518 123 Triple. This system is composed of a 107 year visual-orbit 518 123 pair, the secondary of which was shown to be the more massive 518 123 component from absolute astrometry (Griffin, 1999Obs...119...27G), 518 123 suggesting that it itself was an unresolved binary. Brettman et al., 518 123 1983IBVS.2389....1B reported a periodic variation in the component's 518 123 brightness over roughly a 1 day period, which Griffin 518 123 (1999Obs...119...27G) later disproved based on Hipparcos photometry 518 123 and instead showed it to be a spectroscopic binary with a 47.7 day 518 123 period, estimating component masses of 0.98, 0.95, and 0.22M_{sun}_ 518 123 for the three components. 1292 1237 Binary, one planet. In a systematic search for faint companions to 1292 1237 planet hosts, Chauvin et al. (2006A&A...456.1165C) discovered a CPM 1292 1237 companion to this star using VLT NACO adaptive optics (AO) and 1292 1237 demonstrated orbital motion. Chauvin et al. (2007A&A...475..723C) 1292 1237 characterized the companion as M4+/-1V. 3093 3651 Binary, one planet. Luhman et al. (2007ApJ...654..570L) reported the 3093 3651 discovery of a T7.5+/-0.5 companion 43" away from this planet-host 3093 3651 star using Spitzer Infrared Array Camera (IRAC) images, and confirmed 3093 3651 CPM using 2MASS images. The brown dwarf's infrared colors are 3093 3651 consistent with the distance to the primary, confirming 3093 3651 companionship. They estimate the companion's mass as 3093 3651 0.051+/-0.014M_{sun}_ and age as 7+/-3Gyr by comparing luminosity 3093 3651 with evolutionary tracks. This was the first substellar object imaged 3093 3651 around an exoplanet host. An additional component listed in the WDS 3093 3651 is clearly optical (see Table 6). 3583 4391 Triple. The WDS lists three measurements of a companion with 3583 4391 separations ranging 10.0"-16.6" over 98 years, and we discovered an 3583 4391 additional companion 49" away by blinking archival images (see 3583 4391 Section 3.1.1). Our VRI images, obtained in 2007 July and October at 3583 4391 the CTIO 0.9m telescope, clearly reveal both companions, confirming 3583 4391 CPM. The closer companion was saturated in all but one V-band image, 3583 4391 but the differential photometry extracted from this image allowed 3583 4391 confirmation as a companion (see Table 10). For the newly discovered 3583 4391 wider companion, our absolute VRI photometry along with 2MASS JHKS 3583 4391 magnitudes confirmed a physical association (see Table 5). 3765 4628 Single, candidate Binary. Heintz & Borgman (1984AJ.....89.1068H) 3765 4628 detected a companion, 2.7" away, on 11 exposures over two nights, 3765 4628 but did not see the companion on 164 other plates or on multiple 3765 4628 visual checks with a micrometer. Their two observations about 25 days 3765 4628 apart show evidence of variation in the companion's brightness by 3765 4628 about 1 mag. Heintz (1994AJ....108.2338H) notes an acceleration in 3765 4628 proper motion for the primary and speculates that this might be 3765 4628 caused by the companion reported earlier. Roberts et al. 3765 4628 (2005AJ....130.2262R) did not detect a companion using AO down to 3765 4628 {Delta}I<~10 and note that only a white dwarf companion could have 3765 4628 escaped detection, while the flaring companion as seen by Heintz 3765 4628 should have been detected. Moreover, the Hipparcos and Tycho-2 proper 3765 4628 motions of HD 4628 match to within 2{sigma}, and the INT4 3765 4628 (http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/int4) 3765 4628 lists several null results with speckle interferometry and AO. 3765 4628 B.D.M. and D.R. observed this target using the KPNO 4m telescope in 3765 4628 2008 June, and while the separation was too wide and the {Delta}m too 3765 4628 large for speckle observations, the finder TV showed a faint source 3765 4628 about 5" away at about 230{deg}. Could this be the companion seen by 3765 4628 Heintz after about 30 years of orbital motion? While a possibility, 3765 4628 follow-up observations by Elliott Horch 2 days later with the WIYN 3765 4628 3.6m telescope on KPNO failed to identify the source. Additionally, 3765 4628 5s exposures in VRI taken by T.J.H. at the CTIO 0.9m telescope in 3765 4628 2008 June also failed to identify any companion, although saturation 3765 4628 around the primary could hide the companion in these images. Nidever 3765 4628 et al. (2002ApJS..141..503N) report that the primary shows no 3765 4628 variations in its radial-velocity measurements. At this time, we do 3765 4628 not have sufficient information to confirm or refute this companion, 3765 4628 although, chances of a physical companion appear slim. The wider 3765 4628 component listed in the WDS is clearly optical (see Table 6). 3810 4676 Binary. Boden et al. (1999ApJ...527..360B) presented a visual orbit 3810 4676 based on LBOI observations for this 14 day SB2 and derived component 3810 4676 masses of 1.223+/-0.021M_{sun}_ and 1.170+/-0.018M_{sun}_. Earlier, 3810 4676 Nadal et al. (1979A&AS...35..203N) had speculated on the presence of 3810 4676 a third companion based on temporal changes in the spectroscopic 3810 4676 orbital elements. While this suspected companion has been mentioned 3810 4676 in subsequent literature (Fekel, 1981ApJ...246..879F; Tokovinin et 3810 4676 al., 2006A&A...450..681T), it was refuted by Boden et al. 3810 4676 (1999ApJ...527..360B) based on imaging and spectroscopic evidence. 3810 4676 Two additional components listed in the WDS are clearly optical (see 3810 4676 Table 6). 7513 9826 Binary, three planets. Lowrance et al. (2002ApJ...572L..79L) 7513 9826 discovered an M4.5V companion, 55" away from planet host u And and 7513 9826 confirmed its physical association by demonstrating CPM and showing 7513 9826 that its spectral type is consistent with its magnitudes at the 7513 9826 primary's distance. Two additional components listed in the WDS are 7513 9826 clearly optical (see Table 6). 10138 13445 Binary, one planet. This planet-host star with a 4MJ planet exhibits a 10138 13445 long-term trend in radial velocity, consistent with a stellar 10138 13445 companion beyond 20AU (Queloz et al., 2000A&A...354...99Q). A 10138 13445 significant difference between the Hipparcos and Tycho-2 proper 10138 13445 motions (see Table 8) also suggests a nearby unseen companion. Later 10138 13445 work has resolved this companion and demonstrated orbital motion 10138 13445 (Lagrange et al., 2006A&A...459..955L). The companion was initially 10138 13445 misidentified as a T dwarf (Els et al., 2001A&A...370L...1E) and 10138 13445 later shown to be a white dwarf based on spectroscopy (Mugrauer & 10138 13445 Neuhauser, 2005MNRAS.361L..15M) and a dynamical analysis of 10138 13445 astrometry and radial velocities (Lagrange et al., 10138 13445 2006A&A...459..955L). 14879 20010 Binary, candidate Triple. The secondary of a 5" CPM pair with a 14879 20010 preliminary visual orbit is listed in the CNS (1969VeARI..22....1G) 14879 20010 as "RV-Var?". Eggen, 1956AJ.....61..405E, mentions that there is a 14879 20010 strong evidence of variability, quoting a 1928 publication by van 14879 20010 den Bos, but this reference could not be found. With insufficient 14879 20010 evidence to confirm or refute a physical association, the additional 14879 20010 companion is retained as a candidate. 15371 20807 Binary. The wide CPM companion, HD 20766, lies 309" away and is 15371 20807 confirmed by matching proper motions and parallax. Additionally,the 15371 20807 WDS lists a single speckle interferometry measure of a companion in 15371 20807 1978, 0.046" away at 11{deg} (Bonneau et al., 1980A&AS...42..185B). 15371 20807 However, Bonneau et al. failed to resolve the companion in 1979 and 15371 20807 da Silva & Foy (1987A&A...177..204D) mention that the 1978 measure 15371 20807 was in fact an artifact in the diffraction pattern of the telescope 15371 20807 spider. 15799 21175 Binary. While this companion only has three ground-based measurements, 15799 21175 they span more than 50 years and are consistent with a bound pair. 15799 21175 The Hipparcos catalog (Cat. I/239) also identifies this star as a 15799 21175 suspected binary because the astrometry did not adequately fit either 15799 21175 a single or binary solution (H59="X"). Soderhjelm 15799 21175 (1999A&A...341..121S) presents a visual orbit combining Hipparcos and 15799 21175 ground-based measures, confirming a physical association. 