WDS binary stars

Binaries in RA: 15:15:02 to 18:27:11, dec: 48:59:59 to 30:01:01.

Min Primary mv: 10.0, Max Delta mv: 5.0, Separation: 0.1" - 1.0".

Explanation

There were 128 pairs found.

J2000 coordinates	WDS Id	Dsc Id	A mv	B mv	Spectrum	first θ	last θ	first ρ	last ρ	First Obs	Last Obs	AKA	Comments	Notes
15:15:03.25 +36:49:48.9	15151+3650	STT 295	8.80	9.45	F5	115	150.90 160.89	0.8	0.290 0.18	1843	2010	-	Last Obs ToD (5) 1	-
15:23:12.22 +30:17:17.7	15232+3017	STF1937AB	5.64	5.95	F8V+G0V	35	212.50 209.05	1.1	0.620 0.63	1826	2015	eta CrB, 2 CrB.	Last Obs ToD (1) 1	Note0
16:30:55.71 +38:03:52.6	16309+3804	STF2059	8.75	8.79	F5	209	181.90 179.91	1.2	0.373 0.31	1829	2009	-	Last Obs ToD (5) 1	-
18:25:18.19 +48:45:42.49	18253+4846	HU 66AB	7.90	8.40	G5	24	215.90 197.58	0.5	0.213 0.13	1883	2011	-	Last Obs ToD (4) 1 2	Note38
18:25:18.19 +48:45:42.49	18253+4846	STT 351AC	7.90	8.25	G5	45	26.10	0.3	0.830	1843	2015	-	-	Note39
18:25:18.19 +48:45:42.49	18253+4846	HU 66BC	8.40	8.25	G5	223	26.60 25.80	0.5	0.820 0.89	1898	2015	-	Last Obs ToD (5) 1 2	Note40
18:46:34.62 +38:21:04	18466+3821	HU 1191	8.67	9.42	G9V	279	258.00 354.25	0.2	0.235 0.21	1905	2008	-	Last Obs ToD (1) 1	Note1

Note 0.
15232+3017, STF1937, KIR 4
eta CrB = 2 CrB.
See Baize & Petit (1989) catalog of doubles with variable component.
Masses and bolometric magnitudes are derived for the two components of
this system by Mason et al. (1999), based on assumed spectral types
Spectral types and masses of components assigned by ten Brummelaar et
al., based on adaptive optics observations.
and available parallaxes.
Pourbaix gives combined solution for this resolved SB2, yielding
orbital parallaxes and component masses.
Combined spectroscopic/astrometric solution of SB2. Calculated masses
1.243 +/- 0.054 and 1.100 +/- 0.039 Msun, distance 18.50 +/- 0.22 pc.
AB: H 1 16.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.11 +/- 0.09, 2.24, and 2.14 Msun, respectively.
AB: SB2, P=41.628y
AE. Data from 2MASS. Kirkpatrick et al. (2001) derive spectral types
G1V+G3V and L8V, determine is a physical pair, separation ~3600 AU.
Find that WDS C and D components of system are not physical.

Note 1.
15277+4253, KU 108
LDS5837.
NLTT 40312/40309
HJL 223.
AB: A is SB1, P=16.55y. B is SB1, P=17.430d

Note 2.
15307+3810, HU 1163
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 7.08 +/- 5.05, 3.33, and 0.95 Msun, respectively.

Note 3.
15329+3122, COU 610
the CrB = 4 CrB. Variable.

Note 4.
15382+3615, HU 1167AB, STF1964
Masses and effective temperatures are determined for these four
components of ADS 9731, based on dynamical parallax (assuming both
pairs are at the same distance) and derived blackbody curves.
AC: HJL 227.
AC: H 4 61.

Note 5.
16080+4523, BU 355
Measures of a wider component by Lewis and Bowyer were incorrectly
attributed to this system and assigned the designation L 38AD. These
measures were actually of 16089+4521STF2015AC.

Note 6.
16128+3922, STF2028
Pair was listed, but in a "rejected" list, not part of discoverer's
regular numbering sequence.

Note 7.
16137+4638, A 1642
Pair suspected of variability. The quadrant reversal assumed in
Dommanget orbit did not take place.

Note 8.
16206+4535, HDS2309
Cvetkovic et al. (2014) derive spectral types F2 and K0, masses 1.56
and 0.90 Msun. Dynamical parallax is 11.58 +/- 0.95 mas.

