HD 4775-76 Has SB1 orbit (Mason et al., 1997AJ....114.1607M); is resolved by HD 4775-76 ifm. (WDS, Cat. ), with same orbital period and a=0.034" HD 4775-76 (Hartkopf et al., 2001AJ....122.3472H)). Not considered triple, HD 4775-76 included here because of omission from Paper V (Parsons & Ake, HD 4775-76 1998, Cat. . HD 5373 Has SB1 orbit (Griffin, 1990Obs...110..150G); is resolved by HD 5373 Hipparcos at 0.3". SED fit favors Seaton extinction law with HD 5373 scaling parameter d~2.0. Iso=> Calculated a ~2mas and {Delta}V of HD 5373 0.5 are at odds with Hipparcos sep. and {Delta}Hp of 3.2mag. So HD 5373 the SB pairing must be distinct from the resolved pairing. HD 23089-90 Has SB1 orbit with 16 day uncertainty in P (Griffin, HD 23089-90 1990JApA...11..491G). Sometimes resolved by speckle with possible HD 23089-90 motion (Hartkopf et al., 2001AJ....122.3480H) (~8{deg} in 15yr; HD 23089-90 maybe not the same pair as SB, but SB orbit has high HD 23089-90 eccentricity). Iso=> {pi} too large; needs some adjustment in mass HD 23089-90 (less massive primary, more massive secondary, or both) for HD 23089-90 sensible i. HD 24480 ADS 2867A; has variable RV? Two-component SED fit is consistent HD 24480 with Tycho components' photometry. Iso=> {pi} is probably too HD 24480 large without adjusting masses, though this adjustment could HD 24480 produce a {Delta}V discrepancy. HD 26673-74 Has SB1 orbit (Parsons, 1983ApJS...53..553P); is unresolved by HD 26673-74 speckle (Hartkopf et al., 2001AJ....122.3480H), though Hipparcos HD 26673-74 found acceleration. Has good, well-constrained SED fit. IUE HD 26673-74 high-dispersion data hint at double secondary, as does the K line HD 26673-74 (Ginestet & Carquillat, 2002, Cat. ). Iso=> sini HD 26673-74 test is consistent only if HD 26673-74 secondary is double. HD 29094-95 Has astrometric orbit plus SB1 orbit (Batten et al., 1989, HD 29094-95 Cat. , revised by Parsons, 1983ApJS...53..553P) that implies HD 29094-95 a ~0.051" and i~81{deg} (Wyller, 1957AJ.....62..384W ; Hartkopf et HD 29094-95 al., 2001AJ....122.3472H)), but is unresolved by speckle (Hartkopf HD 29094-95 et al., 2001AJ....122.3480H). Good, very well constrained SED fit HD 29094-95 implies K1 primary, favors Seaton extinction law with d=1.7. HD 29094-95 Iso=> favors a larger than 0.08", and either greatly reduced mass HD 29094-95 of primary or a double secondary. HD 29104 ADS 3316AB, has sep. measures of 0.3" (1902) and 0.065" (1994) but HD 29104 is not reported resolved otherwise (Simbad; Hartkopf et al., HD 29104 2001AJ....122.3480H). Has SB1 orbit with large mass function, HD 29104 suggestive of a triple system (Griffin, 1990JApA...11..491G); HD 29104 primary and secondary may each be a short-period binary HD 29104 (Strassmeier & Fekel, 1990A&A...230..389S). SED fit is fair with HD 29104 extinction not tightly constrained. Iso=> sini test consistent HD 29104 only if secondary is double; {Delta}V is not well matched with HD 29104 other determinations, though. HD 39118-19 Has SB1 orbit (Griffin, 1990JApA...11..491G); K line and large HD 39118-19 mass function imply hot component is double. Has no ifm. measures. HD 39118-19 SED fit is good, with primary's type now constrained by 2MASS. HD 39118-19 Iso=> sini test consistent only if secondary is double. HD 49126 ADS 5437AB; member of NGC 2287, whose distance modulus is 9.2 HD 49126 (Harris et al., 1993, Cat. ). RV(G star)=+36:, HD 49126 compared with RV(B9 star)=-5: (Simbad, two measures) implies SB2. HD 49126 {Delta}V(SED) of 0.9 is at odds with observed 4.0. Iso=> P~6000yr HD 49126 calculated from measured sep. 1.2" (WDS, Cat. ) and HD 49126 estimated masses is not consistent with implied timescale of HD 49126 decades or less for RV variation. The spectrum of component 'B' is HD 49126 therefore unknown, not being the UV source. The age of 2x108yr HD 49126 (Table 4) is in excellent agreement with Harris et al. (1993, HD 49126 Cat. ); the cluster MV of -1.7 for the primary, HD 49126 after adjusting it for the (Ab) component's contribution to V, is HD 49126 just within the expected error of 0.6 in the binarity MV method. HD 64440 Has SB1 orbit (Parsons, 1983ApJS...53..553P), which needs HD 64440 improvement; is unresolved by speckle (Hartkopf et al., HD 64440 2001AJ....122.3480H) but shows acceleration in Hipparcos data HD 64440 (V. Makarov 2003, priv. com.). Fair SED fit shows some flux HD 64440 differences among IUE epochs. High-dispersion IUE data imply an HD 64440 SB3 system, but signal-to-noise ratio is not sufficient for HD 64440 quantitative results. Iso=> consistent {pi} with double, not HD 64440 triple, system. HD 71129-30 Unresolved by speckle in one 1978 measurement (Hartkopf et al., HD 71129-30 2001AJ....122.3480H), while Hipparcos sep.=0.42". IUE spectra show HD 71129-30 pronounced stellar wind features. Tycho not fitted well without a HD 71129-30 mid-type star paired with B2 star and of comparable brightness HD 71129-30 (Fig. 3). Iso=> No simultaneous fit of observed components plus a HD 71129-30 mid-type star; further discussed in Sect. 5. This is the one case HD 71129-30 where the extended mass loss Geneva models differ noticeably from HD 71129-30 the standard models (Sect. 3.2) : the primary's current mass is 7% HD 71129-30 higher with the best-fitting extended mass loss isochrone, but the HD 71129-30 other results in Table 5 (from fitting to standard model HD 71129-30 isochrones) are not changed significantly. HD 74874 ADS 6993AB, has SB1 and speckle orbits with a=0.25" (Hartkopf, HD 74874 Mason & McAlister, 1996, Cat. ); second HD 74874 periodicity ~70 days is suspected (BSC). The Hipparcos sep.=2.87", HD 74874 {Delta}Hp =3.1mag measures then refer to the pairing A/C. HD 74874 Component 'C' itself is SB1 with P=9.9days (MSC, HD 74874 Cat. ). SED fit is well constrained for primary, HD 74874 but mid-UV flux is only available from high-dispersion; may favor HD 74874 Seaton extinction law with d~2.5. Iso=> consistent in both {pi} HD 74874 and a with double or multiple system; adding mass to the primary HD 74874 for a main-sequence companion fainter by ~2.5mag, for the HD 74874 suspected 70 day pairing, brings consistency with the determined HD 74874 orbital inclination. HD 76072-73 Separation measured by speckle (Hartkopf et al., HD 76072-73 2001AJ....122.3480H) shows motion; RV range at least +3 to +18 HD 76072-73 (Andersen et al., 1985A&AS...59...15A; Parsons, HD 76072-73 1983ApJS...53..553P). Iso=> The {pi} is too large unless masses HD 76072-73 are adjusted. However, this increases an apparent discrepancy in HD 76072-73 {Delta}V. HD 101379-80 Designated GT Mus, has SB1 orbit plus eclipsing 56.03-day pair of HD 101379-80 A stars, implying three components (Strassmeier et al., 1988, HD 101379-80 Cat. ). The sep. measured by speckle (Hartkopf et al., HD 101379-80 2001AJ....122.3480H), with P~91yr HD 101379-80 (MSC, Cat. ), is not the 61 day or 56 day system HD 101379-80 but another pairing A/B. Strong Ca II and radio emission (Simbad), HD 101379-80 implies one of the pairings is related to RS CVn binaries? SED is HD 101379-80 well fitted with two components. Iso=> {pi} consistent with triple HD 101379-80 system; a ~3mas is again very much smaller than speckle measures. HD 120901-02 DL Vir; has SB1 orbit (which can be improved), with third HD 120901-02 component partially eclipsing the A star at 1.315 day period HD 120901-02 (Batten et al., 1989, Cat. ; MSC, Cat. ). Is HD 120901-02 unresolved by speckle (Hartkopf et al., 2001AJ....122.3480H). SED HD 120901-02 fit with two components is fairly well constrained and also fits HD 120901-02 the in-eclipse IUE data with a drop of 2.4mag in the flux from the HD 120901-02 A star. Iso=> The sini test