# A Survey of Herbig Ae/Be Multiplicity

S. Thomas, B. Rodgers, N. van der Bliek, G. Doppmann, J. Bouvier, C. Araya

Salvo, J.-L. Beuzit, F. Rigaut

► To cite this version:

S. Thomas, B. Rodgers, N. van der Bliek, G. Doppmann, J. Bouvier, et al., A Survey of Herbig Ae/Be Multiplicity. The Astronomical Journal, 2023, 165 (3), pp.135. 10.3847/1538-3881/aca803. hal-04966278

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# A Survey of Herbig Ae/Be Multiplicity

S. J. Thomas<fnref n="1" />, B. Rodgers<fnref n="2" />, N. S. van der Bliek<fnref n="3" />, G. Doppmann<fnref n="4" />, J. Bouvier<fnref n="5" />, C. Araya Salvo<fnref n="6" />, J.-L. Beuzit<fnref n="7" /> and F. Rigaut<fnref n="8" />

Received 2022 March 29; revised 2022 November 4; accepted 2022 November 8; published 2023 February 28

## Abstract

Although the majority of Herbig Ae/Be (HAEBE) stars are likely multiple systems, relatively few multiples have been identified. We aim to create a statistically significant survey of HAEBE multiplicity as a function of stellar mass, to shed light on mixed-mass star formation. Two independent adaptive optics IR imaging surveys were conducted, between 1993 and 2007. A total of 143 stars were observed, including 126 HAEBE stars. These surveys are significantly more sensitive than previous imaging work and, combined with accurate distance and proper-motion data from GAIA Data Release 3, provide a broad survey of intermediate-mass multiplicity. We perform a statistical probability analysis to identify the likely physical companions, and analyze multipepoch observations for common proper motions. We find 250 stellar detections around 88 sample stars. Of these, 70 systems are likely multiple systems, and 42 companions around 29 systems are reported here for the first time. Correcting for completeness, we find a multiplicity fraction of 54%. Multiples are found randomly across all spectral types, but high-order multiples are more common among the hottest stars. Statistically likely companions are found at distances of up to several thousand astronomical units and $\Delta K$ magnitudes ranging from <0.1 to ~9, although companions with $\Delta K < 1.5$ are rare. Companions around Herbig Ae stars tend to be closer than those around Herbig Be stars. We confirm 24 proper-motion companions in 21 systems, including roughly half of the statistically very likely companions; however, many proper-motion results are inconclusive.

Unified Astronomy Thesaurus concepts: Multiple stars (1081); Herbig Ae/Be stars (723); Surveys (1671)

Supporting material: machine-readable tables

## 1. Introduction

Herbig Ae/Be (HAEBE) stars are pre-main-sequence stars of intermediate mass (~2–9 solar masses; Herbig 1960). They exhibit emission lines in the optical and IR (e.g., Ca II, H$\alpha$ I, and H$\beta$ I) and continuum excess in the near-IR (NIR), attributed primarily to circumstellar activity (accretion flows, winds, and disk atmospheres) and circumstellar disk emission, respectively (Muzerolle et al. 2004). With masses between those of low-mass T Tauri stars and high-mass young stars, HAEBE stars fill an important parameter space in addressing the question of star formation as a function of mass.

Star formation theories tend to treat the formation of low-mass, intermediate-mass, and high-mass stars distinctly, but studies of young stellar clusters and star-forming regions reveal that stars of different masses actually form and evolve in close proximity (see Testi et al. 1998).

Therefore, a promising approach to constraining star formation models for stars of various masses is to investigate the frequencies of multiple systems and their properties (separations, mass ratio, etc.) as a function of mass of the primaries (Delgado-Donate et al. 2004). Companions to Herbig stars are often assumed to be T Tauri stars, although this is not

universally the case. Bouvier & Corporon (2001) find that low-mass companions often lack NIR excess and have weak emission lines, unlike classical T Tauri stars, suggesting that a high-mass primary star may affect the evolution of its companions, potentially shortening the lifetime of its circumstellar disk.