16537 22049 Single, one planet. This is epsilon Eri, the well-studied exoplanet 16537 22049 host. The WDS lists a single speckle resolution of a potential 16537 22049 stellar companion, 0.048" away (Blazit et al., 1977ApJ...214L..79B), 16537 22049 significantly closer than the planet. However, 13 other attempts by 16537 22049 speckle and AO have failed to resolve the companion (e.g., McAlister, 16537 22049 1978PASP...90..288M; Hartkopf & McAlister, 1984PASP...96..105H; 16537 22049 Oppenheimer et al., 2001AJ....121.2189O). Presumably, the Blazit 16537 22049 measure is spurious. The WDS lists 10 additional components, all of 16537 22049 which were confirmed as optical by blinking archival images (see 16537 22049 Table 6). 17439 23484 Single, candidate Binary. The CNS (1969VeARI..22....1G) lists this as 17439 23484 "RV-Var," but no radial-velocity data could be found in modern 17439 23484 surveys. Catalogs - Abt & Biggs, 1972bsrv.book.....A; Duflot et al., 17439 23484 1995A&AS..114..269D; Gontcharov, 2006AstL...32..759G - list 17439 23484 velocities with rms scatter of about 3km/s, but this could be due to 17439 23484 measurement errors or zero-point variances. This candidate companion 17439 23484 is retained as a candidate. 18267 24496 Binary. The two measurements with {rho}=2.6-2.7" and 18267 24496 {theta}=254-256{deg} listed in the WDS are by Wulff Heintz, nine 18267 24496 years apart and consistent with a bound pair. The first measure is 18267 24496 based on observations over three nights and the second on 18267 24496 observations over two additional nights. Given the quality of the 18267 24496 observations ({Delta}m=4-5 measured) and the reasonably high proper 18267 24496 motion of the primary, this is likely a physical companion, but one 18267 24496 that could use new measurements. 19076 25680 Binary. A companion 0.2" away was discovered by McAlister et al., 19076 25680 1993AJ....106.1639M, with speckle interferometry and confirmed by the 19076 25680 same technique by Hartkopf et al., 2008AJ....135.1334H. These 19076 25680 measures show evidence of orbital motion, and given the 0.2"/yr 19076 25680 proper motion of the primary and an elapsed time of 15 years between 19076 25680 them, this companion can be confirmed as physical. Due to the 19076 25680 constant radial velocity of the primary (D. W. Latham et al., 19076 25680 2010, in preparation), this might be close to a face-on orbit. The 19076 25680 WDS (Cat. B/wds) lists another potential companion 177" away, which 19076 25680 we also identified by blinking archival images. This candidate 19076 25680 (HIP 19075) was however refuted based on its significantly different 19076 25680 proper motion in Hipparcos (Cat. I/239) from the corresponding value 19076 25680 of the primary (see Table 4). The two additional WDS entries are 19076 25680 clearly optical (see Table 6). 19233 26491 Binary. A comparison of Hipparcos and Tycho-2 proper motions shows a 19233 26491 significant difference suggesting a companion (see Section 3.2.2), 19233 26491 which is confirmed by radial-velocity variations (Jones et al., 19233 26491 2002MNRAS.337.1170J). A preliminary spectroscopic orbit exists (H. 19233 26491 Jones, 2008, private communication). 23835 32923 Single. The WDS lists 19 measurements at roughly 0.1" separation over 23835 32923 76 years, and Eggen (1956AJ.....61..405E) even derived two 23835 32923 preliminary visual orbits from these measures. However, Heintz & 23835 32923 Borgman (1984AJ.....89.1068H) suggest that this is likely spurious 23835 32923 and show that the observations are not consistent with orbital motion 23835 32923 of any period. Three additional speckle observations exist since the 23835 32923 Heintz & Borgman publication, from 1984 to 1987 (Tokovinin, 23835 32923 1985A&AS...61..483T; Tokovinin & Ismailov, 1988A&AS...72..563T; 23835 32923 McAlister et al., 1993AJ....106.1639M), but there are 17 null 23835 32923 detections listed in the INT4 23835 32923 (http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/int4) 23835 32923 by speckle interferometry as well as by AO. This star has a stable 23835 32923 radial velocity in Nidever et al. (2002ApJS..141..503N) and D. W. 23835 32923 Latham et al. (2010, in preparation). It appears that these multiple, 23835 32923 but sporadic, measures are spurious. 25278 35296 Binary. DM91 (1991A&A...248..485D) noted the primary of a 12' CPM pair 25278 35296 as "SB", but one that was not confirmed by their work. Modern 25278 35296 measures (Nidever et al., 2002ApJS..141..503N; D. W. Latham et al., 25278 35296 2010, in preparation) show this star to have a stable radial 25278 35296 velocity, refuting the earlier claim. 25647 36705 Quadruple. The WDS lists two measures of this 10" pair (AB Dor AB), 25647 36705 separated by 69 years and consistent with a bound pair. The first 25647 36705 observation, by Rossiter (1955POMic..11....1R), measured a 25647 36705 {Delta}m~6, explaining the lack of many more observations. Close et 25647 36705 al. (2005Natur.433..286C) recovered this pair with AO at the VLT, and 25647 36705 it is also seen in VRI images obtained by T.J.H. in 2008 September at 25647 36705 the CTIO 0.9m telescope. While the photometric distance estimate 25647 36705 varies from the primary's Hipparcos distance by 7{sigma} (see 25647 36705 Table 10), the V magnitude from Rossiter (1955POMic..11....1R) is 25647 36705 likely approximate. Given the high proper motion of the primary, the 25647 36705 consistent measures over 79 years indicate a physical association. 25647 36705 The 2MASS colors indicate an M dwarf with a V magnitude estimate of 25647 36705 about 12.0, in good agreement with the measure of Rossiter 25647 36705 (1955POMic..11....1R) and consistent with the primary's Hipparcos 25647 36705 distance. High-contrast AO efforts have split each of these 25647 36705 components into binaries themselves. The primary was identified by 25647 36705 Hipparcos as showing accelerating proper motion, indicating an unseen 25647 36705 companion, and this is supported by the significant difference 25647 36705 between Hipparcos and Tycho-2 proper motions (see Section 3.2.2). The 25647 36705 suspected companion has since been revealed by very long baseline 25647 36705 interferometry (Guirado et al., 1997ApJ...490..835G), resolved by AO 25647 36705 (Close et al., 2005Natur.433..286C), and confirmed as a physical 25647 36705 association by photometry and spectroscopy (Close et al., 25647 36705 2005Natur.433..286C, 2007ApJ...665..736C; Boccaletti et al., 25647 36705 2008A&A...482..939B, and references therein). Close et al. 25647 36705 (2005Natur.433..286C) also split the secondary into a 0.070" pair, 25647 36705 which was later confirmed by Janson et al. (2007A&A...462..615J) 25647 36705 who measured it 66.1 mas away at 238.5{deg}. 28267 40397 Triple. The five measures in the WDS for AB between 1902 and 1932 are 28267 40397 consistent with a bound pair. The measured {Delta}m~7 makes this a 28267 40397 difficult target for classical techniques and out of the reach of 28267 40397 speckle interferometry. Given that more than 70 years have passed 28267 40397 since the latest measure, this is a good candidate for follow-up AO 28267 40397 observations. This pair also has a wide CPM companion, NLTT 15867, 28267 40397 which was confirmed by photometric distance estimates (see Table 10), 28267 40397 and an additional WDS component, which is clearly optical (see Table 28267 40397 6). 29271 43834 Binary. Eggenberger et al. (2007A&A...474..273E) detected a companion, 29271 43834 3" away, three times over three years with AO at the VLT, 29271 43834 demonstrating CPM and showing a hint of orbital motion. They also 29271 43834 mention a linear trend in CORALIE radial velocities consistent with 29271 43834 this companion, confirming a physical association, and estimate the 29271 43834 companion to be M3.5-M6.5 with a mass of 0.14+/-0.01M_{sun}_. 30314 45270 Single, candidate Binary. The WDS lists three measurements spanning 43 30314 45270 years of a {Delta}m~4 companion separated by about 16", which are 30314 45270 consistent with a bound pair. Curiously, no additional measurements 30314 45270 exist. This companion was listed in the Hipparcos input catalog, but 30314 45270 not resolved by Hipparcos. 2MASS lists a source near this candidate 30314 45270 companion, but it is clearly not the same star because its infrared 30314 45270 colors are more than 3 mag fainter than the visual magnitude of 10.6 30314 45270 from the Hipparcos input catalog. No additional information was found 30314 45270 on this companion and hence it is retained as a candidate. 