01128-3751 HIP 5661 = AI Scl = TOK 181. A new binary HAeBe star with a very faint companion, {Delta}I=6.2mag at 1.4". The measure in the y filter is below the formal detection limit, but it is assisted by the I-filter data.
01166+1831 HIP 5952 = HDS 169. The primary is a metal-poor G5 dwarf; based on magnitude difference, the secondary is late-K or early-M. A is a 274 day SB1 (MSC). A very preliminary orbit (period 144 years) yields a mass sum too high for these spectral types, however.
01187-2630 HIP 6136 = TOK 182 Ba,Bb. This is a new subsystem in the SEE 11 AB pair, with a very faint companion Bb at 0.39" from Ba. The AB pair was observed but not detected as a triple in 2008 (Tokovinin et al., 2010, Cat. J/AJ/139/743).
01308-5940 HIP 7040 = TOK 183. A new close companion at 0.05" is found. This is a nearby G0V dwarf with variable RV.
01417-1119 HIP 7916 = STF 147. This pair has closed from ~4" in the early 1820s to 0.1" in 2009 and now 50mas in 2011. Nearly two centuries of motion have been well characterized by a rectilinear fit to those data. However, a noticeable acceleration has been seen in recent observations, as the large residuals to that linear fit in Table 2 will attest. Observations over the next few years should allow better definition of this apparently physical pair.
01496-4646 HIP 8498 = TOK 184. A faint companion at 0.25", {Delta}I=3.9mag, is found. It is unresolved in the y filter. This G5V dwarf is already known as an astrometric and spectroscopic binary. The estimated period is on the order of 50 years.
02057-2423 HIP 9774 = I 454. A preliminary orbit of the AB pair in this quadruple yields a period of just over 200 years. The subsystem WSI 71 Aa,Ab is too close to be resolved here; its preliminary orbit in Tokovinin et al. (2010PASP..122.1483T) predicts a separation of 14mas.
02166-5026 HIP 10611 = TOK 185. The companion at 0.05" is resolved here for the first time. This is a nearby G5V dwarf previously known as an astrometric binary.
02225-2349 HIP 11072 = LAF 27. This is the nearby G dwarf {kappa} For, an astrometric binary with P=26.5-years. It was first resolved at SOAR in 2007. Our orbital solution fixes P and e to the astrometric values derived by Gontcharov & Kiyaeva (2002AstL...28..261G). This orbit must be considered preliminary, due to the lack of phase coverage, but the resulting mass sum is in reasonably good agreement with the values expected for a G1V + early-M pair.
02374-5233 HIP 12225 = {eta} Hor = TOK 186 Aa,Ab. The near-circular three-year astrometric orbit of Goldin & Makarov (2007ApJS..173..137G) implies a semimajor axis on the order of 70mas, given the Hipparcos parallax. The astrometric orbit predicts a photocenter displacement of 21mas at 71{deg} while we measure a separation of 70mas at 60{deg} and {Delta}y=1.4mag. Frequent measures of this nearby and apparently young system with debris disk are needed to confirm the orbit and to compute masses.
02415-7128 HIP 12548 = B 1923. This is a nearby G dwarf; the companion is perhaps early-K. The orbit (P ~ 100 years) given in Table 4 must be considered preliminary, but yields a reasonable mass sum.
02434-3756 HIP 12716 = TOK 187. This is a nearby dwarf triple; the primary is G6V. The new companion at 0.38" with {Delta}I=3.3mag resolved here should correspond to the astrometric binary discovered by Makarov & Kaplan (2005, Cat. J/AJ/129/2420). The estimated period is 40 years. The A component is the SB2 UX For with 0.955 day period, also an X-ray source (MSC).