Note 9.
16240+4822, BUP 168, HEN 1
Distance 1128.4".
Discovery designation is per Todd Henry 03/02/98.
Hipparcos astrometric solution adopted some elements from the orbit of
Marcy & Moore (1989).
GJ 623. Martinache et al. derive dynamical masses of 0.371 +/- 0.015
and 0.115 +/- 0.0023 Msun. Based on IR colors and velocities, they
conclude that the pair is of low metallicity and probably old disk
population. Models do not fit all the dtaa adequately, however.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 0.50 +/- 0.02, 0.58, and 0.40 Msun, respectively.

Note 10.
16248+3925, HU 1276
Magnitude 13.0, assigned to companion in ADS, is much too faint.

Note 11.
16301+3353, HU 1173
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.77 +/- 1.59, 3.32, and 0.95 Msun, respectively.

Note 12.
16326+4007, STT 313
Called G5II comp? by Bidelman.

Note 13.
16341+4226, LAB 4
sig Her = 35 Her. Double-lined spectrum.
1972.28, 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-yr period estimated from Kepler's law.
This object was misidentified as tau Her by McAlister (1978). The
observation on 1976.2963 which was reported there as yielding a
negative result does indeed show duplicity, as was correctly reported
by McAlister later that year. The negative result reported in the
earlier paper for 1976.2991 is spurious.
1977.1781: This is a previously unpublished photographic measure.
1977.3284: Theta incorrectly given as 5.7 deg by McAlister & Hendry
(1982); correct value published by McAlister et al. (1989)
1983.3098: Very poor atmospheric conditions.
Measure of 1988.258 made by MAPPIT.
Martin et al. (1998) derive component masses 3.036 +/- 0.714 and
1.498 +/- 0.519 Msun.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 6.05 +/- 1.14, 6.07, and 2.57 Msun, respectively.

Note 14.
16384+3514, COU 985
A premature orbit has been computed.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 5.46 +/- 4.84, 2.16, and 0.79 Msun, respectively.

Note 15.
16386+3820, STF2080
See ADS for rectangular measures.

Note 16.
16439+4329, D 15
Errors for orbit of Alzner (2007) provided by author (private comm.)
With the Hipparcos parallax of 36.59 +/- 2.13 mas, the Alzner solution
yields a mass sum of 1.31Msun, which matches well a pair of K5 main
sequence stars.
Additional notes may be found in Duruy (1944) and
Worley (1956).
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.27 +/- 0.16, 1.52, and 0.65 Msun, respectively.

Note 17.
16492+4559, BU 627
52 Her. Star A (mag 4.9, A3p) is an Alpha CVn-type variable, V637 Her.
The magnitudes of B and C are quite uncertain.
See Baize & Petit (1989) catalog of doubles with variable component.

Note 18.
16584+3943, COU1289
1986.395: The separation of this partially-resolved pair was
calculated under the assumption of zero or otherwise known magnitude
difference.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.52 +/- 0.99, 2.95, and 1.05 Msun, respectively.

Note 19.
17075+3810, COU1291
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.39 +/- 0.87, 2.43, and 0.95 Msun, respectively.

Note 20.
17080+3556, HU 1176
Van de Kamp & Moore point out that Eggen's orbit yields a mass sum
of 52.5, 'an impossible figure'.
The speckle observations now resolve the former ambiguity.
Hipparcos astrometric solution adopted some elements from the orbit of
Hartkopf et al. (1989).
Calculated mass sum is 3.32 +/- 0.39 Msun. Spectral types are early A
or F, but spectral class has been reported as either dwarf or giant.
This total mass is more consistent with dwarf stars.
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 3.09 +/- 0.14, 3.33, and 1.82 Msun, respectively.

Note 21.
17184+3240, BU 628
A premature orbit has been computed.

Note 22.
17237+3709, MCA 48, STF2161
Aa,Ab: rho Her. Suspected of variable velocity, and resolved by
speckle interferometry.
AB: H 2 3.

Note 23.
17240+3835, HU 1179
1985.741: The residuals of these measurements (as well as those of
McAlister) are irregular and do not permit the correction of an orbit.
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 3.81 +/- 1.50, 3.55, and 1.70 Msun, respectively.