Like their low-mass counterparts, the T Tauri stars, HAEBE stars are often found in groups: e.g., Bouvier & Corporon (2001) find that HAEBE stars have a binary fraction that is significantly higher than those of both field G dwarfs and low-mass young stars (both of order 60%), while Testi et al. (1997) find a correlation between stellar density and spectral type. However, unlike T Tauri stars, relatively few multiplicity studies exist in the literature for HAEBE stars.

A number of imaging multiplicity surveys of HAEBEs were conducted in the 1990s, but the sample sizes were quite small (e.g., Leinert et al. 1997; Pirzkal et al. 1997). Another useful study, conducted by Perrin (2006), was focused on the study of circumstellar disks around HAEBE stars, during which a number of binaries were discovered. In addition, a number of spectroscopic multiplicity studies have been published, such as those of Baines et al. (2006) and Carmona et al. (2010), and see also the additional references within Vioque et al. (2018). The domain of discovery from these studies does not overlap with the imaging results that are the focus of this work.

Adaptive optics (AO) IR imaging offers a diffraction-limited spatial resolution and allows direct detections of the companion objects, providing position and photometry information. It thus

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<footnote n="1">¹Vera C. Rubin Observatory, Tucson, AZ, USA; sthomas@lsst.org</footnote>

<footnote n="2">²Willamette University, Portland, OR, USA; bmrodgers@willamette.edu</footnote>

<footnote n="3">³NOIRLab, La Serena, Chile; nicole.vanderbliek@noirlab.edu</footnote>

<footnote n="4">⁴W.M. Keck Observatory, Kamuela, HI, USA; gdoppmann@keck.hawaii.edu</footnote>

<footnote n="5">⁵Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, France; jerome.bouvier@univ-grenoble-alpes.fr</footnote>

<footnote n="6">⁶Colegio Los Alerces, Santiago, Chile; claudia.araya.salvo@gmail.com</footnote>

<footnote n="7">⁷Laboratoire d'Astrophysique de Marseille, France; jean-luc.beuzit@lam.fr</footnote>