02442-2530 HIP 12780 = FIN 379 Aa,Ab. This comprises the close pair in a physical triple. Combined with the Hipparcos parallax (24.2+/-1.6mas) the orbit in Table 4 yields a mass sum of 1.55M_{sun}_ (the expected value is ~2.1M_{sun}_). If we adopt the Hipparcos parallax, we can place the triple system on the color-magnitude diagram (K, V-K). The Aa,Ab is ~1mag above the main sequence (MS), as expected, and B is on the MS. If we instead adopt the dynamical parallax, the stars will move up by 0.2mag. It is likely that the Hipparcos parallax was biased slightly, due to the rapid motion of the binary.
02449+1007 HIP 12828 = TOK 1. This is not resolved here. It must have closed in since its last observation on 2008.77 (0.1", {Delta}y=3.5mag, Tokovinin et al., 2010, Cat. J/AJ/139/743).
02539-4436 HIP 13498 = I 1480. This is the wide pair in a triple system; the A component is an SB2 without published orbit, and also an X-ray source (MSC). An initial orbit for AB finds a period of about 50 years. The primary is a K0:III; the derived mass sum and magnitude difference are both consistent with a late-A dwarf companion.
02572-2458 HIP 13772 = BEU 4 Ca,Cb. This shows fast motion. This pair and BU 741 belong to the low-mass quintuple system GJ 120.1 (MSC).
03099-0654 HIP 14699 = TOK 188 Aa,Ab. This is the W-UMa-type eclipsing binary UX Eri. The new close companion at 0.044" appears real, based on examination of other stars observed contemporaneously. This tertiary companion was suspected from eclipse timing, but was unresolved with AO by Rucinski et al. (2007, Cat. J/AJ/134/2353), probably being too close.
03167-0332 HIP 15247 = TOK 189 Aa,Ab. A new faint red companion is found at 0.88", {Delta}I=3.5mag, {Delta}y=5.2mag, estimated period 200 years. This is a young nearby F5 dwarf with variable RV, possibly triple, and also an X-ray source.
03309-6200 HIP 16370 = TOK 190. This is resolved for the first time at 0.07". It is a nearby F7V dwarf, an astrometric and spectroscopic binary, and an X-ray source.
03442-6448 HIP 17440 = TOK 191 Aa,Ab. This is the nearby star HR 1175 = {beta} Ret, K2III. The new companion resolved at 0.08", {Delta}I=2.8mag may correspond to the 5.2 year astrometric subsystem found by Ramm et al. (2009, Cat. J/MNRAS/394/1695) with estimated semimajor axis of ~0.15". However, its non-resolution in y is strange, given the red color of the primary.
03544-4021 HIP 18262 = FIN 344. This consists of a K0III and A3V stars; a preliminary orbit yields a period of 14 years and a mass sum of 4.2M_{sun}_. The primary has variable RV.
04049-3527 = HIP 19052 = CHR 224 BC. This shows fast motion, estimated period 10 years. Together with I 152 AB this is a hierarchical resolved triple system.
04205-0119 HIP 20257 = RST 4769. Table 4 updates the orbit of Heintz (1997ApJS..111..335H) for this pair of A3 dwarfs; the predicted mass sum of 3.5M_{sun}_ is a little low.
04286+1558 HIP 20885 = MCA 15. This was resolved, but no consistent measure could be obtained because of large {Delta}y~3mag and the influence of vibrations. This pair belongs to the quadruple system HR 1412+1411.
04375+0509 HIP 21543 = CHR 153. This is a triple Hyades dwarf. The inner 1.8 year astrometric/spectroscopic subsystem is not resolved. Recent measures showed significant runoff from the solution of Olevic & Cvetkovic (2003IAUDS.150....1O); the data appear to be better described by a simple rectilinear fit (see Figure 4(a)), suggesting the companion is just another Hyades member projected close to the primary. A non-Hyad background star is ruled out, as it would have moved by ~20" since discovery.
04422+0259 HIP 21880 = A 2424. This is unresolved despite {Delta}m=0.46mag and a separation of 0.15" predicted by the orbit of Wilson (1976MNRAS.174P..75W).