31711 48189 Binary. The WDS lists 19 measurements over 105 years that are 31711 48189 consistent with a bound pair. During this time, the separation has 31711 48189 closed in from about 3" to about 0.3" and the position angle has 31711 48189 changed by about 15{deg}. Given the small projected separation of 31711 48189 6-60AU, one might expect a greater change in position angle as 31711 48189 evidence of orbital motion. The change of only 15{deg} indicates that 31711 48189 the semimajor axis is larger than the observed separations, perhaps 31711 48189 due to a high inclination. While a more robust confirmation is not 31711 48189 available, the primary has moved about 9" during the measures, and 31711 48189 the companion seems to be moving along with it, indicating a physical 31711 48189 association. 36357 0 Triple, candidate Quadruple. The primary of this system, HD 58946, 36357 0 lies about 13' away, and its physical association is confirmed by 36357 0 matching parallax and proper motion. The primary has a closer 36357 0 companion, about 3" away, confirmed by greater than 11{sigma} 36357 0 difference between Hipparcos and Tycho-2 proper motions (see Table 8) 36357 0 and five measurements in the WDS over 25 years which demonstrate CPM 36357 0 and orbital motion. Additionally, proper-motion variations suggest an 36357 0 unseen companion to HIP 36357 as well, but one we could not confirm 36357 0 (see Table 8). Two wider WDS components are clearly optical (see 36357 0 Table 6). 38625 64606 Binary. For the primary of an SB1 pair, the WDS lists two measures of 38625 64606 a {Delta}m~4 component separated by 4.9", one each from Hipparcos and 38625 64606 Tycho. The Hipparcos solution is flagged as "poor" quality, and there 38625 64606 is no independent confirmation of this companion. T.J.H. observed 38625 64606 this star using the CTIO 0.9m telescope in 2008 September and 38625 64606 obtained 1s exposure images in VRI. No source was found at the 38625 64606 expected position in those images, whereas a companion of {Delta}m~4 38625 64606 should easily have been seen above the background. While the SB1 38625 64606 pair is real, this astrometric detection is refuted. 38908 65907 Triple. LHS 1960 is a companion to this star, separated by about 60", 38908 65907 and confirmed by photometric distance estimates (see Table 5). The 38908 65907 WDS (Cat. B/wds) lists four measures of an additional companion to 38908 65907 LHS 1960, observed 1930-1983, indicating that this component itself 38908 65907 is a 3" CPM binary. No further evidence of companionship could be 38908 65907 found, but given the high proper motion of the primary and the four 38908 65907 consistent measurements by four different telescopes over 53 years, 38908 65907 this system can be confirmed as a triple. 40167 68257 Quintuple, candidate Sextuple. The three brightest roughly solar-type 40167 68257 components ({zeta} Cancri A, B, and C) are supported by over 1000 40167 68257 visual measurements each, corresponding to two visual orbits. 40167 68257 Component C has been noted to have an irregular motion for most of 40167 68257 its history and was identified as an SB1 with an orbit of 6302+/-59 40167 68257 days (Griffin, 2000Obs...120....1G), consistent with earlier 40167 68257 astrometric orbits. However, earlier efforts (Heintz, 40167 68257 1996AJ....111..408H) had noted a mass ratio for the C component 40167 68257 binary of about 1, and with C being a G0 star, the non-detection was 40167 68257 puzzling and attributed to the companion being a white dwarf or 40167 68257 itself a binary. Hutchings et al., (2000PASP..112..833H) finally 40167 68257 observed this pair (Ca, Cb) via AO observations at infrared 40167 68257 wavelengths, designated Cb as an M2 dwarf based on its infrared 40167 68257 colors, and argued on the basis of prior mass-ratio estimates that 40167 68257 it itself is an unresolved binary (Cb1, Cb2). Richichi 40167 68257 (2000A&A...364..225R) confirmed the presence of Cb via lunar 40167 68257 occultation measures. While he could not confirm its binary nature, 40167 68257 his K-band photometry supported the binary M-dwarf hypothesis, for 40167 68257 which he determined an upper limit for projected separation of 40167 68257 20-30mas. Further, Richichi reported the potential discovery of a 40167 68257 sixth component in this system (Cb3). While seen just above his 40167 68257 detection limit and hence retained as a candidate for this work, he 40167 68257 nonetheless confirmed its presence by three independent data analysis 40167 68257 methods and excluded it from being the unresolved companion Cb2 noted 40167 68257 above due to its larger separation of at least 1.6AU from the lunar 40167 68257 occultations. He tentatively identified Cb3 as an M2-M4 dwarf. In 40167 68257 addition to all these, we identified a potential wide companion, 372" 40167 68257 away at 107{deg}, which was later refuted (see Table 4), as were six 40167 68257 additional WDS components, which are clearly optical (see Table 6). 42074 72760 Binary. This companion was suggested by a significant difference in 42074 72760 Hipparcos and Tycho-2 proper motions. Recently, Metchev & 42074 72760 Hillenbrand (2009ApJS..181...62M) resolved the companion in a 42074 72760 Palomar/Keck AO survey, confirmed companionship based on color and 42074 72760 magnitude measurements, and estimated the companion's mass as 42074 72760 0.13M_{sun}_. 42333 73350 Single. The WDS lists a B component 60" away and a C component about 42333 73350 10" from B. While the DSS images were taken over just a two-year 42333 73350 interval, the SSS image provides a longer time baseline and helps 42333 73350 confirm component B (HD 73351) as a field star (see Table 6). 42333 73350 Component C is a CPM companion of B based on three consistent 42333 73350 measures separated by over 100 years, and hence also physically 42333 73350 unassociated with our sample star. 42430 73752 Binary. The CNS (1969VeARI..22....1G) lists the primary of the 1.3" 42430 73752 visual binary as "SB" and notes that there are suspected 42430 73752 perturbations in its proper motion. The reference detailing the 42430 73752 perturbations (Hirst, 1943MNSSA...2..100H) presents a 35 year inner 42430 73752 orbit, which is noted as very preliminary with several different 42430 73752 orbits equally permissible. The author also states that systematic 42430 73752 effects alone may explain the residuals. His 214 year outer orbit was 42430 73752 later revised to 145 years by Heintz (1968AJ.....73..512H), who also 42430 73752 points out that the observed range of radial velocities could be 42430 73752 ascribed to scatter. Adopting a parallax of 0.058", he derived a mass 42430 73752 sum of 1.1M_{sun}_, and noted that at least one component must be 42430 73752 overluminous. If we adopt the HIP parallax of 50.2mas, we get a mass 42430 73752 sum of 1.9M_{sun}_, so the components are likely not overluminous. 42430 73752 Radial-velocity catalogs (Abt & Biggs, 1972bsrv.book.....A; 42430 73752 Gontcharov, 2006AstL...32..759G) list velocities in the range 42430 73752 40-48km/s, but the differences could be due to zero-point offsets 42430 73752 between observers. The early claim of a possible companion is not 42430 73752 supported by subsequent observations, which in fact question it. 42430 73752 While the visual binary is real, the third component is refuted. An 42430 73752 additional wide component listed in the WDS is clearly optical (see 42430 73752 Table 6). 