<footnote n="8">⁸Australian National University, Australia; francois.rigaut@anu.edu.au</footnote>
<table><caption>Table 1
Observed Sample</caption><thead><tr><th>Name</th><th>R.A. (J2000)</th><th>Decl. (J2000)</th><th>SpecType</th><th>Teff (K)</th><th>Distance (pc)</th><th>Spt Ref/Dist Ref</th><th>Ndet</th><th>Ncomp</th><th>Instrument</th></tr></thead><tbody><tr><td>HIP 592°</td><td>00 07 12</td><td>+65 39 15</td><td>Be:</td><td>None</td><td>726<sup>732</sup><sub>720</sub></td><td>MAC68/GAIA3</td><td>2</td><td>0</td><td>NIRI/2006</td></tr><tr><td>LkHA 198</td><td>00 11 25.97</td><td>+58 49 29.1</td><td>B9</td><td>10,500*</td><td>600</td><td>HER04/TES98</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>VX Cas</td><td>00 31 30.685</td><td>+61 58 50.97</td><td>A0</td><td>9500</td><td>539<sup>534</sup><sub>545</sub></td><td>ALE13/GAIA3</td><td>2</td><td>1</td><td>NIRI/2006</td></tr><tr><td>BD+61 154</td><td>00 43 18.2567</td><td>+61 54 40.131</td><td>B8</td><td>11,500</td><td>558<sup>554</sup><sub>562</sub></td><td>WIC20/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 201</td><td>00 43 25.34</td><td>+61 38 23.4</td><td>B2</td><td>22,000*</td><td>2673<sup>2583</sup><sub>2769</sub></td><td>HER04/GAIA3</td><td>2</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HBC 334</td><td>02 16 30.1</td><td>+55 22 57</td><td>B3</td><td>18,700*</td><td>1600</td><td>HER04/TES98</td><td>5</td><td>2</td><td>NIRI/2006</td></tr><tr><td>IP Per</td><td>03 40 46.967</td><td>+32 31 53.73</td><td>A4</td><td>8500</td><td>290<sup>288</sup><sub>293</sub></td><td>ALE13/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>XY Per</td><td>03 49 36.3405</td><td>+38 58 55.453</td><td>A2</td><td>9000</td><td>425<sup>419</sup><sub>430</sub></td><td>ALE13/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>V892 Tau</td><td>04 18 40.61</td><td>+28 19 15.5</td><td>B8</td><td>11,900*</td><td>134<sup>133</sup><sub>136</sub></td><td>HER04/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>LkHA 101</td><td>04 30 14.39</td><td>+35 16 24.3</td><td>Cont</td><td>None</td><td>618<sup>583</sup><sub>658</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 283817°</td><td>04 40 32.6382</td><td>+24 26 31.323</td><td>A3:</td><td>8720*</td><td>397<sup>393</sup><sub>400</sub></td><td>WAL90/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>AB Aur</td><td>04 55 45.8445</td><td>+30 33 04.292</td><td>A0</td><td>9800</td><td>156<sup>155</sup><sub>157</sub></td><td>ALE13/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 31648</td><td>04 58 46.2665</td><td>+29 50 36.999</td><td>A5</td><td>8200</td><td>156<sup>155</sup><sub>157</sub></td><td>ALE13/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>UX Ori</td><td>05 04 29.9908</td><td>-03 47 14.280</td><td>A4</td><td>8500</td><td>323<sup>320</sup><sub>326</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V1012 Ori</td><td>05 11 36.55</td><td>-02 22 48.5</td><td>A4</td><td>8500</td><td>378<sup>372</sup><sub>384</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V1366 Ori</td><td>05 16 00.4779</td><td>-09 48 35.421</td><td>A0</td><td>9500</td><td>309<sup>306</sup><sub>311</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V346 Ori</td><td>05 24 42.8015</td><td>+01 43 48.254</td><td>A7</td><td>7750</td><td>339<sup>337</sup><sub>341</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>CO Ori</td><td>05 27 38.3370</td><td>+11 25 38.933</td><td>F7Vev</td><td>6280*</td><td>399<sup>396</sup><sub>403</sub></td><td>MOR01/GAIA3</td><td>1</td><td>1</td><td>ADONIS/93/96</td></tr><tr><td>HD 35929</td><td>05 27 42.7911</td><td>-08 19 