WIDE COOL AND ULTRACOOL COMPANIONS TO NEARBY STARS FROM Pan-STARRS 1

To identify objects with proper motion in common with nearby stars, we first began by collating lists of stars to search in. We started with stars from the Hipparcos catalog (van Leeuwen 2007). To limit the contamination by distant background stars in our sample, we included only Hipparcos stars with proper motions above 01 yr⁻¹ and parallaxes more significant than 5σ (d ≲ 200 pc). This provided us with a relatively complete sample of stars in the solar neighborhood with spectral types A–K. We supplemented this catalog with lower-mass primaries drawn from the LSPM (Lépine & Shara 2005; μ >015 yr⁻¹, δ > 0°) and rNLTT (Salim & Gould 2003; μ > 02 yr⁻¹) proper motion catalogs and with the bright M dwarf catalog of Lépine & Gaidos (2011) to which we applied a proper motion cut of μ > 01 yr⁻¹. See Table 1 for details on the number of primary stars from each input catalog.

Pan-STARRS 1 is an ongoing survey and as such the available data products are constantly evolving. We conducted our search over several iterations of the Pan-STARRS 1 3π database. In all our searches we queried the most up-to-date Pan-STARRS 1 3π database using the Desktop Virtual Observatory software (Magnier et al. 2008). Initially, our search involved combining 2MASS and Pan-STARRS 1 data to calculate proper motions in a similar process to that used by Deacon et al. (2011). For this PS1 + 2MASS search, we required that objects had more than one detection in the y_P1 band. PS1 detections were required to have a significance greater than 5σ to be included in the astrometric and photometric solutions of their parent object. We also required that the objects be classified as good quality, point-source detections in both Pan-STARRS 1 and 2MASS.

Since 2012 June, we have used proper motions calculated using Pan-STARRS 1 only data (although 2MASS data is included if a detection is within 1'' of the mean Pan-STARRS 1 position). In these cases, we required that the proper motion measurement of the candidate companion was more significant than 5σ, be calculated from more than seven position measurements, and that the time baseline over which it was calculated be greater than 400 days. Note that the Pan-STARRS 1 survey strategy consists of pairs of observations in the same filter taken ∼25 minutes apart and often two filters will be taken in the same night. Hence our requirement of seven position measurements does not imply seven independent epochs evenly spread across the time baseline of the proper motion calculation.

In the case of the Hipparcos and Lépine & Gaidos (2011) catalogs, distance estimates were available for all our target stars. Hence we searched for companions out to projected separations of 10,000 AU. For the LSPM and rNLTT catalogs, where distance estimates are not available for all the stars, we used a maximum search radius of 20 arcmin. In all cases we made an initial cut on our candidates, requiring that candidates have proper motions that agree with their supposed primaries' proper motions to within 01 yr⁻¹ in both R.A. and declination. This initial cut uses a tolerance that is much larger than our typical Pan-STARRS 1 proper motion errors of ∼5 mas yr⁻¹. Next, we made much more stringent cuts on proper motion to select only likely companions.

We restricted our search to objects which had proper motion differences compared to their primaries that were less significant than 5σ; here σ is the quadrature sum of the proper motion difference in each axis divided by the total proper motion error in that axis.

$$\begin{equation} \sigma ^2 = \frac{(\mu _{\alpha,1}-\mu _{\alpha,2})^2}{\sigma _{\mu _{\alpha,1}}^2+\sigma _{\mu _{\alpha,2}}^2} + \frac{(\mu _{\delta,1}-\mu _{\delta,2})^2}{\sigma _{\mu _{\delta,1}}^2+\sigma _{\mu _{\delta,2}}^2} \end{equation} \tag{ 1 }$$

Our typical proper motion errors in Pan-STARRS 1 + 2MASS data are ∼5 mas yr⁻¹. We selected two samples for follow-up observations. In all cases we set a zone of exclusion around the Galactic center |b| < 5° and l < 90 or l > 270.

• 1.  
  Ultracool companions. Objects with red Pan-STARRS1 colors (z_P1 − y_P1 > 0.8 mag) or (y_P1 − J_2MASS > 1.8 mag) were selected as candidate ultracool companions. These cuts should only select objects of spectral types M7 or later (Deacon et al. 2011). These targets also had their Pan-STARRS 1 and 2MASS colors inspected to ensure they truly were red objects and had not entered our sample due to erroneous z_P1 or y_P1 photometry. This involved removing objects with more than one g_P1 detection or with blue i_P1 − y_P1 colors.Note that two objects (the companions to LSPM J2153+1157 and NLTT 39312) are both close companions that did not meet our z_P1 − y_P1 color cut but were selected due to their red y_P1 − J_2MASS colors (>1.6) and close proximity (<12'') to their primaries. These were subsequently spectrally typed as ultracool dwarfs. These two objects may have had their photometry affected by the proximity of their primary.This sample yielded a total of 38 new discoveries, one of which (HIP 13589B) was simultaneously discovered by Allen et al. (2012). We have also re-identified and typed the NLTT 22073 system originally identified by Deacon & Hambly (2007) and HIP 78184 B originally proposed as a candidate companion by Pinfield et al. (2006).
• 2.  
  Bright companions. We selected the brightest of our common proper motion candidates (J_2MASS < 15.5 mag) for a poor-weather back-up program for our NASA IRTF SpeX observations regardless of their color. These objects were mostly within an arcminute of the primary, with all having separations smaller than 3'. This resulted in the discovery of 16 new, bright companions and the typing of 26 previously known companions.

As part of our ongoing search for T dwarfs in Pan-STARRS 1 data (see Deacon et al. 2011 and Liu et al. 2011 for more details), we have been obtaining follow-up near-infrared photometry of Pan-STARRS 1 selected candidates. UKIDSS (Lawrence et al. 2007) or VISTA (Emerson & Sutherland 2010) data were used where available; otherwise our candidate T dwarfs were observed using WFCAM (Casali et al. 2007) on the United Kingdom Infrared Telescope (UKIRT). We then cross-matched all our observed candidates with our combined proper motion catalog from Lépine & Shara (2005), Salim & Gould (2003), and Lépine & Gaidos (2011) with a pairing radius of 20'. Objects that had y_P1 − J_2MASS > 2.2 mag were initially selected to be T dwarf candidates. However, if the additional near-IR photometry did not match our y_P1 − J_MKO > 2.4 mag and J_MKO − H_MKO < 0.7 mag high priority T dwarf cut, but still met our y_P1 − J_MKO > 2.0 mag criterion, those objects were considered to be candidate L dwarfs. Any of these ∼500 candidates that then had proper motions which did not deviate by more than 5σ from their supposed primary stars were selected as candidate L companions for this search.

One of the serendipitous candidates we selected was a possible companion to the late-type high proper motion star NLTT 730. After searching the SIMBAD database, we identified our candidate object as 2MASS J00150206+2959323, a blue L7.5 dwarf found by Kirkpatrick et al. (2010) as a field object. As a blue L benchmark, this is similar to the G 203–50AB system identified by Radigan et al. (2008) although it is substantially wider (5070 AU versus 135 AU). This object is included in our subsequent analysis. In total we selected five serendipitous candidate companions.

Our proper motion companions are reported in Tables 2 and 3. A comparison between their proper motions and photometric distances (see Section 4.1.1) and the proper motions and distances of their primaries are shown in Table 4 for the Hipparcos companions and Table 5 for the companions to M dwarfs. In all our tables, the proper motions from the secondaries come from Pan-STARRS 1 + 2MASS proper motions. Where the object's 2MASS position was not included in the initial astrometric analysis we recalculated the proper motion solution including the 2MASS data. The proper motions and distances for all of our Hipparcos primaries come from van Leeuwen (2007).

Where companions have confused or noisy photometry, we have used UKIRT/WFCAM (Casali et al. 2007) to acquire additional near-infrared photometry. These data were reduced at the Cambridge Astronomical Survey Unit using the WFCAM survey pipeline (Irwin et al. 2004; Hodgkin et al. 2009). See Table 6 for the near-infrared photometry of our companions from our UKIRT observations, 2MASS (Skrutskie et al. 2006), UKIDSS (Lawrence et al. 2007), VISTA; (Emerson & Sutherland 2010), pre-release photometry from the UKIRT Hemisphere Survey (UHS; S. Dye et al., in preparation, accessed through the WFCAM Science Archive; Hambly et al. 2008) and Table 7 for mid-infrared photometry from WISE (Wright et al. 2010; Cutri et al. 2012).

To characterize our companions, we obtained 0.8–2.5 μm spectroscopy using the SpeX instrument (Rayner et al. 2003) on the NASA Infrared Telescope (IRTF). To minimize the possibility of observing an unrelated background object due to a non-physical chance alignment with one of our primaries, we preferentially followed-up (i.e., we were more likely to follow-up) companions closer than five arcminutes but did not follow-up all of our candidate companions. In total 115 candidate companions to stars were passed to the IRTF queue, 87 are presented here as true companions, 1 we classify as an unlikely companion, 2 are candidate white dwarf companions not presented in this work, and the remaining 26 were not observed.

Depending on the brightness of the object and the weather conditions, we used either the low-resolution (R ≈ 75–120) single-order prism mode or the moderate-resolution (R ≈ 750–2000) multiple-order cross-dispersed SXD mode. The slit width was chosen to match the seeing and was oriented along the parallactic angle to minimize atmospheric dispersion. The observations were taken in nodded ABBA patterns. The standards were taken contemporaneously with each science target and at similar airmass and sky position. We reduced all our spectra using version 3.4 of the SpeXtool software package (Cushing et al. 2004; Vacca et al. 2003). See Table 8 for details of the exposure times, weather conditions, and standard stars used for each object.

We spectrally classified our objects by visually comparing with the M and L near-infrared standards from Kirkpatrick et al. (2010). Additionally, for our L dwarf companions we measured three flux indices (H₂O-J, H₂O-H, and CH₄-K) from Burgasser et al. (2006) relevant for L dwarfs. We then applied the polynomial relations of Burgasser (2007) to derive spectral types, averaging over the types derived from each index. We note that the CH₄-K index does not depend strongly on spectral type earlier than mid-L and hence excluded this from the averaging for objects with this visual classification (see Table 9). Figures 1 and 2 show our early to mid-M dwarf companions to Hipparcos stars, Figure 3 shows our late-M and L dwarf Hipparcos companions, and Figure 4 shows our companions around non-Hipparcos primaries and serendipitous discoveries. Additionally, we observed a number of our primary stars that lacked spectral types in the literature. The spectra for these objects are shown in Figure 5.

For objects with spectral types earlier than M, there are no near-infrared standards so we compared with the spectral library of Cushing et al. (2005) and Rayner et al. (2009), selecting the best comparison spectrum visually. For any of our objects with spectral types earlier than M5, we specifically examined the ∼0.85 μm TiO feature in the Z-band and the Y-band 1 μm FeH feature. For two primaries classified as G dwarfs we also examined the strengths of metal and hydrogen lines. We identified one of our companions (HIP 88728 B) as having blue continua and weak Paschen lines. Hence we classify this object as a DA white dwarf (see Figure 6).

As a number of our primaries were poorly characterized, we obtained optical spectroscopy from both the Kitt Peak Mayall 4 m telescope and the University of Hawaii 2.2 m telescope.

3.3.1. Kitt Peak Mayall 4 m Spectroscopy

3.3.2. University of Hawaii 2.2 m Telescope/SNIFS Spectroscopy

In order to assess whether our candidate companions are merely alignments of unassociated stars, we undertook a test similar to Lépine & Bongiorno (2007). This consisted of taking all the objects in our input lists (Hipparcos, LSPM/rNLTT, and Lépine & Gaidos 2011) and offsetting their positions by two degrees in right ascension. We then searched for common proper motion companions to this list of modified positions. This test should only yield non-physical (coincident) pairings. To accurately reflect the probability of our objects being coincident contaminants, we applied the same cuts that were applied to our initial target sample. As an additional cut to exclude spuriously red objects (which we have excluded from our candidate sample by checking the objects' g_P1, r_P1, and i_P1 magnitudes) we excluded objects with more than one g_P1 detection.

In Figure 8, we compare the separation and proper motion differences for our HIP samples and the coincident population. All objects in both our bright and ultracool companion samples that were followed up spectroscopically lie in portions of the plot sparsely populated by coincident pairings. This is likely due to our approach of preferentially following-up closer companions. Figure 9 shows the results for companions to non-Hipparcos primaries and our serendipitous discoveries. Most of our discoveries lie in a completely different area of the plot from the coincident pairings. However, one object, the apparent companion to NLTT 35593, is in a region of the diagram populated by many coincident pairings, and therefore we do not consider it to be a bona-fide companion. Excluding this object, we consider it likely that less than five of our companions to Hipparcos stars will be chance alignments with background stars. For our faint non-Hipparcos primaries, at most, two could be chance alignments. All of these coincident pairs would lie in the lowest proper motion bin of our sample.

4.1.1. Photometric Distance

To further check the companionship of the objects, we derived photometric distances for all of our companions based on their spectral type. For objects of spectral types M6 and later, we derived the absolute magnitudes for our objects using the relations of Dupuy & Liu (2012) in J, H, and K/K_S. For earlier-type objects, we used the spectral energy distribution (SED) templates of Kraus & Hillenbrand (2007), who do not quote an rms for their relations. To estimate this we calculated the standard deviation of non-saturated 2MASS photometry of the FGK stars in Valenti & Fischer (2005) about the main sequence. These were found to be 0.25, 0.22, and 0.22 mag in J, H and K_s, respectively. Cruz & Reid (2002) calculated fits to the J-band absolute magnitude as a function of temperature-sensitive spectral features for M dwarfs. They found that the M dwarf population was well-fitted by two relations, one covering early M with an rms of ∼0.2 mag and the other covering late M with an rms of ∼0.35 mag. This latter number is comparable with the 0.39 mag rms on the 2MASS J-band relation of Dupuy & Liu (2012). Hence we use the rms of Dupuy & Liu (2012) for objects of spectral type M5 and later and our calculated rms for earlier-type objects.

Next, we calculated absolutes magnitude from the Kraus & Hillenbrand (2007) or Dupuy & Liu (2012) relations and compared these with the object's 2MASS photometry, or if available VISTA, UKIDSS, or UKIRT photometry, producing a distance estimate for each filter. Where non-2MASS near-infrared photometry was available for an object in a particular filter, we used this instead of 2MASS, making use of the Dupuy & Liu (2012) MKO relations for ultracool dwarfs and converting to the 2MASS system using the transformations of Carpenter (2001) for comparisons to the Kraus & Hillenbrand (2007) SEDs. We calculated the errors in distance caused by an uncertainty in spectral type, by the rms of the fits, and by the error on the 2MASS photometry. We then calculated the weighted mean of these distance estimates, weighting only by our measurement errors, i.e., the quadrature sum of the error in the photometric measurements and the propagated error in spectral typing. We then calculated a final error on this distance based on the quadrature sum of the photometric error, intrinsic scatter, and propagated error in spectral type for each band. Hence the final quoted error includes both the effects of measurement errors and the rms intrinsic scatter about the photometric relations. The calculated photometric distances are shown in Tables 4 and 5. Note that our white dwarf companion (HIP 88728 B), which was saturated in Pan-STARRS 1, is not resolved in plate images.

Zoom In Zoom Out Reset image size

Zoom In Zoom Out Reset image size

We also calculated photometric distances for our primaries that lacked trigonometric parallaxes. For primaries with measured spectral types, we applied a similar process as for our secondaries. Where there were no literature spectral distances we used relations from Lépine (2005) and the errors in those distances were calculated in the same way as for the secondaries. For our two white dwarf primaries we used the photometric distance relations of Limoges et al. (2013). For this we assumed a DA spectral type and a mass of 0.6 M_☉. Limoges et al. (2013) quote a photometric distance error of 15 pc for their sample with approximate distances of 30 pc. Hence we assume errors of 50% for our white dwarf photometric distances. It appears that most of our companions have photometric distances that are in good agreement with the distances to their primaries. This is shown in Figure 10.

4.2.1. Spectral Types

4.2.2. Age Estimates

Our sample contains 24 new L-dwarf companions to main sequence stars (including the previously typed but unrecognized L7 companion to NLTT 730 but not the unlikely L2 companion to NLTT 35593). Additionally we identified 21 new wide M-dwarf companions with spectral types of M7 or later and typed two previously proposed companions.