04536+2522 HIP 22747 = CHR 127. This is resolved, but no trace of the subsystem A 184 AC is seen here. Motion of the AB pair appears to be well fit by a ~60 year period orbit.
05245-0224 HIP 25281 = DA 5 AB. This is the quadruple star HR 1788 = {eta} Ori; A is an eight-day SB2 with a spectroscopic tertiary companion known as MCA 18. This subsystem, with a 9.44 year period, is unresolved here and in Tokovinin et al. (2010, Cat. J/AJ/139/743).
05353-0523 HIP 26221 = WGT 1 Ca,Cb. {theta} Ori C was apparently resolved during SAM tests in November, but we are not certain of the identification; it could have been another star in the trapezium.
05418-5000 HIP 26830 = HU 1568. This is composed of a pair of early-K dwarfs. A preliminary 300 year period orbital solution yields a mass sum consistent with these types.
05540+1225 HIP 27878 = TOK 192 Aa,Ab. A new faint companion is found at 1.4", {Delta}I=5.7mag, unresolved in the y filter. This is a nearby quadruple F8 dwarf containing a spectroscopic subsystem and a CPM companion at 90".
06003-3102 HIP 28442 = TOK 9 CE. This was discovered in 2004 on AO-corrected images in the IR (Tokovinin et al., 2005A&A...441..695T). Later it was resolved at SOAR in the visible. It is marginally resolved here in the I band (0.08") and has closed down as expected. The second observation on 2010.966 gave unrealistically small separation with a small {Delta}m derived from the power-spectrum fit. The CE pair follows a ~23 year preliminary orbit (Table 4) and, together with HU 1399, belongs to the quadruple system of nearby dwarfs GJ 225.2 with high proper motion.
06032+1922 HIP 28671 = HDS 823 Aa,Ab. This belongs to a nearby G-type triple system with a physical tertiary at 6.9"; its estimated orbital period is ~10 years. The pair has opened up after passing through periastron; it was unresolved in Tokovinin et al. (2010, Cat. J/AJ/139/743).
06173+0506 HIP 29860 = CAT 1 Aa,Ab. This is a G0V star at 19.3pc from the Sun with four companions listed in the WDS. Three (B, C, D) are optical, but LEP 24AE at 103" is physical. The inner Aa,Ab pair was discovered as a spectroscopic binary by Vogt et al. (2002ApJ...568..352V), who proposed an orbital solution with a period of 33.7+/-1.5 years. Their observations cover only 10%of the period around periastron. The system was first resolved in the IR by Catala et al. (2006AJ....132.2318C) using the PUEO AO system. They revised the period to 28.8+/-1.1 years by fitting a combined spectro-visual orbit to all the data; other elements were a=0.621", i=35.4{deg}, and {Omega}=166.8{deg}. They estimated that the companion with {Delta}V~5.5mag is not detectable in the visible. However, we measured it in Tokovinin et al. (2010, Cat. J/AJ/139/743) and here, with {Delta}y=5.2mag. A slight runoff of the residuals prompted us to adjust the orbital elements. The seven Campbell elements are in Table 4, other spectroscopic elements are K1=4325.00+/-5.81km/s and V0=457.11+/-10.97km/s. This orbit, combined with the Hipparcos parallax, lead to a mass sum of 1.50M_{sun}_. Lower weight was given to our measure obtained on a technical night on 2008.773, because of a large residual in position angle (P.A.).
06290+2013 HIP 30883 = {nu} Gem = BTZ 1. Our measure confirms the 18 year orbit by Cvetkovic & Ninkovic (2008NewA...13..587C) and casts doubt on the 9.6 year spectroscopic orbit based on poor-quality data. The pair BU 1192 Ba,Bb also measured here may form a physical quadruple with BTZ 1, but most likely it is optical.
06439-5434 HIP 32242 = HDS 934. The nearby K-dwarf pair shows quite rapid motion, and has completed nearly two revolutions since its discovery in 1991. We compute its orbit with P=12.37-years (Table 4) which matches the expected mass sum.
