00057+4549AB    The Sixth Catalog of Orbits of Visual Binary Stars lists two 
00057+4549AB     orbits for the AB pair of that system (separated by about 6"): 
00057+4549AB     one with a period of 1550yr (Popovic and Pavlovic, 
00057+4549AB     1996BOBeo.153...57P) and another with a period of 509yr 
00057+4549AB     (Kiyaeva et al., 2001AstL...27..391K), indicating that the 
00057+4549AB     solution is not yet well constrained. Radial velocities 
00057+4549AB     obtained by CORAVEL and by Tokovinin & Smekhov 
00057+4549AB     (2002A&A...382..118T), as listed in Table A.4 and displayed in 
00057+4549AB     Fig. A.1, correspond to a radial velocity difference VB-VA 
00057+4549AB     slightly decreasing from -2.7km/s in 1980 to -3.8km/s in 1996. 
00057+4549AB     The value -3.0km/s has been used by Kiyaeva et al. 
00057+4549AB     (2001AstL...27..391K) to determine unambiguously the ascending 
00057+4549AB     node. This result is confirmed thanks to the precise 
00057+4549AB     radial-velocity measurements of Marcy (2013, priv. comm.) that 
00057+4549AB     show a linear variation for VB-VA amounting to -6.4m/s/yr from 
00057+4549AB     2000 to 2010, while a value of -11.5m/s/yr is calculated from 
00057+4549AB     the visual orbit. Thus we have computed the position of the 
00057+4549AB     orbital pole but it is not expected to be precise. Kiyaeva et 
00057+4549AB     al. (2001AstL...27..391K) also suggested that ADS 48 ABF is a 
00057+4549AB     hierarchical triple system whose orbits (AB) and (AB-F) are not
00057+4549AB     coplanar. This hypothesis was contradicted by Cvetkovic et al. 
00057+4549AB     (2012AJ....144...80C), who concluded that the F component has a
00057+4549AB     common proper motion with 
00057+4549AB    the AB pair, but that it is not bound by gravity.

00184+4401AB    Indeterminate visual orbit.

00321+6715Aa,Ab and AB. The preliminary visual orbits of this triple 
00321+6715Aa,Ab  hierarchical system were computed by Docobo et al. 
00321+6715Aa,Ab  (2008A&A...478..187D). No radial velocity measurements are 
00321+6715Aa,Ab  available to resolve the ambiguity of the ascending node.

00321+6715AB    and Aa,Ab. The preliminary visual orbits of this triple 
00321+6715AB     hierarchical system were computed by Docobo et al. 
00321+6715AB     (2008A&A...478..187D). No radial velocity measurements are 
00321+6715AB     available to resolve the ambiguity of the ascending node.