In order to study the wide ultracool (spectral type ⩾M7) binary population, we compiled a list of wide ultracool companions to stars (see Table 12). We began with the compilation of Faherty et al. (2010; excluding the companion to NLTT 20346 that Dupuy & Liu 2012 concluded was not physically related due to its high proper motion difference from its primary) and added spectroscopically confirmed objects from the literature discovered since then. We do not include objects that have been identified as candidate binaries but that lack spectral types such as from the studies of Deacon et al. (2009), Dhital et al. (2010), and Smith et al. (2014). Figure 12 shows the spectral type of the secondary plotted against the projected separation (r_AU). At first glance, there is an apparent scarcity of T dwarf companions wider than 3000 AU. In fact, this is due to previous efforts focusing on identifying close companions and from the known population being drawn from a series of heterogeneous surveys. Figure 13 shows a histogram comparing the combined contribution of this work, Deacon et al. (2012b) and Deacon et al. (2012a) to the total number of companions. This paper's contribution is most significant beyond log₁₀r_AU = 3.5 where we have doubled the population of L dwarf companions. In total we have increased the wide (>300 AU) L dwarf companion population by 82% and doubled the number of ultracool M dwarf companions in the same range. While the L dwarf population exhibits an approximately flat distribution in log₁₀r_AU, the T dwarf companion population peaks between log₁₀r_AU = 3.0 and 3.5. However, any claim of a preferred separation for T dwarf companions (or of a log-flat distribution for L dwarfs) should be treated with caution as the sample is drawn from a disparate set of surveys. Similarly the apparent cut-off above 10,000 AU is likely due to incompleteness in surveys (including our own) and the difficulty of disentangling the widest binaries from coincident alignments from field stars. In a future paper we aim to take the final results of our survey, model our selection biases, and determine the true separation distribution of the ultracool companion population.

In order to determine the stability of the population of systems containing a wide, ultracool companion, we estimated the total mass of each system. Where an object had a mass quoted in the literature, we used that value. For known L and T dwarfs with no quoted mass estimates and our new L and T companions, we used a value of 0.075 M_☉, in essence making our total mass estimates for these systems upper limits. For A–M stars with no mass in the literature, we converted their spectral type to mass using the relations of Kraus & Hillenbrand (2007).¹⁵ The results are plotted in Figure 14 along with the maximum separation versus total mass relations suggested by Close et al. (2003) and Reid et al. (2001). It is clear that a substantial number of late-type companions lie outside both of these suggested maximum boundaries and are hence loosely bound. Dhital et al. (2010) used a simple model of interactions in the Galactic disk (based on Weinberg et al. 1987) to calculate the typical maximum separation for a given system age and total mass. This is also plotted in Figure 14 for a number of different ages. It is clear that, though loosely bound, very few of the widest systems would be disrupted over the lifetime of the Galactic disk.

5.2.1. HIP 6407Bab

We initially classified HIP 6407B as an L0 based on visual comparison to standards. However, the object has significantly stronger water absorption features suggestive of an object two or three subtypes later. As this may result from the contribution of an unresolved additional component, we observed this object on 2013 October 14 UT at the Keck II telescope using the facility near-infrared camera NIRC2 with laser guide star adaptive optics (LGS AO; Wizinowich et al. 2006; van Dam et al. 2006). We kept the LGS centered in NIRC2's narrow field-of-view camera while we obtained dithered images of the target in the Y_NIRC2, J_MKO, H_MKO, and CH₄s bandpassess. The wavefront sensor recorded flux from the LGS equivalent to a V ≈ 9.6–9.8 mag star. The primary star HIP 6407 was used as the tip-tilt reference star, and the lower bandwidth sensor monitoring this source recorded flux equivalent to a R ≈ 7.6 mag star. Our procedure for reducing and analyzing Keck LGS data is described in detail in our previous work (e.g., Liu et al. 2006; Dupuy et al. 2010). To summarize briefly, we measure binary parameters by fitting three-component Gaussians to determine the position and flux of each binary component, and we derive uncertainties by computing the scatter among individual dithered images. We used the NIRC2 astrometric calibration from Yelda et al. (2010), which includes a correction for the nonlinear distortion of the camera and has a pixel scale of 9.952 ± 0.002 mas per pixel and an orientation for the detector's +y axis of +0252 ± 0009 east of north. We resolved HIP 6407B as a 0131 (7.4 AU) binary. Table 13 gives the binary parameters we measured in each bandpass along with the weighted average of the separation (ρ) and position angle (P.A.) values. Given the objects' separation and maximum total mass of 0.16 M_☉ (as it consists of two substellar objects), the likely period of this system is >300 yr, making it a poor mass–age benchmark.

Table 2. Summary Information on Our Wide Companions

Object	WDS	Position	SpT	SpT	yP1	J2MASS	dprimary	Separation	Separation	Metallicityk	Age
	Designation	(Eq. = J2000 Ep. = 2010.0)	Primary	Secondary	(mag)	(mag)	(pc)	('')	(AU)	(dex)	(Gyr)
HIP search companions
HIP 2397 B	...	00 30 24.94 +22 44 47.1	K5	L0.5	16.606 ± 0.008	14.586 ± 0.038	[33.9$_{-1.3}^{+1.4}$]	117.1	3970	...	0.5–∼10y
HIP 6217 C	...	01 19 44.74 +00 06 18.5	K0	M9.5	16.859 ± 0.009	15.441 ± 0.060	[$70.9_{-11.7}^{+14.0}$]	27.4	2767	...	0.4–∼10y1
HIP 6407 B	...	01 22 16.99 +03 31 22.0	G5	L1+T3l	17.527 ± 0.027	15.471 ± 0.046	[57.2$_{-3.0}^{+3.3}$]	44.9	2570	...	0.5–∼10y
HIP 9269 B‡	...	01 59 10.98 +33 12 27.8	G5	L6	18.266 ± 0.031	15.956 ± 0.088	[25.0$_{-0.4}^{+0.3}$]	52.1	1300	0.15	2.2–10.2i
HIP 10033 B	...	02 09 10.58 −02 19 19.0	F8	M5	15.14 ± 0.003	13.761 ± 0.027	[69.7$_{-3.1}^{+3.4}$]	42.9	2990	−0.08	2.7–3.7j
HIP 11161 B	...	02 23 36.59 +52 40 05.9	F5	L1.5	18.785 ± 0.067	16.636 ± 0.161	[69.3$_{-3.6}^{+4.1}$]	47.7	3300	−0.23	0.5–2.4j
HIP 13589 B*	...	02 55 07.10 +21 36 21.1	G0	M7.5	17.098 ± 0.009	14.928 ± 0.034	[72.8$_{-4.0}^{+4.6}$]	49.2	3580	...	0.4–∼10y
HIP 26653 B	...	05 39 49.51 +52 53 58.3	G5	L5	16.905 ± 0.012	14.756 ± 0.044	[$18.8_{-3.1}^{+3.7}$]	27.0	753	−0.07	1.1–9.3i
										−0.1	1.6–13.8j
HIP 32728 B	...	06 49 30.59 +36 26 26.0	G0	M6.5	16.060 ± 0.006	14.508 ± 0.031	[46.6$_{-2.6}^{+2.9}$]	94.3	4400	...	0.3–∼10y
HIP 37283 B†	07394+5032 B	07 39 32.03 +50 31 07.3	F5	M6	14.214 ± 0.002	12.797 ± 0.027	[45.5$_{-1.2}^{+1.2}$]	106.1	4830	−0.1	0.4–2.1j
HIP 46984 B	...	09 34 33.18 +03 34 07.0	F8	M4	14.521 ± 0.002	13.285 ± 0.027	[74.7$_{-6.9}^{+8.6}$]	37.5	2800	...	0.4–∼10y
HIP 49046 B†	10004+2716 B	10 00 35.71 +27 17 06.7	M0	M6.5	14.482 ± 0.002	13.022 ± 0.022	[34.7$_{-2.3}^{+2.6}$]	136.1	4720	...	0.3–∼10z
HIP 51877 B	...	10 35 54.72 +36 55 41.0	G5	M9.5	16.935 ± 0.008	15.205 ± 0.063	[$57.4_{-9.6}^{+11.5}$]	17.6	954	0.22u	2.4–7.5i
HIP 52463 B†	10435–1852 B	10 43 26.65 −18 52 18.2	G4	M5	15.043 ± 0.003	13.703 ± 0.024	[74.2$_{-4.5}^{+5.2}$]	43.5	3230	0.14	1.0–4.9j
HIP 55666 B‡	...	11 24 23.43 −05 54 09.8	F5	M5.5	14.533 ± 0.037	12.674 ± 0.024	[49.8$_{-1.5}^{+1.5}$]	37.2	1850	0.14	3.6–5.1j
HIP 58918 B†	12049+3437 B	12 04 52.15 +34 37 23.2	K1	M7	15.849 ± 0.004	14.471 ± 0.03	[55.8$_{-5.1}^{+6.2}$]	20.0	1110	...	0.1–∼10y
HIP 59310 B†	12101+1859 B	12 10 09.79 +18 58 07.9	K5	M7	15.252 ± 0.002	13.691 ± 0.027	[44.4$_{-2.8}^{+3.2}$]	82.1	3650	...	0.2–∼10y
HIP 59933 B	...	12 17 36.41 +14 27 11.7	F8	L1	18.111 ± 0.032	16.101 ± 0.088	[57.0$_{-2.4}^{+2.7}$]	38.1	2170	0.03	0.3–2.5j
HIP 60501 B†	12241+0357 B	12 24 09.68 +03 56 03.3	M0	M5	12.876 ± 0.022	11.378 ± 0.027	[56.6$_{-6.0}^{+7.6}$]	37.1	2100	...	0.3–∼10z
HIP 60987 B†c	12300–0601 B	12 30 01.60 −06 01 23.7	F2	K7	...	...	[61.9$_{-2.3}^{+2.4}$]	∼5	∼300	−0.12	1.3–2.4j
HIP 60987 C†	12300–0601 C	12 30 00.68 −06 01 17.9	F2	M3	12.553 ± 0.001	11.402 ± 0.028	[61.9$_{-2.3}^{+2.4}$]	19.0	1170	−0.12	2.0j
HIP 63506 Cf	13008+4213 C	13 00 50.27 +42 14 47.6	M0	L1	16.999 ± 0.008	15.15 ± 0.042	[42.5$_{-3.9}^{+4.7}$]	132.8	5640	...	0.3–∼10z
HIP 65706 B†	13284+3005 B	13 28 20.77 +30 03 17.0	K7	M7	15.016 ± 0.003	13.315 ± 0.022	[51.1$_{-4.0}^{+4.8}$]	52.6	2690	...	0.3–∼10z
HIP 65780 Cf	13291+1128 C	13 29 06.09 +11 27 52.2	K0	M5	14.327 ± 0.001	13.580 ± 0.002h	[58.0$_{-3.3}^{+3.7}$]	16.0	928	...	0.5–∼10y
HIP 70623 B†	14268–0511 B	14 26 45.74 −05 10 20.9	K0	M5.5	13.619 ± 0.003	12.191 ± 0.026	[72.6$_{-4.7}^{+5.5}$]	41.9	3040	0.46	3.3–6.0i
HIP 75310 B	...	15 23 10.01 −10 28 58.4	G5	M5	14.668 ± 0.003	13.291 ± 0.032	[66.9$_{-5.1}^{+6.0}$]	22.9	1530	−0.22	6.3–9.3j
HIP 76456 B	...	15 36 56.27 +29 59 31.1	F5	M6.5	14.753 ± 0.002	13.300 ± 0.031	[36.8$_{-0.6}^{+0.6}$]	36.1	1330	−0.25	0.4–2.2j
HIP 76641 B	...	15 38 59.53 +43 52 17.2	G5	M3.5	12.158 ± 0.001	10.817 ± 0.018	[82.1$_{-4.7}^{+5.3}$]	42.1	3460	...	0.4–∼10y
HIP 78184 Bm	15578+5916 B	15 57 55.32 +59 14 25.3	M0	M9	16.219 ± 0.024	14.32 ± 0.031	[31.4$_{-1.3}^{+1.4}$]	121.8	3820	...	0.3–∼10z
HIP 78859 B†	16059+3500 B	16 05 49.62 +34 59 53.9	G0	M5	13.57 ± 0.009	12.258 ± 0.021	[57.2$_{-2.1}^{+2.3}$]	42.6	2440	...	0.7–∼10y
HIP 78916 B	...	16 06 32.22 +22 53 34.5	G0	M8	16.694 ± 0.008	15.227 ± 0.043	[92.9$_{-9.2}^{+11.5}$]	35.5	3294	...	0.4–∼10y
HIP 78923 B	...	16 06 38.65 +34 06 19.3	G5	M8	15.565 ± 0.004	14.052 ± 0.048	[46.1$_{-1.7}^{+1.8}$]	15.5	714	−0.1j	0.4–4.0j
HIP 79180 B†	16097+6550 B	16 09 42.06 +65 49 18.1	K7	M5	15.315 ± 0.003	13.941 ± 0.022	[74.7$_{-3.4}^{+3.7}$]	29.0	2170	...	0.3–∼10z
HIP 80258 B†	16231+3650 B	16 23 09.09 +36 50 50.2	K3	M4	14.487 ± 0.004	13.113 ± 0.021	[63.7$_{-7.5}^{+9.6}$]	54.9	3500	...	0.1–∼10y
HIP 81910 B	...	16 43 49.50 −26 48 40.2	G2	M6	13.852 ± 0.025	12.44 ± 0.024	[46.4$_{-0.8}^{+0.9}$]	26.7	1240	0.19	4.0–5.8j
HIP 82233 B	...	16 48 03.98 −15 57 56.7	G2	M5.5	13.198 ± 0.009	11.889 ± 0.024	[42.1$_{-1.2}^{+1.3}$]	30.4	1280	−0.05	0.7–4.7j
HIP 83651 B†	17058+0458 B	17 05 49.00 +04 57 24.8	K5	M3	12.529 ± 0.052	10.599 ± 0.024	[50.9$_{-4.2}^{+4.9}$]	28.9	1470	...	0.1–∼10y
HIP 84840 B2	...	17 20 22.02 +20 17 01.1	G1.5	M4	13.852 ± 0.007	12.508 ± 0.024	[$112_{-15}^{+19}$]	16.9	1890	...	0.1–∼10y
HIP 85365 B	...	17 26 22.29 −05 02 11.2	F3	L5.5	18.55 ± 0.045	16.693 ± 0.168	[30.1$_{-0.2}^{+0.2}$]	294.1	8850	−0.09	1.6–1.9j
HIP 86722 B†b	17433+2137 B	17 43 15.32 +21 36 04.2	K0	M5.5	12.971 ± 0.018	11.511 ± 0.025	[22.7$_{-0.5}^{+0.4}$]	22.8	520	−0.33	3.0–11.8j
HIP 88728 B	...	18 06 50.92 +08 52 24.0	F5	DA	12.571 ± 0.019	10.269 ± 0.097	[$40.4_{-1.1}^{+1.2}$]	9.6	316	−0.1o	1.5–∼10y
HIP 90273 B†	18251+3016 B	18 25 11.57 +30 16 43.2	K7	M3.5	12.891 ± 0.054	11.56 ± 0.022	[55.4$_{-7.3}^{+10.0}$]	26.9	1490	...	0.3–∼10z
HIP 90869 B	...	18 32 11.05 −26 29 45.1	G2	M2	12.428 ± 0.042	11.101 ± 0.029	[56.4$_{-3.0}^{+3.4}$]	17.5	990	−0.46	5.3–10.8j
										1.9–5.7k
HIP 93967 B	...	19 07 56.43 −15 14 16.3	F9	M3.5	14.529 ± 0.007	13.357 ± 0.03	[122.1$_{-19.6}^{+29.0}$]	22.2	2710	...	0.2–∼10y
HIP 97168 B†	19450+5136 B	19 44 59.38 +51 35 31.3	G4	M5.5	14.997 ± 0.004	13.679 ± 0.027	[97.5$_{-10.4}^{+13.1}$]	12.6	1230	...	0.1–∼10y
HIP 98535 C‡f	20011+4816 E	20 01 02.17 +48 16 27.8	F5	M5.5	14.763 ± 0.065	13.252 ± 0.031	[60.0$_{-3.3}^{+3.8}$]	61.7	3700	−0.02	0.6–13.2j
HIP 102582 B†	20473+1052 B	20 47 16.75 +10 51 45.1	K2	M5	13.256 ± 0.001	11.963 ± 0.033	[31.3$_{-1.3}^{+1.4}$]	14.7	459	...	0.2–∼10y
HIP 103199 B†	20547+3046 B	20 54 33.60 +30 45 40.6	G5	M3.5	13.161 ± 0.01	11.817 ± 0.027	[59.5$_{-4.3}^{+5.1}$]	10.9	650	...	0.2–∼10y
HIP 105202 B†	21187+0857 B	21 18 42.31 +08 56 45.0	F5	M4	13.456 ± 0.019	12.124 ± 0.024	[41.8$_{-1.3}^{+1.4}$]	89.4	3740	−0.29	0.6–2.9j
HIP 106551 B	...	21 34 45.17 +38 31 00.1	K3III	M5	14.597 ± 0.01	13.224 ± 0.025	[71.0$_{-2.1}^{+2.2}$]	66.1	4690	...	⩽10aa
HIP 108822 B†	22028+1207 B	22 02 48.15 +12 07 05.0	K7	M3	12.079 ± 0.002	10.622 ± 0.022	[44.4$_{-6.1}^{+8.5}$]	31.8	1410	...	0.3–∼10z
HIP 109454 B	...	22 10 27.58 +30 48 28.1	F5	M3	13.729 ± 0.116	12.422 ± 0.026	[100.9$_{-5.8}^{+6.5}$]	18.2	1840	−0.19	1.4–2.1j
HIP 111657 B†	22371+1159 B	22 37 08.65 +11 58 53.0	K7	M4	11.978 ± 0.041	10.587 ± 0.032	[41.9$_{-3.0}^{+3.3}$]	7.8	330	...	0.3–∼10z
HIP 112422 B‡b	22463+3319 C	22 46 18.57 +33 19 30.5	K2	L1.5	17.776 ± 0.021	16.023 ± 0.113	[65.4$_{-6.6}^{+8.3}$]	16.0	1040	...	0.1–∼10*y
HIP 114424 B	...	23 10 22.08 −07 48 54.7	G0	M5.5	13.089 ± 0.001	11.595 ± 0.026	[35.1$_{-0.9}^{+1.1}$]	42.0	1480	0.08	0.6–4.5j
										0.06	3.7–11.7i
HIP 114456 B†‡a	23108+4531 C	23 10 54.78 +45 30 43.8	K0	M5	12.371 ± 0.003	10.844 ± 0.021	[24.3$_{-0.3}^{+0.3}$]	50.4	1220	0.19	2.1–9.6k
HIP 115819 B	...	23 27 49.76 +04 51 00.1	K5	M8	16.865 ± 0.022	15.095 ± 0.034	[65.7$_{-8.2}^{+11.0}$]	30.4	2000	...	0.2–∼10y
HIP 116052 B†	23309+2747 B	23 30 52.38 +27 46 32.3	G5	M3.5	13.718 ± 0.002	12.361 ± 0.019	[49.6$_{-2.3}^{+2.5}$][]	26.8	1330	...	0.3–∼10y
Companions to faint non-HIP primaries
NLTT 1011 B	...	00 19 32.68 +40 18 55.4	K7	L2	17.615 ± 0.015	15.544 ± 0.059	68.2$_{-6.5}^{+6.6}$	58.5	3990	...	0.3–∼10z
GD 280 B	...	01 54 58.13 +48 19 59.1	DA	M9	17.624 ± 0.013	16.034 ± 0.082	$77_{-26}^{+35}$	63.4	4882	...	<10aa
NLTT 8245 B	...	02 33 23.52 +65 45 47.6	M0	M7	16.465 ± 0.007	14.922 ± 0.052	$53.0_{-7.5}^{+8.7}$	10.6	562	...	0.3–∼10z
LSPM J0241+2553 B	...	02 41 51.51 +25 53 43.4	WD	L1	19.074 ± 0.05	17.027 ± 0.180	$69_{-23}^{+35}$	31.2	2153	...	<10aa
HD 253662 B	...	06 13 53.35 +15 14 04.4	G8IV	L0.5	17.691 ± 0.02	15.961 ±.0082	>62.3	20.1	>1252	...	<10aa
LSPMJ0632+5053 B	...	06 32 48.55 +50 53 33.6	G2	L1.5	18.86 ± 0.04	16.383 ± 0.108	95.0$_{-13.9}^{+16.3}$	47.4	4499	...	0.2–∼10y
NLTT 18587 B	...	07 54 13.38 +37 21 42.6	M2	M7.5	18.03 ± 0.026	16.894 ± 0.199	$132_{-31}^{+40}$	92.4	12200	...	0.3–∼1z
NLTT 19109 B	...	08 11 59.00 −08 58 01.6	M4	M8.5	18.36 ± 0.044	16.933 ± 0.170	$132_{-36}^{+49}$	7.5	362	...	0.3–∼10z
NLTT 22073 Bg	...	09 33 37.11 −27 52 45.4	M2	M7.5	16.303 ± 0.007	14.671 ± 0.037	29.9$_{-6.9}^{+12.7}$	26	776	...	0.4–∼10x
NLTT 23716 B	...	10 13 17.05 −06 01 22.9	K7	M8	15.884 ± 0.006	14.300 ± 0.036	$48.2_{-6.8}^{+7.9}$	15.0	723	...	0.3–∼10z
NLTT 26746 B	...	11 15 01.22 +16 07 00.8	M4	L4	18.36 ± 0.06	16.403 ± 0.118	41.0$_{-10.3}^{+12.2}$	18.0	661	...	0.3–∼10z
NLTT 29395 B	...	12 03 02.61 +58 06 02.4	M3	M8	17.397 ± 0.013	15.810 ± 0.080	$56.4_{-13.0}^{+16.9}$	11.9	671	...	0.3–∼10z
NLTT 30510 B	...	12 22 18.59 +36 43 48.1	M2	M9.5	17.716 ± 0.016	15.971 ± 0.080	$49.1_{-11.3}^{+14.8}$	19.6	962	...	0.3–∼10z
NLTT 31450 B	...	12 39 49.19 +32 09 03.1	M4	L6	18.34 ± 0.03	16.135 ± 0.105	34.6$_{-8.7}^{+10.3}$	12.3	487	...	0.3–∼10z
PMI 13410+0542 B	...	13 41 02.39 +05 42 48.8	M1	L4	18.00 ± 0.02	16.187 ± 0.143	51.3$_{-11.8}^{+21.7}$	9.4	484	...	0.3–∼10z
PMI 13518+4157 B	...	13 51 47.41 +41 57 47.4	M2.5	L1.5	17.17 ± 0.01	15.081 ± 0.032	43.1$_{-8.8}^{+9.9}$	21.6	613	...	0.3–∼10z
NLTT 38489 B	...	14 48 46.28 +56 10 57.8	M4	M9	18.62 ± 0.04	16.64 ± 0.143	62.3$_{-17.0}^{+23.3}$	6.7	418	...	1.2–∼10x
NLTT 39312 B	...	15 05 59.27 +33 39 30.2	M2	M8	17.768 ± 0.018	16.09 ± 0.096	140.9$_{-32.7}^{+42.6}$	5.1	713	...	0.3–∼10z
LSPM J1627+3328 B	...	16 27 01.44 +33 28 21.4	K7	M9	16.386 ± 0.018	14.362 ± 0.083	38.0$_{-5.4}^{+6.3}$	9.0	341	...	0.3–∼10z
NLTT 44368 B	...	17 11 57.29 +54 30 43.8	M3	L1.5	16.754 ± 0.016	14.736 ± 0.058	55.0$_{-11.3}^{+12.7}$	90.2	7760	...	0.3–∼10z
LSPM J1717+5925 B	...	17 17 30.94 +59 25 30.2	G6	M9	18.043 ± 0.015	16.580 ± 0.168	108.0$_{-26.4}^{+34.8}$	14.4	1555	...	0.2–∼10y
NLTT 52268 B	...	21 51 07.23 +30 45 54.7	M3	M9	16.67 ± 0.03	14.945 ± 0.052	37.3$_{-8.7}^{+11.3}$	14.7	549	...	0.3–∼10z
LSPM J2153+1157 B	...	21 53 46.92 +11 57 46.4	M3	M7	16.005 ± 0.004	14.403 ± 0.038	36.2$_{-8.4}^{+10.9}$	11.3	408	...	0.3–∼10z
PM I22118−1005 B	...	22 11 41.25 −10 08 20.8	M2	L1.5	17.412 ± 0.010	15.246 ± 0.049	37.4$_{-7.7}^{+8.6}$	204.5	8892	...	0.3–∼10z
NLTT 55219 B	...	22 54 28.58 +22 02 56.1	M2	L5.5	18.791 ± 0.039	16.313 ± 0.122	44.7$_{-10.4}^{+13.5}$	9.7	432	...	0.3–∼10z
Serendipitous Companion Discoveries
NLTT 730 B	...	00 15 02.40 +29 59 29.8	M4	L7.5pd	18.37 ± 0.06	16.16 ± 0.08	21.7$_{-5.3}^{+8.1}$	233.6	5070	...	3–∼10z
NLTT 27966 B	...	11 36 39.44 +48 52 43.0	M5	L4	18.48 ± 0.05	16.155 ± 0.103	39.6$_{-10.2}^{+13.3}$	15.9	630	...	0.3–∼10z
LSPMJ1336+2541 B	...	13 36 24.89 +25 40 37.2	M3	L4	19.45 ± 0.09	16.863 ± 0.16	60.7$_{-13.9}^{+15.7}$	121.7	8793	...	0.3–∼10z
HIP 73169 Be	...	14 57 11.35 −06 19 27.4	M0	L2.5	18.42 ± 0.09	16.007 ± 0.09	[27.3$_{-6.3}^{+8.3}$]	29.1	796	...	0.3–∼10z
PM I23492+3458 B	...	23 49 15.11 +34 58 55.3	M2	L9	18.80 ± 0.04	16.298 ± 0.105	30.7$_{-6.3}^{+7.1}$	34.9	949	...	0.3–∼10z
Unlikely Companions
NLTT 35593 B	...	13 54 34.92−06 07 34.3	M2	L2	18.56 ± 0.03	16.299 ± 0.114	63.0$_{-14.6}^{+19.1}$	1105.8	69706	...	0.3–∼10'z