is consistent with a triple system, HD 120901-02 not double. The minimum combined mass of components (Ba + Bb) HD 120901-02 required to obtain a real number for the inclination (3.3M_{Sun}_) HD 120901-02 happens to equal the mass sum of the A star (2.2) and a K star HD 120901-02 component (1.1), according to Schoeffel (1977A&A....61..107S). HD 136415-16 Binary sep. 0.83" was measured by speckle (Hartkopf et al., HD 136415-16 2001AJ....122.3480H), and preliminary orbit has P~270yr, a=2.5" HD 136415-16 (WDS, Cat. ; Hartkopf et al., 2001AJ....122.3472H)); no HD 136415-16 evidence of RV variations (Simbad). The Tycho component measures HD 136415-16 require the primary to be several spectral subclasses cooler than HD 136415-16 the best SED fit without Tycho data (Figs. 1 and 2); the fit HD 136415-16 favors a Seaton extinction law with d~3.5. Iso=> No fit unless HD 136415-16 {Delta}V is adjusted for the hot star being double; calculated a HD 136415-16 ~0.3" is at odds with the above. The binarity parallax greatly HD 136415-16 disagrees with Hipparcos. HD 149379 ADS 10111, has position angle approximately constant over at least HD 149379 8yr baseline (Hartkopf et al., 2001AJ....122.3480H). Has no known HD 149379 RV measures. SED plus Tycho component measures require nearly HD 149379 equal brightness G8: + F6: stars for optical to mid-UV, plus F0: HD 149379 star about 3mag fainter for the far-UV (Fig. 4). Iso=> all three HD 149379 components fit well simultaneously (Fig. 5); further discussed HD 149379 in Sect. 5. HD 157978-79 Has SB3 orbit, with two A0 stars in mutual orbit at 3.76 days HD 157978-79 (Fekel, 1981ApJ...246..879F; MSC, Cat. ). Is HD 157978-79 unresolved by speckle (Hartkopf et al., 2001AJ....122.3480H). Has HD 157978-79 well-constrained SED fit with two components, prefers Seaton HD 157978-79 extinction law with d=1.2. Iso=> sini test is consistent with HD 157978-79 triple system, not double; calculated a ~20mas may be at odds with HD 157978-79 6mas orbit? HD 169985-86 ADS 11353A, has sep.=0.25" ifm. at one epoch (Hartkopf et al., HD 169985-86 2001AJ....122.3480H; MSC, Cat. ); this evidently HD 169985-86 refers to the pairing 'A/P'. Visual primary 'A' is SB3: its A-type HD 169985-86 secondary is binary with period 1.85 days (Batten et al., 1989, HD 169985-86 Cat. ); orbit needs improvement. Component B at 3.8" may HD 169985-86 also be SB but is not relevant to IUE data. SED fit is good, but HD 169985-86 primary's type is not tightly constrained. Iso=> consistent with HD 169985-86 {pi} and with mass ratio of 1.5 between (Ab + Ac) and (Aa). HD 175635 ADS 11834A; has SB1 orbit (Griffin, 1990JApA...11..491G), HD 175635 presumably for components (Aa/Ab), unresolved by speckle (Hartkopf HD 175635 et al., 2001AJ....122.3480H). SED fit including Tycho component HD 175635 measures requires a fainter but blue star for the component 'B' HD 175635 seen by Tycho. Iso=> The sin i test favors a higher mass for HD 175635 component (Ab) than expected. Taking component 'B' into account in HD 175635 simultaneous isochrone fitting, the luminosity of (Ab) cannot be HD 175635 diminished much to account for the proposed (Ac) component's HD 175635 contribution to the SED {Delta}V; but (Ac) can have sufficient HD 175635 mass to pass the sini test without having much effect on the HD 175635 (Ab + Ac) combined flux. HD 179002 ADS 12126AB, has sep. measured by speckle (Hartkopf et al., HD 179002 2001AJ....122.3480H), with early micrometer data implying 109.0yr HD 179002 period for a fair-quality visual orbit (Stephenson & Sanwal, HD 179002 1969AJ.....74..689S). It is probably time to redo the orbit. Only HD 179002 one RV measure is known (Abt & Biggs, 1972, Cat. ). The HD 179002 {Delta}V~2.0 from SED analysis is at odds with {Delta}Hp=0.5mag, HD 179002 so component 'B' is probably not the component seen with IUE. The