06573-4929 HIP 33455 = RST 5253 AB. The update to the solution of Costa (1975, Inf. Circ., 66, 1) yields a mass sum of 2.1M_{sun}_, in excellent agreement with the values expected for a G5/6III primary and an early-G companion.
07043-0303 HIP 34110 = A 519. This is a nearby triple G-dwarf containing a 5.7 day SB1 subsystem. It was not resolved here despite predicted separation of 0.07"; the visual orbit of Docobo & Ling (2009AJ....138.1159D) therefore needs revision.
07185-5721 HIP 35374 = HDS 1013 Aa,Ab. This is a nearby G0V dwarf with perhaps a mid-G companion. This close 60 year pair (see the new orbit in Table 4) forms a quadruple system with RST 244 Ba,Bb at 2.5". We do not resolve the Ba,Bb pair here.
07187-2457 HIP 35415 = FIN 313 Aa,Ab. This is a quadruple star containing a 1.3 day eclipsing binary Ab and a 155 day SB Aa (MSC). Its distant (0.95") companion C also measured here may be just another member of the cluster NGC 2362.
07277+2127 HIP 36238 = MCA 30 Aa,Ab. This belongs to a nearby multiple system with five components. It was not resolved here or in Tokovinin et al. (2010, Cat. J/AJ/139/743) despite predicted separation of 0.044" and {Delta}m=1mag. The orbit of Muterspaugh et al. (2010, Cat. J/AJ/140/1623) appears very reliable, however.
07374-3458 HIP 37096 = FIN 324. This is a triple system with comparable separations ("trapezium") according to the WDS. However, we figured out that all published speckle measures (except one) refer to the AC pair. Its motion appears to be reasonably well fit by an 80 year orbit (Table 4 and Figure 3). The existence of the component B with 0.1" separation, not seen here and in Tokovinin et al. (2010, Cat. J/AJ/139/743), is highly questionable on dynamical grounds, while its historical measures remain unexplained.
07456-3410 HIP 37853 = TOK 193 Aa,Ab. A new faint red companion at 0.32", {Delta}I=3.0mag, is found. This nearby F9V dwarf GJ 288A is also known as an astrometric and spectroscopic binary. There is also a physical white dwarf companion at 914" (Raghavan et al., Cat. J/ApJS/190/1). Another faint companion at 1.4", 20{deg}is seen in the y and I filters, but it is not measured here.
07490-2455 HIP 38146 = TOK 194. Goldin & Makarov (2007ApJS..173..137G) find a three-year astrometric orbit for this G0III star with a parallax of 11.6+/-1.1mas. A semimajor axis of 30mas is expected. At the moment of our resolution (21{deg}, 40mas, {Delta}y=1.2mag) the astrometric orbit predicts a displacement of 16mas at 164{deg}.
07522-4035 HIP 38414 = a Pup = TOK 195. This K1.5II giant is a 7 year spectroscopic binary (Parsons, 1983ApJS...53..553P). Given the Hipparcos parallax of 9.3+/-0.8mas, a semimajor axis of 50mas is expected. An astrometric orbit was determined by Jancart et al. (2005, Cat. J/A+A/442/365), fixing some elements at their spectroscopic values. This orbit predicts a photocenter displacement by 20mas at 15{deg} for the moment of our observation. We measured the companion ({Delta}y=0.8mag) at 20mas and 19 deg.
07523-2626 HIP 38430 = WSI 54. This is resolved here as a binary, with a hint at the triple structure seen in Tokovinin et al. (2010, Cat. J/AJ/139/743) in the y filter. This star, of spectral type O6e, belongs to the cluster NGC 2467. Lorenzo et al. (2010ASPC..435..409L) find that the object is quadruple and contains two SB2s.