Notes.^[] Denotes distance from trigonometric parallax; all other distances are photometric. † Previously known in the Washington Double Star Catalog. ‡ Additional possibly spurious companion in the system in the Washington Double Star Catalog. * Simultaneously discovered by Allen et al. (2012). ^aOur object appears in the Washington Double Star Catalog as component C due to a spurious companion listed as B. ^bPrimary is itself a close double listed as Aa and Ab in the Washington Double Star Catalog. ^cThe companion was identified as a visual double during IRTF acquisition; due to saturation, it does not appear in our PS1 catalog. Position is taken from VISTA image. ^dSpectral type from Kirkpatrick et al. (2010). We identify this object as a companion to NLTT 730. ^eWhile HIP 73169 appears in the Hipparcos catalog, its parallax measurement was too low significance for it to be included in our input Hipparcos sample. Hence it appears in our sample of other primaries due to it being a nearby M dwarf in the proper motion catalog of Salim & Gould (2003). ^fPrimary is itself a binary with a listing in the Washington Double Star Catalog. Our companion is component C. ^gPreviously identified by Deacon & Hambly (2007) as a binary pair. The secondary is also known as SIPS 0933−2752 ^hThe 2MASS photometry is only an upper limit; photometry taken from UKIDSS Lawrence et al. (2007). ⁱValenti & Fischer (2005). ^jCasagrande et al. (2011). ^kMetallicity definition depends on source; metallicities from ⁱ are [M/H] while those from ^j are [Fe/H]. ^lEstimated spectral types from spectral deblending. See Section 5.2.1. ^mPreviously identified as a candidate companion by Pinfield et al. (2006). ^oMetallicity from Lee et al. (2011). ^wRobinson et al. (2007). ^xThis work, minimum age calculated from lack of activity and the activity lifetimes of West et al. (2008), approximate maximum age from disk-like kinematics. ^yThis work, minimum age calculated from limiting X-ray flux and the relations of Mamajek & Hillenbrand (2008), approximate maximum age from disk-like kinematics. ^zThis work, minimum age is that from Shkolnik et al. (2009) for objects with no X-ray emission, approximate maximum age from disk-like kinematics. ^aaThis work, approximate maximum age from disk-like kinematics. ¹ Object primary is a spectroscopic binary. ² Previously identified in Lépine & Bongiorno (2007).