43557 75767 Quadruple. Tokovinin et al. (2006A&A...450..681T) reported the 43557 75767 discovery of a wide {Delta}m=4.3 companion to a 10.3 day SB1 binary 43557 75767 with NACO AO and confirmed CPM using a partial resolution in 2MASS 43557 75767 images. This companion was independently discovered by Fuhrmann et 43557 75767 al. (2005MNRAS.361..803F), who obtained two observations four years 43557 75767 apart, demonstrating CPM, and confirmed companionship by showing 43557 75767 consistent radial velocity with the primary. Their spectra also 43557 75767 enabled them to identify the companion itself as a double-lined 43557 75767 binary, as evidenced by its H{alpha} emission and near-infrared 43557 75767 absorption lines appearing as pairs with an offset of about 21km/s. 43557 75767 Using composite-spectrum analysis, they derived spectral types of M3 43557 75767 and M4. Blinking archival images revealed a possible fifth companion 43557 75767 385" away, and its photometric distance estimate matches the 43557 75767 primary's Hipparcos value within 2{sigma}. However, the Lepine & 43557 75767 Shara (2005AJ....129.1483L) proper motions of the two stars are 43557 75767 significantly different, indicating that this might be a comoving 43557 75767 star perhaps born out of the same cloud as HD 75767, but one that is 43557 75767 not gravitationally bound to it. 45170 79096 Quadruple. Wilson et al. (2001AJ....122.1989W) discovered an L8V 45170 79096 companion (Gl 337C) 43" from the SB2VB pair from 2MASS images. The 45170 79096 two images, separated by 2.5 years, demonstrated CPM. They also 45170 79096 showed that the magnitudes are consistent with the primary's 45170 79096 distance to within 1{sigma}, confirming companionship. Burgasser et 45170 79096 al. (2005AJ....129.2849B) later resolved Gl 337C as a nearly 45170 79096 equal-magnitude binary separated by 0.53+/-0.03" at 291+/-8{deg} 45170 79096 using Lick natural guide star AO. Companionship was confirmed based 45170 79096 on proximity and CPM, which was demonstrated by the absence of a 45170 79096 source in 2MASS images at the expected position of a background star. 45170 79096 Three other components listed in the WDS are clearly optical (see 45170 79096 Table 6). 49081 86728 Binary, candidate Triple. Gizis et al. (2000MNRAS.311..385G) 49081 86728 identified a wide CPM companion from 2MASS and confirmed it with a 49081 86728 spectral-type classification of M6.5. However, based on it being 49081 86728 overluminous (MK=8.19 using 2MASS magnitudes and Hipparcos parallax 49081 86728 versus 9.60 for its spectral type) and having high activity (emission 49081 86728 observed twice), they argued that it is an unresolved equal-mass 49081 86728 binary, or even possibly a triple. We could not find any follow-up 49081 86728 work confirming or refuting this claim, so while this system is 49081 86728 confirmed as a binary, we retain the third component as a candidate. 49081 86728 Additionally, the Dwarf Archives lists a brown dwarf about 25' away 49081 86728 from the primary, but its photometric distance estimate suggests a 49081 86728 distant field object. 51459 90839 Binary, candidate Triple. The CNS (1969VeARI..22....1G) lists the 51459 90839 primary of a wide CPM pair as "SB?" and the secondary (HD 237903, 51459 90839 GJ 394) as "RV-Var". The primary is a constant velocity star (see 51459 90839 Table 12), refuting the CNS claim, but the modern surveys did not 51459 90839 observe the secondary. DM91 (Duquennoy & Mayor, 1991A&A...248..485D) 51459 90839 listed this companion with a constant velocity of 8.24-8.62km/s over 51459 90839 700 days. Heintz (1981ApJS...46..247H) listed velocities of 51459 90839 7.7-8.4km/s over 4 days but noted that the coverage was too weak to 51459 90839 definitively show velocity variations. He also noted that the 51459 90839 spectrum had emission features. Wilson (1967AJ.....72..905W) listed a 51459 90839 velocity of 7.8km/s over three plates with a range of 7.7km/s and 51459 90839 standard deviation of 3.1km/s. Radial-velocity catalogs (Abt & 51459 90839 Biggs, 1972bsrv.book.....A; Duflot et al., 1995A&AS..114..269D) list 51459 90839 values that range over many km/s, but this could be due to zero-point 51459 90839 differences between observers, and these catalogs do not note any 51459 90839 variation. While the wide binary is confirmed based on matching 51459 90839 parallax and proper motion and the primary's SB claim is refuted, the 51459 90839 possible radial-velocity variation of the secondary is inconclusive 51459 90839 and hence retained as a candidate. An additional WDS component is 51459 90839 clearly optical (see Table 6). 54745 97334 Triple. Kirkpatrick et al. (2001AJ....121.3235K) discovered an L4.5V 54745 97334 CPM companion (Gl 417B) 90" away at 245{deg} from the primary using 54745 97334 2MASS images and confirmed a physical association by demonstrating 54745 97334 CPM and consistent parallaxes. Bouy et al. (2003AJ....126.1526B) 54745 97334 later resolved this brown dwarf into a binary (0.070+/-0.0028" at 54745 97334 79.6+/-1.2{deg}) using HST WFPC2. While companionship of this pair 54745 97334 has not been established conclusively, proximity argues for a 54745 97334 physical association. Three additional WDS components are clearly 54745 97334 optical (see Table 6). 55203 98230 Quadruple. {xi} UMa is a quadruple system composed of a 60 year 55203 98230 visual binary, the primary of which is an SB1VB and the secondary is 55203 98230 an SB1. Mason et al. (1995AJ....109..332M) reported a possible fifth 55203 98230 companion detected via speckle interferometry near the secondary. 55203 98230 While the single detection reported is quite convincing, this 55203 98230 companion has never again been seen, despite multiple attempts. Our 55203 98230 efforts with CHARA, while limited to {Delta}K<~2.5, also failed to 55203 98230 resolve any additional components. Given only one measure and about a 55203 98230 dozen null results with the same technique, this new companion is 55203 98230 likely a chance alignment of an unrelated star. An additional wide 55203 98230 component listed in the WDS is clearly optical (see Table 6). 56242 100180 Binary, candidate Triple. The primary of the 15" CPM binary (see 56242 100180 Table 5) has two speckle interferometry measurements of a close 56242 100180 companion in the WDS (Cat. B/wds), observed 0.035" away at 6.8{deg} 56242 100180 in 2001 and 0.122" at 355.8{deg} in 2004. One of the two attempts by 56242 100180 B.D.M. and D.R. at the KPNO 4m telescope in 2008 June resulted in an 56242 100180 "uncertain" measure of 0.218" at 14.6{deg}. Given the 0.378"/yr 56242 100180 proper motion of the primary, these measures are consistent with a 56242 100180 bound pair, but further observations are warranted to obtain a 56242 100180 definitive confirmation, especially given the constant radial 56242 100180 velocity reported by Nidever et al. (2002ApJS..141..503N). 56452 100623 Binary. The WDS lists only a single measure of this large {Delta}m 56452 100623 companion discovered by Luyten in 1960. While the proximity and large 56452 100623 magnitude difference make follow-up observations difficult, Henry et 56452 100623 al. (2002AJ....123.2002H) obtained spectra of this 15th magnitude 56452 100623 companion and showed that it is a DC or DQ white dwarf, not an 56452 100623 M-dwarf as reported in the CNS (1969VeARI..22....1G). The second 56452 100623 observation confirms CPM, and the spectral type and photometry are 56452 100623 consistent with a physical association. 57443 102365 Binary. The companion, discovered by Luyten in 1960, is LHS 313 and 57443 102365 has a proper motion that matches the primary's 1.6"/yr. Hawley et 57443 102365 al. (1996AJ....112.2799H) identified the companion as M4V, which was 57443 102365 recovered by 2MASS at a similar position angle and separation as 57443 102365 Luyten's observation. Its infrared colors are consistent with an M4 57443 102365 dwarf at the primary's distance. 57939 103095 Single. The CNS (1969VeARI..22....1G) and DM91 (Duquennoy & Mayor, 57939 103095 1991A&A...248..485D)listed a companion with separation 2" at 57939 103095 175{deg}. DM91 noted that the companion was flaring with magnitudes 57939 103095 of 8.5-12 and also mentioned that it was normally not seen. The INT4 57939 103095 (http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/int4) 57939 103095 lists four null measurements with speckle interferometry and there 57939 103095 are no radial-velocity variations. Three attempts by B.D.M. and D.R. 57939 103095 in 2008 June at the KPNO 4m telescope failed to identify a companion. 57939 103095 Recently, Schaefer et al. (2000ApJ...529.1026S) have shown that the 57939 103095 brightness enhancements observed are likely due to superflares on the 57939 103095 stellar surface rather than due to a companion. 61317 109358 Single. The WDS (Cat. B/wds) lists a single speckle measure of a 61317 109358 companion 0.1" away (Bonneau & Foy, 1980A&A....86..295B), but the 61317 109358 INT4 has over 20 null speckle detections. B.D.M. and D.R. failed to 61317 109358 resolve the suspected companion in 2008 June at the KPNO 4m 61317 109358 telescope. Given the mention of telescope artifacts as being 61317 109358 responsible for some detections by this observer (da Silva & Foy, 61317 109358 1987A&A...177..204D), we side with the many null detections, 61317 109358 including one by the same observer. Additionally, the CNS (Gliese, 61317 109358 1969VeARI..22....1G)listed this star as "SB" and Abt & Levy 61317 109358 (1976ApJS...30..273A) presented a preliminary orbital solution. 