08151-0655 HIP 40419 = MET 52. The companion at 1.43" measured here was first resolved by Metchev & Hillenbrandt (2009, Cat. J/ApJS/181/62) in 2002 at 101{deg}, 1.23", {Delta}K=3.9mag. This is a nearby G5 dwarf possibly containing an SB subsystem.
08250-4246 HIP 41250 = CHR 226 Aa,Ab. The quadrant of the close pair is fixed by the wider system AB. Intriguingly, we measure {Delta}y=2.8mag, while {Delta}y=0.2mag was found on 2009.26 by Tokovinin et al., 2010, Cat. J/AJ/139/74. The system is variable, with a suspected eclipsing binary.
08263-3904 HIP 41361 = B 1605 Ba,Bb. This belongs to the quadruple system HR 3327, with Aa,Ab being the 1.3 day eclipsing pair NO Pup (MSC). The A component was observed and found unresolved here and in Tokovinin et al. (2010, Cat. J/AJ/139/743). The Ba and Bb components are probably both early-A dwarfs, in an orbit of about a century-long period (Table 4).
08280-3507 HIP 41515 = FIN 314. This contains the possibly eclipsing subsystem XY Pix (MSC). The ~36 year period orbit in Table 4 fits the speckle data well, but the early eyepiece interferometry had to be given zero weight in the solution.
08380-0844 HIP 42345 = HDS 1242. This is a nearby mid-G dwarf (plus early-K companion?) with a period of ~31 years (Table 4).
08421-5245 HIP 42695 = B 1624. This is a nearby early-G + early-K dwarf. The revised orbit in Table 4 yields a mass sum of 2.0M_{sun}_, in reasonable agreement with these types.
08447-4238 HIP 42916 = CHR 238. This is a nearby pair comprised of a K0: and mid-K dwarfs. Goldin & Makarov (2007ApJS..173..137G) derived an 815 day astrometric orbit with P=815-days and e=0.68. Our orbit, although based on only three measures, is in remarkably good agreement, with P=824.7-days and e=0.671. The derived mass sum is also in quite good agreement with the value expected for these spectral types.
08538-4731 HIP 43671 = FIN 316. The A component is a 9.1 day SB2 (MSC). The primary spectral type is A9 IV-V; given the magnitude difference of near zero, the secondary is probably similar. In calculating the orbit in Table 4, all data were used to derive the period, then only the higher-quality interferometric data were used in determining all other elements.
08547+1637 HIP 43751 = TOK 196 Aa,Ab. A new 0.11" subsystem in AG 338 AB is found in this nearby G5V dwarf. Its estimated period is ~10 years.
08563-3707 HIP 43880 = RST 2593. This is a nearby G1 dwarf (secondary perhaps late-K) which has moved by 106{deg} since its discovery in 1935. A preliminary orbit finds a period of about 160 years (Hartkopf & Mason 2011, Inf. Circ., 175).
08571-2951 HIP 43947+43946 = TOK 63. Both A and B are close binaries resolved at Gemini (Tokovinin et al., 2010AJ....140..510T) and confirmed here at the same positions. This is a quadruple G5V dwarf with an erroneous Hipparcos parallax of 26mas (the true parallax is about 10mas); the parallax error is likely caused by the companions, unknown at the time of the Hipparcos data reduction.
08589+0829 = GJ 3522 = DEL 2. This is a nearby M-dwarf pair with a 7.6 day spectroscopic subsystem (MSC). Orbital motion is quite rapid: with 5.7 year period (Table 4), the pair has completed 2.5 revolutions since its discovery in 1997.
09024-6624 HIP 44382 = TOK 197. This is a nearby HAeBe star and an astrometric binary (Makarov & Kaplan, Cat. J/AJ/129/2420). It is tentatively resolved here into a 0.032" pair. The reality of the elongation is supported by comparison with other stars observed before and after, but this could still be an artifact (unresolved on 2011.037).