38.444</td><td>F1</td><td>7000</td><td>380<sup>377</sup><sub>384</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 36112</td><td>05 30 27.5296</td><td>+25 19 57.083</td><td>A7</td><td>7800</td><td>156<sup>155</sup><sub>157</sub></td><td>ALE13/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HK Ori</td><td>05 31 28.04</td><td>+12 09 10.3</td><td>A4</td><td>8500</td><td>460</td><td>FAI15/HIL92</td><td>2</td><td>2</td><td>NIRI/2006</td></tr><tr><td>HD 244604</td><td>05 31 57.3</td><td>+11 17 41</td><td>A2</td><td>9000</td><td>403<sup>400</sup><sub>407</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 245185</td><td>05 35 09.605</td><td>+10 01 51.51</td><td>A0</td><td>10,000</td><td>415<sup>410</sup><sub>420</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>T Ori</td><td>05 35 50.45</td><td>-05 28 35.0</td><td>A2</td><td>9000</td><td>403<sup>398</sup><sub>407</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NACO/2006</td></tr><tr><td>CQ Tau</td><td>05 35 58.4670</td><td>+24 44 54.092</td><td>F3</td><td>6750</td><td>149<sup>148</sup><sub>151</sub></td><td>ALE13/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>BD-06 1253</td><td>05 36 25.4313</td><td>-06 42 57.704</td><td>A0</td><td>9750</td><td>378<sup>363</sup><sub>395</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>BN Ori</td><td>05 36 29.347</td><td>+06 50 02.17</td><td>F4</td><td>6590*</td><td>311<sup>307</sup><sub>315</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 37258</td><td>05 36 59.250</td><td>-06 09 16.36</td><td>A0</td><td>9750</td><td>380<sup>376</sup><sub>384</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>BF Ori</td><td>05 37 13.2626</td><td>-06 35 00.580</td><td>A2</td><td>9000</td><td>382<sup>378</sup><sub>386</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HD 37357</td><td>05 37 47.079</td><td>-06 42 30.25</td><td>A0</td><td>9500</td><td>466<sup>321</sup><sub>321</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HD 37411</td><td>05 38 14.505</td><td>-05 25 13.30</td><td>A0</td><td>9750</td><td>350<sup>345</sup><sub>356</sub></td><td>FAI15/GAIA3</td><td>2</td><td>2</td><td>NIRI/2006</td></tr><tr><td>HD 37490</td><td>05 39 11.1463</td><td>+04 07 17.281</td><td>B3</td><td>19,000</td><td>506<sup>470</sup><sub>548</sub></td><td>LEV06/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 245906</td><td>05 39 30.481</td><td>+26 19 55.08</td><td>A6</td><td>8350*</td><td>2000</td><td>HER04/HER04</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>RR Tau</td><td>05 39 30.53</td><td>+26 22 26.4</td><td>A0</td><td>9520*</td><td>810<sup>791</sup><sub>830</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V350 Ori</td><td>05 40 11.77</td><td>-09 42 11.1</td><td>A2</td><td>9000</td><td>396<sup>389</sup><sub>404</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HD 37806</td><td>05 41 02.2927</td><td>-02 43 00.729</td><td>B9</td><td>11,000</td><td>402<sup>407</sup><sub>406</sub></td><td>ALE13/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 250550</td><td>06 01 59.9885</td><td>+16 30 56.730</td><td>B9</td><td>11,000</td><td>760<sup>733</sup><sub>790</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 341</td><td>06 30 50.13</td><td>+10 33 09.8</td><td>F3</td><td>6740*</td><td>1298<sup>260</sup><sub>1337</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>VY Mon°</td><td>06 31 06.94</td><td>+10 26 05.0</td><td>B8</td><td>12,000</td><td>800</td><td>FAI15/TES98</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 215</td><td>06 32 41.795</td><td>+10 09 33.64</td><td>B6</td><td>14,000</td><td>739<sup>724</sup><sub>754</sub></td><td>ALE13/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HD 