01083+5455Aa,Ab Drummond et al. (1995ApJ...450..380D) obtained the first 
01083+5455Aa,Ab  relative astrometric orbit for that system from their direct 
01083+5455Aa,Ab  detection of the faint B component. Combining that orbit with 
01083+5455Aa,Ab  earlier photocentric positions (Lippincott 1981ApJ...248.1053L;
01083+5455Aa,Ab  Russell & Gatewood, 1984PASP...96..429R), masses could be 
01083+5455Aa,Ab  derived: MA=0.74+/-0.06M_{sun}_ and MB=0.17+/-0.01M_{sun}_.
01083+5455Aa,Ab  Duquennoy & Mayor (1991A&A...248..485D) derived a preliminary 
01083+5455Aa,Ab  spectroscopic orbit, and Abt & Willmarth (2006ApJS..162..207A) 
01083+5455Aa,Ab  obtained thereafter more radial velocities; however, Abt & 
01083+5455Aa,Ab  Willmarth (2006ApJS..162..207A) did not attempt to compute a 
01083+5455Aa,Ab  combined orbit, and merged the orbital elements of Duquennoy & 
01083+5455Aa,Ab  Mayor (1991A&A...248..485D) and Drummond et al. 
01083+5455Aa,Ab  (1995ApJ...450..380D). Because this is not fully satisfactory 
01083+5455Aa,Ab  and is prone to confusion (as further discussed below), 
01083+5455Aa,Ab  especially regarding the ambiguity on {omega}, we decided to 
01083+5455Aa,Ab  compute a new combined orbit (Fig. A.2), using data of 
01083+5455Aa,Ab  Duquennoy & Mayor (1991A&A...248..485D) as well as more recent 
01083+5455Aa,Ab  unpublished CORAVEL data (Table A.5), plus velocities reported 
01083+5455Aa,Ab  by Abt & Willmarth (2006ApJS..162..207A). The astrometric 
01083+5455Aa,Ab  positions of B relative to A taken from the WDS database at 
01083+5455Aa,Ab  USNO were used as well. As shown in Table A.2, the value of 
01083+5455Aa,Ab  {omega} for the astrometric orbit of B around A is 
01083+5455Aa,Ab  329.4{deg}+/-3.8{deg} (thus a change of 180{deg} from the 
01083+5455Aa,Ab  relative orbit of Drummond et al., 1995ApJ...450..380D; their 
01083+5455Aa,Ab  Table 9), and we stress that the value (332.7{deg}+/-3.1{deg}) 
01083+5455Aa,Ab  listed by Abt & Willmarth (2006ApJS..162..207A) for the 
01083+5455Aa,Ab  spectroscopic orbit (of A around the centre of mass of the 
01083+5455Aa,Ab  system) is incorrect, as it should differ by 180{deg} from the 
01083+5455Aa,Ab  astrometric value, confirming the suspected confusion. It is in
01083+5455Aa,Ab  fact just the value reported by Drummond et al. 
01083+5455Aa,Ab  (1995ApJ...450..380D), which should not have been copied 
01083+5455Aa,Ab  without change! Instead, the value (147.9{deg}+/-4.9{deg}) of 
01083+5455Aa,Ab  Duquennoy & Mayor (1991A&A...248..485D) for the spectroscopic 
01083+5455Aa,Ab  orbit is correct. 

01398-5612AB    Indeterminate visual orbit. In the absence of recent 
01398-5612AB     radial-velocity measurements it is not possible to lift the 
01398-5612AB     ambiguity on the position of the ascending node.

01418+4237AB    Spectroscopic orbits were published by Duquennoy & Mayor 
01418+4237AB     (1991A&A...248..485D) and Abt & Willmarth 
01418+4237AB     (2006ApJS..162..207A). The present orbit (Table A.2) improves 
01418+4237AB     upon those, as it includes several unpublished CORAVEL 
01418+4237AB     velocities given in Table A.6. Lippincott et al. 
01418+4237AB     (1983PASP...95..271L) and Soderhjelm (1999A&A...341..121S) 
01418+4237AB     published astrometric orbits. Here, we obtained a combined 
01418+4237AB     astrometric/spectroscopic solution by considering the 
01418+4237AB     astrometric measurements from the Fourth Catalogue of 
01418+4237AB     Interferometric Measurements of Binary Stars. This solution 
01418+4237AB     agree well with the existing solutions quoted above.

01425+2016AB    This system was announced as an astrometric binary with a period
01425+2016AB     of 0.567yr by the Double and Multiple Star Annex (DMSA) of the 
01425+2016AB     Hipparcos Catalogue (ESA, 1997, Cat. I/239), Cat. I/239). 
01425+2016AB     However, reprocessing the Hipparcos data along the method 
01425+2016AB     outlined by Pourbaix (2000A&AS..145..215P) for a combined 
01425+2016AB     solution including the CORAVEL velocities does not allow us to 
01425+2016AB     confirm the Hipparcos DMSA/O solution. This system was 
01425+2016AB     therefore dropped from our final list.