61317 109358 However, those claims were subsequently refuted (Morbey & Griffin, 61317 109358 1987ApJ...317..343M). The wide AB pair in the WDS is clearly optical, 61317 109358 as seen on blinking the archival images (see Table 6). 62505 111312 Binary, candidate Triple. This is a 2.7 year SB2. The WDS lists a 62505 111312 single speckle measure with a separation of 0.089" at 90.6{deg} in 62505 111312 2001 and the pair was seen again in 2006 with a separation of 0.050" 62505 111312 at 44.6{deg} by B.D.M. These measurements are consistent with the 62505 111312 spectroscopic binary and more observations are needed to develop a 62505 111312 visual orbit. The WDS (Cat. B/wds) lists an additional companion, 62505 111312 2.7" away with {Delta}m~4 based on Hipparcos and Tycho measures. The 62505 111312 Hipparcos solution is flagged as "poor" quality, and there is no 62505 111312 independent confirmation of this companion. Its orbital period, if 62505 111312 real, would be too long to affect the velocities obtained over some 62505 111312 seven years. With no conclusive evidence to confirm or refute this 62505 111312 companion, it is retained as a candidate requiring further 62505 111312 observations. 63366 112758 Triple. This is a triple system with an inner SB1 pair and a wider 63366 112758 visual component which was first resolved by van den Bos in 1945 and 63366 112758 then again in 1960 with {Delta}m~5. McAlister et al. 63366 112758 (1987AJ.....93..688M) recovered this visual companion in 1983, and 63366 112758 the three observations show evidence of orbital motion. The McAlister 63366 112758 et al. measurement with speckle interferometry implies {Delta}m<~3, 63366 112758 suggesting that the companion may be variable. B.D.M. and D.R. 63366 112758 attempted to resolve this companion at the KPNO 4m telescope in 2008 63366 112758 June, but could not see it, perhaps because of the large magnitude 63366 112758 difference. 63742 113449 Binary. Hipparcos presents a photocentric orbit for this star with a 63742 113449 period of about 231 days. Moore & Paddock (1950ApJ...112...48M) noted 63742 113449 this star as a radial-velocity variable, Gaidos et al. 63742 113449 (2000AJ....120.1006G) mentioned that the velocity changed by 20km/s 63742 113449 over 10 months, and variations are also seen in the measurements 63742 113449 reported in D. W. Latham et al. (2010, in preparation). However, no 63742 113449 definitive orbit exists. The companion was resolved at the Palomar 63742 113449 200 inch telescope with aperture masking in 2007 January, 63742 113449 35.65+/-0.6mas away at 225.2+/-0.5{deg} with {Delta}H~1.6, and 63742 113449 confirmed at the Keck telescope more than a year later (M. Ireland, 63742 113449 2008, private communication). With consistent astrometric and 63742 113449 spectroscopic evidence, this is a bound pair. 67275 120136 Binary, one planet. {tau} Boo hosts a 4.13MJ minimum-mass planet in a 67275 120136 3 day orbit. Additionally, 56 observations over 170 years in the WDS 67275 120136 confirm a stellar companion based on CPM and orbital motion, which 67275 120136 has a preliminary orbital solution (see Table 11). Wright et al. 67275 120136 (2007ApJ...657..533W) and references therein mention a long-term 67275 120136 drift in radial velocity consistent with this visual companion. 67742 120780 Triple. The WDS lists two measures of a 6" pair 51 years apart and 67742 120780 consistent with a bound system, but follow-up observations have been 67742 120780 difficult due to a magnitude difference of ~5.5. We obtained I-band 67742 120780 images in 2006 July and 2007 June at the CTIO 0.9m telescope. The 67742 120780 companion was seen at both epochs about 5.6" away at 89{deg} with 67742 120780 {Delta}I~3.3. These three observations demonstrate CPM with a 67742 120780 fast-moving primary (0.6"/yr), and, in fact, hint at orbital motion, 67742 120780 confirming companionship. Additionally, Hipparcos identifies this 67742 120780 star as an accelerating proper-motion binary, and the Tycho-2 proper 67742 120780 motion differs from the Hipparcos value by a 19{sigma} significance 67742 120780 (see Table 8). While the Tycho-2 proper motion, averaged over about 67742 120780 100 years, is no doubt affected by the wide pair mentioned above, 67742 120780 whose orbital period could be about 1000 years, the Hipparcos 67742 120780 observations are over some three years and indicate a closer 67742 120780 companion. 69701 124850 Single, candidate Binary. The ORB6 catalog 69701 124850 (http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6) 69701 124850 lists a photocentric orbit for this star with a period of 55 years 69701 124850 and an inclination of 60{deg}. The corresponding preliminary orbit 69701 124850 was recently presented by Gontcharov & Kiyaeva (2010NewA...15..324G) 69701 124850 by combining Hipparcos data with astrometric ground-based 69701 124850 observational catalogs, but we do not find the motion convincing 69701 124850 enough to confirm the companion. This star was not included in the 69701 124850 Nidever et al. (2002ApJS..141..503N) or D. W. Latham et al. (2010, 69701 124850 in preparation) survey, and radial-velocity catalogs (Abt & Biggs, 69701 124850 1972bsrv.book.....A; Duflot et al., 1995A&AS..114..269D; de Medeiros 69701 124850 & Mayor, 1999A&AS..139..433D; Gontcharov, 2006AstL...32..759G) do not 69701 124850 indicate variations. B.D.M. and D.R. could not resolve any companion 69701 124850 via speckle interferometry on the KPNO 4m telescope in 2008 June. 69701 124850 With inconclusive evidence to confirm or refute this companion, it is 69701 124850 retained as a candidate. 69965 125276 Single, candidate Binary. The Hipparcos and Tycho-2 proper motions 69965 125276 differ by greater than a 3{sigma} significance, suggesting an unseen 69965 125276 companion (see Table 8). These proper-motion variations could be due 69965 125276 to a WDS and CNS companion, separated by 3"-8" over four measures 69965 125276 between 1891 and 1936. Some of these measures indicate a {Delta}m~8, 69965 125276 which might explain the several non-detections also included in the 69965 125276 WDS. An attempt by B.D.M. and D.R. at the KPNO 4m telescope in 2008 69965 125276 June could not detect this companion. While the pair is too wide and 69965 125276 too high in contrast for detection via speckle, the finder TV, 69965 125276 sensitive to faint companions, did not reveal any source at the 69965 125276 expected position. Without conclusive evidence to confirm or refute 69965 125276 this companion, it is retained as a candidate. An additional WDS 69965 125276 companion is clearly a background star as seen by blinking archival 69965 125276 images (see Table 6). 70016 125455 Binary. This companion was discovered by Kuiper in 1937 and has 70016 125455 measurements in 1960 and 1987 that are consistent with a bound 70016 125455 system. The companion is LHS 2895 with a proper motion that matches 70016 125455 the primary's, and its 2MASS colors indicate a late M-dwarf at 70016 125455 approximately the primary's distance. 71683 128620 Triple. This is the closest known star system, {alpha} Centauri, which 71683 128620 is composed of an SB2VB pair and a wide companion, Proxima Centauri, 71683 128620 about 2{deg} away. While the angular separation to Proxima is extreme 71683 128620 for bound systems, it translates to a linear projected separation of 71683 128620 10000AU, which is well within the limits of gravitationally bound 71683 128620 pairs. Wertheimer & Laughlin (2006AJ....132.1995W) used kinematic and 71683 128620 radial-velocity data to show that Proxima Centauri is bound to 71683 128620 {alpha} Centauri. A possible new substellar companion to Proxima 71683 128620 Centauri was reported by Schultz et al. (1998AJ....115..345S) 0.34" 71683 128620 away using the HST FOS as a coronagraphic camera. In a follow-up 71683 128620 effort, Golimowski & Schroeder (1998AJ....116..440G) used HST WFPC2 71683 128620 to show that the Faint Object Spectrograph (FOS) feature seen was 71683 128620 likely an instrumental effect and exclude any stellar or substellar 71683 128620 companion within 0.09"-0.85" of Proxima Centauri. 