Download table as:  ASCIITypeset images: 1 2 3

Table 3. PS1 Data of Our Wide Companions

Object	Position	SpT	gP1	rP1	iP1	zP1	yP1
	(Eq. = J2000 Ep. = 2010.0)		(mag)	(mag)	(mag)	(mag)	(mag)
HIP search companions
HIP 2397 B	00 30 24.94 +22 44 47.1	L0.5	...	...	19.085 ± 0.013	17.49 ± 0.022	16.606 ± 0.008
HIP 6217 C	01 19 44.74 +00 06 18.5	M9.5	21.656 ± 0.11	21.076 ± 0.071	18.6 ± 0.019	17.444 ± 0.007	16.859 ± 0.009
HIP 6407 B	01 22 16.99 +03 31 22.0	L1+T3d	...	...	20.094 ± 0.042	18.534 ± 0.015	17.527 ± 0.027
HIP 9269 B‡	01 59 10.98 +33 12 27.8	L6	...	...	...	...	18.266 ± 0.031
HIP 10033 B	02 09 10.58 −02 19 19.0	M5	19.709 ± 0.017	18.297 ± 0.007	16.456 ± 0.003	15.54 ± 0.003	15.14 ± 0.003
HIP 11161 B	02 23 36.59 +52 40 05.9	L1.5	...	...	21.24 ± 0.095	19.475 ± 0.051	18.785 ± 0.067
HIP 13589 B*	02 55 07.10 +21 36 21.1	M7.5	...	...	...	18.003 ± 0.012	17.098 ± 0.009
HIP 26653	05 39 49.51 +52 53 58.3	L5	...	20.542 ± 0.043	...	17.719 ± 0.011	16.905 ± 0.012
HIP 32728 B	06 49 30.59 +36 26 26.0	M6.5	...	21.26 ± 0.08	18.057 ± 0.006	16.721 ± 0.007	16.060 ± 0.006
HIP 37283 B†	07 39 32.03 +50 31 07.3	M6	18.985 ± 0.01	17.622 ± 0.006	15.593 ± 0.002	14.639 ± 0.001	14.214 ± 0.002
HIP 46984 B	09 34 33.18 +03 34 07.0	M4	18.199 ± 0.006	17.038 ± 0.004	15.444 ± 0.003	14.848 ± 0.002	14.521 ± 0.002
HIP 49046 B†	10 00 35.71 +27 17 06.7	M6.5	20.127 ± 0.021	18.7 ± 0.007	16.282 ± 0.002	15.138 ± 0.002	14.482 ± 0.002
HIP 51877 B	10 35 54.72 +36 55 41.0	M9.5	...	20.23 ± 0.039	19.207 ± 0.011	17.801 ± 0.004	16.935 ± 0.008
HIP 52463 B	10 43 26.65 −18 52 18.2	M5	19.576 ± 0.018	18.25 ± 0.02	16.599 ± 0.011	15.479 ± 0.001	15.043 ± 0.003
HIP 55666 B‡	11 24 23.43 −05 54 09.8	M5.5	...	...	...	...	14.533 ± 0.037
HIP 58918 B†	12 04 52.15 +34 37 23.2	M7	21.445 ± 0.092	20.122 ± 0.026	17.623 ± 0.006	16.491 ± 0.004	15.849 ± 0.004
HIP 59310 B†	12 10 09.79 +18 58 07.9	M7	21.021 ± 0.052	19.579 ± 0.012	17.077 ± 0.005	15.88 ± 0.002	15.252 ± 0.002
HIP 59933 B	12 17 36.41 +14 27 11.7	L1	...	...	...	19.079 ± 0.025	18.111 ± 0.032
HIP 60501 B†	12 24 09.68 +03 56 03.3	M5	17.074 ± 0.004	15.814 ± 0.002	14.207 ± 0.038	13.313 ± 0.001	12.876 ± 0.022
HIP 60987 B†c	12 30 01.60 −06 01 23.7	K7
HIP 60987 C†	12 30 00.68 −06 01 17.9	M3	15.395 ± 0.005	14.336 ± 0.001	...	12.825 ± 0.001	12.553 ± 0.001
HIP 63506 C‡	13 00 50.27 +42 14 47.6	L1	...	22.019 ± 0.122	19.49 ± 0.014	17.964 ± 0.007	16.999 ± 0.008
HIP 65706 B†	13 28 20.77 +30 03 17.0	M7	...	...	...	...	15.016 ± 0.003
HIP 65780 Cf	13 29 06.09 +11 27 52.2	M5	18.523 ± 0.001	17.393 ± 0.001	15.669 ± 0.001	14.724 ± 0.001	14.327 ± 0.001
HIP 70623 C†	14 26 45.74 −05 10 20.9	M5.5	17.424 ± 0.008	16.233 ± 0.013	14.762 ± 0.061	13.981 ± 0.001	13.619 ± 0.003
HIP 75310 B	15 23 10.01 −10 28 58.4	M5	20.018 ± 0.062	...	15.647 ± 0.003	15.055 ± 0.003	14.668 ± 0.003
HIP 76456 B†	15 36 56.27 +29 59 31.1	M6.5	19.827 ± 0.017	19.027 ± 0.006	16.513 ± 0.002	15.343 ± 0.002	14.753 ± 0.002
HIP 76641 B	15 38 59.53 +43 52 17.2	M3.5	...	...	17.225 ± 0.036	13.026 ± 0.001	12.158 ± 0.001
HIP 78184 B	15 57 55.32 +59 14 25.3	M9	...	21.043 ± 0.054	18.642 ± 0.014	17.167 ± 0.013	16.219 ± 0.024
HIP 78859 B†	16 05 49.62 +34 59 53.9	M5	16.9 ± 0.004	15.633 ± 0.024	14.422 ± 0.004	13.832 ± 0.009	13.57 ± 0.009
HIP 78916 B	16 06 32.22 +22 53 34.5	M8	22.05 ± 0.16	19.694 ± 0.021	18.506 ± 0.009	17.354 ± 0.006	16.694 ± 0.008
HIP 78923 B	16 06 38.65 +34 06 19.3	M8	...	...	17.219 ± 0.006	16.187 ± 0.002	15.565 ± 0.004
HIP 79180 B†	16 09 42.06 +65 49 18.1	M5	20.008 ± 0.02	18.815 ± 0.013	16.718 ± 0.003	15.985 ± 0.003	15.315 ± 0.003
HIP 80258 B†	16 23 09.09 +36 50 50.2	M4	18.321 ± 0.062	16.993 ± 0.023	15.497 ± 0.002	14.782 ± 0.111	14.487 ± 0.004
HIP 81910 B	16 43 49.50 −26 48 40.2	M6	...	17.478 ± 0.068	15.494 ± 0.012	14.678 ± 0.344	13.852 ± 0.025
HIP 82233 B	16 48 03.98 −15 57 56.7	M5.5	...	15.693 ± 0.003	14.218 ± 0.001	...	13.198 ± 0.009
HIP 83651 B†	17 05 49.00 +04 57 24.8	M3	14.977 ± 0.001	13.978 ± 0.035	12.809 ± 0.07	12.018 ± 0.001	12.529 ± 0.052
HIP 84840 B	17 20 22.02 +20 17 01.1	M4	17.489 ± 0.019	16.272 ± 0.008	14.869 ± 0.002	14.126 ± 0.014	13.852 ± 0.007
HIP 85365 B	17 26 22.29 −05 02 11.2	L5.5	...	...	21.606 ± 0.13	19.547 ± 0.05	18.55 ± 0.045
HIP 86722 B†	17 43 15.32 +21 36 04.2	M5.5	...	...	...	14.184 ± 0.003	12.971 ± 0.018
HIP 88728 B	18 06 50.92 +08 52 24.0	DA	...	14.377 ± 0.203	...	13.66 ± 0.002	12.571 ± 0.019
HIP 90273 B	18 25 11.57 +30 16 43.2	M3.5	16.348 ± 0.003	15.307 ± 0.294	13.905 ± 0.066	13.117 ± 0.004	12.891 ± 0.054
HIP 90869 B	18 32 11.05 −26 29 45.1	M2	15.375 ± 0.024	14.156 ± 0.026	...	12.443 ± 0.001	12.428 ± 0.042
HIP 93967 B	19 07 56.43 −15 14 16.3	M3.5	17.723 ± 0.023	...	15.433 ± 0.028	14.75 ± 0.027	14.529 ± 0.007
HIP 97168 B	19 44 59.38 +51 35 31.3	M5.5	18.5 ± 0.014	17.241 ± 0.009	16.081 ± 0.007	15.38 ± 0.007	14.997 ± 0.004
HIP 98535 Cf	20 01 02.17 +48 16 27.8	M5.5	19.513 ± 0.046	...	16.077 ± 0.031	15.183 ± 0.057	14.763 ± 0.065
HIP 102582 B†	20 47 16.75 +10 51 45.1	M5	17.437 ± 0.003	16.140 ± 0.003	14.408 ± 0.001	13.601 ± 0.002	13.256 ± 0.001
HIP 103199 B†	20 54 33.60 +30 45 40.6	M3.5	16.513 ± 0.004	...	15.03 ± 0.912	13.415 ± 0.005	13.161 ± 0.01
HIP 105202 B†	21 18 42.31 +08 56 45.0	M4	17.221 ± 0.097	15.867 ± 0.031	14.41 ± 0.01	13.718 ± 0.002	13.456 ± 0.019
HIP 106551 B	21 34 45.17 +38 31 00.1	M5	19.019 ± 0.056	17.677 ± 0.034	15.958 ± 0.01	14.979 ± 0.01	14.597 ± 0.01
HIP 108822 B†	22 02 48.15 +12 07 05.0	M3	15.019 ± 0.007	13.995 ± 0.185	13.459 ± 0.451	12.478 ± 0.092	12.079 ± 0.002
HIP 109454 B	22 10 27.58 +30 48 28.1	M3	16.605 ± 0.004	...	...	13.895 ± 0.002	13.729 ± 0.116
HIP 111657 B†	22 37 08.65 +11 58 53.0	M4	15.678 ± 0.011	14.389 ± 0.015	14.477 ± 0.337	...	11.978 ± 0.041
HIP 112422 B‡b	22 46 18.57 +33 19 30.5	L1.5	...	...	19.899 ± 0.041	18.907 ± 0.016	17.776 ± 0.021
HIP 114424 B†‡	23 10 22.08 −07 48 54.7	M5.5	...	16.296 ± 0.004	14.444 ± 0.004	13.548 ± 0.076	13.089 ± 0.001
HIP 114456 B†‡a	23 10 54.78 +45 30 43.8	M5	17.26 ± 0.054	...	14.055 ± 0.001	13.063 ± 0.001	12.371 ± 0.003
HIP 115819 B	23 27 49.76 +04 51 00.1	M8	...	...	19.272 ± 0.023	...	16.865 ± 0.022
HIP 116052 B‡	23 30 52.38 +27 46 32.3	M3.5	...	...	...	14.013 ± 0.02	13.718 ± 0.002
Companions to faint non-HIP primaries
NLTT 1011 B	00 19 32.68 +40 18 55.4	L2	...	...	20.203 ± 0.034	18.651 ± 0.013	17.615 ± 0.015
GD 280	01 54 58.13 +48 19 59.1	M9	...	...	19.915 ± 0.017	18.524 ± 0.017	17.624 ± 0.013
NLTT 8245	02 33 23.52 +65 45 47.6	M7	...	...	18.689 ± 0.015	17.362 ± 0.005	16.465 ± 0.007
LSPM J0241+2553	02 41 51.51 +25 53 43.4	L1	...	...	21.357 ± 0.132	19.986 ± 0.065	19.074 ± 0.05
HD 253662	06 13 53.35 +15 14 04.4	L0.5	...	21.39 ± 0.109	20.306 ± 0.073	18.692 ± 0.022	17.691 ± 0.02
LSPMJ0632+5053 B	06 32 48.55 +50 53 33.6	L1.5	...	...	...	19.86 ± 0.12	18.86 ± 0.04
NLTT 18587	07 54 13.38 +37 21 42.6	M7.5	...	...	20.507 ± 0.057	18.879 ± 0.019	18.03 ± 0.026
NLTT 19109	08 11 59.00 −08 58 01.6	M8.5	...	...	20.679 ± 0.042	19.193 ± 0.023	18.36 ± 0.044
NLTT 22073 B	09 33 37.11 −27 52 45.4	M7.5	...	21.185 ± 0.047	18.619 ± 0.007	17.115 ± 0.006	16.303 ± 0.007
NLTT 23716	10 13 17.05 −06 01 22.9	M8	22.289 ± 0.221	...	17.995 ± 0.006	16.703 ± 0.005	15.884 ± 0.006
NLTT 26746 B	11 15 01.22 +16 07 00.8	L4	...	...	21.23 ± 0.07	19.43 ± 0.05	18.36 ± 0.06
NLTT 29395	12 03 02.61 +58 06 02.4	M8	...	...	19.605 ± 0.018	18.181 ± 0.008	17.397 ± 0.013
NLTT 30510	12 22 18.59 +36 43 48.1	M9.5	...	...	20.371 ± 0.064	18.657 ± 0.014	17.716 ± 0.016
NLTT 31450 B	12 39 49.19 +32 09 03.1	L6	...	...	20.8 ± 0.09	19.29 ± 0.02	18.34 ± 0.03
PMI 13410+0542 B	13 41 02.39 +05 42 48.8	L4	...	21.5 ± 0.2	20.10 ± 0.05	18.92 ± 0.03	18.00 ± 0.02
PMI 13518+4157 B	13 51 47.41 +41 57 47.4	L1.5	...	21.64 ± 0.13	19.636 ± 0.018	18.190 ± 0.009	17.17 ± 0.01
NLTT 38489 B	14 48 46.28 +56 10 57.8	M9	...	...	20.88 ± 0.05	19.52 ± 0.04	18.62 ± 0.04
NLTT 39312 B	15 05 59.27 +33 39 30.2	M8	...	...	19.588 ± 0.018	18.476 ± 0.017	17.768 ± 0.018
LSPM J1627+3328 B	16 27 01.44 +33 28 21.4	M9	...	...	18.94 ± 0.16	17.32 ± 0.03	16.386 ± 0.018
NLTT 44368 B	17 11 57.29 +54 30 43.8	L1.5	...	21.28 ± 0.07	...	17.688 ± 0.011	16.754 ± 0.016
LSPM J1717+5925 B	17 17 30.94 +59 25 30.2	M9	...	...	20.232 ± 0.053	18.890 ± 0.013	18.043 ± 0.015
NLTT 52268 B	21 51 07.23 +30 45 54.7	M9	...	...	19.08 ± 0.01	17.63 ± 0.01	16.67 ± 0.03
LSPM J2153+1157 B	21 53 46.92 +11 57 46.4	M7	22.28 ± 0.08	20.90 ± 0.03	18.149 ± 0.005	16.787 ± 0.003	16.005 ± 0.004
PM I22118−1005 B	22 11 41.25 −10 08 20.8	L1.5	...	22.28 ± 0.14	19.77 ± 0.02	18.347 ± 0.010	17.412 ± 0.010
NLTT 55219 B	22 54 28.58 +22 02 56.1	L5.5	...	...	...	19.665 ± 0.04	18.791 ± 0.039
Serendipitous Companion Discoveries
NLTT 730 B	00 15 02.40 +29 59 29.8	L7.5pd	...	...	21.63 ± 0.11	19.49 ± 0.04	18.37 ± 0.06
NLTT 27966 B	11 36 39.44 +48 52 43.0	L4	...	...	21.06 ± 0.13	19.52 ± 0.03	18.48 ± 0.05
LSPMJ1336+2541 B	13 36 24.89 +25 40 37.2	L4	...	...	22.19 ± 0.16	20.21 ± 0.07	19.45 ± 0.09
HIP 73169 Be	14 57 11.35 −06 19 27.4	L2.5	...	...	20.55 ± 0.18	19.06 ± 0.02	18.42 ± 0.09
PM I23492+3458 B	23 49 15.11 +34 58 55.3	L9	...	...	...	19.99 ± 0.04	18.80 ± 0.04
Unlikely Companions
NLTT 35593 B	13 54 34.92−06 07 34.3	L2	...	...	20.74 ± 0.12	19.37 ± 0.11	18.56 ± 0.03

Notes. † Previously known in the Washington Double Star Catalog. ‡ Additional possibly spurious companion in the system in the Washington Double Star Catalog. * Simultaneously discovered by Allen et al. (2012). ^aOur object appears in the Washington Double Star Catalog as component C due to a spurious companion listed as B. ^bPrimary is itself a close double listed as Aa and Ab in the Washington Double Star Catalog. ^cThe companion was identified as visual double during IRTF acquisition, due to saturation, it does not appear in our PS1 catalog, position is taken from VISTA image. ^dSpectral type from Kirkpatrick et al. (2010). We identify this object as a companion to NLTT 730. ^eWhile HIP 73169 appears in the Hipparcos catalog, its parallax measurement was too low-significance for it to be included in our input Hipparcos sample. Hence it appears in our sample of other primaries due to it being a nearby M dwarf in the proper motion catalog of Salim & Gould (2003). ^fPrimary is itself a binary with a listing in the Washington Double Star Catalog. Our companion is component C. ^gPreviously identified by Deacon & Hambly (2007) as a binary pair. The secondary is also known as SIPS 0933−2752.

