024044.94+611656.1 = HD 16429. McSwain (2003ApJ...595.1124M) found that the spectrum is a composite of an SB1 system and constant velocity component. We assumed that one of these is the angularly resolved companion for counting purposes.
025107.97+602503.9 = HD 17505. The companion is resolved on the y-axis only and is far off-axis along the x direction. The results are consistent with the separation 2.15'' and position angle 92.7{deg} found by Maiz Apellaniz 2010 (cat. J/A+A/518/A1), although our estimated magnitude difference is slightly larger. Sota et al. 2011 (cat. III/274) obtained resolved spectra of both components and found that both are O-type stars. Note that component A of this pair is itself a spectroscopic triple star system (Hillwig et al. 2006, cat. J/ApJ/639/1069).
040751.39+621948.4 = HD 25639 = SZ Cam. Resolved on both axes for the first observation (at a position consistent with that found by Balega et al. 2007, cat. J/other/AstBu/62.339), but only resolved along the y-axis in the second observation. We adopted the magnitude difference from the first observation and the second derivative amplitude a_x_ to estimate |{Delta}x| for the second observation. Gorda et al. (2007AstBu..62..352G) show that the system consists of a short-period eclipsing binary with a distant companion that is probably also a binary (making the system a hierarchical quadruple). We assumed that the resolved component CHR 209 Ea,Eb is this second system for counting purposes.
051618.15+341844.3 = HD 34078. We did not detect the close ({rho}=0.35'') companion of AE Aur discovered by Turner et al. (2008AJ....136..554T; TRN 17 Aa,Ab), which may have been an artifact of their AO observations (see Section 4).
051756.06-691603.9 = HDE 269321. This close pair is resolved along the y-axis only in both of our closely spaced observations.
051814.36-691501.1 = HD 35343 = S Dor. The companion is beyond the x-axis scan range in the second (short scan) observation.
053051.48-690258.6 = HDE 269662. The companion is close, faint, and detected along the y-axis only in two closely spaced observations.
053522.90-052457.8 = HD 37041A = {theta}^2^ Ori A. The CHR 249 Aa,Ab pair is clearly resolved in the first observation, but in the second short scan observation the companion is beyond the scan range in x and is only partially resolved in the y direction.
062715.78+145321.2 = HD 45314. Mason et al. (1998AJ....115..821M) used speckle interferometry to resolve this target as a binary with a separation of 0.054'' (named CHR 251 AB), but it was not resolved again in subsequent speckle observations (Mason et al. 2009, cat. J/AJ/137/3358). It appears single in the Fine Guidance Sensor (FGS) scans.
064548.70-071839.0 = ALS85. This is a triple system where components B and C are comparable in brightness. Consequently, the correspondence between the components observed in both axes is ambiguous. Table 2 lists the result where the closer component is assumed to be B in both cases. If B has the larger projected separation in the y-axis scan, then the result for A,B is {theta}=219.87{deg}+/-0.18{deg} and {rho}=0.3378''+/-0.0013'' and the result for A,C is {theta}=233.29{deg}+/-0.20{deg} and {rho}=0.3117''+/-0.0011''.
071842.49-245715.8 = HD 57061. {tau} CMa is a multiple system with two components revealed by the Fine Guidance Sensor (FGS) observations. The wider component was detected along both axes in the first observation, but only along the x-axis in the second observation. There is a low-amplitude peak in the cross correlation function for the second observation near the expected projected separation ({Delta}y~+0.19) but it is below the adopted detection threshold. The system consists of a long-period SB1 and a short-period eclipsing system (van Leeuwen & van Genderen, 1997A&A...327.1070V; Stickland et al., 1998Obs...118....7S), and we assumed that these two correspond to the bright resolved pair FIN 313 Aa,Ab. The WDS currently identifies Ab as the brighter of the two central objects, so we subtracted 180{deg} in position angle and changed the sign of {Delta}m to make our results consistent with the others in the WDS for the Aa,Ab pair. The wider component Ab,E appears in the WDS with a 180{deg} difference in position angle, but a reassessment of AstraLux Lucky Imaging observations by Maiz Apellaniz 2010 (cat. J/A+A/518/A1) indicates a placement consistent with the Fine Guidance Sensor (FGS) results.