259431</td><td>06 33 05.1899</td><td>+10 19 19.984</td><td>B6</td><td>14,000</td><td>653<sup>642</sup><sub>665</sub></td><td>ALE13/GAIA3</td><td>2</td><td>2</td><td>NIRI/2006</td></tr><tr><td>R Mon°</td><td>06 39 09.95</td><td>+08 44 10.7</td><td>B8</td><td>12,000</td><td>800</td><td>FAI15/TES98</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HBC 531</td><td>06 39 41.57</td><td>+09 34 40.5</td><td>G1</td><td>5930*</td><td>711<sup>703</sup><sub>719</sub></td><td>HER04/GAIA3</td><td>3</td><td>0</td><td>NIRI/2006</td></tr><tr><td>HBC 217</td><td>06 40 42.18</td><td>+09 33 37.5</td><td>F7</td><td>6280*</td><td>727<sup>720</sup><sub>735</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 25</td><td>06 40 44.64</td><td>+09 48 02.2</td><td>B7</td><td>12,500</td><td>707<sup>656</sup><sub>768</sub></td><td>FAI15/GAIA3</td><td>1</td><td>0</td><td>NIRI/2006</td></tr><tr><td>HBC 222</td><td>06 40 51.19</td><td>+09 44 46.2</td><td>F7</td><td>6280*</td><td>722<sup>715</sup><sub>729</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HBC 535</td><td>06 40 56.50</td><td>+09 54 10.4</td><td>G2</td><td>5830*</td><td>719<sup>712</sup><sub>726</sub></td><td>HER04/GAIA3</td><td>3</td><td>0</td><td>NIRI/2006</td></tr><tr><td>S Mon</td><td>06 40 58.6607</td><td>+09 53 44.715</td><td>B1</td><td>25,200</td><td>760</td><td>LEV06/SUN97</td><td>1</td><td>1</td><td>ADONIS/1995</td></tr><tr><td>LkHA 53</td><td>06 41 06.20</td><td>+09 36 23.0</td><td>G4</td><td>5740*</td><td>734<sup>726</sup><sub>742</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 52721</td><td>07 01 49.5104</td><td>-11 18 03.328</td><td>B2</td><td>22,500</td><td>1150</td><td>FAI15/HER82</td><td>1</td><td>1</td><td>ADONIS/93/96</td></tr><tr><td>LkHA 218</td><td>07 02 42.53</td><td>-11 26 11.8</td><td>B9</td><td>10,500</td><td>1178<sup>1156</sup><sub>1200</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>Z CMa</td><td>07 03 43.1619</td><td>-11 33 06.209</td><td>A4</td><td>8500</td><td>1050<sup>900</sup><sub>1200</sub></td><td>FAI15/SHE99</td><td>1</td><td>1</td><td>NACO/2006</td></tr><tr><td>LkHA 220</td><td>07 04 06.70</td><td>-11 26 08.5</td><td>B7</td><td>13,000</td><td>1159<sup>1139</sup><sub>1180</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 53367</td><td>07 04 25.5315</td><td>-10 27 15.739</td><td>B0</td><td>29,500</td><td>1150</td><td>FAI15/HER82</td><td>1</td><td>1</td><td>ADONIS/93/96</td></tr><tr><td>NX Pup</td><td>07 19 28.2606</td><td>-44 35 11.286</td><td>F1</td><td>7000</td><td>450</td><td>FAI15/HIL92</td><td>2</td><td>2</td><td>NACO/2006</td></tr><tr><td>HD 76534</td><td>08 55 08.7067</td><td>-43 27 59.861</td><td>B3</td><td>19,000</td><td>885<sup>863</sup><sub>909</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>ADONIS/93/95</td></tr><tr><td>RCW 34</td><td>08 56 25.0</td><td>-43 05 40</td><td>O8.5:</td><td>35,900*</td><td>2068<sup>2005</sup><sub>2134</sub></td><td>BIK10/GAIA3</td><td>5</td><td>5</td><td>ADONIS/1993</td></tr><tr><td>HD 85567</td><td>09 50 28.5367</td><td>-60 58 02.959</td><td>B7</td><td>13,000</td><td>1047<sup>1030</sup><sub>1066</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr></tbody></table>
<table><caption>**Table 1**