02278+0426AB    The most recent and thorough analysis of that system was 
02278+0426AB     presented by Andrade (2007RMxAA..43..237A), including a revised
02278+0426AB     visual orbit. CORAVEL data (Table A.7) make it possible now to 
02278+0426AB     compute a combined SB2/astrometric orbit, which thus gives 
02278+0426AB     access for the first time to the masses of the system 
02278+0426AB     components. The combined orbital elements and other physical 
02278+0426AB     parameters of the system (such as orbital parallax and 
02278+0426AB     component masses) are listed in Table A.3, which identifies the
02278+0426AB     components as 1 and 2 rather than A and B. It must be stressed 
02278+0426AB     that there is no easy way to identify for sure the 
02278+0426AB     spectroscopic component 1 with either visual component A or B, 
02278+0426AB     since both components fall in the spectrograph slit and are of 
02278+0426AB     almost equal brightness: Hipparcos gives mHp,A=9.45 and 
02278+0426AB     mHp,B=9.63. An indirect way to identify components A and B is 
02278+0426AB     by noting that in Table A.3, the velocity semi-amplitude K2 is 
02278+0426AB     higher than K1, hence M2 is smaller than M1. Since both 
02278+0426AB     components lie on the main sequence, component 2 should thus be
02278+0426AB     less luminous than component 1, hence component 2 should be 
02278+0426AB     identified with B. It is possible to check quantitatively this 
02278+0426AB     assumption by using the mass-luminosity relationship provided 
02278+0426AB     by Kroupa et al. (1993MNRAS.262..545K), namely MV,1=5.4 for 
02278+0426AB     M1=0.95M_{sun}_ and MV,2=6.2 for M2=0.85M_{sun}_, or 
02278+0426AB     MV,2-MV,1=0.8, somewhat larger than the observed 
02278+0426AB     mHp,B-mHp,A=0.18, but certainly consistent with the error bars 
02278+0426AB     on M1,2. Although Andrade (2007RMxAA..43..237A) classified 
02278+0426AB     HD 15285 A as K7V based on several spectral features, among 
02278+0426AB     which the presence of weak TiO bands, its inferred mass of 
02278+0426AB     0.95M_{sun}_ is more typical of a G5V type, while the mass of 
02278+0426AB     component B would flag it as K0V (Cox, 2000, Allen's 
02278+0426AB     Astrophysical Quantities (New York: Springer)).
02278+0426AB     These masses were derived from the orbital parallax of 
02278+0426AB     52+/-2mas, to be compared with the Hipparcos value of 
02278+0426AB     60.2+/-1.7mas (ESA, 1997, Cat. I/239) or 58.3+/-1.1mas 
02278+0426AB     (van Leeuwen, 2007, Cat. I/311), which yield total masses of 
02278+0426AB     1.16 and 1.28M_{sun}_, respectively, to be compared with 
02278+0426AB     1.8M_{sun}_ for the orbital parallax. From the fractional mass 
02278+0426AB     M2/(M1+M2)=0.47 (Table A.3), one obtains, (M1,M2)=(0.62,0.54) 
02278+0426AB     and (0.68, 0.60)M_{sun}_. These values agree much better with a
02278+0426AB     K7V spectral type for component A. 

02361+0653A     The 22 CORAVEL measurements available for component A (spanning 
02361+0653A      6837d) yield a standard deviation of 0.29km/s, identical to the
02361+0653A      average error on a single measurement. The constancy of the 
02361+0653A      radial velocity was confirmed by Chubak et al. (2012, 
02361+0653A      arXiv:1207.6212), who obtained 62 measurements spanning 1299d,
02361+0653A      with a standard deviation of 0.142km/s. Hence, radial 
02361+0653A      velocities cannot be used to lift the ambiguity on the 
02361+0653A      orbital orientation.

02442+4914AB    Indeterminate visual orbit and roughly constant radial velocity 
02442+4914AB     between 1900 and 1990.

03575-0110AB    Indeterminate visual orbit and almost constant radial velocity 
03575-0110AB     between 1984 and 1993.

04153-0739BC    In the triple system STF 518 A-BC, B is the white dwarf omi Eri 
04153-0739BC     B and C the flare star DY Eri.

04312+5858Aa,Ab Triple system, with the A component being an astrometric binary 
04312+5858Aa,Ab  in the visual binary STI 2051 AB.

05074+1839AB    Visual orbit highly conjectural and radial velocity from 
05074+1839AB     Duquennoy & Mayor (1991A&A...248..485D) is constant.

06003-3102AC    A quadruple system (Tokovinin et al., 2005A&A...441...69L): 
06003-3102AC     HU 1399 AB (P=67.7yr, a=0.912"), HJ 3823 AC (P=390.6yr, 
06003-3102AC     a=3.95" by Baize (1980, Inf. Circ. IAU Comm., 26, 80), not 
06003-3102AC     confirmed by Tokovinin et al., 2005A&A...441...69L), 
06003-3102AC     TOK 9 C,CE (P=23.7yr, a=0.12"). A, B and C, CE are coplanar 
06003-3102AC     (Tokovinin et al., 2005A&A...441...69L).