075220.28-262546.7 = HD 64315. This system was resolved as a binary by Mason et al. 2009 (cat. J/AJ/137/3358) and named WSI 54 AB. Recent observations by Hartkopf et al. 2012 (cat. J/AJ/143/42) agree with the position angle and separation estimated from the Fine Guidance Sensor (FGS) observations (Table 2). However, speckle observations by Tokovinin et al. 2010 (cat. J/AJ/139/743) suggest that the system may consist of a triple in a linear configuration, and hence our binary measurements may correspond to the center of light of the two companions. The fit of the x-axis scan with two components is marginal, but experiments with three component fits made little or no improvement, so we present the binary results in Table 2 for simplicity. Lorenzo et al. (2010ASPC..435..409L) present a spectroscopic study and argue that the system consists of one SB2 system with a period of P=2.71days plus one SBE system with a period of 1.018days. We assumed that each of these correspond to components of the resolved binary for counting purposes.
081517.15-354414.6 = CD-35 4384. This is a triple system with an inner companion Ab detected by Fine Guidance Sensor (FGS). It was difficult to rectify the low frequency trends in these long scans (particularly for the x-axis) and the magnitude difference for the wide pair Aa,B is taken from the y-axis result. Note that the actual uncertainty in magnitude difference may be larger than quoted in Table 2, because we do not account for spatial photometric sensitivity variations that become significant for widely separated systems.
081903.90-360844.9 = CD-35 4471. The companion was resolved along the y-axis only, but the second derivative test was nearly met for the x-axis result. Thus, we estimated |{Delta}x| from the y-axis magnitude difference and second derivative amplitude a_x_. The result given in Table 2 corresponds to an assumed position at +{Delta}x; for a projected position of -{Delta}x, the position angle is {theta}=146.4{deg}+/-6.1{deg}.
084351.09-460346.5 = CD-45 4462. The Fine Guidance Sensor (FGS) scans reveal this as a triple system. All three components appear in the y-axis scan, but the central pair is blended together in the x-axis scan. However, the second derivative amplitude is quite large for the central blend, so we estimated |{Delta}x| from the y-axis magnitude difference and second derivative amplitude a_x_. Table 2 lists the position angle of A,B for +{Delta}x, and the position angle for -{Delta}x is {theta}=20.0{deg}+/-3.3{deg}. All the magnitude differences are from the y-scan results.
085322.01-460208.8 = CD-45 4676. The B companion is resolved along the y-axis and blended with the central fringe along the x-axis. The second derivative test criterion is met in the latter case, so we estimated |{Delta}x| from the y-axis magnitude difference and second derivative amplitude a_x_. The position angle for +{Delta}x is given in Table 2, and that for -{Delta}x is {theta}=342.31{deg}+/-0.09{deg}.
090221.56-484154.4 = CD-48 4352. This target appears as a triple in the y-axis scan and appears single in the x-axis scan. However, the central fringe in the x-axis scan passes the second derivative test, and we assume that the implied fringe broadening is due only to the closer and brighter B component (i.e., that the wider and fainter C component falls beyond the recorded x-axis scan). Then we estimated |{Delta}x| from the y-axis magnitude difference and second derivative amplitude a_x_. The +|{Delta}x| solution is used for the position angle in Table 2, and the result for -|{Delta}x| is {theta}=18.6{deg}+/-2.9{deg}.
100639.88-572533.1 = CPD-56 2853. The faint companion is resolved along the y-axis only. In this case the projected separation ({Delta}y=0.2'') is wide enough that we cannot say whether or not the the companion is blended or off-scan along the x-axis, and consequently we simply present a lower limit for the separation in Table 2.
104505.85-594006.4 = HDE 303308. This target was detected as a close binary in earlier Fine Guidance Sensor (FGS) observations by Nelan et al. (2004AJ....128..323N, 2010AJ....139.2714N) with {theta}=122{deg}+/-32{deg} and {rho}=0.015''+/-0.002'' (resolved on the y-axis only). We obtained two additional observations that do not resolve the system. However, the second derivative test was suggestive of a companion (reaching a S/N of 3.3 for the y-axis scan of the second observation, but still below our detection criterion of S/N>4). Taking the second derivative amplitudes at their face values yields the minimum separations and position angles given in Table 3. Note that solution a_{theta}2_ in the first observation is consistent with a_{theta}1_ in the second observation. The fact that three independent observations all yield similar binary parameters indicates that this system is probably a long-period wide binary. The spectroscopic status is controversial. Chini et al. 2012 (cat. J/MNRAS/424/1925) found the star to be radial velocity constant in 10 observations. On the other hand, Levato et al. (1991ApJS...75..869L) measured one very low radial velocity over an eight-night run, consistent with a short-period eccentric binary orbit. Consequently, we label the spectroscopic status as "SB1?" in Table 1.