Download table as:  ASCIITypeset images: 1 2

Table 4. Astrometric Data on Our Data of Our Multiple Systems

Object	d	μαcos δ	μδ	dμαcos δ	dμδ	dμ	Projected	Projected
							Separation	Separation
	(pc)	('' yr−1)	('' yr−1)	nσ	nσ	nσ	('')	(AU)
HIP 2397	[33.9$_{-1.3}^{+1.4}$]	0.186 ± 0.001	−0.185 ± 0.001	3.2	2.1	3.8	117.1	3970
HIP 2397B	39.2$^{+7.6}_{-6.4}$	0.2 ± 0.004	−0.176 ± 0.004
HIP 6217	[101$^{+18}_{-13}$]	0.119 ± 0.001	0.030 ± 0.001	1.94	1.94	2.74	27.4	2767
HIP 6217 B	70.9$^{+14.0}_{-11.7}$	0.111 ± 0.004	0.022 ± 0.004
HIP 6407	[57.2$_{-3.0}^{+3.3}$]	0.046 ± 0.001	−0.159 ± 0.001	2.1	2.7	3.4	44.9	2570
HIP 6407B	53.6$^{+10.5}_{-8.8}$	0.03 ± 0.008	−0.138 ± 0.008
HIP 9269	[25.0$_{-0.4}^{+0.3}$]	0.244 ± 0.001	−0.352 ± 0.001	0.1	0.5	0.5	52.1	1300
HIP 9269B	27.8$^{+5.4}_{-4.5}$	0.243 ± 0.011	−0.347 ± 0.011
HIP 10033	[69.7$_{-3.1}^{+3.4}$]	−0.093 ± 0.001	−0.046 ± 0.001	2.9	2.6	3.9	42.9	2990
HIP 10033B	89.5$^{+17.3}_{-14.5}$	−0.114 ± 0.007	−0.027 ± 0.007
HIP 11161	[69.3$_{-3.6}^{+4.1}$]	−0.081 ± 0.001	−0.061 ± 0.001	0.4	0.6	0.7	47.7	3300
HIP 11161B	83.6$^{+16.3}_{-13.6}$	−0.079 ± 0.005	−0.058 ± 0.005
HIP 13589	[72.8$_{-4.0}^{+4.6}$]	0.148 ± 0.001	−0.097 ± 0.001	0.5	1.7	1.8	49.2	3580
HIP 13589B	64.6$^{+12.5}_{-10.5}$	0.15 ± 0.005	−0.089 ± 0.005
HIP 26653	27.9$^{+0.8}_{-0.7}$	−0.013 ± 0.001	−0.142 ± 0.001	2.91	2.94	4.66	27.0	753
HIP 26653 B	18.8$^{+3.7}_{-3.1}$	−0.001 ± 0.004	−0.157 ± 0.004
HIP 32728	[46.6$_{-2.6}^{+2.9}$]	0.191 ± 0.001	−0.14 ± 0.001	0.2	0.9	1.0	94.3	4400
HIP 32728B	67.1$^{+13.4}_{-11.2}$	0.188 ± 0.016	−0.13 ± 0.011
HIP 37283	[45.5$_{-1.2}^{+1.2}$]	−0.08 ± 0.001	−0.061 ± 0.001	1.4	0.6	1.6	106.1	4830
HIP 37283B	34.6$^{+7.4}_{-6.1}$	−0.087 ± 0.005	−0.058 ± 0.005
HIP 46984	[74.7$_{-6.9}^{+8.6}$]	0.026 ± 0.002	0.108 ± 0.002	1.6	1.8	2.4	37.5	2800
HIP 46984B	111.9$^{+22.4}_{-18.6}$	0.032 ± 0.004	0.101 ± 0.003
HIP 49046	[34.7$_{-2.3}^{+2.6}$]	−0.015 ± 0.002	0.119 ± 0.001	1.5	1.1	1.9	136.1	4720
HIP 49046B	33.3$^{+6.7}_{-5.6}$	−0.008 ± 0.005	0.113 ± 0.005
HIP 51877	54.2$^{+2.3}_{-2.1}$	−0.063 ± 0.001	−0.122 ± 0.001	0.50	0.33	0.60	17.6	954
HIP 51877 B	57.4$^{+11.5}_{-9.6}$	−0.066 ± 0.006	−0.124 ± 0.006
HIP 52463	[74.2$_{-4.5}^{+5.2}$]	−0.07 ± 0.001	0.083 ± 0.001	1.1	2.2	2.4	43.5	3230
HIP 52463B	84.6$^{+16.9}_{-14.1}$	−0.064 ± 0.006	0.096 ± 0.006
HIP 55666	[49.8$_{-1.5}^{+1.5}$]	−0.085 ± 0.001	−0.093 ± 0.001	0.2	2.3	2.3	37.2	1850
HIP 55666B	42.2$^{+8.3}_{-6.9}$	−0.087 ± 0.009	−0.074 ± 0.009
HIP 58918	[55.8$_{-5.1}^{+6.2}$]	−0.297 ± 0.002	0.018 ± 0.001	1.1	2.9	3.1	20.0	1110
HIP 58918B	61.9$^{+12.3}_{-10.2}$	−0.289 ± 0.007	0.038 ± 0.007
HIP 59310	[44.4$_{-2.8}^{+3.2}$]	−0.157 ± 0.002	−0.041 ± 0.001	2.8	2.7	3.9	82.1	3650
HIP 59310B	42.4$^{+8.4}_{-7.0}$	−0.144 ± 0.004	−0.053 ± 0.004
HIP 59933	[57.0$_{-2.4}^{+2.7}$]	−0.103 ± 0.001	−0.036 ± 0.001	2.0	1.0	2.3	38.1	2170
HIP 59933B	67.8$^{+13.6}_{-11.3}$	−0.088 ± 0.007	−0.029 ± 0.007
HIP 60501	[56.6$_{-6.0}^{+7.6}$]	−0.012 ± 0.002	−0.134 ± 0.001	1.6	0.7	1.8	37.1	2100
HIP 60501B	30.8$^{+6.0}_{-5.0}$	−0.001 ± 0.006	−0.13 ± 0.006
HIP 60987	[61.9$_{-2.3}^{+2.4}$]	−0.108 ± 0.001	−0.068 ± 0.001	1.0	1.5	1.8	19.0	1170
HIP 60987C	64.6$^{+12.9}_{-10.8}$	−0.104 ± 0.004	−0.074 ± 0.004
HIP 63506	[42.5$_{-3.9}^{+4.7}$]	−0.396 ± 0.002	0.026 ± 0.002	0.5	0.0	0.5	132.8	5640
HIP 63506 C	45.0$^{+9.0}_{-7.5}$	−0.401 ± 0.009	0.026 ± 0.009
HIP 65706	[51.1$_{-4.0}^{+4.8}$]	−0.186 ± 0.002	−0.185 ± 0.001	2.2	2.3	3.2	52.6	2690
HIP 65706B	34.4$^{+6.8}_{-5.7}$	−0.176 ± 0.004	−0.175 ± 0.004
HIP 65780	[58.0$_{-3.3}^{+3.7}$]	−0.193 ± 0.001	−0.218 ± 0.001	1.56	1.51	2.2	16.0	928
HIP 65780 C	60.8$^{+11.9}_{-9.9}$	−0.179 ± 0.009	−0.204 ± 0.009
HIP 70623	[72.6$_{-4.7}^{+5.5}$]	−0.152 ± 0.001	−0.148 ± 0.001	0.4	1.7	1.8	41.9	3040
HIP 70623 C	33.1$^{+6.5}_{-5.4}$	−0.154 ± 0.003	−0.142 ± 0.003
HIP 75310	[66.9$_{-5.1}^{+6.0}$]	−0.025 ± 0.001	−0.154 ± 0.001	0.3	0.3	0.4	22.9	1530
HIP 75310B	71.8$^{+14.3}_{-12.0}$	−0.023 ± 0.004	−0.153 ± 0.004
HIP 76456	[36.8$_{-0.6}^{+0.6}$]	0.089 ± 0.001	−0.057 ± 0.001	0.3	1.8	1.9	36.1	1330
HIP 76456B	41.6$^{+8.3}_{-6.9}$	0.09 ± 0.004	−0.064 ± 0.004
HIP 76641	[82.1$_{-4.7}^{+5.3}$]	−0.104 ± 0.001	0.031 ± 0.001	1.7	0.7	1.8	42.1	3460
HIP 76641B	41.6$_{-9.6}^{+13.4}$	−0.11 ± 0.004	0.028 ± 0.004
HIP 78184	[31.4$_{-1.3}^{+1.4}$]	−0.296 ± 0.001	0.202 ± 0.002	1.6	1.5	2.2	121.8	3820
HIP 78184B	40.3$^{+7.9}_{-6.6}$	−0.285 ± 0.006	0.213 ± 0.006
HIP 78859	[57.2$_{-2.1}^{+2.3}$]	−0.06 ± 0.001	−0.252 ± 0.001	1.2	0.6	1.4	42.6	2440
HIP 78859B	44.9$^{+8.7}_{-7.3}$	−0.056 ± 0.003	−0.254 ± 0.003
HIP 78916	[92.9$_{-9.2}^{+11.5}$]	−0.098 ± 0.0010	0.092 ± 0.0010	2.9	0.6	3.0	35.5	3294
HIP 78916 B	70.6$^{+13.8}_{-11.6}$	−0.080 ± 0.006	0.095 ± 0.006
HIP 78923	[46.1$_{-1.7}^{+1.8}$]	−0.301 ± 0.0010	0.184 ± 0.0010	1.9	3.2	3.7	15.5	714
HIP 78923 B	44.5$^{+8.8}_{-7.3}$	−0.315 ± 0.007	0.206 ± 0.007
HIP 79180	[74.7$_{-3.4}^{+3.7}$]	0.092 ± 0.001	−0.258 ± 0.001	0.9	1.6	1.9	29.0	2170
HIP 79180B	93.7$^{+18.7}_{-15.6}$	0.096 ± 0.005	−0.265 ± 0.004
HIP 80258	[63.7$_{-7.5}^{+9.6}$]	−0.181 ± 0.002	0.144 ± 0.002	2.2	2.4	3.3	54.9	3500
HIP 80258B	103$^{+21}_{-17}$	−0.173 ± 0.003	0.135 ± 0.003
HIP 81910	[46.4$_{-0.8}^{+0.9}$]	−0.02 ± 0.001	−0.103 ± 0.001	0.6	1.5	1.6	26.7	1240
HIP 81910B	31.3$^{+6.1}_{-5.1}$	−0.023 ± 0.007	−0.093 ± 0.007
HIP 82233	[42.1$_{-1.2}^{+1.3}$]	0.076 ± 0.001	−0.092 ± 0.001	1.4	2.6	3.0	30.4	1280
HIP 82233B	29.7$^{+5.9}_{-4.9}$	0.085 ± 0.006	−0.075 ± 0.006
HIP 83651	[50.9$_{-4.2}^{+4.9}$]	−0.142 ± 0.002	0.136 ± 0.002	1.6	1.7	2.4	28.9	1470
HIP 83651B	53.8$^{+10.8}_{-9.0}$	−0.149 ± 0.003	0.13 ± 0.003
HIP 84840	[$112_{-15}^{+19}$]	−0.051 ± 0.001	−0.174 ± 0.001	0.6	1.9	2.0	16.9	1890
HIP 84840B	77.9$_{-13.0}^{+15.6}$	−0.049 ± 0.003	−0.168 ± 0.003
HIP 85365	[30.1$_{-0.2}^{+0.2}$]	−0.092 ± 0.001	−0.043 ± 0.001	0.8	3.8	3.9	294.1	8850
HIP 85365B	34.7$^{+6.8}_{-5.7}$	−0.087 ± 0.006	−0.019 ± 0.006
HIP 86722	[22.7$_{-0.5}^{+0.4}$]	−0.123 ± 0.001	−0.62 ± 0.001	1.7	1.2	2.1	22.8	520
HIP 86722B	25.7$^{+5.0}_{-4.2}$	−0.112 ± 0.007	−0.628 ± 0.007
HIP 88728	[$40.4_{-1.1}^{+1.2}$]	0.040 ± 0.001	−0.150 ± 0.001	0.6	3.3	3.4	9.6	316
HIP 88728B	...	0.036 ±0.005	−0.133 ± 0.005
HIP 90273	[55.4$_{-7.3}^{+10.0}$]	0.006 ± 0.002	0.257 ± 0.003	2.5	0.8	2.7	26.9	1490
HIP 90273B	59.5$^{+11.8}_{-9.8}$	0.016 ± 0.003	0.26 ± 0.003
HIP 90869	[56.4$_{-3.0}^{+3.4}$]	−0.144 ± 0.001	−0.122 ± 0.001	2.5	0.1	2.5	17.5	990
HIP 90869B	83.6$^{+16.9}_{-14.1}$	−0.134 ± 0.004	−0.121 ± 0.004
HIP 93967	[122.1$_{-19.6}^{+29.0}$]	−0.146 ± 0.002	−0.276 ± 0.001	0.3	0.1	0.3	22.2	2710
HIP 93967B	135.1$^{+26.9}_{-22.4}$	−0.145 ± 0.005	−0.275 ± 0.005
HIP 97168	[97.5$_{-10.4}^{+13.1}$]	0.127 ± 0.001	0.136 ± 0.001	0.6	3.1	3.2	12.6	1230
HIP 97168B	72.9$^{+14.3}_{-12.0}$	0.124 ± 0.004	0.149 ± 0.004
HIP 98535	[60.0$_{-3.3}^{+3.8}$]	−0.113 ± 0.001	−0.095 ± 0.001	0.2	1.9	1.9	61.7	3700
HIP 98535C	56.0$^{+11.0}_{-9.2}$	−0.114 ± 0.005	−0.086 ± 0.005
HIP 102582	[31.3$_{-1.3}^{+1.4}$]	0.091 ± 0.0020	−0.592 ± 0.0010	0.5	1.8	1.9	14.7	459
HIP 102582 B	40.7$^{+7.9}_{-6.6}$	0.093 ± 0.005	−0.583 ± 0.005
HIP 103199	[59.5$_{-4.3}^{+5.1}$]	0.15 ± 0.001	0.057 ± 0.001	3.1	2.3	3.8	10.9	650
HIP 103199B	73.6$^{+14.7}_{-12.3}$	0.135 ± 0.005	0.046 ± 0.005
HIP 105202	[41.8$_{-1.3}^{+1.4}$]	0.144 ± 0.001	−0.041 ± 0.001	0.9	0.3	1.0	89.4	3740
HIP 105202B	64.1$^{+12.8}_{-10.7}$	0.147 ± 0.003	−0.04 ± 0.003
HIP 106551	[71.0$_{-2.1}^{+2.2}$]	0.116 ± 0.001	0.095 ± 0.001	0.9	0.8	1.2	66.1	4690
HIP 106551B	67.9$^{+13.2}_{-11.0}$	0.119 ± 0.004	0.092 ± 0.004
HIP 108822	[44.4$_{-6.1}^{+8.5}$]	−0.025 ± 0.004	−0.354 ± 0.004	3.6	1.2	3.8	31.8	1410
HIP 108822B	53.1$^{+10.7}_{-8.9}$	−0.046 ± 0.004	−0.347 ± 0.004
HIP 109454	[100.9$_{-5.8}^{+6.5}$]	−0.069 ± 0.001	−0.091 ± 0.001	0.4	1.9	1.9	18.2	1840
HIP 109454B	109.7$^{+22.0}_{-18.3}$	−0.072 ± 0.005	−0.081 ± 0.005
HIP 111657	[41.9$_{-3.0}^{+3.3}$]	−0.248 ± 0.002	−0.187 ± 0.002	2.4	2.5	3.5	7.8	330
HIP 111657B	34.9$^{+7.0}_{-5.8}$	−0.259 ± 0.004	−0.176 ± 0.004
HIP 112422	[65.4$_{-6.6}^{+8.3}$]	0.148 ± 0.002	0.031 ± 0.001	1.6	1.1	1.9	16.0	1040
HIP 112422B	64.7$^{+12.6}_{-10.5}$	0.168 ± 0.012	0.044 ± 0.012
HIP 114424	[35.1$_{-0.9}^{+1.1}$]	0.138 ± 0.001	−0.136 ± 0.001	2.0	0.0	2.0	42.0	1480
HIP 114424B	26.3$^{+5.2}_{-4.3}$	0.146 ± 0.004	−0.136 ± 0.004
HIP 114456	[24.3$_{-0.3}^{+0.3}$]	−0.087 ± 0.001	−0.287 ± 0.001	2.2	2.7	3.5	50.4	1220
HIP 114456B	23.9$^{+4.6}_{-3.9}$	−0.097 ± 0.005	−0.3 ± 0.005
HIP 115819	[65.7$_{-8.2}^{+11.0}$]	0.441 ± 0.003	0.181 ± 0.002	0.9	2.4	2.5	30.4	2000
HIP 115819B	64.0$^{+12.5}_{-10.5}$	0.435 ± 0.006	0.196 ± 0.006
HIP 116052	[49.6$_{-2.3}^{+2.5}$]	−0.137 ± 0.001	−0.133 ± 0.001	0.2	1.0	1.0	26.8	1330
HIP 116052 B	87.2$^{+17.5}_{-14.6}$	−0.136 ± 0.004	−0.129 ± 0.004

Notes. n_σ is the number of standard deviations the proper motions differ by. [...] denotes distance from trigonometric parallax; all other distances are photometric.