HD 179002 2MASS data imply a K2-K3 component at a {Delta}V that is HD 179002 compatible with Hipparcos; but the three components do not fit a HD 179002 single isochrone. Table 4 contains the scenario that is consistent HD 179002 with the Hipparcos parallax, in which the K component is way too HD 179002 cool to fit at its apparent luminosity. Yet the (Aa + Ab) mass sum HD 179002 of ~4M_{sun}_ is consistent with the period and sep. for the A/B HD 179002 pairing. This system is a puzzle. HD 179950 ADS 12214AB; has SB3 orbit that needs improvement, with periods HD 179950 ~7319 days, 10.8 days (Strassmeier & Fekel, 1990A&A...230..389S; HD 179950 Batten et al., 1989, Cat. ). The sep. measured by speckle HD 179950 shows orbital motion, with i=81{deg}, a = 0.130", P=7089 days HD 179950 (Hartkopf et al., 2001AJ....122.3472H)). Iso=> consistent with HD 179950 triple system, though there are moderate disagreements in mass, HD 179950 {pi}, and a. HD 187299 Has SB1 orbit (Griffin & Radford, 1977Obs....97..169G); is HD 187299 unresolved by speckle (Hartkopf et al., 2001AJ....122.3480H) but HD 187299 shows acceleration in Hipparcos data (V. Makarov 2003, priv. HD 187299 com.). SED fit favors Seaton extinction law with d=1.2. HD 187299 Iso=> Very large sini discrepancy requires a third component, and HD 187299 even suggests adjustment of the primary's theoretical mass from HD 187299 6M_{sun}_ down to 5M_{sun}_ to satisfy the sini test. The HD 187299 luminosity from isochrone fitting is at odds with MV~-5.7 (our HD 187299 calculation) or -6.2 (as given) if a member of Vul OB1 association HD 187299 (Humphreys, 1978ApJS...38..309H). HD 193495-96 Has SB2 orbit, also with period 8.7 days for hot component SB1 HD 193495-96 (Batten et al., 1989, Cat. ); sep. measured by speckle HD 193495-96 (Hartkopf et al., 2001AJ....122.3480H) shows orbital motion with HD 193495-96 determinations of a=0.050" (MSC, Cat. ) or 0.089" HD 193495-96 (Hartkopf et al., 2001AJ....122.3472H)). Iso=> consistent with HD 193495-96 {pi} and with a; also with inclination when third star is less HD 193495-96 massive than the hot secondary in accordance with the SB2 mass HD 193495-96 ratio. HD 196093-94 Designated V2125 Cyg for irregular variability. Has SB1 orbit HD 196093-94 (Griffin, 1992Obs...112..111G), which can be improved; HD 196093-94 approximately constant position angle and sep. measured by speckle HD 196093-94 (Hartkopf et al., 2001AJ....122.3480H), with P~144yr (MSC, HD 196093-94 Cat. ), is not the same pairing as the SB. SED fit HD 196093-94 favors Seaton extinction law with d=1.9. Iso=> not consistent with HD 196093-94 {pi}, but worse with third mass. HD 197177 ADS 14158; probably component 'B' (HD 197178, of type A:) was HD 197177 included in slit at 2.5", {Delta}V=2.1 (WDS, Cat. ); close HD 197177 pair 'Aa' = (Aa/Ab) is listed at 0.24" in 1979 (WDS, Cat. ) HD 197177 but otherwise reported unresolved by speckle (Prieur et al., HD 197177 2002ApJS..142...95P; Hartkopf et al., 2001AJ....122.3480H). With HD 197177 nature of component 'a' = (Ab) unknown, current results probably HD 197177 apply to 'A' + 'B' since the {Delta}V and Tycho component HD 197177 magnitudes are well matched. RV range may be at least -28 to -23, HD 197177 while component 'B' shows two A0 spectra with huge RV differences HD 197177 between epochs (Simbad). HD 199378-79 Has SB1 orbit (Griffin & Griffin, 1990JApA...11..491G); is HD 199378-79 unresolved by speckle (Simbad). Not considered triple, included HD 199378-79 here because of omission from Paper V (Parsons & Ake, 1998, HD 199378-79 Cat. . HD 200428-29 Has SB1 orbit (Batten et al., 1989, Cat. ); is unresolved by HD 200428-29 speckle (Simbad). Not considered triple, included here because of HD 200428-29 omission from Paper V (Cat. ). SED fit favors HD 200428-29 Seaton extinction law with d=3.0. HD 200497 ADS 14592; component 