72567 130948 Triple. Potter et al. (2002ApJ...567L.133P) discovered a pair of brown 72567 130948 dwarf companions using AO on the Gemini North 8m telescope. They 72567 130948 demonstrated CPM with observations over 7 months and confirmed 72567 130948 companionship based on their infrared colors, spectral-type of 72567 130948 dL2+/-2, and a consistent age with the primary of less than 0.8Gyr 72567 130948 derived by comparing their position on an H-R diagram with 72567 130948 theoretical models. They also noted that the relative youth is 72567 130948 consistent with the high X-ray activity, Li abundance, and fast 72567 130948 rotation. The Dwarf Archives lists an additional brown dwarf 523" 72567 130948 away from the primary, but its photometric distance estimate 72567 130948 suggests a distant field object. An additional CNS (Gliese W., 72567 130948 1969VeARI..22....1G) claim of an SB companion was refuted by modern 72567 130948 surveys (see Table 12). 74537 135204 Binary. A companion, 0.1" away, is listed in the WDS and CNS (Gliese 74537 135204 W., 1969VeARI..22....1G) and confirmed by the 17 measurements in the 74537 135204 WDS (Cat. B/wds) over 82 years which not only demonstrate CPM, but 74537 135204 also orbital motion. 75312 137107 Triple. Kirkpatrick et al. (2001AJ....121.3235K) discovered a wide L8V 75312 137107 companion (Gl 584C) to the SB2VB binary using 2MASS images and 75312 137107 confirmed the physical association with additional measures and 75312 137107 spectroscopy. Two additional WDS components are clearly optical (see 75312 137107 Table 6). 75718 137763 Quadruple. The primary of a 52" CPM binary is itself SB2, and also has 75718 137763 a wide companion about 20' away that was first mentioned by CNS 75718 137763 (Gliese W., 1969VeARI..22....1G) and confirmed by a spectral-type 75718 137763 identification of M4.5 and a distance estimate of 21.6+/-1.9pc 75718 137763 (Reid et al., 1995AJ....110.1838R). Another wide WDS (Cat. B/wds) 75718 137763 component is clearly optical (see Table 6). 77358 140901 Binary. The WDS lists seven measures for this companion from 1897 to 77358 140901 1960 which are consistent with a bound system. We obtained VRI images 77358 140901 at the CTIO 0.9m telescope in 2006 July and 2007 July, which reveal 77358 140901 the companion at the expected position, confirming CPM. The magnitude 77358 140901 difference of over six makes photometry difficult, but given the 77358 140901 large matching proper motion and proximity, this companion can be 77358 140901 confirmed as physical. An additional WDS component is clearly 77358 140901 optical, as seen when blinking the archival images (see Table 6). 77408 141272 Binary. The WDS lists four micrometer observations of this pair over 77408 141272 56 years that are consistent with a bound system. Eisenbeiss et al. 77408 141272 (2007AN....328..521E) confirm companionship using photometry and 77408 141272 spectroscopy, and derive an estimated mass for the dM3+/-0.5 77408 141272 companion of 0.26^+0.07^_-0.06_M_{sun}_. 78459 143761 Single planet-host or binary with no known planets. {rho} CrB 78459 143761 definitely has a companion, but it is not clear whether it is 78459 143761 planetary or stellar in nature. Hipparcos identified a photocentric 78459 143761 orbit with a period of 78 days, exactly twice that of the planetary 78459 143761 companion reported by Noyes et al. (1997ApJ...487L.195N). Gatewood et 78459 143761 al. (2001ApJ...548L..61G) used Hipparcos and ground-based 78459 143761 observations to conclude that the photocentric orbit is of the same 78459 143761 period as the planet, and in fact the "planet" is an M-dwarf 78459 143761 companion with a mass estimate of 0.14M_{sun}_ in a nearly face-on 78459 143761 orbit. Bender et al. (2005AJ....129..402B) failed to identify such a 78459 143761 companion using high-resolution infrared spectroscopy, and placed an 78459 143761 upper limit on the companion's mass of 0.11-0.15M_{sun}_. Baines et 78459 143761 al. (2008ApJ...682..577B) attempted to resolve this question with 78459 143761 LBOI observations at the CHARA Array, and could not settle the issue 78459 143761 once again. While interferometric visibilities did not perfectly fit 78459 143761 a single-star solution, additional data are required for a definitive 78459 143761 conclusion. This system has a stellar or planetary companion, but not 78459 143761 both. Further observations are warranted. A WDS component is clearly 78459 143761 optical (see Table 6). 78527 144284 Binary. Mazeh et al. (2002ApJ...564.1007M) presented a 3 day SB2 orbit 78527 144284 for this star using infrared spectroscopy to measure the faint 78527 144284 companion, deriving a mass ratio of 0.380+/-0.013. Mayor & Mazeh 78527 144284 (1987A&A...171..157M) had identified this system as a possible triple 78527 144284 based on a 1.7km/s variation in the velocity semiamplitude between 78527 144284 their solution and that of Luyten (1936ApJ....84...85L). While the 78527 144284 velocity semiamplitude does seem to vary for the different orbital 78527 144284 solutions presented for this pair (Luyten, 1936ApJ....84...85L; Mazeh 78527 144284 et al. 2002ApJ...564.1007M; DM91 (Duquennoy & Mayor, 78527 144284 1991A&A...248..485D)) and the D. W. Latham et al. (2010, in 78527 144284 preparation) SB1 orbital solution has residuals of up to 2km/s on 78527 144284 each side, there is no obvious periodic pattern or long-term drift 78527 144284 over the 4.8 years of velocity coverage. The most recent velocity 78527 144284 measure of this star in D. W. Latham et al. (2010, in preparation) is 78527 144284 from 1990, so additional observations are warranted. 78775 144579 Binary. The proper motion of the primary is 0.574"/yr and of the CPM 78775 144579 candidate is 0.550"/yr from the LSPM. The companion's distance 78775 144579 estimate has a large uncertainty and differs from the primary's 78775 144579 Hipparcos value by 1.5{sigma} (see Table 5). Given the proximity of 78775 144579 these two stars in the sky, the very large and similar proper 78775 144579 motions, and similar distances, this appears to be a physical 78775 144579 companion, as it has been previously recognized (DM91, 78775 144579 1991A&A...248..485D; CNS, Gliese W., 1969VeARI..22....1G). The 78775 144579 differences in the proper motions might indicate that the companion 78775 144579 or the primary has a close unresolved companion and warrants further 78775 144579 observations. 79492 145958 Binary, candidate Triple. The primary of a 4" visual binary has two 79492 145958 additional possible companions, one of which was refuted by this 79492 145958 effort and the other remains a candidate. The WDS lists a nearby 79492 145958 companion, 0.2" away, detected by H.A.M. in 1983. The INT4 catalog 79492 145958 (http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/int4) 79492 145958 lists this as a weak detection and possibly spurious, and includes a 79492 145958 null detection using the same technique. B.D.M. and D.R. failed to 79492 145958 resolve a companion at the KPNO 4m telescope in 2008 June. Nidever et 79492 145958 al. (2002ApJS..141..503N) identify this as a constant velocity star. 79492 145958 Evidence seems to be mounting against this candidate companion, which 79492 145958 is considered refuted for this work. Separately, the Dwarf Archives 79492 145958 includes a T6 object about 27' away from this star. Looper et al. 79492 145958 (2007AJ....134.1162L) discovered this T dwarf in the 2MASS survey, 79492 145958 obtained spectra, typing it as T6, and estimated its proper motion 79492 145958 and distance, but did not suggest an association with HD 145958. 79492 145958 Their proper motion and distance estimates are similar to the 79492 145958 primary's corresponding values from van Leeuwen, 2007A&A...474..653V. 79492 145958 While the projected linear separation is very large at about 40000AU, 79492 145958 this could be a loosely bound companion to HD 145958, and is 79492 145958 retained as a candidate. An additional wide component listed in the 79492 145958 WDS (Cat. B/wds) is clearly optical (see Table 6). 79607 146361 Quintuple. See Raghavan et al. (2009ApJ...690..394R) for a 79607 146361 comprehensive treatment of all components of this system. 