01379-8259 HIP 7601 is a nearby (27pc) dwarf also known as GJ 67.1 or HR 512. According to Wichman et al. (2003A&A...400..293W), it is a young spectroscopic triple detected in X-rays (1RXS J013755.4-825838). GCS also recognized the star as SB2. Spectroscopic monitoring (A. Tokovinin 2015, in preparation) shows that all three components are similar stars of approximately one solar mass. Here we resolved the outer subsystem AB and observed its fast motion. In fact it was already resolved at SOAR on 2011.036 at 221.0{deg} and 0.044'', but this low-quality observation has not been published. The available data indicate that the period of AB is 1.7years; the pair completed nearly two revolutions since its first resolution in 2011.
02098-4052 HIP 10096 is SB2 according to GCS. The separation corresponds to a period of ~5years.
03046-5119 HIP 14307 and 14313 form the 38'' pair DUN 10 AB belonging to the FG-67 sample. The component B is resolved here at 0.19''. The estimated period of Ba,Bb is ~25 years. No motion is seen in 2 months. The subsystem Ba,Bb is also manifested by asymmetric line profiles (A. Tokovinin 2015, in preparation). The A component has never been observed at high angular resolution.
04386-0921 HIP 21265 is an X-ray source and an SB2 according to GCS (one observation only). It is resolved here at 56mas, which corresponds to a period of ~5 years.
04469-6036 First resolution of HIP 22229 at 0.043'', {Delta}I=1.2. The measure is uncertain, but the elongation is confirmed with 2ms exposure and is not seen in other observed stars, so it is not caused by vibration. This is a triple system containing an eclipsing binary AL Dor of Algol type with an eccentric orbit (Bulut & Demirkan 2007, cat. J/MNRAS/378/179). The separation implies an orbital period of the outer system on the order of 5 years.
05354-0450 This is HIP 26237, HD 37018, HR 1892, 42 Ori, a young star in Orion which has not been observed at high angular resolution so far, according to INT4. We resolved the known binary AB=DA 4 and discovered the spectacular subsystem Aa,Ab at 0.16'' (Figure 2).
06303-5252 HIP 30995 is an SB2 according to GCS. The new companion at 0.2 with {Delta}I=4.1mag is unlikely to correspond to the SB2, so the system is probably triple.
06497-7433 HIP 32735 has an acceleration detected in HIP2, but no radial velocity data. The resolved 0.3'' pair implies a period of ~80 years. The spectral type K0IV given in SIMBAD may be inaccurate because the luminosity and color of the components correspond to main sequence stars with masses of 1.0 and 0.6M_{Sun}_.
06499-2806 The 0.2'' pair HDS 947 had not been observed since its discovery by Hipparcos. Here it is revealed as a triple system (Figure 2) with comparable separations between components. HDS 947 probably corresponds to AB, while the fainter C component is new.
07038-4334 HIP 34052=HD 53680=HIP 34065C=GJ 264 is a spectroscopic and astrometric binary for which Sahlmann et al. 2011 (cat. J/A+A/525/A95) give an orbit with P=1688days=4.62years and an estimated semi-major axis of 0.15''. There is also an astrometric orbit (Makarov et al., 2008ApJ...687..566M) with P=4.11years that predicts {theta}=327{deg} for the moment of our first observation. The binary is resolved at 0.23'', {Delta}I=4.4mag and shows some orbital motion. The binary makes a quadruple system together with components A and B (GJ 264.1 and 264) that form a 20.5'' pair at 185'' from C. The B component was also observed here and found unresolved.
07294-1500 is another nearby multiple system. The main component HIP 36395 is a visual binary with a known 728-year orbit, also measured here. The C component (NLTT 17952) at 20.4'' is physical, and yet another CPM component F is found at 1072'' (Tokovinin & Lepine 2012, cat. J/AJ/144/102), while the WDS components D and E are optical. We observed C and resolved it at 0.09''. The orbital period of Ca,Cb is on the order of 6 years, estimated masses are 0.6 and 0.4M_{Sun}_. We also targeted F and did not resolve it. The magnitudes and colors of C and F are quite similar.