06262+1845AB    Triple system, with A known as SB2 with P=6.99d 
06262+1845AB     (Griffin & Emerson, 1975Obs....95...23G).

06293-0248AB    Solution for the SB2 orbit includes masses and orbital parallax 
06293-0248AB     (Segransan et al., 2000A&A...364..665S). Although not clearly 
06293-0248AB     stated, the orbital elements listed by Segransan et al. 
06293-0248AB     (2000A&A...364..665S) correspond to the spectroscopic orbit 
06293-0248AB     (hence {omega} and {Omega} listed in our Table 3 differ by 
06293-0248AB     180{deg} from theirs).

06579-4417AB    Indeterminate visual orbit.

07100+3832      The spectro-visual orbit of this system was only recently 
07100+3832       computed by Barry et al. (2012ApJ...760...55B).

07175-4659AB    The visual orbit is still very uncertain. The total mass of the 
07175-4659AB     system is abnormally low given the spectral type.

07346+3153AB    A difficult system since both A and B are spectroscopic binaries
07346+3153AB     (Vinter Hansen et al., 1940LicOB..19...89V), with P=9.21d and 
07346+3153AB     P=2.93 d, respectively. Batten (1967, IAU Symp., 30, 199) has 
07346+3153AB     lifted the ambiguity on the ascending node for that system, and
07346+3153AB     we used the orbital elements of the 6th Catalogue of Visual 
07346+3153AB     Binary Orbits to compute the position of the pole, agreeing 
07346+3153AB     with that of Batten (1967, IAU Symp., 30, 199), allowing for 
07346+3153AB     the fact that our poles follow the right-hand rule, opposite to
07346+3153AB     that of Batten.

07393+0514AB    The pole ambiguity was lifted from the radial-velocity drift 
07393+0514AB     present in the Duquennoy et al. (1991A&AS...88..281D) data. 

08592+4803A,BC  Indeterminate visual orbit. It might be a quadruple system, 
08592+4803A,BC   since Aa seems to be a SB1 system with a period P~11yr 
08592+4803A,BC   (Abt, 1965ApJS...11..429A) although the spectroscopic orbit is 
08592+4803A,BC   not of an excellent quality.

09006+4147AB    The period of 21.05yr for that visual binary is well established
09006+4147AB     (Muterspaugh et al., 2010AJ....140.1623M). Based on an older 
09006+4147AB     (albeit similar) value of the visual period from Heintz (1967, 
09006+4147AB     VeMun, 7, 31), Abt & Levy (1976ApJS...30..273A) proposed a 
09006+4147AB     spectroscopic orbit based on Heintz' visual elements plus 
09006+4147AB     approximate values for the systemic velocity and the 
09006+4147AB     semi-amplitude, which could account for Abt & Levy's own 
09006+4147AB     velocity measurements and older ones from Underhill 
09006+4147AB     (1963PDAO...12..159U). Although it is rather uncertain, this 
09006+4147AB     orbit is still the one quoted by the SB9 catalogue (Pourbaix et
09006+4147AB     al., 2004A&A...424..727P). The spectroscopic orbit is 
09006+4147AB     difficult to derive because (i) the components are not 
09006+4147AB     separated widely enough on the sky to record their spectra 
09006+4147AB     separately; (ii) the velocity semi-amplitude is small; and 
09006+4147AB     (iii) component A appears to rotate relatively fast. Therefore,
09006+4147AB     the available unpublished CORAVEL measurements appear useless, 
09006+4147AB     since the two components appear hopelessly blended in the 
09006+4147AB     cross-correlation function. More recent HERMES/Mercator spectra
09006+4147AB     (Raskin et al., 2011A&A...526A..69R) have a resolution high 
09006+4147AB     enough to allow a comfortable double-Gaussian fit of the 
09006+4147AB     cross-correlation function (CCF; Fig. A.5). Although such a 
09006+4147AB     fit has not necessarily a unique solution, we found it 
09006+4147AB     re-assuring that the CCFs for all seven available dates 
09006+4147AB     (Table A.1) are well fitted with Gaussians having the same 
09006+4147AB     properties: height ~0.08 and {sigma}=14km/s for the F4V 
09006+4147AB     component A (V=4.2), and height ~0.04 and {sigma}=4km/s for the
09006+4147AB     K0V component B (V=6.5). It thus appears that component A is a 
09006+4147AB     relatively fast rotator. The assignment of either of the two 
09006+4147AB     CCF peaks to component A thus relies on the assumption that 
09006+4147AB     component A, being of spectral type F4V, should correspond to 
09006+4147AB     the deepest peak when computed with a F0V template. 
09006+4147AB     The validity of our double-Gaussian fits, and of the resulting 
09006+4147AB     orbital elements listed in Table A.3, may be assessed a 
09006+4147AB     posteriori by the comparison of the orbital parallax 
09006+4147AB     (53.8+/-1.0mas) with the Hipparcos parallax (60.9+/-1.3mas; 
09006+4147AB     ESA, 1997, Cat. I/239). The discrepancy probably comes from 
09006+4147AB     the fact that the limited phase coverage for the radial 
09006+4147AB     velocities does not yet impose strong enough constraints on the
09006+4147AB     velocity semi-amplitudes (Fig. A.4). The astrometrically 
09006+4147AB     derived masses (MA=1.37M_{sun}_, MB=1.04M_{sun}_, in relatively
09006+4147AB     good agreement with the spectral types; Martin & Mignard, 
09006+4147AB     1998A&A...330..585M; Soderhjelm, 1999A&A...341..121S) are 
09006+4147AB     different from the types derived from our combined orbit 
09006+4147AB     (MA=1.73M_{sun}_, MB=1.69M_{sun}_), which also hints at 
09006+4147AB     inaccurate velocity semi-amplitudes.