80366 147776 Binary, candidate Triple. The WDS (Cat. B/wds) lists three candidate 80366 147776 companions, but the details actually correspond to four stars. The 80366 147776 {Delta}m~4 component 103" away at 281{deg} is clearly a field star, 80366 147776 as seen by blinking the archival images (see Table 6). Three 80366 147776 additional companions were reported by Sinachopoulos 80366 147776 (1988A&AS...76..189S) - 6.4" separation at 173{deg} with {Delta}m~3, 80366 147776 9.7" separation at 14{deg}, and 71.9" separation at 28{deg}. The 80366 147776 latter two components do not have differential-magnitude 80366 147776 measurements. Sinachopoulos measured these pairs using a 1.5m 80366 147776 telescope by combining 4-16 exposures of a few seconds each. The wide 80366 147776 companion 72" away should have been seen in the DSS images, but no 80366 147776 stellar source was seen at the expected position. The closest star to 80366 147776 this position in the 1995 DSS image is 83" away at 15{deg} and is 80366 147776 clearly a field star. The other two sources seen by them would be 80366 147776 buried in the saturation around the primary in the DSS images, so we 80366 147776 obtained VRI frames in 2008 May and August at the CTIO 0.9m 80366 147776 telescope. The images clearly show a faint companion about 9" away at 80366 147776 19{deg}. This is likely the 9.7" companion seen by Sinachopoulos 80366 147776 (1988A&AS...76..189S), exhibiting CPM, and given the proximity, is 80366 147776 likely physical. The closest source seen by Sinachopoulos is not 80366 147776 detected in the CTIO images and remains a candidate. Additionally, 80366 147776 the CNS (Gliese W., 1969VeARI..22....1G) lists a companion for this 80366 147776 star 3" away at 281{deg} in 1909. This is likely the same as the 80366 147776 component measured by Burnham as listed in the WDS, which was seen 80366 147776 103" away at 281{deg} in 1909 and as discussed above, is clearly 80366 147776 optical. 80925 148704 Binary. This is a 32 day SB2 binary for which Hipparcos and Tycho 80925 148704 identified another companion 4.1" away at 221{deg}. Our CTIO 0.9m 80925 148704 images obtained in 2008 October do not reveal any companion at the 80925 148704 expected position, while a {Delta}m~3 companion as indicated by 80925 148704 Hipparcos should have been seen above the tail of the primary's 80925 148704 point-spread function (PSF). However, given the proper motion of the 80925 148704 primary, a field star would have moved closer and possibly could be 80925 148704 buried within the primary's PSF. Gray et al. (2006AJ....132..161G) 80925 148704 list the spectral type of the companion as G9V and its coordinates 80925 148704 imply a separation of 2.4" at 55{deg}, the exact position where a 80925 148704 field star would be 15 years since the Hipparcos measure. The Gray et 80925 148704 al. spectral type, along with the Tycho-2 V=10.5, implies a 80925 148704 significantly larger distance to this star compared to the primary, 80925 148704 enabling us to refute this candidate. 81375 149806 Binary. This companion was first reported by Rossiter 81375 149806 (1955POMic..11....1R) 5.9" away at 22{deg} and has two additional 81375 149806 measurements in the WDS (Cat. B/wds) over the next 54 years, which 81375 149806 are consistent with a bound system. While the photometric distance 81375 149806 estimate is not a good match (see Table 10), the R magnitude listed 81375 149806 is likely approximate. Given the moderate proper motion of the 81375 149806 primary, the consistent measures over 54 years indicate a physical 81375 149806 association. The 2MASS colors indicate an M-dwarf with a V magnitude 81375 149806 estimate of about 12, in fair agreement with the measure of Rossiter 81375 149806 (1955POMic..11....1R). B.D.M. and D.R. attempted to observe this 81375 149806 companion at the KPNO 4m telescope in 2008 June. While the separation 81375 149806 and {Delta}m are too large to be resolved using speckle, the finder 81375 149806 image at the telescope showed a source at the expected position with 81375 149806 a {Delta}m similar to those of prior observations. 83020 153557 Triple. The WDS (Cat. B/wds) lists 17 measurements over 95 years with 83020 153557 separations of 1.9"-4.9", which are consistent with a bound system, 83020 153557 and given the 0.3"/yr proper motion of the primary, imply a physical 83020 153557 association. This pair also has a wider companion, HD 153525, about 83020 153557 2' away, which is confirmed by matching proper motion and parallax. 88601 165341 Binary. CNS (Gliese W., 1969VeARI..22....1G) lists component A of an 88601 165341 88 year SB2VB as a possible binary with a period of about 17 years, 88601 165341 but this is inconsistent with modern measurements (D. W. Latham et 88601 165341 al. 2010, in preparation). Heintz (1988JRASC..82..140H) presented a 88601 165341 revised orbit of the SB2 and excluded the possibility of any 88601 165341 additional companions with periods below 55 years, stating that the 88601 165341 once suspected velocity variation of A is disallowed by the more 88601 165341 precise recent measurements. The WDS lists 15 more components for 88601 165341 this star, all of which are clearly optical (see Table 6). 88745 165908 Binary, candidate Triple. This is a 56 year visual binary orbit. 88745 165908 Additionally, the WDS (Cat. B/wds) lists one speckle measure with a 88745 165908 separation of 0.228" at 50.2{deg} from Scardia et al. 88745 165908 (2008AN....329...54S), who list this new discovery as "faint". They 88745 165908 also resolved the known VB companion about 1" away, and noted it as 88745 165908 "very faint." In the absence of additional measures that can help 88745 165908 confirm CPM, this close companion is retained as a candidate. Five 88745 165908 other components listed in the WDS are clearly optical (see Table 6). 93966 178428 Binary. The primary of a 22 day SB1 has a single 1987 measure listed 93966 178428 in the WDS (Cat. B/wds) with a separation of 0.2". However, the INT4 93966 178428 (http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/int4) 93966 178428 lists six null results and attempts by B.D.M. and D.R. at the KPNO 4m 93966 178428 telescope in 2008 June once again failed to reveal any visual 93966 178428 companion. A wider component listed in the WDS is clearly optical 93966 178428 (see Table 6). 96895 186408 Triple, one planet. This close companion to 16 Cyg A was first 96895 186408 resolved 3" away by Turner et al. (2001AJ....121.3254T) with AO at 96895 186408 the Mount Wilson Observatory and confirmed by Patience et al. 96895 186408 (2002ApJ...581..654P), who demonstrated CPM and measured infrared 96895 186408 magnitudes consistent with the primary's distance. Four velocity 96895 186408 measures over 25 years show a slow drift (D. W. Latham et al. 2010, 96895 186408 in preparation), consistent with this companion. This system also has 96895 186408 a wide companion, 16 Cyg B, which is a planet host. The WDS (Cat. 96895 186408 B/wds) lists an additional source, 16" away from 16 Cyg B, but 96895 186408 Patience et al. (2002ApJ...581..654P) measured the infrared 96895 186408 magnitudes of this candidate, demonstrating that it is a background 96895 186408 star. This is the only planetary system in this study with more than 96895 186408 two stars. 98677 190067 Binary. This companion was discovered by Turner et al. 98677 190067 (2001AJ....121.3254T) with AO at the Mount Wilson Observatory, but 98677 190067 the single-epoch measure with no color information does not allow 98677 190067 confirmation of a physical association. B.D.M. and D.R. observed this 98677 190067 star at the KPNO 4m telescope in 2008 June. While the separation and 98677 190067 {Delta}m are too large for speckle observations, a stellar source was 98677 190067 seen at the expected position, confirming CPM, and given the 98677 190067 proximity to a large proper motion (0.6"/yr) primary, the physical 98677 190067 association of this companion is very likely. 98819 190406 Binary. Liu et al. (2002ApJ...571..519L) discovered a faint companion 98819 190406 0.8" from this star with AO at the Gemini North and Keck II 98819 190406 telescopes and confirmed a physical association by demonstrating CPM, 98819 190406 consistent spectroscopy, and long-term radial-velocity trend. They 98819 190406 determined a spectral type for the companion of L4.5+/-1.5, estimated 98819 190406 its mass to be 55-78MJ and age as 1-3Gyr. This is the first 98819 190406 substellar object imaged so close to a solar-type star and indicates 98819 190406 that brown dwarfs can exist in extra solar systems at positions 98819 190406 comparable to the gas giants in our solar system. Eight additional 98819 190406 WDS (Cat. B/wds) components are clearly optical (see Table 6). 99316 191499 Binary. The WDS (Cat. B/wds) lists 51 measurements of this companion 99316 191499 between 1782 and 2003, which are consistent with a bound system. 