07304+1352 is a quadruple system. The 7farcs7 pair AB (STF 1102) is HIP 36485, the CPM component D=HIP 36497=HD 59450 is located at 112'' from it, while the WDS components C and E are optical. The physical nature of AD is established by common PM, distance, and radial velocity. D is a known SB1 with P=2708days=7.4years (Halbwachs et al. 2012, cat. J/MNRAS/422/14) and an estimated semi-major axis of 93mas, also an acceleration binary. We resolved the Da,Db pair at 0.11'', {Delta}I=2.6. The minimum mass of Db derived from its SB orbit is 0.27M_{Sun}_, while we estimate the masses of Da and Db as 1.05 and 0.6M_{Sun}_ from their luminosity. A previous non-resolution of D is reported in INT4; it was also unresolved with Robo-AO (Riddle et al. 2015, cat. J/ApJ/799/4).
07312+0210 HIP 36557=HD 59688. According to observations by D. Latham (2012, private communication), this is a spectroscopic triple with an inner period of 70 days (double-lined, also detected by GCS, mass ratio 0.7) and an outer period of 2007 days or 5.5 years. The outer system is also detected by astrometric acceleration (Makarov & Kaplan 2005, cat. J/AJ/129/2420). We resolve it here at 0.057'', {Delta}I=2.0, {Delta}y=2.5mag, and see the orbital motion. The estimated mass of Ab is 0.88M_{Sun}_. The semi-major axis of the 70 days inner binary Aa,Ab is 7 mas, so accurate measurements of AB can detect the sub-motion to determine the orientation of the inner orbit.
08021-1710 This is the high-PM M-dwarf LP 784-12 (HIP 39293) at 30pc from the Sun. A new distant component C was found at 1.8'' in addition to the known pair HDS 1140 which closed from 0.4'' in 1991.25 to 0.33'' now (Figure 2). It is confirmed as physical by its fixed position during one year, the quadrant of the triple was determined in run 5.
08447-2126 Like the previous object, the late-type nearby binary HDS 1260 was discovered by Hipparcos and is expected to move rapidly (HIP 42910, BD-20{deg} 2665). It was targeted at SOAR for the first time. To our surprise, the object turned out to be a resolved triple, with the secondary being a 0.16'' pair of equal stars (Figure 2). Hipparcos failed to recognize the triple nature of this star. The estimated period of BC is 15 years. The outer pair AB has closed from 0.8'' to 0.5'' and moved in position angle since its discovery. The separations between components are comparable, so this triple system may be interesting dynamically.
09299-3629 HIP 46572 is called a "high proper motion star" in SIMBAD, although its PM and radial velocity are actually quite moderate. The binary AB has moved little in the 24 years since its resolution by Hipparcos. We discover the subsystem BC (Figure 2) with an estimated period of ~100 years.
09586-2420 HIP 48906 is a double-lined binary according to the GCS, first resolved here at 64mas. The period should be ~20 years.
10056-8405 HIP 49442=HD 88948 is a nearby dwarf in the 3.9'' visual binary HJ 4310 AB. According to GCS, the radial velocity of the main component A varies by 3.5km/s. Here it is resolved into a 0.18'' Aa,Ab pair with an estimated orbital period of 25 years. No astrometric acceleration was detected, however. The visual secondary B was targeted separately and found unresolved.
10070-7129 HIP 49546 is an astrometric binary of 1.5 year period (Goldin & Makarov, 2006ApJS..166..341G) with variable radial velocity. The period corresponds to a semi-major axis of 25mas. The star is resolved here tentatively at 26mas (with 2ms exposure). This resolution is below the diffraction limit and needs confirmation. The measured position angle of 346{deg} is close to 342{deg} predicted by the astrometric orbit.
10223-1032 HIP 50796 is a single-lined and astrometric binary according to Torres (2006AJ....131.1022T), with a period of 570.98 days (1.56 years), K1=20.76km/s, e=0.611. The Hipparcos parallax corrected for the binary motion is 20.6+/-1.9mas. The spectroscopic secondary companion is over-massive, most likely a close pair of M-dwarfs. If so, the new speckle companion at 1.66'' with a period on the order of 500 years makes the system quadruple. The speckle companion might contribute to the IR excess found by Torres. The system is an X-ray source, and is possibly young.