09079-0708 HIP 44804 = TOK 64 Aa,Ab. This is another subsystem in a nearby triple G-dwarf discovered by Tokovinin et al. (2010AJ....140..510T). We see some motion since discovery; the estimated period is ~130 years.
09128-6055 HIP 45214 = HDO 207 AB. We corrected the orbit of the AB pair (Mason & Hartkopf 2011a). The subsystem CHR 144 Aa,Ab is unresolved here and in Tokovinin et al. (2010, Cat. J/AJ/139/743); it has never been confirmed.
09191-4128 HIP 45705 = CHR 239. This is a nearby G-dwarf binary with an estimated period ~10 years, also an astrometric and spectroscopic binary.
09194-7739 HIP 45734. This is a young quadruple system of spectral type G3 consisting of the 0.12" pair KOH 83 Aa,Ab resolved here and the SB2 subsystem in the component B, which was also observed and found unresolved.
09228-0950 HIP 45999 = A 1342. The companion C at 2" was outside the field, so not measured here.
09380-5924 HIP 47263. This is a nearby G-dwarf astrometric binary. A tentative companion at 329{deg}, 0.090", and {Delta}I=3.0mag was detected, but not accepted as real.
09387-3937 HIP 47328 = I 202. This is a nearby dwarf pair; the primary is F6V, the secondary about G4/5. Recent measures have shown large residuals from the orbit of Seymour et al. (2002, Cat. J/AJ/123/1023), so a new solution was attempted. Although still grade 4 ("preliminary"), the new elements predict a mass sum in excellent agreement with the spectral types.
09412+0954 HIP 47508 = HMM 1 Aa,Ab. This was unresolved in Tokovinin et al. (2010, Cat. J/AJ/139/743) and is marginally resolved here in the y filter only at a position roughly consistent with its orbit. The 0.6" companion ARI 1 Aa,Ac is not seen, it could be bogus.
09416-3830 HIP 47543 = TOK 198. This is a nearby G2V dwarf with variable RV. A new faint companion is found at 0.47", {Delta}I=4.5mag, unresolved in y. The estimated period of this system is ~100 years.
10000+2433 GJ 3580 = DH Leo = CHR 145. This is another nearby K-dwarf pair, with orbital period of 44 years similar to that found for CHR 219 (Table 4).
10028+0106 HIP 49217 = HDS 1451. This is triple, with a 0.4 day eclipsing subsystem Y Sex (MSC). Eclipse timing indicates a tertiary period of 58 years, probably too short for measured separation of 0.45".
10161-2837 HIP 50288 = TOK 199. This is a nearby chromospherically active G1V dwarf with variable RV, resolved here at 40mas.
10232+0542 HIP 50870. This is a nearby G-dwarf astrometric and spectroscopic binary. We detect a new faint companion at 1.07", {Delta}I=5.1mag. It is not clear if this is binary or a triple. The visual companion at 63" is optical.
10282-2548 HIP 51255 = B 199 + FIN 308. This comprises a resolved triple. The position angle of FIN 308 is different by ~180 deg from its ephemeris, but quadrant reversal is not allowed by the wide subsystem. We revise its orbit in Table 4.
10311-2411 HIP 51501 = B 201 AB. This is measured, but the subsystem CHR 132 is not resolved here and in Tokovinin et al. (2010, Cat. J/AJ/139/743). This may be a spurious component.
10370-0850 HIP 51966 = A 556 AB + TOK 44 Aa,Ab. This is a nearby triple G-dwarf. The inner Aa,Ab subsystem was first resolved by Metchev & Hillenbrandt (2009, Cat. J/ApJS/181/62). This pair has closed down from 0.43" in 2009 to 0.12" in 2010; its estimated period is ~10 years.
10465-6416 HIP 52701 = FIN 364 AB. This late-B pair, likely a member of the cluster IC 2602, contains a 5.5 day SB1 subsystem (MSC). The faint tertiary TOK 45 AC at 0.7" is confirmed.