(Continued)</caption><thead><tr><th>Name</th><th>R.A. (J2000)</th><th>Decl. (J2000)</th><th>SpecType</th><th>Teff (K)</th><th>Distance (pc)</th><th>Spt Ref/Dist Ref</th><th>Ndet</th><th>Ncomp</th><th>Instrument</th></tr></thead><tbody><tr><td>HD 94509</td><td>10 53 27.262</td><td>-58 25 24.54</td><td>B8</td><td>11,500</td><td>1640<sup>1596</sup><sub>1688</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 95881</td><td>11 01 57.620</td><td>-71 30 48.35</td><td>A0</td><td>10,000</td><td>1110<sup>1086</sup><sub>1135</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NACO/2006</td></tr><tr><td>HD 97048</td><td>11 08 03.3183</td><td>-77 39 17.486</td><td>B9</td><td>10,500</td><td>184<sup>184</sup><sub>185</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NACO/2006</td></tr><tr><td>HD 97300</td><td>11 09 50.0183</td><td>-76 36 47.723</td><td>B9V:</td><td>10,500*</td><td>189<sup>188</sup><sub>190</sub></td><td>RYD80/GAIA3</td><td>1</td><td>1</td><td>NACO/2006</td></tr><tr><td>HD 98922</td><td>11 22 31.6739</td><td>-53 22 11.452</td><td>B9</td><td>10,500</td><td>651<sup>660</sup><sub>662</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 100546</td><td>11 33 25.4408</td><td>-70 11 41.239</td><td>A0</td><td>9750</td><td>108<sup>108</sup><sub>109</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>ADONIS/1995</td></tr><tr><td>HD 101412</td><td>11 39 44.462</td><td>-60 10 27.74</td><td>A0</td><td>9750</td><td>412<sup>410</sup><sub>415</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>ADONIS/1995</td></tr><tr><td>DX Cha</td><td>12 00 05.0846</td><td>-78 11 34.564</td><td>A7</td><td>8000</td><td>107<sup>106</sup><sub>107</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>ADONIS/1995</td></tr><tr><td>HD 132947</td><td>15 04 56.053</td><td>-63 07 52.63</td><td>B9</td><td>10,250</td><td>380<sup>377</sup><sub>383</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>ADONIS/1995</td></tr><tr><td>HD 135344</td><td>15 15 48.439</td><td>-37 09 16.03</td><td>F6</td><td>6375</td><td>135<sup>134</sup><sub>136</sub></td><td>FAI15/GAIA3</td><td>0</td><td>0</td><td>ADONIS/1995</td></tr><tr><td>HD 141569</td><td>15 49 57.7489</td><td>-03 55 16.360</td><td>A0</td><td>9500</td><td>112<sup>111</sup><sub>112</sub></td><td>WIC20/GAIA3</td><td>2</td><td>2</td><td>NIRI/2007</td></tr><tr><td>HD 142666</td><td>15 56 40.023</td><td>-22 01 40.01</td><td>F0</td><td>7250</td><td>146<sup>146</sup><sub>147</sub></td><td>WIC20/GAIA3</td><td>0</td><td>0</td><td>ADONIS/1995</td></tr><tr><td>HD 144432</td><td>16 06 57.9575</td><td>-27 43 09.806</td><td>A8</td><td>7500</td><td>155<sup>154</sup><sub>155</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>ADONIS/95/96</td></tr><tr><td>V856 Sco</td><td>16 08 34.2868</td><td>-39 06 18.337</td><td>A4</td><td>8500</td><td>159<sup>158</sup><sub>159</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>ADONIS/1995</td></tr><tr><td>PDS415</td><td>16 18 37.3</td><td>-24 05 22.5</td><td>F7</td><td>6250</td><td>156<sup>156</sup><sub>156</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NIRI/2007</td></tr><tr><td>HD 149914</td><td>16 38 28.6536</td><td>-18 13 13.724</td><td>B9.5:IV</td><td>10,500*</td><td>154<sup>154</sup><sub>155</sub></td><td>HOU88/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 150193</td><td>16 40 17.9221</td><td>-23 53 45.180</td><td>A1</td><td>9250</td><td>151<sup>50</sup><sub>51</sub></td><td>WIC20/GAIA3</td><td>1</td><td>1</td><td>NIRI/2007</td></tr><tr><td>KK Oph</td><td>17 10 08.065</td><td>-27 15 18.24</td><td>A4</td><td>8500</td><td>167<sup>163</sup><sub>171</sub></td><td>FAI15/GAIA3</td><td>1</td><td>1</td><td>NACO/2006</td></tr><tr><td>PDS453</td><td>17 20 56.2</td><td>-26 03 30.8</td><td>F2V</td><td>6890*</td><td>129<sup>122</sup><sub>137</sub></td><td>VIE03/GAIA3</td><td>10</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 158352</td><td>17 28 49.6549</td><td>+00 19 50.251</td><td>A8Vp</td><td>7580*</td><td>64<sup>64</sup><sub>64</sub></td><td>MOR01/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>BD-22 4400</td><td>17 43 55.644</td><td>-22 05 44.71</td><td>B0.5V:</td><td>30,000*</td><td>1544<sup>1502</sup><sub>1589</sub></td><td>GAR77/GAIA3</td><td>10</td><td>0</td><td>NIRI/2007</td></tr><tr><td>Hen 3-1475</td><td>17 45 14.16</td><td>-17 56 46.6</td><td>B7e AGB?