10530+0458 D. Latham (2012, private communication) identified HIP 53212=HD 94292 as SB2 with a period of 8.3 years and a highly eccentric orbit. It is resolved here securely at 50mas.
12176+1427 HIP 59933 has a variable radial velocity according to GCS. The 32mas separation corresponds to an orbital period of ~2 years. However, the separations in the y and I filters are somewhat discordant; further confirmation is needed.
12250-0414 HIP 60574 is a spectroscopic triple with periods 14 days and 22 years (D. Latham 2012, private communication), also an acceleration binary. We resolved the outer pair at 0.22'' separation, matching the spectroscopic period. The lines of the visual secondary Ab could potentially be detected in the spectrum by cross-correlation, leading eventually to a full 3D orbit.
12528+1225 HIP 62933 (41 Vir) was observed on request by F. Fekel who studies its spectroscopic orbit. Apparently it is resolved for the first time.
13132-0501 HIP 64499 has a variable radial velocity, with a preliminary spectroscopic orbit of 17 years period (D. Latham 2012, private communication). It is resolved at 0.1'' and shows no motion in one month.
13321-1115 No previous indication of binarity was available for HIP 66018, apart from the CPM companion B at 84''. We discovered another faint component Ab at 0.89'', {Delta}I=4.6, likely to be physical (low background density). The B component (V=14.8) was targeted, but its speckle signal was weak and no obvious close companions to B were found.
13344-5931 HIP 66230 has a variable radial velocity in the GCS and an astrometric acceleration. We resolved it at 0.1'', {Delta}I=2.5, estimated period ~10 years. The pair moved by 4{deg} in one month.
13382-2341 HIP 66530 has a variable radial velocity according to the GCS. It is resolved at 0.16'' in the I band only, estimated period ~20 years. This is a triple system, considering the CPM companion B at 28'' (LDS 4385 AB).
13401-6033 HIP 66676 (A) and HD 118735 (B, G6V, V=9.17) at 77'' share common proper motion (although it is small, 58mas/yr) which, together with photometry, indicates with high probability that it is a physical pair AB (Tokovinin & Lepine 2012, cat. J/AJ/144/102). We targeted the secondary component B and found it to be a resolved triple. The faint star C, at 0.92'' from B, is itself a close 0.16'' pair Ca,Cb (Figure 2). Note that this is a region of the sky with very high stellar density, raising suspicion that the Ca,Cb pair might be a random background object. Re-observation of the triple in 2015 (to be published) shows, however, that it is physical because the center of C=(Ca,Cb) moves relative to B with a speed of 11mas/yr (or 3km/s), compatible with the expected orbital motion of BC and much less than the system's proper motion of 58mas/yr. The estimated period of Ca,Cb is ~30 years, the period of BC is ~300 years.
13495-2621 HIP 67458 is a double-lined chromospherically active binary with orbital period of 7.2 days (D. Latham 2012, private communication). We found a faint tertiary companion at 0farcs73 with an estimated orbital period on the order of 100 years. The speckle survey of chromospherically active stars by Mason et al. (1998AJ....116.2975M) did not detect this tertiary, lacking the dynamic range of HRCam.
14014-3137 HIP 68507 is an acceleration binary with a variable radial velocity resolved here at 0.06''. The period of Aa,Ab is on the order of 5 years. There is a faint physical companion B at 6.7'' found in 2MASS (Tokovinin 2011, cat. J/AJ/141/52). Another visual companion at 14'', SEE 195, is optical, as revealed by its fast relative motion.
14382+1402 HIP 71572 is an acceleration binary without radial velocity data. It is found to be a tight 90mas pair with a small {Delta}m and an estimated period under 10 years (some motion is seen in one month). Very likely it can be studied as a double-lined SB.
14464-3346 HIP 72235B is located at 9'' from the primary star and shares its proper motion (AB=HDS 2082). Pre-discovery measurements of this Hipparcos pair were published by Wycoff et al. 2006 (cat. J/AJ/132/50). The radial velocity of A may be variable (D. Latham 2012, private communication). The star B turns out to be a 0.4'' binary Ba,Bb with masses of 0.70 and 0.17M_{Sun}_ estimated from the luminosity. Its period is on the order of 100 years. The whole system could thus be quadruple.