10529-1717 HIP 53206 = HDS 1556. This is a nearby G-dwarf binary for which we compute the first 14.6 year orbit in Table 4. The one zero-weighted speckle measure was made with the USNO 26 inch, and is close to the resolution limit of that telescope.
11009-4030 HIP 53840 = FIN 365. This is a nearby F7-dwarf binary with a preliminary orbital period of 46 years (Table 4).
11102-1122 HIP 54580 = HDS 1590. This is a nearby early-G dwarf binary; the preliminary orbit (Table 4, P=20.6-years) indicates that it has completed one full revolution since its discovery.
11221-2447 HIP 55505 = I 507 AB. This is a post-main-sequence quadruple with 262 day and 315 day SB subsystems (MSC) which we do not resolve here. Its first orbit (Tokovinin, 1999AstL...25..669T) could now be improved.
11514+1148 HIP 57821 = HDS 1672. This was not resolved in Tokovinin et al. (2010, Cat. J/AJ/139/743) but now has opened up to 0.16". It is a nearby G-dwarf with an estimated period ~10 years.
13064+2109 HIP 63948 = COU 11 AB. This is resolved here, but the subsystem CHR 150 Aa,Ab is not. The closer pair was seen at 0.04" on 2009.26.
13081-6518 HIP 64094 = CHR 247 Aa,Ab. This is marginally resolved with 5 ms exposure time, although the measure could still be affected by vibrations. This is the Wolf-Rayet multiple system {theta} Mus, containing a 18 day SB2 (MSC).
13147-6335 HIP 64624. This is an O9V star known previously to be a visual triple. Both the 1.7" MLO 3 AB pair and the inner WSI 58 Aa,Ab subsystem were measured in Tokovinin et al. (2010, Cat. J/AJ/139/743) and here. However, we also see an additional faint peak in the two ACFs in the I-band. Figure 5 shows a fragment of two co-added ACFs where we attribute the faint peak to a new companion Bb. A rough measure indicates that the pair Ba,Bb has a separation of 0.32" and a position angle of 90{deg}, the magnitude difference could be around 3m (6m with respect to Aa). The new companion must be redder than the other stars, otherwise it would be seen in the y band. This object is on the list of O-stars surveyed by Mason et al. (2009, Cat. J/AJ/137/3358).
13175-4033 HIP 64835 = I 425. Although a quite close pair, the motion illustrated in Figure 4(b) suggests that the two components are not physically related. The two stars are predicted to reach a minimum apparent separation of only 166mas in 2034.
13276+2116 HD 117078 = TOK 46. This is a quadruple system comprising two SBs (5.5 days and 204 days), first resolved in Tokovinin et al. (2010, Cat. J/AJ/139/743). The separation and observed motion (12{deg} in two years) agree with the 36 year period estimated spectroscopically by Griffin (2005, Proc. 13th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (ESA SP-560), ed. F. Favata, G. A. J. Hussain, & B. Battrick (Noordwijk: ESA), 595).
13317-0219 HIP 65982 = HDS 1895. This is a late-G (plus mid-K?) dwarf pair and SB1 with a very fast direct motion. We combined interferometric measures with the spectroscopic data of Latham et al. (2002, Cat. J/AJ/124/1144) which are truly complementary. The 3.24 year period is confirmed, the eccentricity is somewhat less than in the SB orbit. The new orbit can be considered very reliable. The Hipparcos measure had to be ignored for obvious reason: although the star was indeed resolved, it moved substantially during the Hipparcos mission. The fitted separation and angle are reasonable, but their attribution to the average epoch 1991.25 makes no sense. Re-reduction of Hipparcos data with the new orbit can lead to a better parallax measurement. Campbell elements are given in Table 4; the additional spectroscopic elements are K1=2.80+/-0.13km/s, V0=-51.13+/-0.07km/s.