09144+5241AB    For this long-period binary, the determination of the orbital 
09144+5241AB     pole is based on the agreement between the variation of the 
09144+5241AB     radial velocities VA and VB measured between 1910 and 1997 and 
09144+5241AB     the value predicted using the elements of the visual orbit. 
09144+5241AB     This result is confirmed by the value of the measurement of 
09144+5241AB     (VB-VA) performed with the HERMES spectrograph in 2012 
09144+5241AB     (see Table A.1).

09313-1329AB    Mass-ratio derived from the astrometry (Soderhjelm, 
09313-1329AB     1999A&A...341..121S). Two HERMES radial-velocity measurements 
09313-1329AB     obtained one year apart neither showed any significant drift 
09313-1329AB     (Vr=7.93km/s on JD=2455657.5 and Vr=7.89km/s on JD=2456038.4), 
09313-1329AB     nor any line doubling, as would be expected for a system 
09313-1329AB     consisting of two components only 0.6 arcsec apart.

09357+3549AB    Indeterminate visual orbit.

10454+3831AB    Triple system, Aa being the speckle binary CHR 191. A value of 
10454+3831AB     (VB-VA) obtained with the HERMES spectrograph in 2012 is 
10454+3831AB     listed in Table A.1.

11182+3132AB    Quadruple system, A and B are both SB1 with P=670.24d and 
11182+3132AB     P=3.98d respectively (Griffin, 1998Obs...118..273G).

11247-6139AB    Abnormally high total mass, inconsistent with the spectral types

13100+1732AB    Spectral types and masses of components from ten Brummelaar et 
13100+1732AB     al. (2000AJ....119.2403T).

13198+4747AB    Triple system (Aa=CHR 193; Beuzit et al., 2004A&A...425..997B). 
13198+4747AB     CORAVEL sees this star as SB3, but no satisfactory attribution 
13198+4747AB     of the various peaks to the corresponding components could be 
13198+4747AB     made, making it very difficult to isolate the trend of Vr(A).

13473+1727AB    Indeterminate orbit. The component {tau} BooAb is a star with 
13473+1727AB     planet.

13491+2659AB    The pole ambiguity was lifted from unpublished CORAVEL 
13491+2659AB     velocities yielding the sign of Vr(B)-Vr(A) (=-3.3km/s) during
13491+2659AB     the observation span 1983-1988 (Table A.1).

13547+1824      Jancart et al. (2005A&A...442..365J) obtained a combined 
13547+1824       spectroscopic/astrometric orbit based on Hipparcos data and the
13547+1824       spectroscopic orbit of Bertiau (1957ApJ...125..696B). The value
13547+1824       of {omega} from Jancart et al. (2005A&A...442..365J) has been 
13547+1824       adopted in Table 3.