Download table as:  ASCIITypeset images: 1 2 3

Table 5. The Data of Our Non-Hipparcos and Serendipitous Pairs

Object	distance	μαcos δ	μδ	dμαcos δ	dμδ	dμ	Projected	Projected
							Separation	Separation
	(pc)	('' yr−1)	('' yr−1)	nσ	nσ	nσ	('')	(AU)
Other Companion Discoveries
NLTT 1011	68.2$_{-6.5}^{+6.6}$a	−0.076 ± 0.008f	−0.192 ± 0.008	0.08	0.43	0.44	58.5	3990
NLTT 1011B	46.1$^{+9.3}_{-7.7}$b	−0.077 ± 0.007	−0.197 ± 0.007
GD 280	77$^{+35}_{-26}$	0.171 ± 0.008	−0.059 ± 0.008f	0.32	0.53	0.62	63.4	4882
GD 280 B	82.3$^{+16.7}_{-13.9}$	0.174 ± 0.005	−0.054 ± 0.005
NLTT 8245	53.0$^{+8.7}_{-7.5}$	−0.096 ± 0.008	−0.164 ± 0.008f	0.42	0.21	0.47	10.6	562
NLTT 8245 B	72.9$^{+14.6}_{-12.2}$	−0.092 ± 0.005	−0.162 ± 0.005
LSPM J0241+2553	69$^{+35}_{-23}$	−0.032 ± 0.008	−0.158 ± 0.008f	1.41	0.70	1.58	31.2	2153
LSPM J0241+2553 B	93.1$^{+20.2}_{-16.62}$	−0.048 ± 0.008	−0.150 ± 0.008
HD 253662	>62.3	0.020 ± 0.001	−0.157 ± 0.001i	0.20	0.50	0.54	20.1	>1252
HD 253662 B	67.2$^{+13.7}_{-11.4}$	−0.022 ± 0.010	−0.162 ± 0.010
LSPM J0632+5053	95.0$_{-13.9}^{+16.3}$a	0.035 ± 0.008f	−0.154 ± 0.008	2.1	1.2	2.4	47.4	4499
LSPM J0632+5053 B	85.3$^{+16.7}_{-14.0}$b	0.054 ± 0.004	−0.143 ± 0.004
NLTT 18587	132$^{+40}_{-31}$	0.167 ± 0.008	−0.089 ± 0.008f	1.06	0.09	2.37	92.4	12200
NLTT 18587 B	158$^{+36}_{-29}$	0.155 ± 0.008	−0.0.88 ± 0.008
NLTT 19109	48.2$^{+7.9}_{-6.8}$	0.035 ± 0.008	−0.181 ± 0.008g	1.59	1.9	2.48	7.5	362
NLTT 19109 B	127$^{+25}_{-21}$	0.050 ± 0.005	−0.163 ± 0.005
NLTT 22073	29.9$_{-6.9}^{+12.7}$c	−0.315 ± 0.008	0.16 ± 0.008g	1.1	1.5	1.8	26	776
NLTT 22073 B	62.2$^{+12.4}_{-10.4}$	−0.301 ± 0.014	0.141 ± 0.014
NLTT 23716	48.2$^{+7.9}_{-6.8}$	0.054 ± 0.005	−0.286 ± 0.005h	1.41	1.41	1.99	15.0	723
NLTT 23716 B	47.5$^{+9.3}_{-7.8}$	0.063 ±.004	−0.277 ± 0.004
NLTT 26746	41.0$_{-10.3}^{+12.2}$d	−0.251 ± 0.008f	−0.147 ± 0.008	1.22	0.87	1.5	18.0	661
NLTT 26746 B	42.5$^{+8.3}_{-6.9}$b	−0.235 ± 0.01	−0.136 ± 0.01
NLTT 29395	56.4$^{+16.9}_{-13.0}$	−0.182 ± 0.008	−0.115 ± 0.008f	2.01	0.78	2.16	11.9	671
NLTT 29395 B	96.0$^{+19.5}_{-16.2}$	−0.164 ± 0.004	−0.108 ± 0.004
NLTT 30510	49.1$^{+14.8}_{-11.3}$	0.215 ± 0.008	−0.067 ± 0.008	f 0.4	0.2.5	2.53	19.6	962
NLTT 30510 B	88.8$^{+18.1}_{-15.0}$	0.219 ± 0.006	−0.042 ± 0.006
NLTT 31450	34.6$_{-8.7}^{+10.3}$d	−0.034 ± 0.008f	−0.202 ± 0.008	−0.03	1.75	1.75	12.3	487
NLTT 31450 B	27.2$^{+5.3}_{-4.4}$b	−0.034 ± 0.01	−0.18 ± 0.01
PMI 13410+0542	51.3$_{-11.8}^{+21.7}$c	0.047 ± 0.008g	−0.014 ± 0.008	1.7	1.8	2.5	9.4	484
PMI 13410+0542 B	44.3$^{+8.7}_{-7.2}$	0.062 ± 0.004	−0.030 ± 0.004
PMI 13518+4157	43.1$_{-8.8}^{+9.9}$d	−0.059 ± 0.008g	−0.058 ± 0.008	0.7	0.6	1.0	21.6	613
PMI 13518+4157 B	39.6$^{+7.9}_{-6.6}$	−0.05 ± 0.009	−0.065 ± 0.009
NLTT 38489	62.3$_{-17.0}^{+23.3}$a	−0.147 ± 0.008f	0.183 ± 0.008	0.7	1.4	1.6	6.7	418
NLTT 38489 B	128$^{+25}_{-21}$b	−0.141 ± 0.004	0.170 ± 0.004
NLTT 39312	141$_{-33}^{+43}$a	−0.025 ± 0.008f	−0.347 ± 0.008	4.3	1.2	4.4	5.1	713
NLTT 39312 B	124$^{+24}_{-20}$	0.09 ± 0.02	−0.32 ± 0.02
LSPM J1627+3328	38.0$_{-5.4}^{+6.3}$c	−0.171 ± 0.008f	−0.014 ± 0.008	3.29	−1.64	3.67	9.0	341
LSPM J1627+3328	49.9$^{+9.7}_{-8.1}$	−0.140 ± 0.005	−0.030 ± 0.005
NLTT 44368	55.0$_{-11.3}^{+12.7}$d	−0.056 ± 0.008f	0.215 ± 0.008	0.33	−0.37	0.49	90.2	7760
NLTT 44368 B	35.3$^{+6.9}_{-5.8}$b	−0.053 ± 0.006	0.211 ± 0.006
LSPM J1717+5925	108$_{-26}^{+35}$d	−0.085 ± 0.008i	−0.143 ± 0.008	1.8	1.6	2.4	14.4	1555
LSPM J1717+5925 B	119$^{+27}_{-22}$	−0.101 ± 0.004	−0.157 ± 0.004
NLTT 52268	37.3$_{-8.7}^{+11.3}$a	0.16 ± 0.008	−0.089 ± 0.008f	0.5	0.2	0.6	14.7	549
NLTT 52268 B	55.6$^{+10.8}_{-9.1}$	0.155 ± 0.006	−0.087 ± 0.006
LSPM J2153+1157	36.2$_{-8.4}^{+10.9}$a	−0.093 ± 0.008f	−0.128 ± 0.008	0.8	0.8	1.2	11.3	408
LSPM J2153+1157 B	58.1$^{+11.4}_{-9.5}$	−0.085 ± 0.006	−0.136 ± 0.006
PM I22118−1005	37.4$_{-7.7}^{+8.6}$d	0.028 ± 0.008g	−0.25 ± 0.008	1.6	0.9	1.9	204.5	8892
PM I22118−1005 B	43.9$^{+8.8}_{-7.3}$	0.05 ± 0.011	−0.262 ± 0.010
NLTT 55219	44.7$_{-10.4}^{+13.5}$a	0.324 ± 0.008f	0.16 ± 0.008	0.9	3.1	3.2	9.7	432
NLTT 55219 B	40.0$^{+7.8}_{-6.5}$	0.35 ± 0.03	0.26 ± 0.03
Serendipitous Companion Discoveries
NLTT 730	21.7$_{-5.3}^{+8.1}$d	0.375 ± 0.008f	−0.234 ± 0.008	0.5	1.58	1.66	233.6	5070
NLTT 730 B	23.7$^{+4.6}_{-3.9}$b	0.381 ± 0.009	−0.215 ± 0.009
NLTT 27966	39.6$_{-10.2}^{+13.3}$a	−0.153 ± 0.008f	0.182 ± 0.008	−0.79	0.42	0.89	15.9	630
NLTT 27966 B	42.3$^{+8.2}_{-6.9}$b	−0.164 ± 0.011	0.188 ± 0.011
LSPMJ1336+2541	60.7$_{-13.9}^{+15.7}$d	−0.157 ± 0.008f	0.057 ± 0.008	2.1	2.8	3.5	121.7	8793
LSPM J1336+2541 B	63.2$^{+12.4}_{-10.3}$b	−0.177 ± 0.005	0.031 ± 0.005
HIP 73169	[27.3$_{-6.3}^{+8.3}$e]	−0.267 ± 0.007	−0.076 ± 0.007	0.5	0.42	0.65	29.1	796
HIP 73169 B	50.7$^{+9.9}_{-8.3}$b	−0.261 ± 0.009	−0.081 ± 0.009
PM I23492+3458	30.7$_{-6.3}^{+7.1}$d	−0.011 ± 0.008f	−0.108 ± 0.008	1.0	1.0	1.4	34.9	949
PM I23492+3458 B	23.3$^{+4.5}_{-3.8}$b	−0.002 ± 0.005	−0.099 ± 0.005
Unlikely companions
NLTT 35593	63.0$_{-14.6}^{+19.1}$a	−0.184 ± 0.005h	−0.055 ± 0.005	1.76	−0.34	1.79	1105.8	69706
NLTT 35593 B	65.5$^{+12.8}_{-10.7}$b	−0.162 ± 0.011	−0.059 ± 0.011

Notes. n_σ is the number of standard deviations the proper motions differ by. [...] Denotes distance from trigonometric parallax; all other distances are photometric. ^aPhotometric distance from Lépine (2005). ^bPhotometric distance from 2MASS magnitudes and Dupuy & Liu (2012). ^cPhotometric distance from Lépine & Gaidos (2011). ^dPhotometric distance from spectral type and spectrophotometric relations of Kraus & Hillenbrand (2007). ^eTrigonometric parallax from van Leeuwen (2007). ^fProper motion from Lépine & Shara (2005). ^gProper motion from Lépine & Gaidos (2011). ^hProper motion from Salim & Gould (2003). ⁱProper motion from Hog et al. (2000).