'B' (HD 200496) of type A3 V (BSC) was HD 200497 probably included in slit at 2.5", {Delta}V=1.7 (WDS, HD 200497 Cat. ). The close pair 'Aa' = (Aa/Ab) at 0.05"-0.07" sep. HD 200497 measured by speckle (Hartkopf et al., 2001AJ....122.3480H) shows HD 200497 motion, P~6760 day RV range is at least -4 to +6 (Simbad). Tycho HD 200497 fit requires three components, very consistent with (Aa-Ab-B). HD 203156 ADS 14859AB; a low-amplitude Cepheid with SB1 orbit (Evans, HD 203156 2000AJ....119.3050E). Separation 0.13" (BSC), ~0.06" (Hartkopf et HD 203156 al., 2001AJ....122.3480H), often unresolved by speckle. Evans was HD 203156 able to determine from velocities that the hot component must be HD 203156 the sometimes-resolved 'B,' while the SB secondary is an unseen HD 203156 component; she estimates masses of ~5.0, 3.1-4.4, and 4.4M_{sun}_ HD 203156 for these components (Aa), (Ab), and (B). Iso=> Our isochrone fit HD 203156 uses the first crossing from blue to red, not the huge HD 203156 extrapolation of the blue loop done by Evans. But then we only HD 203156 get close to the expected MV by adding significant mass to the HD 203156 secondary instead of the primary, making the {Delta}V discrepancy HD 203156 worse: early observers described the A/B components as having HD 203156 nearly equal brightness. HD 208253 Has SB1 orbit (Griffin, 1990JApA...11..491G); is unresolved by HD 208253 speckle (Hartkopf et al., 2001AJ....122.3480H). Hipparcos HD 208253 sep.=1.35", {Delta}Hp=3.8mag apparently is not relevant to HD 208253 cool + hot binary. The SED fit implies that the A star has HD 208253 slightly greater visual luminosity than the G star; fit is HD 208253 somewhat ambiguous, with cool type and {Delta}V not constrained HD 208253 well. Iso=> consistent. HD 213503-04 Has SB1 orbit, though large mass function suggests three stars HD 213503-04 (Griffin, 1990JApA...11..491G; Griffin, Carquillat, & Ginestet, HD 213503-04 2002Obs...122...90G); has no ifm. data. SED: near- and far-UV fit HD 213503-04 well, cool type now well constrained at K2 thanks to 2MASS data. HD 213503-04 Iso=> sini test consistent with triple system, not double. HD 215182 ADS 16211A; sep. measured by speckle (Hartkopf et al., HD 215182 2001AJ....122.3480H) shows orbital motion with a=0.045" (which HD 215182 includes Hipparcos and Tycho data) (Martin & Mignard, HD 215182 1998A&A...330..585M). Has SB1 orbit (Batten et al., 1989, HD 215182 Cat. ), improved by S.B. Parsons (unpublished) to HD 215182 P=817.43 days, K=14.7, and f(m)=0.26, with e=0.15 still. HD 215182 High-dispersion IUE spectra imply that the A-type component is HD 215182 double (S.B. Parsons, unpublished). Cool type is very well HD 215182 constrained by SED at G7. Iso=> The {pi} is consistent with double HD 215182 system, not with an additional A-type star; sini is matched to the HD 215182 observed value with only slight adjustment to either of the HD 215182 masses. So a third component is possible but probably not of HD 215182 significant mass, and we are left with no explanation of the IUE HD 215182 line-profile variations. HD 218640-41 The sep. measured by speckle (Hartkopf et al., HD 218640-41 2001AJ....122.3480H) shows orbital motion with P~201yr, a=0.45"; HD 218640-41 RV range may be at least -5 to -1 (Abt & Biggs 1972, Cat. ; HD 218640-41 Beavers & Eitter, 1986ApJS...62..147B). Iso=> {pi} is too large HD 218640-41 without adjusting masses. HD 223047 The sep. measured by speckle shows two pairings: 0.28" 'Aa' or HD 223047 'Aab,' 0.14" 'Ab' or 'Aac' (Hartkopf et al., 2001AJ....122.3480H). HD 223047 RV is approximately constant (de Medeiros et al., 2002, HD 223047 Cat. ; Simbad). IUE spectra show unusual absorption HD 223047 feature at about 1410{AA}. Iso=> the periods calculated from the HD 223047 speckle separations are reasonably close to the astrometric HD 223047 estimates.