164120.41-484546.6 = HD 150136. The companion resolved in x only is consistent in position and magnitude difference with the known A,B pair. A companion with {rho}=0.0073'' detected in VLTI Amber observations by Sanchez-Bermudez (2013A&A...554L...4S) is too close to be resolved in the Fine Guidance Sensor (FGS) data. Sana et al. (2013A&A...553A.131S) discuss the orbits of the close binary and third star, and we include their period estimates in the spectroscopic category for Figure 4.
172912.93-313203.4 = HD 158186. A companion is detected along the y-axis only. We adopt {Delta}x=0 in Table 2.
181512.97-202316.7 = HD 167263. The close pair of 16 Sgr (CHR255 Aa,Ab) was observed in 3 previous speckle measurements with a position angle difference of 180{deg} from the Fine Guidance Sensor (FGS) results, but this is not unexpected for stars of similar brightness.
181805.90-121433.3 = HD 167971. De Becker et al. (2012MNRAS.423.2711D) resolved this system with the VLTI and argued that it has an orbital period P>20yr. However, the separation was about 9 mas in 2008, which was too close for resolution with the somewhat noisier Fine Guidance Sensor (FGS) scans we obtained. It is a hierarchical triple system with a close central binary.
182119.55-162226.1 = HD 168625. This target appears triple in the x-scans but double in the y-scan. It is not clear which of the two components in the x-scan corresponds to the single component in the y-scan, but we assumed that the component B with the smaller projected separation along the x-axis corresponds to the resolved component along the y-axis (and that component C falls beyond the range recorded for the y-scan). The magnitude differences are taken from the x-axis data. The central fringe appeared somewhat asymmetrical in both x and y compared to those for the calibrator stars. Note that in the long scans made after 2009.1 (like this case) we often observe a weak feature at {Delta}x=-1.2'' that has a systematic origin and should not be confused with a faint companion. Only companion B is recorded along the x-axis in the second, short scan observation. Component B is probably the companion detected in VLT-NACO observations by Martayan et al. (2012ASPC..464..293M).
200329.40+360130.5 = HD 190429. Long scans were made to detect the signal of the wide B component. There are a few reports of a closer and fainter companion MCA 59 Aa,Ab at a separation of ~0.1'' (most recently by Mason et al., 1998AJ....115..821M). However, this close companion is not detected in the Fine Guidance Sensor (FGS) scans.
201806.99+404355.5 = HD 193322A. This is a remarkable multiple system that is the subject of a detailed study with the CHARA Array long baseline interferometer by ten Brummelaar et al. (2011AJ....142...21T). The Fine Guidance Sensor (FGS) observations resolve the Aa,Ab pair along the y-axis, but the pair is blended in the x-axis scan. A blend is indicated by the second derivative test and we used the y-scan magnitude difference and second derivative amplitude to find |{Delta}x|. The solution using is listed in Table 2, and the separation and position angle estimates agree well with contemporaneous CHARA array measurements (ten Brummelaar et al., 2011AJ....142...21T).
201851.71+381646.5 = HD 193443A. This system appears in the WDS with the brighter component identified as B, so we added 180{deg} to the position angle and changed the sign of {Delta}m for consistency with the results in the WDS.
213857.62+572920.5 = HD 206267. This pair is resolved along the y-axis only, but the projected separation and magnitude difference are consistent with those for the known MIU 2 Aa,Ab system if the projected separation is small along the x-axis. The results in Table 2 assume {Delat}x=0. The system is an hierarchical triple (Stickland, 1995Obs...115..180S; Burkholder et al. 1997, cat. J/ApJ/490/328), and we assumed that the resolved companion is the third star identified in the spectrum.