Download table as:  ASCIITypeset images: 1 2

Table 6. The IR Data of Our Secondaries

Object	Y	J	H	K/Ks	Source
	(mag)	(mag)	(mag)	(mag)
HIP search companions
HIP 2397 B	...	14.586 ± 0.038*	13.975 ± 0.048*	>13.181*	2MASS
	...	14.552 ± 0.012	13.912 ± 0.011	...	UKIRT
HIP 6217 B		15.441 ± 0.060*	14.731 ± 0.081*	14.423 ± 0.079*	2MASS
	...	...	...	14.461 ± 0.009	UKIDSS
HIP 6407 B	...	15.471 ± 0.046	14.651 ± 0.061	14.402 ± 0.08	2MASS
	16.442 ± 0.008	15.345 ± 0.005	14.738 ± 0.006	14.203 ± 0.006	UKIDSS
HIP 9269 B	...	15.956 ± 0.088*	14.99 ± 0.096*	14.317 ± 0.085*	2MASS
	...	16.126 ± 0.017	15.082 ± 0.014	14.298 ± 0.019	UKIRT
HIP 10033 B	...	13.761 ± 0.027	13.185 ± 0.031	12.929 ± 0.033	2MASS
	...	13.746 ± 0.013	13.245 ± 0.011	...	UKIRT
HIP 11161 B	...	16.636 ± 0.161*	15.77 ± 0.173	15.392 ± 0.195*	2MASS
	...	16.512 ± 0.019	15.862 ± 0.017	15.25 ± 0.028	UKIRT
HIP 13589 B	...	14.928 ± 0.034	14.275 ± 0.037	13.838 ± 0.046	2MASS
	...	14.794 ± 0.034	14.226 ± 0.012	...	UKIRT
HIP 26653 B		14.756 ± 0.044*	13.91 ± 0.042*	13.322 ± 0.029*	2MASS
HIP 32728 B	...	14.508 ± 0.031	13.933 ± 0.038	13.509 ± 0.035	2MASS
HIP 37283 B	...	12.797 ± 0.027	12.234 ± 0.03	11.943 ± 0.024	2MASS
HIP 46984 B	...	13.285 ± 0.027*	12.745 ± 0.024	12.483 ± 0.027*	2MASS
	13.794 ± 0.002	13.215 ± 0.002	12.767 ± 0.002	12.463 ± 0.002	UKIDSS
HIP 49046 B	...	13.022 ± 0.022	12.418 ± 0.024	12.038 ± 0.021	2MASS
	...	12.930 ± 0.092	...	...	UKIRT
HIP 51877 B		15.205 ± 0.063*	14.510 ± 0.062*	13.988 ± 0.052*	2MASS
HIP 52463 B	...	13.703 ± 0.024	13.117 ± 0.027	12.801 ± 0.031	2MASS
HIP 55666 B	...	12.674 ± 0.024	12.108 ± 0.024	11.746 ± 0.019	2MASS
	13.322 ± 0.002	12.581 ± 0.001	12.103 ± 0.003	11.762 ± 0.002	VISTA
HIP 58918 B	...	14.471 ± 0.03*	13.899 ± 0.044	13.524 ± 0.023	2MASS
HIP 59310 B	...	13.691 ± 0.027	13.052 ± 0.033	12.692 ± 0.024	2MASS
HIP 59933 B	...	16.101 ± 0.088*	15.162 ± 0.075*	14.616 ± 0.084	2MASS
	17.126 ± 0.015	15.995 ± 0.008	15.218 ± 0.009	14.62 ± 0.01	UKIDSS
HIP 60501 B	...	11.378 ± 0.027	10.792 ± 0.024	10.453 ± 0.023	2MASS
	11.916 ± 0.001	11.309 ± 0.001	10.979 ± 0.001	10.554 ± 0.001	UKIDSS
HIP 60987 B	...	...	...	10.869 ± 0.001	VISTA†
HIP 60987 C	...	11.402 ± 0.028*	10.81 ± 0.029	10.592 ± 0.024	2MASS
	11.782 ± 0.001	11.267 ± 0.001	10.7497 ± 0.001	10.488 ± 0.001	VISTA
HIP 63506 C	...	15.15 ± 0.042	14.426 ± 0.045	14.006 ± 0.047	2MASS
HIP 65706 B	...	13.315 ± 0.022	12.642 ± 0.026	12.297 ± 0.024	2MASS
	14.011 ± 0.002	13.246 ± 0.001	12.693 ± 0.001	12.258 ± 0.002	UKIDSS
HIP 65780 C	...	>12.717	>12.197	12.007 ± 0.034*	2MASS
	13.580 ± 0.002	12.937 ± 0.001	12.404 ± 0.002	12.044 ± 0.002	UKIDSS
HIP 70623 C	...	12.191 ± 0.026	11.506 ± 0.023	11.224 ± 0.019	2MASS
	...	12.039 ± 0.001	11.541 ± 0.001	11.233 ± 0.001	VISTA
HIP 75310 B	...	13.291 ± 0.032*	12.724 ± 0.03	12.51 ± 0.027	2MASS
HIP 76456 B	...	13.300 ± 0.031*	12.762 ± 0.028*	12.43 ± 0.029*	2MASS
	13.973 ± 0.002	13.240 ± 0.002	12.809 ± 0.002	12.397 ± 0.002	UKIDSS
HIP 76641 B	...	10.817 ± 0.018	10.176 ± 0.016	9.919 ± 0.014	2MASS
HIP 78184 B	...	14.32 ± 0.031	13.607 ± 0.035	13.122 ± 0.03	2MASS
	...	14.252 ± 0.022	13.615 ± 0.037	13.091 ± 0.028	UKIRT
HIP 78859 B	...	12.258 ± 0.021	11.694 ± 0.02	11.496 ± 0.02	2MASS
	...	12.214 ± 0.010	11.734 ± 0.010	...	UKIRT
HIP 78916 B	...	15.227 ± 0.043*	14.542 ± 0.045	14.193 ± 0.053	2MASS
	...	15.148 ± 0.0179	14.603 ± 0.028	...	UKIRT
HIP 78923 B	...	14.052 ± 0.048*	13.566 ± 0.051*	13.28 ± 0.041*	2MASS
	...	14.136 ± 0.011	13.621 ± 0.11	...	UKIRT
HIP 79180 B	...	13.941 ± 0.022	13.361 ± 0.027	12.965 ± 0.033	2MASS
HIP 80258 B	...	13.113 ± 0.021	12.556 ± 0.023	12.28 ± 0.021	2MASS
	...	13.101 ± 0.016	12.562 ± 0.010	...	UKIRT
HIP 81910 B	...	12.44 ± 0.024*	11.887 ± 0.026	11.526 ± 0.025	2MASS
	...	12.400 ± 0.010	11.858 ± 0.010	...	UKIRT
HIP 82233 B	...	11.889 ± 0.024	11.288 ± 0.021	11.043 ± 0.023	2MASS
	...	11.874 ± 0.011	11.366 ± 0.010	...	UKIRT
HIP 83651 B	...	10.599 ± 0.024	10.057 ± 0.024	9.771 ± 0.021	2MASS
	...	10.734 ± 0.010	10.877 ± 0.011	...	UKIRT
HIP 84840 B	...	12.508 ± 0.022	11.901 ± 0.023	11.685 ± 0.018	2MASS
	...	12.491 ± 0.019	11.950 ± 0.010	...	UKIRT
HIP 85365 B	...	16.693 ± 0.168*	15.471 ± 0.118	>14.664	2MASS
	...	16.184 ± 0.010	...	14.718 ± 0.010	VISTA
HIP 86722 B	...	11.511 ± 0.025	11.016 ± 0.021	10.7 ± 0.019	2MASS
	...	11.506 ± 0.015	11.089 ± 0.01	...	UKIRT
HIP 88728 B	...	10.269 ± 0.097*	10.043 ± 0.047*	9.876 ± 0.057*	2MASS
	...	11.103 ± 0.019	10.965 ± 0.018	10.953 ± 0.027	UKIRT
HIP 90273 B	...	11.56 ± 0.022	11.019 ± 0.022	10.731 ± 0.018	2MASS
	...	11.495 ± 0.010	11.012 ± 0.018	...	UKIRT
HIP 90869 B	...	11.101 ± 0.029*	10.569 ± 0.027	10.358 ± 0.023	2MASS
	...	11.071 ± 0.10	10.818 ± 0.010	...	UKIRT
HIP 93967 B	...	13.357 ± 0.03	12.74 ± 0.025	12.525 ± 0.019	2MASS
	...	13.24 ± 0.02	12.751 ± 0.02	...	UKIRT
HIP 97168 B	...	13.679 ± 0.027*	13.212 ± 0.026*	13.012 ± 0.033*	2MASS
	...	13.784 ± 0.014	13.332 ± 0.014	...	UKIRT
HIP 98535 C	...	13.252 ± 0.031	12.724 ± 0.031	12.445 ± 0.032	2MASS
	...	13.223 ± 0.010	12.752 ± 0.010	...	UKIRT
HIP 102582 B	...	11.963 ± 0.033*	11.494 ± 0.034	11.232 ± 0.032*	2MASS
	...	11.972 ± 0.015	11.551 ± 0.010	...	UKIRT
HIP 103199 B	...	11.817 ± 0.027*	11.229 ± 0.024*	10.997 ± 0.019*	2MASS
	12.378 ± 0.014	11.850 ± 0.18	11.307 ± 0.010	11.250 ± 0.010	UKIRT
HIP 105202 B	...	12.124 ± 0.024	11.53 ± 0.022	11.246 ± 0.023	2MASS
	...	12.0337 ± 0.010	11.571 ± 0.014	...	UKIRT
HIP 106551 B	...	13.224 ± 0.025*	12.606 ± 0.03	12.287 ± 0.022	2MASS
	...	13.211 ± 0.010	12.630 ± 0.010	...	UKIRT
HIP 108822 B	...	10.622 ± 0.022	10.051 ± 0.021	9.821 ± 0.02	2MASS
	...	10.805 ± 0.020	10.650 ± 0.010	...	UKIRT
HIP 109454 B	...	12.422 ± 0.026*	11.863 ± 0.032	11.62 ± 0.02	2MASS
	...	12.452 ± 0.01	11.904 ± 0.017	...	UKIRT
HIP 111657 B	...	10.587 ± 0.032*	10.028 ± 0.034*	9.73 ± 0.027*	2MASS
	...	10.583 ± 0.010	10.545 ± 0.016	...	UKIRT
HIP 112422 B	...	16.023 ± 0.113*	15.111 ± 0.103*	14.651 ± 0.093*	2MASS
	17.171 ± 0.022	16.016 ± 0.017	15.251 ± 0.015	...	UKIRT
HIP 114424 B	...	11.595 ± 0.026	10.976 ± 0.022	10.663 ± 0.022	2MASS
	...	11.483 ± 0.010	11.185 ± 0.010	...	UKIRT
HIP 114456 B	...	10.844 ± 0.021*	10.227 ± 0.028*	9.896 ± 0.024*	2MASS
	...	10.840 ± 0.014	10.446 ± 0.010	...	UKIRT
HIP 115819 B	...	15.095 ± 0.034	14.357 ± 0.029	13.974 ± 0.045	2MASS
	15.844 ± 0.007	14.965 ± 0.005	14.370 ± 0.004	13.907 ± 0.005	UKIDSS
HIP 116052 B	...	12.361 ± 0.019	11.79 ± 0.024	11.512 ± 0.025	2MASS
	...	12.332 ± 0.019	11.793 ± 0.010	...	UKIRT
Companions to faint non-HIP primaries
NLTT 1011	...	15.544 ± 0.059	14.928 ± 0.069	14.318 ± 0.066	2MASS
GD 280 B		16.034 ± 0.082	14.993 ± 0.09	14.547 ± 0.08	2MASS
NLTT 8245 B		14.922 ± 0.052*	14.221 ± 0.068*	13.812 ± 0.056*	2MASS
LSPM J0241+2553 B		17.027 ± 0.180	16.028 ± 0.180	15.331 ± 0.149	2MASS
HD 253662 B		15.961 ± 0.082*	15.182 ± 0.087*	14.506 ± 0.095*	2MASS
	16.511 ± 0.009	15.653 ± 0.007	...	...	UKIDSS
LSPM J0632+5053 B	...	16.383 ± 0.108	15.421 ± 0.133	15.171 ± 0.122	2MASS
	...	16.612 ± 0.027	15.864 ± 0.022	...	UKIRT
NLTT 18587 B		16.894 ± 0.199	15.921 ± 0.215	>15.221	2MASS‡
NLTT 19109 B		16.933 ± 0.17*	15.89 ± 0.169*	15.463 ± 0.21*	2MASS
	...	16.512 ± 0.017	...	15.679 ± 0.026	VISTA
NLTT 22073 B	...	14.671 ± 0.037	14.070 ± 0.044	13.696 ± 0.049	2MASS
NLTT 23716 B		14.300 ± 0.036*	13.716 ± 0.035*	13.348 ± 0.028*	2MASS
	15.085 ± 0.005	14.225 ± 0.003	13.713 ± 0.004	13.309 ± 0.005	VISTA
NLTT 26746 B	...	16.403 ± 0.118*	15.224 ± 0.092	14.555 ± 0.105	2MASS
	17.377 ± 0.015	16.056 ± 0.008	15.295 ± 0.0090	14.61 ± 0.008	UKIDSS
NLTT 29395 B		15.81 ± 0.08*	15.133 ± 0.076*	14.781 ± 0.091*	2MASS
NLTT 30510 B		15.971 ± 0.08*	15.267 ± 0.095	14.854 ± 0.09	2MASS
NLTT 31450 B	...	16.135 ± 0.105*	15.048 ± 0.095*	14.331 ± 0.092*	2MASS
	...	16.004 ± 0.21	15.081 ± 0.023	...	UKIRT
PMI 13410+0542 B	...	16.187 ± 0.143*	15.128 ± 0.131*	14.799 ± 0.138*	2MASS
	17.349 ± 0.017	16.125 ± 0.009	15.358 ± 0.008	14.727 ± 0.008	UKIDSS
PMI 13518+4157 B	...	15.081 ± 0.032	14.352 ± 0.049	13.851 ± 0.04	2MASS
NLTT 38489 B	...	16.64 ± 0.143*	15.789 ± 0.176*	15.481 ± 0.154*	2MASS
	...	16.717 ± 0.031	16.147 ± 0.037	...	UKIRT
NLTT 39312 B	...	16.09 ± 0.096*	15.573 ± 0.118*	>13.601	2MASS
	...	16.277 ± 0.035	16.006 ± 0.045	...	UKIRT
LSPM J1627+3328 B	...	14.362 ± 0.083*	13.742 ± 0.066*	13.417 ± 0.055*	2MASS
	...	14.730 ± 0.012	14.052 ± 0.011	...	UKIRT
NLTT 44368 B	...	14.736 ± 0.058	13.907 ± 0.064	13.467 ± 0.049*	2MASS
	...	14.637 ± 0.013	13.993 ± 0.012	...	UKIRT
LSPM J1717+5925 B	...	16.580 ± 0.168*	15.934 ± 0.174*	15.581 ± 0.255*	2MASS
	...	16.509 ± 0.018	...	...	UHS
NLTT 52268 B	...	14.945 ± 0.052*	14.29 ± 0.05	13.839 ± 0.05	2MASS
	...	14.950 ± 0.02	14.295 ± 0.015	...	UKIRT
LSPM J2153+1157 B	...	14.403 ± 0.038*	13.785 ± 0.044*	13.427 ± 0.045*	2MASS
	...	14.450 ± 0.011	13.834 ± 0.011	13.368 ± 0.011	UKIRT
PM I22118−1005 B	...	15.246 ± 0.049	14.69 ± 0.063	14.051 ± 0.052	2MASS
NLTT 55219 B	...	16.313 ± 0.122*	15.469 ± 0.137*	14.778 ± 0.145*	2MASS
	...	16.612 ± 0.028	15.769 ± 0.024	...	UKIRT
Serendipitous Companion Discoveries
NLTT 730 B	...	16.16 ± 0.08	15.23 ± 0.08	14.48 ± 0.07	2MASS
	...	16.16 ± 0.03	15.22 ± 0.03	...	UKIRT
NLTT 27966 B	...	16.155 ± 0.103	15.27 ± 0.11	14.58 ± 0.082	2MASS
	17.308 ± 0.044	16.106 ± 0.019	15.283 ± 0.018	...	UKIRT
LSPM J1336+2541 B	...	16.863 ± 0.16	16.017 ± 0.172	15.713 ± 0.2	2MASS
	18.228 ± 0.033	16.935 ± 0.017	16.122 ± 0.018	15.478 ± 0.016	UKIDSS
HIP 73169 B	...	16.007 ± 0.09*	15.047 ± 0.083	14.36 ± 0.081	2MASS
	17.223 ± 0.033	15.929 ± 0.02	15.054 ± 0.015	14.446 ± 0.016	VISTA
PM I23492+3458 B	...	16.298 ± 0.105	15.45 ± 0.112	15.008 ± 0.127	2MASS
	...	16.387 ± 0.029	15.472 ± 0.021	...	UKIRT
Unlikely companions
NLTT 35593 B	...	16.299 ± 0.114	15.408 ± 0.117	14.737 ± 0.098	2MASS
	17.468 ± 0.02	16.227 ± 0.01	15.469 ± 0.011	14.876 ± 0.011	VISTA

Notes. † Object saturated in VISTA data. * Object has a confusion flag (ccflag) set in this filter. ‡ Photometry from the 2MASS reject table.

Download table as:  ASCIITypeset images: 1 2 3

Table 7. The WISE Data of Our Companions

Object	W1	W2	W3	W4	Note
	(mag)	(mag)	(mag)	(mag)
HIP search companions
HIP 2397 B	13.077 ± 0.026	12.818 ± 0.027	12.167	8.924 ± 0.409
HIP 6217 B	14.154 ± 0.03*	13.836 ± 0.042*	>12.790	>8.943
HIP 6407 B	13.91 ± 0.027*	13.584 ± 0.035*	>12.375	>9.305
HIP 9269 B	13.486 ± 0.026*	13.265 ± 0.033*	>12.573*	9.119 ± 0.473
HIP 10033 B	12.597 ± 0.023*	12.33 ± 0.023*	12.578 ± 0.337*	>9.229
HIP 11161 B	15.173 ± 0.043*	15.274 ± 0.111*	>12.738*	>9.179
HIP 13589 B	13.572 ± 0.026*	13.295 ± 0.035*	>12.558*	>9.002
HIP 26653 B	...	...	...	...
HIP 32728 B	13.326 ± 0027	13.133 ± 0.033	>12.04	>9.08
HIP 37283 B	11.631 ± 0.024*	11.425 ± 0.021*	11.101 ± 0.105	9.329
HIP 46984 B	12.313 ± 0.025*	12.129 ± 0.024*	12.3 ± 0.4	>8.6
HIP 49046 B	11.777 ± 0.025	11.582 ± 0.023	11.424 ± 0.145	8.916
HIP 51877 B	...	...	...	...
HIP 52463 B	12.595 ± 0.025*	12.44 ± 0.025*	12.1 ± 0.3	>8.9
HIP 55666 B	11.525 ± 0.023*	11.289 ± 0.023*	11.463 ± 0.176	9.097
HIP 58918 B	13.252 ± 0.025*	12.954 ± 0.029*	>12.284	>9.101
HIP 59310 B	12.400 ± 0.024	12.198 ± 0.024*	12.232 ± 0.310	>8.855
HIP 59933 B	14.271 ± 0.031*	13.939 ± 0.048*	>12.707	>8.876
HIP 60501 B	10.281 ± 0.023	10.12 ± 0.022*	10.038 ± 0.067	8.39 ± 0.325
HIP 60987 B	...	...	...	...	†
HIP 60987 C	10.434 ± 0.022*	10.279 ± 0.019*	10.167 ± 0.066>8.887
HIP 63506 C	13.696 ± 0.027	13.405 ± 0.031	>12.498	>9.324
HIP 65706 B	12.007 ± 0.024*	11.799 ± 0.023*	11.697 ± 0.162	>9.243
HIP 65780 C	...	...	...	...	†
HIP 70623 C	11.06 ± 0.022*	10.921 ± 0.021*	10.851 ± 0.084	>8.628
HIP 75310 B	12.181 ± 0.025*	11.984 ± 0.024*	11.342 ± 0.178	>8.493
HIP 76456 B	12.139 ± 0.023*	11.867 ± 0.022*	11.525 ± 0.100*	>8.974
HIP 76641 B	9.776 ± 0.023*	9.676 ± 0.021*	9.5590.024	9.362 ± 0.360
HIP 78184 B	12.8 ± 0.023	12.516 ± 0.022	12.403 ± 0.153	>9.755
HIP 78859 B	11.285 ± 0.022*	11.086 ± 0.021*	11.038 ± 0.059	>9.703
HIP 78916 B	...	...	...	...	†
HIP 78923 B	...	...	...	...	†
HIP 79180 B	12.746 ± 0.023*	12.558 ± 0.022*	12.241 ± 0.157	>9.305
HIP 80258 B	12.078 ± 0.024	11.884 ± 0.024*	12.218 ± 0.248	>9.435
HIP 81910 B	11.143 ± 0.025*	11.011 ± 0.025*	10.793 ± 0.147*	>8.691
HIP 82233 B	10.855 ± 0.023*	10.661 ± 0.02*	10.588 ± 0.092	>8.774
HIP 83651 B	9.631 ± 0.024*	9.495 ± 0.021*	9.387 ± 0.033	9.004 ± 0.428
HIP 84840 B	11.45 ± 0.023*	11.294 ± 0.021*	11.376 ± 0.105*	>9.348
HIP 85365 B	13.875 ± 0.03	13.643 ± 0.044	>12.394	>9.059
HIP 86722 B	10.517 ± 0.024*	10.253 ± 0.022*	9.908 ± 0.041*	9.376 ± 0.54
HIP 88728 B	...	...	...	...
HIP 90273 B	10.523 ± 0.023*	10.361 ± 0.021*	10.208 ± 0.048	9.386 ± 0.513
HIP 90869 B	10.148 ± 0.022*	10.012 ± 0.020*	10.089 ± 0.064	8.217 ± 0.288
HIP 93967 B	12.331 ± 0.023*	12.137 ± 0.026	>11.605	>8.52
HIP 97168 B	...	...	...	...	†
HIP 98535 C	12.14 ± 0.023*	11.917 ± 0.021*	12.603 ± 0.321	>9.516
HIP 102582 B	11.059 ± 0.025*	10.795 ± 0.026*	10.771 ± 0.096	>9.105
HIP 103199 B	10.855 ± 0.056*	10.644 ± 0.041*	10.61 ± 0.107	>9.209
HIP 105202 B	11.046 ± 0.024*	10.865 ± 0.021*	10.583 ± 0.08	>9.01
HIP 106551 B	...	...	...	...	†
HIP 108822 B	9.708 ± 0.024*	9.564 ± 0.020*	9.461 ± 0.032	8.63 ± 0.276
HIP 109454 B	11.5 ± 0.025*	11.233 ± 0.022*	11.171 ± 0.111	>9.279
HIP 111657 B	9.566 ± 0.050*	9.371 ± 0.038*	9.259 ± 0.05	8.819 ± 0.517
HIP 112422 B	...	...	...	...	†
HIP 114424 B	10.418 ± 0.023*	10.213 ± 0.020*	10.154 ± 0.062	>8.394
HIP 114456 B	9.685 ± 0.023*	9.511 ± 0.020*	9.299 ± 0.025*	8.744 ± 0.242
HIP 115819 B	13.511 ± 0.026*	13.184 ± 0.033*	12.42 ± 0.467	8.425 ± 0.313
HIP 116052 B	11.324 ± 0.025*	11.135 ± 0.023*	10.925 ± 0.091	>9.236
Companions to faint non-HIP primaries
NLTT 1011	13.762 ± 0.026	13.414 ± 0.032*	>12.3	>8.7
GD 280 B	14.396 ± 0.032	14.149 ± 0.052	>12.794	>9.206
NLTT 8245 B	...	...	...	...	†
LSPM J0241+2553 B	14.994 ± 0.044	14.826 ± 0.093	12.301 ± 0.396	>8.97
HD 253662 B	...	...	...	...
LSPM J0632+5053 B	14.94 ± 0.038*	14.757 ± 0.078	>12.814	>9.183
NLTT 18587 B	15.096 ± 0.043	14.828 ± 0.085	>12.008	>9.129
NLTT 19109 B	...	...	...	...	†
NLTT 22073 B	13.295 ± 0.027*	13.000 ± 0.030*	>12.224	>8.756
NLTT 23716 B	...	...	...	...	†
NLTT 26746 B	14.058 ± 0.029*	13.871 ± 0.045	>12.715	>8.755
NLTT 29395 B	...	...	...	...	†
NLTT 30510 B	14.546 ± 0.032*	14.247 ± 0.051*	>12.617	>8.982
NLTT 31450 B	...	...	...	...	†
PM I13410+0542	...	...	...	...	†
PM I13518+4157	13.556 ± 0.026*	13.222 ± 0.029	12.46 ± 0.31	>9.328
NLTT 38489 B	...	...	...	...	†
NLTT 39312 B	...	...	...	...	†
LSPM J1627+3328 B	...	...	...	...	†
NLTT 44368 B	12.951 ± 0.026	12.692 ± 0.025	12.054 ± 0.15	>8.934
LSPM J1717+5925 B	...	...	...	...	†
NLTT 52268 B	...	...	...	...	†
LSPM J2153+1157 B	...	...	...	...	†
PM I22118−1005 B	13.571 ± 0.027	13.335 ± 0.036	>11.969	>8.984
NLTT 55219 B	...	...	...	...	†
Serendipitous Companion Discoveries
NLTT 730 B	13.69 ± 0.03	13.38 ± 0.04	11.7 ± 0.2	>9.011
NLTT 27966 B	14.204 ± 0.028	13.853 ± 0.042	>12.773	>9.18
LSPM J1336+2541 B	14.844 ± 0.034	14.553 ± 0.06	>12.869	>8.916
HIP 73169 B	13.988 ± 0.027*	13.678 ± 0.035*	12.692 ± 0.409	>9.423
PM I23492+3458 B	14.036 ± 0.028*	13.396 ± 0.032*	12.311 ± 0.305	>8.985
Unlikely companions
NLTT 35593 B	14.44 ± 0.03	14.287 ± 0.052	>12.517	>9.277

Notes. * Has contaminated photometry in at least one WISE band. † Too close to their primary to have an independent photometry measurement in WISE.