Note 24.
17247+3802, HSL 1
Aa,Ab. Masses of 0.887+/-0.030 and 0.788+/-0.021 are determined.
Aa,Ab: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 2.37 +/- 0.30, 2.12, and 0.95 Msun, respectively.
Aa,Ab: For the Horch et al. (2015) combined solution, spectroscopic
elements are fixed to those of Goldberg et al. (2002 AJ 124, 1132).
Assigned spectral types for Aa, Ab, and Ac are G5V, G8V, and K6V;
derived masses for Aa and Ab are 0.92 and 0.84 Msun.

Note 25.
17326+3445, HU 1181
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.79 +/- 0.33, 2.12, and 1.05 Msun, respectively.

Note 26.
17407+3117, STTA157
B is BD+31@3077.

Note 27.
17412+4139, STF2203
BDS 8128, STTA158.

Note 28.
17471+4737, CHR 64
A spectroscopic binary, P = 2.8d. Hence triple.

Note 29.
17490+3704, COU1145
1981.333: This observation was incorrectly attributed to COU 1445 in
Tokovinin (1982).
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 1.84 +/- 0.14, 2.27, and 1.05 Msun, respectively.

Note 30.
17523+4057, A 699
Also unresolved 1960.

Note 31.
18025+4414, BU 1127
A premature orbit has been computed.
L 18 is probably the same star
See Baize & Petit (1989) catalog of doubles with variable component.
L 18.

Note 32.
18040+3923, L 19
Not found by van den Bos in 1958. Not the same as STF2275, although
some measures were misidentified.

Note 33.
18043+4206, COU1786
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.80 +/- 1.44, 3.07, and 1.45 Msun, respectively.

Note 34.
18063+3824, HU 1186
Malkov et al. (2012) derive dynamical, photometric, and spectroscopic
masses of 2.00 +/- 0.69, 2.28, and 1.10 Msun, respectively.

Note 35.
18118+3327, B 2545
Called a spectroscopic binary. Variation undoubtedly due to motion in
the visual orbit.
1979.360: Theta incorrectly given as 42.4 deg in McAlister & Hendry.
1980.4768: Rho incorrectly given as 0".091 in McAlister et al (1983)
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 6.14 +/- 2.37, 7.96, and 2.00 Msun, respectively.

Note 36.
18118+3327, B 2545
Called a spectroscopic binary. Variation undoubtedly due to motion in
the visual orbit.
1979.360: Theta incorrectly given as 42.4 deg in McAlister & Hendry.
1980.4768: Rho incorrectly given as 0".091 in McAlister et al (1983)
AB: Malkov et al. (2012) derive dynamical, photometric, and
spectroscopic masses 6.14 +/- 2.37, 7.96, and 2.00 Msun, respectively.

Note 37.
18126+3836, BU 1091
Prieur et al. (2012) derive a dynamical parallax of 6.0 mas and
(using their orbital elements and the revised Hipparcos parallax of
van Leeuwen 2007 A&A 474, 653) a total mass 2.2 +/- 0.9 Msun.

Note 38.
18253+4846, HU 66, STT 351
Van Biesbroeck (1954) was unable to resolve this system in 1943,
1944 or 1945 on the 82-inch telescope at the McDonald Observatory.
However, since he resolved the system successfully in 1946 with the
same telescope, and in 1940 with a smaller (40-inch) telescope, the
non-resolution is probably due to bad seeing or ID error.
AC: Additional notes may be found in Muller (1955).

Note 39.
18253+4846, HU 66, STT 351
Van Biesbroeck (1954) was unable to resolve this system in 1943,
1944 or 1945 on the 82-inch telescope at the McDonald Observatory.
However, since he resolved the system successfully in 1946 with the
same telescope, and in 1940 with a smaller (40-inch) telescope, the
non-resolution is probably due to bad seeing or ID error.
AC: Additional notes may be found in Muller (1955).

Note 40.
18253+4846, HU 66, STT 351
Van Biesbroeck (1954) was unable to resolve this system in 1943,
1944 or 1945 on the 82-inch telescope at the McDonald Observatory.
However, since he resolved the system successfully in 1946 with the
same telescope, and in 1940 with a smaller (40-inch) telescope, the
non-resolution is probably due to bad seeing or ID error.
AC: Additional notes may be found in Muller (1955).