15362-0623 HIP 76400 is identified by the GCS as an SB2 with a mass ratio q=0.93, but there is no spectroscopic orbit available. We resolved the 0.19'' pair with {Delta}I=3.9, indicating a mass ratio of ~0.5 and an orbital period of ~30 years. Very likely the resolved binary does not match the spectroscopic double-lined system. Considering the CPM component B at 80'' (Tokovinin & Lepine 2012, cat. J/AJ/144/102), this system could be a quadruple with a 3-tier "3+1" hierarchy.
15367-4208 HIP 76435 is a G5V star from the FG-67 sample. Its companion C (AC=FAL 78) at 13.5'' is physical, while the Hipparcos companion B at 4.3'' is not seen in the 2MASS images and has not been confirmed otherwise. We targeted C and resolved it into a close binary. Estimated masses of Ca and Cb are 0.70 and 0.66M_{Sun}_, period ~4 years.
16142-5047 HIP 79576 has a variable radial velocity (GCS). The 79mas separation implies an orbital period of ~5 years. This is the high-PM star LTT 6467 with a low metallicity [Fe/H]=-0.78. Ivanov et al. (2013A&A...560A..21I) found no CPM companions.
16195-3054 HIP 79980 and HIP 79979 form a 23'' CPM pair AB where the F6III primary is slightly evolved, while the G1/G2 secondary is closer to the main sequence, but still above it. The Hipparcos parallax of B, -4.7mas, is obviously wrong, so we assume the parallax of the primary, 20.7mas. The radial velocity(B) is variable (GCS), and we resolve it into a 40mas pair with an estimated period on the order of 1 year. The pair moved by 10{deg} in a month. Binary motion is the likely cause of the incorrect Hipparcos parallax.
16454-7150 HIP 82032 is located in a crowded field, so the new faint Ab companion found here at 1.3'' could be optical. The star was observed because of its suspected variable radial velocity (GCS), but the newly found companion, even if physical, is too distant to explain this variability. Another visual companion B at 11.5'' (AB=B2392) is optical, as evidenced by its fast relative motion. The star is on the HARPS exo-planet program.
16563-4040 HIP 82876 is a distant O7V star. The 0.26'' pair AB (HDS 2394) was measured among other neglected binaries. We found another faint companion C at 1.46'' (Figure 2). The star has an extensive literature, including multiplicity surveys with speckle interferometry and radial velocity (Chini et al. 2012, cat. J/MNRAS/424/1925). Owing to the large distance, no detectable orbital motion is expected. Indeed, the AB pair was measured with HRCam in 2008.5 at the same position as it is now. Those observations in the y band did not detect the companion C owing to a lower signal-to-noise ratio.
17054-3346 The radial velocity of HIP 83612 varies by 52km/s (GCS). It is a very close pair with an estimated period of ~1.5 years, and the measure near the diffraction limit derived from the elongated power spectrum is tentative. The Hipparcos parallax is likely biased by the binary. The visual component B = HIP 83609 (AB=WNO5) at 25'' is optical.
17098-1031 HIP 83962=HR 6375 has a variable radial velocity according to the GCS, while N. Gorynya (2013, private communication) detected double lines. It is resolved tentatively at 33mas with {Delta}y=1.8mag (the 5ms exposure makes it unlikely that the asymmetry is caused by vibrations). The separation corresponds to an orbital period on the order of 1 year, which could bias the Hipparcos parallax. However, Eggleton & Tokovinin 2008 (cat. J/MNRAS/389/869) consider the star as single. The new pair was not resolved in 2014.3; presumably it became closer.
17264-4837 HIP 85342 and HIP 85326 form a physical pair AB at 127'' separation (common proper motion, radial velocity, and parallax). The B component=HIP 85326 has a variable radial velocity and an astrometric acceleration which could hardly be produced by the 1'' speckle companion Bb found here, owing to its long estimated period of ~300 years. It seems that B is triple and the whole system is quadruple. This companion Bb was not detected in the previous speckle observations because it is red: {Delta}I=2.4, {Delta}y=4mag; its color matches a dwarf star at the same distance as the system. However, the field is crowded and the newly found companion could still be optical.