99316 191499 There is little evidence of orbital motion during the roughly 200 99316 191499 years of observations, possibly because the companion is near 99316 191499 apastron in an eccentric orbit or the orbit is highly inclined. 99316 191499 Hipparcos and Tycho-2 proper motions differ by 5.6{sigma}, suggesting 99316 191499 some orbital motion (see Table 8). The photometric distance estimate 99316 191499 is not a very good match (see Table 10), but photometry would be 99316 191499 tricky for this close pair as indicated by the large uncertainties of 99316 191499 the 2MASS magnitudes. Given the evidence of consistent WDS measures, 99316 191499 proper motion differences between Hipparcos and Tycho-2, and similar 99316 191499 distance estimates, this pair likely has a physical association. An 99316 191499 additional wide WDS component is clearly optical (see Table 6). 101345 195564 Binary. The WDS (Cat. B/wds) lists 16 measures over 110 years that are 101345 195564 consistent with a bound pair. While proximity to the primary and 101345 195564 {Delta}m~5 (from WDS) make photometry of the companion difficult, the 101345 195564 proximity and CPM implied by the measures argue for a physical 101345 195564 association. An additional wide WDS component is clearly optical (see 101345 195564 Table 6). 104440 200525 Triple. The CNS (Gliese W., 1969VeARI..22....1G) and Hipparcos 104440 200525 (Cat. I/239) identified the closer pair as a possible binary 104440 200525 (stochastic solution) and Goldin & Makarov (2006ApJS..166..341G) 104440 200525 derived a photocentric orbit using the Hipparcos intermediate 104440 200525 astrometry data. Their orbital solutions using data from the two 104440 200525 independent Hipparcos reduction methods, Fundamental Astronomy by 104440 200525 Space Techniques (FAST) and the Northern Data Analysis Consortium 104440 200525 (NDAC), are consistent. They tested their orbit determination method 104440 200525 satisfactorily against 235 known binaries and derived a better than 104440 200525 99% confidence level based on simulations. The WDS lists four 104440 200525 measurements from 1898 to 1932, during which time the separation 104440 200525 reduced from about 1" to 0.16". The respective position angles of the 104440 200525 measurements are consistent with a high-inclination orbit. Given 104440 200525 these independent measurements leading to similar results, we 104440 200525 conclude that while the orbital elements may be preliminary, this 104440 200525 companion is physically bound. For the wider component, the WDS has 104440 200525 five measures over 88 years that are also consistent with a bound 104440 200525 pair. The companion is NLTT 50542 with a proper motion that matches 104440 200525 the primary's, and the notes in the catalog recognize this component 104440 200525 as gravitationally bound. 2MASS magnitudes have a large error, but 104440 200525 are consistent with a mid-K dwarf companion at approximately the 104440 200525 primary's distance. 103859 200560 Binary. The WDS (Cat. B/wds) has seven measures of a companion with 103859 200560 separations 2.8"-3.3" over 28 years, suggesting a bound system. This 103859 200560 is especially significant given the primary's large proper motion of 103859 200560 0.4"/yr. The companion, GJ 816.1B, is recognized in the CNS (Gliese, 103859 200560 1969VeARI..22....1G) as bound, although no conclusive evidence is 103859 200560 presented. The 2MASS photometry has large errors, and hence is not 103859 200560 very useful. The Hipparcos and Tycho-2 proper motions are different 103859 200560 by about 8{sigma}, providing evidence of orbital motion and lending 103859 200560 credibility to a physical association. The WDS lists this pair as the 103859 200560 CD component of the B3V binary HD 200595 AB, but there is clearly no 103859 200560 physical association between HD 200560 and HD 200595 as seen by 103859 200560 blinking archival images. An additional wide WDS component is also 103859 200560 clearly optical (see Table 6). 104858 202275 Binary. This is a 5.7 year SB2VB. Tokovinin et al. 104858 202275 (2006A&A...450..681T) give an additional orbit with a period of 5.7 104858 202275 days, which is in fact the former orbit listed with an incorrect unit 104858 202275 (A. Tokovinin, 2007, private communication). This system is a binary 104858 202275 with mass estimates of 1.2M_{sun}_ and 1.1M_{sun}_ by Pourbaix 104858 202275 (2000A&AS..145..215P). An additional wide WDS component is clearly 104858 202275 optical (see Table 6). 107350 206860 Binary. Luhman et al. (2007ApJ...654..570L) reported the discovery of 107350 206860 a T2.5+/-0.5 companion using Spitzer IRAC images and confirmed CPM 107350 206860 using 2MASS images. The infrared colors are consistent with the 107350 206860 distance to the primary, confirming companionship. By comparing the 107350 206860 luminosity with evolutionary tracks, they estimate the companion's 107350 206860 mass as 0.021+/-0.009M_{sun}_ and age as 0.3+/-0.2Gyr. An additional, 107350 206860 potentially wide companion was identified 591'' away by blinking 107350 206860 archival images but refuted based on its photometric distance 107350 206860 estimate (see Table 5). 112447 215648 Binary. A companion, 11" away, is listed in the WDS (Cat. B/wds) and 112447 215648 CNS (Gliese, 1969VeARI..22....1G) and confirmed by the 23 112447 215648 measurements in the WDS over 179 years which not only demonstrate 112447 215648 CPM, but also orbital motion. A wider WDS component is clearly 112447 215648 optical (see Table 6). 113421 217107 Single star with two planets or a binary with one planet. The WDS 113421 217107 (Cat. B/wds) lists two measurements, 15 years apart, of a companion 113421 217107 0.3" away from this star, which also hosts two planets. These 113421 217107 speckle interferometry detections could however not be confirmed by 113421 217107 the same technique on at least three other occasions, indicating that 113421 217107 this pair might have a large or varying {Delta}m. Interestingly, the 113421 217107 farther planet is one of the most widely separated planets reported, 113421 217107 at least 5AU from the star. Vogt et al. (2005ApJ...632..638V) present 113421 217107 orbital solutions with periods of 7-9 years, but mention that it 113421 217107 could be three times larger. Wright et al. (2009ApJ...693.1084W) 113421 217107 present an updated orbit with P=11.5+/-0.5 years and a=5.27+/-0.36AU. 113421 217107 At the 20pc distance to the star, these separations are consistent 113421 217107 with the speckle observations. Given the inconsistent measures, if we 113421 217107 assume a {Delta}V near the speckle limit of about 3, the companion to 113421 217107 the G8 IV-V primary (Gray et al., 2003AJ....126.2048G) could be an 113421 217107 early M-dwarf. The mass sum of such a binary is consistent with the 113421 217107 Wright et al. (2009ApJ...693.1084W) orbital elements. Vogt et al. 113421 217107 (2005ApJ...632..638V) note that an AO image obtained with the Keck 113421 217107 telescope did not reveal any stars beyond 0farcs1 from the primary, 113421 217107 and Chauvin et al. (2006A&A...456.1165C) confirm this null result 113421 217107 with VLT and CFHT AO observations. The M-dwarf companion would also 113421 217107 imply a significantly larger velocity semi-amplitude for the 113421 217107 primary, but that possibility is not excluded by the orbital plot in 113421 217107 Wright et al. (2009ApJ...693.1084W). While it appears that this 113421 217107 "planetary" companion could be a star, further observations are 113421 217107 warranted. 115147 220140 Triple. The WDS (Cat. B/wds) has five measurements over 100 years for 115147 220140 the closer visual companion at separations of about 10" that are 115147 220140 consistent with a bound pair. The companion is NLTT 56532 with a 115147 220140 proper motion matching that of the primary and 2MASS colors 115147 220140 consistent with an early M-dwarf at approximately the primary's 115147 220140 distance. The wide CPM companion, 16' away, was first identified by 115147 220140 Lepine & Shara (2005AJ....129.1483L) and confirmed by Makarov et al. 115147 220140 (2007ApJ...668L.155M) who show that the companion's trigonometric 115147 220140 parallax is consistent with the primary's Hipparcos value. Their BVRI 115147 220140 photometry along with 2MASS near-infrared magnitudes show that this 115147 220140 star is overluminous in the Ks band, confirming its suspected 115147 220140 pre-main-sequence status, and enabling an age estimate of 12-20Myr.