14514+1906AB    The visual orbital period is 151 yr (Soderhjelm, 
14514+1906AB     1999A&A...341..121S), so that no strong trend must be expected
14514+1906AB     from the radial velocities over three decades. CORAVEL 
14514+1906AB     observations (Duquennoy et al., 1991A&A...248..485D) 
14514+1906AB     exhibit a weak upward trend between 1977 (1km/s) and 1991 
14514+1906AB     (1.4km/s), which is however not significant based on the 
14514+1906AB     average measurement uncertainty of 0.34km/s. Later measurements
14514+1906AB     by Abt & Willmarth (2006ApJS..162..207A) seem to confirm that 
14514+1906AB     trend, but the trend is made fragile by a possible zero-point 
14514+1906AB     offset between the two data sets. Nevertheless, the pole quoted
14514+1906AB     in Table 3 is based on the assumption that the radial-velocity 
14514+1906AB     trend is real, which then implies that the node given in the 
14514+1906AB     6th USNO Catalogue is the correct one.

14575-2125AB    Indeterminate visual orbit.

15038+4739AB    Triple star: Bb=eclipsing SB2 with P=0.27d 
15038+4739AB     (Lu et al., 2001AJ....122..402L). 

15527+4227      The Hipparcos Double and Multiple Star Annex (DMSA; ESA, 1997, 
15527+4227       Cat. I/239) claims HIP 77760 to be an astrometric binary with 
15527+4227       an orbital period of 0.14yr and an inclination of 131.68{deg}.
15527+4227       These values seem, however, incompatible with the absence of 
15527+4227       (CORAVEL) radial-velocity variations (33 measurements with a 
15527+4227       standard deviation of 0.413km/s, to be compared with the 
15527+4227       average instrumental error of 0.380km/s). 

16413+3136AB    There are many visual orbits available for that system, the most
16413+3136AB     recent ones by Baize (1976A&AS...26..177B) and Soderhjelm 
16413+3136AB     (1999A&A...341..121S). Scarfe et al. (1983JRASC..77..126S) 
16413+3136AB     already computed an orbit combining visual data and a 
16413+3136AB     collection of Coude radial velocities. Unpublished CORAVEL 
16413+3136AB     velocities given in Table A.8 nicely complement Scarfe's 
16413+3136AB     velocities, yielding a somewhat more accurate orbit as listed 
16413+3136AB     in Table A.2. A third component has been detected by IR speckle
16413+3136AB     interferometry (McCarthy, 1983, IAUCo, 76, 107). 

16555-0820AB    A triple system composed of M dwarfs, in which all three stars 
16555-0820AB     are visible in the spectra. Spectroscopic orbits are available 
16555-0820AB     for the inner (Ba-b) and outer pairs (A-Bab), both as SB2 
16555-0820AB     (Segransan et al., 2000A&A...364..665S). The two orbits are 
16555-0820AB     probably coplanar (Mazeh et al., 2001MNRAS.325..343M). The 
16555-0820AB     whole system is probably septuple.

17121+4540AB    A visual orbit for that system was obtained by Hartkopf et al. 
17121+4540AB     (1996AJ....111..370H). The available CORAVEL velocities shown 
17121+4540AB     in Table A.9 make it possible to derive a combined orbit for 
17121+4540AB     the first time. Visual observations are from the CHARA 
17121+4540AB     database. The new combined orbit is presented in Fig. A.7. 

17153-2636AB    Irwin et al. (1996PASP..108..580I) derived precise B-A radial 
17153-2636AB     velocities (except for an acceleration component that they were
17153-2636AB     unable to explain). Velocity measurements of Vr(A) and Vr(B) 
17153-2636AB     were obtained in 2012 by the HERMES spectrograph (Table A.1).

17191-4638AB    Indeterminate visual orbit.

17304-0104AB    A combined astrometric/spectroscopic solution has been computed 
17304-0104AB     by Pourbaix (2000A&AS..145..215P) and has been used to compute 
17304-0104AB     the position of the orbital pole.

17349+1234      Spectral types from Gatewood (2005AJ....130..809G). Kamper et 
17349+1234       al. (1989AJ.....98..686K) performed a combined 
17349+1234       spectroscopic/astrometric analysis of this system, and their 
17349+1234       orbit has been recently updated by Hinkley et al. 
17349+1234       (2011ApJ...726..104H), from whom we adopted the orbital 
17349+1234       elements without requiring any change to comply with our 
17349+1234       conventions.