17266-3258 HIP 85360 is an acceleration and spectroscopic binary. Its preliminary spectroscopic period (D. Latham 2012, private communication) corresponds to a semi-major axis of 80mas. The star is chromospherically active and possibly young. The faint companion found here at 1.16'' is most likely optical, as the field is extremely crowded. Re-observation within a year will resolve its status.
17341-0303 HIP 85963 has a variable radial velocity and is an acceleration binary. The 91mas separation implies an orbital period of ~10 years; the estimated masses are 1.37 and 0.81M_{Sun}_. Despite extensive literature (51 references in SIMBAD), there is no published spectroscopic orbit, while several high-resolution spectroscopic studies addressed the abundance.
17342-1910 B 1863 is a known close binary which has been unexpectedly found to be a triple (Figure 2). The new distant component C is detectable also in the y filter, but we measured only the inner binary in y. The star was observed at the Blanco telescope in 2008.5397, and the pair actually measured then was AC, at 133.8{deg}, 0.217'', {Delta}y=3.7 (same as now, see Table 2). The inner pair AB with a smaller {Delta}m was unresolved in 2008.5, while it is clearly resolved now. Owing to the large distance from the Sun, we expect only a slow motion, so even the inner pair observed since 1929 may not yet be ready for computing its first orbit.
17342-5454 HIP 85969 has a variable radial velocity according to the GCS and confirmed by Jones et al. (2002MNRAS.337.1170J). The 0.55'' separation implies a period on the order of 80 years. The star is on the exo-planet program at the Anglo-Australian Telescope.
18243-0405 The neglected pair YSC 67 turned out to be a new triple (Figure 2). The outer 0.35'' binary AB was known previously, now we detect elongation that implies an inner subsystem Aa,Ab. We compared with stars in the same area of the sky observed before and after to assure that the elongation is not of instrumental origin; it is seen in two filters.
18267-3024 HIP 90397 is an acceleration binary with a variable radial velocity (GCS), resolved here at 69mas (estimated period ~4 years). The star is targeted by exo-planet programs.
18346-2734 HIP 91075 was noted as a double-lined binary by the GCS (one observation only). The separation of 86mas implies a period of ~10 years, while the double-lined observation matches the moderate magnitude difference (estimated masses 1.04 and 0.77M_{Sun}_). The star is an X-ray source, so a future combined orbit could determine masses for testing evolutionary models of young stars. The sky around the object is quite crowded; the 9'' companion I 1026 is optical (it moves too fast).
19206-0645 HIP 95068 is the neglected Hipparcos binary HDS 2735 AB, a distant K-type giant. We did not resolve this 0.1'' binary, which remains unconfirmed, but detected instead another faint star at 1''. The stellar background is crowded, the proper motion is small, and the status of the new companion remains uncertain.
19209-3303 HIP 95106 and 95110 form the 13.7'' pair HJ 5107 AB. The radial velocity variability of A was suspected by the GCS, it is now resolved as a 0.27'' binary with estimated period of ~35 years. The component B was also observed and found unresolved. It contains a spectroscopic pair (A. Tokovinin 2015, in preparation), the whole system is quadruple.
19221-2931 HIP 95203 is another acceleration binary with variable radial velocity resolved here. The relatively large separation of 0.77'' corresponds to a period of ~180 years. The actual period can be as short as 60 years if the pair is seen now near its maximum separation (it would then have been closer at the time of the Hipparcos mission). Most likely, however, the faint visual companion found here and the spectroscopic/acceleration pair make a triple system. There is another companion HIP 95164 at 435''. The status of this wide pair (is it a real binary or just two members of a moving group?) is not clear, but the association of those stars leaves no doubt (common radial velocity, proper motion, and parallax).
