998a)
22504+4157 = HR 8690
--------- The CHR 115 pair was apparently a spurious binary
(6 attempted confirmations, 1980.89 - 1991.90). (McA1993)
22526-0735 = HR 8698
1975.802 Probably unresolved (poor seeing). (Bla1977a)
22535-1137 = HR 8704 = McA 73
1977.4874 Theta was incorrectly given as 92.8 degrees in McA1979b.
23019+4219 = HR 8762
--------- The AB component was first reported in McA1982b for 1976.61 after
which earlier French data were reprocessed to yield the 1975
measures.
23026+4245 = ADS 16467
--------- The equinox-1900 position was incorrectly given as 22590+4213
in McA1982b.
23052-0742 = ADS 16497
1977.9134 Rho was incorrectly given as 0".211 in McA1982b.
23079+7523 = HR 8819
--------- This object was misidentified as HR 8815 in McA1978c.
--------- Visual orbital elements for the AB pair have been published
by Baize (1992 A&AS, 92, 31) and Soderhjelm (1999 A&A ,341,
121), while a spectroscopic orbit for the close Aa pair
was published by Scarfe et al. (1983, MNRAS, 203, 103)
23093+4939 = HDS 3296
1996.5352 Very weak detection, possibly an artifact. (Msn1999b)
23111+5304 = HD 218915
--------- Aslanov et al. (1984) discuss the radial velocities and
the possibility of a low mass companion. We found a
possible binary companion at a separation of 0".08
which needs confirmation. (Msn1998a)
23165+6158 = HDS 3314
1991.9043 This observation confirms the Hipparcos solution at a
similar epoch (1991.25). An elongated secondary peak
yielded an inaccurate value for rho, however. (Msn1999b)
23191-1327 = ADS 16672
--------- Analysis of the spectroscopic/interferometric orbit is given by
McAlister & Hartkopf (McA1982c).
--------- Analysis of this observation by the techniques in use in
1985 was unable to yield a useable result. (Hrt1992b)
1977.6350 This epoch was incorrectly given as 1977.6359 in McA1982b.
--------- McAlister & Hartkopf (McA1982c) published the first visual
orbit solution of this system; a combined speckle/spectroscopic
analysis is in progress. (Hrt1996b)
23305+3050 = ADS 16800
--------- Fekel (1986 private communication) reports that he has
now detected four components in the spectrum of this
star.
23340+3120 = ADS 16836
1975.953 Elements published for this long-period system differ:
Costa (1966 Urania, Barcelona 51, 73) quotes P = 198.6
yr, while Tel'nyuk-Adamchuk (TkA1966) gives P = 425 yr.
The observed theta and rho are in reasonable agreement
with either uncertain orbit. (BLM1978)
23393+4543 = CHR 149
1986.8914 This "prediscovery" confirmation was found by
reexamination of archival data. (McA1990)
23412+4613 = Mlr 4
--------- An orbit for this system was published in Hrt1996a.
23460+4625 = McA 75 Aab
1977.9135 This measure was omitted in McA1982b.
23460+4625 = McA 75 Aac
--------- It is not established whether this third component
belongs to Aa or Ab.
1991.9015 With this measurement we have finally confirmed the
discovery observation of this component, made by
McAlister et al. (McA1984a) in 1981!
23529-0313 = Fin 359
--------- This system has a near zero Delta m as determined by
Evans from lunar occultation (OCC1983a). Couteau (Cou1989c)
and Mason (1994, Ph.D. thesis, Georgia State Univ.; 1995,
PASP, 107, 799) have published orbital solutions, and a more
complete analysis is in progress. (Hrt1996b)
23568+0443 = A 2100
--------- This system has a Delta m of 0.9 +/- 0.4 in the blue,
as determined from lunar occultation measures (OCC1975c).
Orbits of this system have been published by Heintz
(Hei1975b) and later by Mason (1994, Ph.D. thesis, Georgia
State Univ.; 1995, PASP, 107, 799); further analysis is in
progress. (Hrt1996b)