17364+6820Aa,Ab Velocity measurements of Vr(A) and Vr(B) obtained in 2012 by the
17364+6820Aa,Ab  HERMES spectrograph are listed in Table A.1.

17465+2743BC    HD 161797 ({mu} Her) is a quadruple system (Raghavan et al., 
17465+2743BC     2010ApJS..190....1R). The components of the wide pair 
17465+2743BC     STF 2220 AB (35") have common proper motion. The component A is
17465+2743BC     an astrometric binary (period of 65 years, Heintz, 
17465+2743BC     1994AJ....108.2338H). The components B and C form the visual 
17465+2743BC     binary AC 7 for which the orbital pole ambiguity has been 
17465+2743BC     lifted from unpublished CORAVEL velocities, yielding a drift of
17465+2743BC     Vr(B) over 1975-1995.

18070+3034AB    Based on available CORAVEL velocities (unpublished measurements 
18070+3034AB     are given in Table A.10), a combined astrometric/spectroscopic 
18070+3034AB     solution (Table A.2 and Fig. A.8) improves the spectroscopic 
18070+3034AB     orbital elements provided by Abt & Willmarth 
18070+3034AB     (2006ApJS..162..207A) for that system. AC 15 AB is a triple 
18070+3034AB     system, with the separation Aa-Ab amounting to 0.228" and that 
18070+3034AB     of AB to 0.851" in 2005, according to Scardia et al. 
18070+3034AB     (2008AN....329...54S).

18428+5938AB    Velocity measurements (4 for Vr(A) and one for Vr(B)) obtained 
18428+5938AB     by the HERMES spectrograph in 2012 are listed in Table A.1.

18570+3254AB    A combined astrometric/spectroscopic solution confirms the 
18570+3254AB     spectroscopic orbital elements provided by Abt & Willmarth 
18570+3254AB     (2006ApJS..162..207A) for that system. BU 648 AB is a binary 
18570+3254AB     with an exoplanet (Muterspaugh et al., 2010AJ....140.1657M) 
18570+3254AB     in coplanar orbits.

19121+0254AB    Masses are from Benedict et al. (2001AJ....121.1607B). 

19255+0307Aa,Ab Kamper et al. (1989AJ.....98..686K) performed a combined 
19255+0307Aa,Ab  spectroscopic/astrometric analysis of the Aa-Ab pair. We 
19255+0307Aa,Ab  adopted the orbital elements from their Table V, except that 
19255+0307Aa,Ab  180{deg} was added to their value of {omega}, to conform with 
19255+0307Aa,Ab  our convention that {omega} corresponds to the visual orbit of 
19255+0307Aa,Ab  Ab around Aa, rather than to the spectroscopic orbit of Aa 
19255+0307Aa,Ab  around the centre of mass. One HERMES measurement was obtained 
19255+0307Aa,Ab  (Table A.1) that reveals for the first time the companion in 
19255+0307Aa,Ab  the cross-correlation function as a narrow peak on top of the 
19255+0307Aa,Ab  broad peak (Vrsini=84km/s) due to the FV primary (Fig. A.9). 
19255+0307Aa,Ab  The companion does not rotate fast. From the orbit described 
19255+0307Aa,Ab  in Kamper et al. (1989AJ.....98..686K), we estimate that the 
19255+0307Aa,Ab  HERMES data point (Vr(Aa)=-26.68km/s) has been taken at orbital
19255+0307Aa,Ab  phase 0.54+/-0.14, when the velocity is km/s higher than the 
19255+0307Aa,Ab  centre of mass (CoM) velocity. The CoM velocity is thus 
19255+0307Aa,Ab  estimated to be km/s. Combined with Vr(Ab)=-37.70km/s, this 
19255+0307Aa,Ab  yields a surprisingly high mass ratio MAa/MAb of 5.6, or a mass
19255+0307Aa,Ab  of 0.29M_{sun}_ for the companion if the primary is a F0V star 
19255+0307Aa,Ab  of mass 1.6M_{sun}_. The corresponding spectral type would 
19255+0307Aa,Ab  then be M4V for the Ab component, 8.6mag fainter than the 
19255+0307Aa,Ab  primary component. The close pair WDS 19255+0307Aa,Ab, seems to
19255+0307Aa,Ab  form a triple system with the wide pair (WDS 19255+0307AB=
19255+0307Aa,Ab  BUP 190, separation 96 to 133"), but the physical nature of 
19255+0307Aa,Ab  this system is yet to be confirmed.