19409-0152 HIP 96834 has a spectroscopic orbit with a period of 1 year and expected semi-major axis of 27mas (D. Latham 2012, private communication). We resolved this pair, although the measurement near the diffraction limit is uncertain. However, there are some unsolved questions. Why, despite the small magnitude difference {Delta}y=1.2mag, were double lines not seen? Why, despite the 1 year period, was the Hipparcos parallax not strongly affected and the star appears to be on the main sequence?
19453-6823 We resolved the secondary component of HDS 2806 AB into a close pair Ba,Bb (Figure 2). This is a K3 dwarf within 50pc from the Sun. The pair Ba,Bb should be fast and turn around in about 10 years.
22259-7501 HIP 110712 and 110719 form the 20.6'' pair DUN 238 AB. We observed both components. The A component has a variable radial velocity according to the GCS, but not confirmed by Jones et al. (2002); it was unresolved. The newly found pair Ba,Bb has a period on the order of 10 years. Considering the distant companion C found by Caballero (2012Obs...132..176C), the system contains at least 4 stars.
04163-0710 WSI97 is a single-lined nearby binary. Using the radial velocities measured by D. Latham (2012, private communication), we computed a combined orbit (the previous visual orbit reported by Riddle et al. 2015 (cat. J/ApJ/799/4) had a wrong period). The inclination is close to 180{deg} and had to be fixed in order to match the radial velocity amplitude. The complete orbit including radial velocities will be published later.
04506-1505 CHR20 is a Hyades binary for which Griffin (2012JApA...33...29G) published an SB2 orbit. We combined his radial velocities with the speckle data, resulting in a very accurate period. The combined orbit corresponds to a mass sum of 2.1M_{Sun}_ and an orbital parallax of 22mas, in good agreement with the HIP2 parallax of 23.69+/-0.87mas.
05245-0224 MCA18 Aa,Ab has an SB1 orbit with P=9.44years. The orbit given here uses only the speckle data, however.
07490-2455 The period of TOK194 matches the astrometric orbit of Goldin & Makarov (2007ApJS..173..137G). The mass sum in this pair composed of a giant primary and possibly an A-type secondary is 5.9M_{Sun}_. The measure on 2011.93 was ignored as spurious (it was affected by vibrations).
07522-4035 TOK195 is the bright star a Pup (HD64440, HR3080) known as a spectroscopic binary. However, examination of the radial velocity data reveals that the orbit by Parsons (1983ApJS...53..553P) is only approximate. The binary is difficult to measure, always close to the diffraction limit and with {Delta}m~3. Instead of the spectroscopic period of 6.99years, our orbit has P=7.4years and is still preliminary. More radial velocity coverage is obviously needed.
08391-5557 HU1443 A,BC is a triple system. We provide the first very tentative orbit for the outer binary, but note its large residuals from the recent measures of AB. Strictly speaking, the orbit should describe the motion of the center-of-gravity of BC around A, rather than the measures of AB. Such refinement was made for the orbit of A 2592 AB (17156-0949), but it is not warranted for this preliminary orbit.
10161-2837 TOK199 is marked as an SB2 in the GCS, while D. Latham (2012, private communication) derived an orbital period of 916 days, now independently confirmed by our orbit (Figure 4).
17157-0949 This is the triple system HIP84430. We computed the first orbit of the secondary subsystem Ba,Bb which was discovered at SOAR in 2009 and has just completed one full revolution since. Its separation is always close to the diffraction limit. Adopting a mass sum of 2.6M_{Sun}_ for Ba,Bb, the resulting dynamical parallax is 7.6+/-1.5mas, while the HIP2 parallax is 4.9+/-0.9mas. The latest orbit of the outer pair A 2592 AB published in Tokovinin et al. 2014 (cat. J/AJ/147/123) does not account for the fact that the speckle measurements at SOAR refer to A,Ba and not to AB. Here we give a more accurate solution that uses the positions of AB computed from the measures of A,Ba under the assumption that Ba and Bb have equal masses. After this correction and orbit adjustment, the weighted residuals are 4.3mas in separation and 1.3{deg} in angle. Interestingly, there were a considerable number of speckle interferometry measures of this pair obtained in the 1980s and 1990s at 4m telescopes, but none of them recognized the subsystem Ba,Bb, despite its small {Delta}m.