Download table as:  ASCIITypeset images: 1 2

Table 8. Log of Spectroscopic Observations

Object	Date	tint	Conditions	Seeing	Slit	Mode	Resolution	Airmass	Standard
	(UT)	(s)		('')	('')		λ/Δλ
HIP search companions
HIP 2397 B	2012 Jul 5	360	cloudy	1.5	0.8 × 15	prism	75	1.12	HD 222749
HIP 6217 B	2013 Dec 11	360	cloudy	1.3	0.5 × 15	prism	120	1.30	HD 13936
HIP 6407 B	2012 Jul 6	480	clear	1.3	0.3 × 15	prism	200	1.37	HD 219545
HIP 9269 B	2011 Dec 2	1440	thin clouds	0.4	0.8 × 15	prism	75	1.156	HD 23452
HIP 10033 B	2012 Oct 25	720	cloudy	0.5	0.8 × 15	prism	75	1.14	HD 13936
HIP 11161 B	2012 Oct 28	720	thin clouds	0.8	0.8 × 15	prism	75	1.202	HD 21038
HIP 13589 B	2012 Jul 8	480	clear	>1	0.8 × 15	prism	75	1.44	HD 19600
HIP 26653 B	2014 Jan 18	120	clear	0.6	0.8 × 15	prism	75	1.34	HD 32090
HIP 32728 B	2013 Apr 3	360	clear	0.7	0.8 × 15	prism	75	1.05	HD 56386
HIP 37283 B	2012 Nov 16	240	thin clouds	0.4	0.8 × 15	SXD	750	1.18	HD 63586
HIP 46984 B	2013 Apr 5	480	clouds	0.5	0.8 × 15	prism	75	1.21	HD 101369
HIP 49046 B	2012 Nov 16	360	thin clouds	0.6	0.8 × 15	SXD	750	1.04	HD 89239
HIP 51877 B	2014 Jan 17	180	clear	0.5	0.8 × 15	prism	75	1.10	HD 71906
HIP 52463 B	2013 Apr 3	360	clear	0.7	0.8 × 15	prism	75	1.28	HD 90606
HIP 55666 B	2011 Apr 20	80	clear	0.5	0.5 × 15	prism	120	1.509	HD 97585
HIP 58918 B	2013 Apr 16	360	clouds	0.5	0.8 × 15	prism	75	1.14	HD 105388
HIP 59310 B	2013 Apr 16	360	clouds	0.5	0.8 × 15	prism	75	1.04	HD 105388
HIP 59933 B	2011 Mar 31	480	clear	0.3	0.5 × 15	prism	120	1.08	HD 10538
HIP 60501 B	2011 Apr 20	80	clear	0.5	0.5 × 15	prism	120	1.208	HD 109309
HIP 60987 B	2013 Apr 16	360	cloudy	0.4	0.8 × 15	prism	75	1.14	HD 101060
HIP 60987 C	2013 Apr 16	360	cloudy	0.4	0.8 × 15	prism	75	1.16	HD 101060
HIP 63506 C	2013 Jan 26	360	clear	0.7	0.8 × 15	prism	75	1.083	HD 109615
HIP 65706 B	2012 Apr 30	180	fog	1.5	0.8 × 15	prism	75	1.4	HD 116960
HIP 65780 C	2013 Jul 14	180	clear	0.9	0.8 × 15	prism	75	1.73	HD 116960
HIP 70623 C	2012 Jul 7	720	clear	0.5	0.5 × 15	SXD	1200	1.11	HD 132072
HIP 75310 B	2013 Apr 17	720	clear	0.7	0.8 × 15	SXD	750	1.30	HD 144425
HIP 76456 B	2013 Apr 5	120	cloudy	0.8	0.8 × 15	prism	75	1.26	HD 40739
HIP 76641 B	2013 Apr 3	90	clear	0.9	0.8 × 15	prism	75	1.3	HD 136831
HIP 78184 B	2011 Mar 31	160	clear	0.3	0.5 × 15	prism	120	1.37	HD 145127
HIP 78859 B	2012 Aug 10	180	clear	0.5	0.5 × 15	SXD	1200	1.40	q Her
HIP 78916 B	2013 Jul 13	180	clear	0.5	0.8 × 15	prism	75	1.07	HD 165029
HIP 78923 B	2013 Jul 13	180	clear	0.5	0.8 × 15	prism	75	1.14	HD 145647
HIP 79180 B	2013 Apr 3	360	clear	0.9	0.8 × 15	prism	75	1.44	HD 172728
HIP 80258 B	2012 Aug 10	50	thin clouds	0.4	0.8 × 15	prism	75	1.2	26 Ser
HIP 81910 B	2011 Apr 20	80	clear	0.5	0.5 × 15	prism	120	1.485	HD 145127
HIP 82233 B	2011 Apr 20	80	clear	0.5	0.5 × 15	prism	120	1.276	HD 148968
HIP 83651 B	2012 Jul 11	100	thin clouds	0.9	0.8 × 15	prism	75	1.1	HD 159008
HIP 85365 B	2012 Jul 7	600	clear	0.5	0.8 × 15	SXD	750	1.25	HD 159415
HIP 86722 B	2011 Apr 20	80	clear	0.5	0.5 × 15	prism	120	1.006	HD 165029
HIP 88728 B	2012 Jul 6	20	clear	1.3	0.3 × 15	prism	200	1.23	HD 165029
HIP 90273 B	2013 Nov 8	200	cloudy	1.3	0.3 × 15	prism	200	1.17	HD 174567
HIP 90869 B	2012 Aug 10	80	clear	0.3	0.5 × 15	SXD	1200	1.51	HD 184533
HIP 93967 B	2011 Oct 14	300	cloudy	1.0	0.8 × 15	prism	75	1.28	HD 182678
HIP 97168 B	2012 Jul 6	40	clear	1.3	0.3 × 15	prism	200	1.15	HD 199217
HIP 98535 C	2012 Jul 6	120	clear	1.3	0.3 × 15	prism	200	1.14	HD 199217
HIP 102582 B	2013 Jul 13	60	clear	0.5	0.8 × 15	prism	75	1.08	HD 192538
HIP 103199 B	2012 Jul 6	120	clear	1.3	0.3 × 15	prism	200	1.046	HD 210501
HIP 105202 B	2012 Jul 6	150	clear	1.3	0.3 × 15	prism	200	1.043	HD 210501
HIP 106551 B	2012 Aug 11	240	clear	0.7	0.5 × 15	prism	120	1.245	HD199312
HIP 108822 B	2012 Aug 11	80	clear	0.7	0.5 × 15	prism	120	1.247	HD 210501
HIP 109454 B	2011 Oct 15	1440	clear	0.6	0.8 × 15	prism	75	1.04	HD 210501
HIP 111657 B	2012 Oct 2	240	cloudy	0.8	0.8 × 15	SXD	750	1.19	HD 210501
HIP 112422 B	2012 Oct 7	540	thin cloud	0.9	0.8 × 15	prism	75	1.03	HD 210501
HIP 114424 B	2012 Jul 7	140	clear	0.5	0.5 × 15	prism	120	1.163	HD 218639
HIP 114456 B	2012 Oct 2	90	cloudy	0.7	0.8 × 15	SXD	750	1.24	HD 219290
HIP 115819 B	2012 Jul 6	240	clear	1.3	0.8 × 15	prism	75	1.198	HD 203769
HIP 116052 B	2012 Oct 25	420	cloudy	0.6	0.8 × 15	SXD	750	1.01	HD 210501
Non-Hipparcos Companions
NLTT 1011 B	2013 Sep 23	720	clear	0.6	0.8 × 15	prism	75	1.04	HD 210501
GD 280 B	2013 Dec 11	720	cloudy	1.2	0.8 × 15	prism	75	1.30	HD 15090
NLTT 8245 B	2014 Jan 19	180	clear	0.7	0.8 × 15	prism	75	1.51	HD 10897
LSPM J0241+2553 B	2014 Jan 18	960	clear	0.6	0.8 × 15	prism	75	1.22	HD 22401
HD 253662 B	2014 Jan 18	360	clear	0.6	0.8 × 15	prism	75	1.13	HD 43583
LSPM J0632+5053 B	2013 Apr 4	480	clear	0.7	0.8 × 15	prism	75	1.30	HD 248790
NLTT 18587 B	2014 Jan 19	960	clear	0.7	0.8 × 15	prism	75	1.07	HD 58296
NLTT 19109 B	2014 Jan 18	240	clear	0.6	0.8 × 15	prism	75	1.35	HD 73687
NLTT 22073 B	2013 Nov 23	160	clear	1.1	0.8 × 15	prism	75	1.49	HD 87727
NLTT 23716 B	2014 Jan 19	80	clear	0.7	0.8 × 15	prism	75	1.12	HD 79108
NLTT 26746 B	2011 Mar 31	480	clear	0.3	0.5 × 15	prism	120	1.05	HD 105388
NLTT 29395 B	2014 Jan 19	360	clear	0.7	0.8 × 15	prism	75	1.28	HD 128039
NLTT 30510 B	2014 Jan 19	240	clear	0.7	0.8 × 15	prism	75	1.05	HD 109615
NLTT 31450 B	2011 Mar 31	480	clear	0.3	0.5 × 15	prism	120	1.03	HD 105388
PMI 13410+0542 B	2013 Jul 13	360	clear	0.9	0.8 × 15	prism	75	1.12	HD 116960
PMI 13518+4157 B	2013 Jul 13	360	clear	0.9	0.8 × 15	prism	75	1.14	HD 116960
NLTT 38489 B	2013 Apr 18	720	clear	0.5	0.8 × 15	prism	75	1.45	HD 143187
NLTT 39312 B	2013 Jul 13	360	clear	0.9	0.8 × 15	prism	75	1.18	HD 136831
LSPM J1627+3328 B	2013 Apr 17	360	cloudy	0.7	0.8 × 15	prism	75	1.12	HD 145647
NLTT 44368 B	2013 Apr 16	360	thin clouds	0.7	0.8 × 15	prism	75	1.27	HD 199217
LSPM J1717+5925 B	2013 Jul 12	1200	clear	1.0	0.8 × 15	prism	75	1.45	HD 179933
NLTT 52268 B	2013 Jul 12	120	clear	0.8	0.8 × 15	prism	75	1.08	HD 210501
LSPM J2153+1157 B	2013 Jul 12	180	clear	0.8	0.8 × 15	prism	75	1.10	HD 210501
PM I22118−1005 B	2013 Jul 12	720	clear	0.8	0.8 × 15	prism	75	1.18	HD 203769
NLTT 55219 B	2013 Jul 12	720	clear	0.8	0.8 × 15	prism	75	1.04	HD 210501
Serendipitous Companion Discoveries
NLTT 27966 B	2012 Jun 7	360	clear	1.0	0.8 × 15	prism	75	1.16	HD 99966
LSPM J1336+2541 B	2012 Jul 8	960	clear	0.9	0.8 × 15	prism	75	1.06	HD 116960
HIP 73169 B	2012 Jul 6	960	clear	1.0	0.8 × 15	prism	75	1.30	HD 116960
PM 23492+3458 B	2012 Jul 7	720	clear	0.6	0.8 × 15	prism	75	1.31	HD 203030
Unlikely companions
NLTT 35593 B	2013 Apr 18	360	clear	0.5	0.8 × 15	prism	75	1.40	HD 116960
Primary Stars
NLTT 730	2013 Sep 23	180	clear	0.7	0.8 × 15	SXD	750	1.03	HD 210501
LSPMJ0632+5053	2013 Apr 17	90	patchy cloud	0.7	0.3 × 15	SXD	2000	1.24	HD 39250
NLTT 26746	2012 Jul 5	280	clear	1.2	0.3 × 15	SXD	2000	1.30	HD 99966
NLTT 27966	2012 Jul 5	720	clear	1.2	0.3 × 15	SXD	2000	1.56	HD 101060
NLTT 31450	2012 Jul 5	240	clear	0.8	0.3 × 15	SXD	2000	1.30	HD 118214
LSPMJ1336+2541	2013 Jul 12	90	clear	1.0	0.3 × 15	SXD	2000	1.10	HD 109691
PM I13518+4157	2013 Jul 12	90	clear	1.0	0.3 × 15	SXD	2000	1.06	HD 123233
HIP 83651	2013 Apr 17	90	cloudy	0.7	0.8 × 15	SXD	750	1.11	HD 167163
HIP 84840	2013 Apr 16	180	cloudy	0.8	0.3 × 15	SXD	2000	1.07	HD 165029
NLTT 44368	2013 Jul 12	90	clear	0.8	0.3 × 15	SXD	2000	1.32	HD 199217
HIP 97168	2013 Apr 17	90	cloudy	0.7	0.8 × 15	SXD	750	1.20	HD 197291
HIP 108822	2013 Jul 12	90	clear	1.0	0.3 × 15	SXD	2000	1.08	HD 210501
PM I22118−1005	2013 Jul 12	90	clear	1.0	0.3 × 15	SXD	2000	1.25	HD 203893
PM I23492+3458	2013 Jul 12	90	clear	1.0	0.3 × 15	SXD	2000	1.31	HD 219290

Download table as:  ASCIITypeset images: 1 2

We performed spectral decomposition analysis on HIP 6407B using the method described in Section 5.2 of Dupuy & Liu (2012). Briefly, we started with all possible pairs of the 178 IRTF/SpeX prism spectra from the library of Burgasser et al. (2010). For each template pairing, we determined the scale factors needed to minimize the rms deviation from our observed spectrum. We then computed the χ² of our Keck LGS AO flux ratios in J, H, and CH₄s bands compared to the flux ratios computed for each pairing. We excluded pairings that significantly disagreed with our measured flux ratios, p(χ²) < 0.05, and examined the remaining best pairings to determine the component spectral types. Our final spectral types of L1.0 ± 0.5 and T3 ± 1 account for the full range of spectral templates that gave equally good fits to our combined light spectrum. We estimated the flux ratio in the K band as well as flux ratios in the 2MASS photometric system by taking the mean and rms of each flux ratio among the ensemble of best-fit template pairings. Figure 15 shows the best match to our spectrum, which is provided by the templates.

The best match to our spectrum is provided by the templates DENIS-P J170548.3−051645 (L1; Burgasser et al. 2010; Allers & Liu 2013) and SDSS J120602.51+281328.7 (T3; Chiu et al. 2006; Burgasser et al. 2010) scaled to each other by the magnitudes shown in the lower panel of Figure 15, giving magnitude differences of d_J = 2.26 ± 0.05 mag and d_H = 2.51 ± 0.05 mag. We adopt spectral types of L1 ± 1 and T3 ± 1 for the components of HIP 6407B based on the typical uncertainty in infrared types for L dwarfs and the range of good matching templates for the secondary. Note that the template library from Burgasser et al. (2010) nominally only includes objects later than L0, which barely encompasses the spectral type of the proposed primary component. However, Figure 15 shows that the L1 template gives a very good match to the data, so the primary is not likely to be of much earlier type.