21000+4004AB    Fekel et al. (1978AJ.....83.1445F) found that the visual 
21000+4004AB     component A of KUI 103 is itself a spectroscopic binary with a 
21000+4004AB     period of 3.27 d, but no information is available about 
21000+4004AB     coplanarity (Tokovinin, 2008MNRAS.389..925T). Pourbaix 
21000+4004AB     (2000A&AS..145..215P) has made a combined analysis of the 
21000+4004AB     visual and spectroscopic data. However, the authors note that 
21000+4004AB     this orbital solution is somewhat uncertain, given the large 
21000+4004AB     error bars and inconsistencies in the derived values for 
21000+4004AB     stellar masses and orbital parallax. Thus, we decided to base 
21000+4004AB     our determination of the orbital pole of this system on the 
21000+4004AB     analysis of the published radial velocity measurements 
21000+4004AB     (Pourbaix, 2000A&AS..145..215P) and the orbital elements of the
21000+4004AB     new visual orbit proposed by Docobo & Ling (2010, IAU 
21000+4004AB     Commission on Double Stars, 171, 1).

21069+3845AB    The mass ratio is taken from Gorshanov et al. 
21069+3845AB     (2006Ap.....49..386G). The node assignment is based on the 
21069+3845AB     difference Vr(B)-Vr(A)~+1km/s>0, as provided by Table 1 of 
21069+3845AB     Gorshanov et al. (2006Ap.....49..386G) and confirmed by 
21069+3845AB     unpublished CORAVEL measurements.

22234+3228AB    The total mass seems too high for the spectral type.

22280+5742AB    Masses are from Delfosse et al. (2000A&A...364..217D). Among the
22280+5742AB     many radial velocities available in the literature for the 
22280+5742AB     components of this system, we give the highest weight to the 
22280+5742AB     measurement [Vr(A)=-32.7km/s and Vr(B)=-33.2km/s] by Gizis et 
22280+5742AB     al. (2002AJ....123.3356G) because (i) that measurement is 
22280+5742AB     precisely dated (JD 2450005.6) and on the same night for A 
22280+5742AB     and B; and (ii) the 0.5km/s velocity difference is consistent 
22280+5742AB     with the prediction from the visual orbit. The measurement 
22280+5742AB     (Vr(A)=-34.0km/s and Vr(B)=-35.0km/s) by Delfosse et al. 
22280+5742AB     (1998A&A...331..581D) is equally useful (its epoch is not as 
22280+5742AB     precisely known as that report by Gizis, but it was obtained 
22280+5742AB     between September 1995 and March 1997, a short time span with 
22280+5742AB     respect to the 44.7yr orbital period); the 1km/s velocity 
22280+5742AB     difference agrees better with the prediction from the visual 
22280+5742AB     orbit than Gizis' 0.5km/s. The determination of the sign of 
22280+5742AB     Vr(B)-Vr(A)=-1km/s is important and it is opposite to the 
22280+5742AB     prediction from the visual orbital elements from the 6th COVBS.
22280+5742AB     It is thus necessary to add 180{deg} to the values of {Omega} 
22280+5742AB     and {omega} listed in the 6th COVBS. It is noteworthy that the 
22280+5742AB     velocity values listed in the Wilson - Evans - Batten 
22280+5742AB     catalogue (Duflot et al., 1995A&AS..114..269D, Vr(A)=-24.0km/s 
22280+5742AB     and Vr(B)=-28.0km/s) or in Reid et al. (1995AJ....110.1838R) 
22280+5742AB     (Vr(A)=-16.0km/s and Vr(B)=-29.0km/s), although the differences
22280+5742AB     are much larger than anticipated, always have Vr(B)-Vr(A)<0. 

23317+1956AB    Indeterminate visual orbit.

23524+7533AB    Indeterminate visual orbit. A triple system with A being SB2 
23524+7533AB     with a period of 7.75d (Christie, 1934ApJ....80..181C).