13527-1843 HIP 67744 = WSI 78. This has moved by 32{deg}since its first resolution in 2008. It is a spectroscopic triple (Carquillat & Prieur, 2007AN....328..527C) containing the 1.3 day eclipsing system DL Vir. A very preliminary combined solution was made of the 6.2 year period outer pair; Campbell elements are in Table 4, while the spectroscopic elements are K1=17.45+/-0.34km/s, V0=-22.25+/-0.17km/s.
15313-3349 HIP 76001 = B 2036 AB + HWE 78 AC. This forms a visual triple with comparable separation, 0.36" and 1.46". An orbit for the AB pair yields a period of 235 years, although with considerable uncertainty.
16385-5728 HIP 81478 = V841 Ara = RST 869 AB + TOK 51 Aa,Ab. This is a resolved visual triple at 50 pc from the Sun. The companion B is a hot white dwarf (Wray et al., 1979ApJ...234L.187W) and an X-ray source. Its motion hints at an orbital period on the order of 103 years. The closer Aa,Ab subsystem was discovered in 2009 (Tokovinin et al., 2010, Cat. J/AJ/139/743) and is also measured here in the I band, where it is brighter than B ({Delta}IAa, B=4.7mag, {Delta}IAa, Ab=2.7mag). Therefore the Ab companion is a red dwarf with estimated orbital period ~20 years.
16391-3713 HIP 81523 = FIN 340. This is approaching periastron (predicted for mid-2015) with direct motion. The early eyepiece interferometric measures were given zero weight for this preliminary solution with P=47-years (Table 4).
22116-3428 HIP 109561 = BU 769 AB. We measure only the pair AB; the 0.04" subsystem CHR 230 is unresolved here but it was seen in 2008 at 0.05".
22181-0014 HIP 110091 = CHR 107. This is resolved at 0.04". Only one measure is listed in the WDS for this nearby binary G-dwarf with estimated period ~10 years.
22288-0001 HIP 110483 = {zeta} Aqr. This is composed of a 2.2" visual binary STF 2909 AB with unseen astrometric companion on a 25 year orbit. The companion was tentatively resolved in Tokovinin et al. (2010PASP..122.1483T), where the A and B components were observed separately and a feature was detected around B. Going back to our logs, we found that A and B were swapped, so the subsystem detected actually belongs to the A-component, and is now designated TOK 201 Aa,Ab. We can see this companion in the direct shift-and-add (SAA) images after subtracting the rotationally averaged point-spread function (PSF) (Figure 6). This object was observed again, this time A and B together in a wider 6" field. In 2010 November the images were AO-corrected. By subtracting a suitably scaled and shifted image of the B component from the image of A, we can see the Ab clearly (Figure 6). The SAA post-processing of the AO-corrected images (selection of 50% sharpest frames and re-centering on maximum intensity) was done to enhance the resolution (before PSF subtraction). The B/A scaling corresponds to {Delta}I=0.271mag. The subsystem Aa,Ab was also detected in the ACFs recorded in December and January (without AO correction). In this case the measurement of Aa,B and Aa,Ab is done by fitting the triple-star model, as in Tokovinin et al. (2010, Cat. J/AJ/139/743). Owing to the anisoplanatism, the magnitude difference between A and B is grossly exaggerated in this case. The companion Ab shows retrograde motion between 2009 and 2010. Its position and displacement are in broad agreement with the astrometric orbit of Heintz (1984ApJ...284..806H), as noted in Tokovinin et al. (2010PASP..122.1483T). Three elements of this orbit were modified to fit the data: periastron epoch T=2004.0 (instead of 1981.2), semimajor axis a=0.33", and 180{deg} is added to the position angle of nodes. Figure 7 compares the orbit with measurements. We conclude that the resolution of the astrometric subsystem in Tokovinin et al. (2010PASP..122.1483T) was real, but we erroneously attributed it to B, whereas it belongs in fact to A. This confirms the thesis of Heintz (1984ApJ...284..806H) that all previous resolutions were bogus. See further discussion in Tokovinin et al. (2010PASP..122.1483T).