</td><td>13,000*</td><td>?</td><td>VIE03/-</td><td>1</td><td>1</td><td>NACO/2006</td></tr><tr><td>PDS469</td><td>17 50 57.8</td><td>-14 16 11</td><td>A0</td><td>9500</td><td>1009<sup>954</sup><sub>1072</sub></td><td>WIC20/GAIA3</td><td>10</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 165133</td><td>18 05 30.414</td><td>-24 12 12.90</td><td>B2III/Ive</td><td>22,000*</td><td>1342<sup>1301</sup><sub>1387</sub></td><td>THE94/GAIA3</td><td>10</td><td>0</td><td>NIRI/2006</td></tr><tr><td>HD 312787</td><td>18 11 33.2</td><td>-19 30 39</td><td>F8e:</td><td>6200*</td><td>204<sup>202</sup><sub>206</sub></td><td>NES95/GAIA3</td><td>9</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 168607</td><td>18 21 14.8862</td><td>-16 22 31.762</td><td>B9Iae</td><td>10,500*</td><td>1839<sup>1764</sup><sub>1922</sub></td><td>THE94/GAIA3</td><td>1</td><td>1</td><td>NIRI/2007</td></tr><tr><td>MWC 922</td><td>18 21 15.9</td><td>-13 01 27</td><td>B[e]</td><td>None</td><td>1700</td><td>THE94/TUT07</td><td>6</td><td>4</td><td>NIRI/2007</td></tr><tr><td>HD 169142</td><td>18 24 29.7787</td><td>-29 46 49.371</td><td>A8</td><td>7500</td><td>115<sup>115</sup><sub>115</sub></td><td>ALE13/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>MWC 930</td><td>18 26 25.4</td><td>-07 13 11</td><td>B7:</td><td>13,000*</td><td>?</td><td>CAR10/CAR10</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>MWC 297</td><td>18 27 39.6</td><td>-03 49 52</td><td>B1</td><td>24,000</td><td>418<sup>413</sup><sub>423</sub></td><td>WIC20/GAIA3</td><td>1</td><td>1</td><td>NIRI/2007</td></tr><tr><td>VV Ser</td><td>18 28 47.86</td><td>+00 08 40.0</td><td>B6</td><td>14,000</td><td>409<sup>403</sup><sub>415</sub></td><td>WIC20/GAIA3</td><td>1</td><td>0</td><td>NIRI/2006</td></tr><tr><td>MWC 300</td><td>18 29 25.6895</td><td>-06 04 37.279</td><td>B2</td><td>23,000</td><td>1787<sup>1707</sup><sub>1874</sub></td><td>WIC20/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>AS 310</td><td>18 33 21.2</td><td>-04 58 02</td><td>B1</td><td>26,000</td><td>2461<sup>2387</sup><sub>2540</sub></td><td>WIC20/GAIA3</td><td>12</td><td>2</td><td>NIRI/2007</td></tr><tr><td>MWC 939</td><td>18 34 16.24</td><td>-17 36 13.5</td><td>B[e]</td><td>None</td><td>804<sup>839</sup><sub>772</sub></td><td>THE94/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>BD-13 5061</td><td>18 39 26.1039</td><td>-13 50 47.167</td><td>B9Iae</td><td>10,500*</td><td>1708<sup>1668</sup><sub>1750</sub></td><td>THE94/GAIA3</td><td>2</td><td>0</td><td>NIRI/2007</td></tr><tr><td>PDS530</td><td>18 41 34.8</td><td>+08 08 22</td><td>F0V:</td><td>7200*</td><td>1000<sup>600</sup><sub>1000</sub></td><td>VIE03/VIE03</td><td>11</td><td>3</td><td>NIRI/2007</td></tr><tr><td>MWC 953</td><td>18 43 28.423</td><td>-03 46 16.95</td><td>B2Ve</td><td>22,000*</td><td>2151<sup>2070</sup><sub>2238</sub></td><td>CAR10/GAIA3</td><td>9</td><td>3</td><td>NIRI/2007</td></tr><tr><td>AS 321</td><td>18 47 04.833</td><td>-11 41 02.74</td><td>A5V</td><td>8200*</td><td>310<sup>220</sup><sub>440</sub></td><td>CAR10/CAR10</td><td>7</td><td>1</td><td>NIRI/2007</td></tr><tr><td>HD 179218</td><td>19 11 11.2541</td><td>+15 47 15.630</td><td>A0</td><td>9500</td><td>260<sup>258</sup><sub>262</sub></td><td>WIC20/GAIA3</td><td>3</td><td>2</td><td>NIRI/2006</td></tr><tr><td>BD+14 3887</td><td>19 21 33.975</td><td>+14 52 56.89</td><td>B3Ibe</td><td>18,700*</td><td>4496<sup>4120</sup><sub>4948</sub></td><td>CAR10/GAIA3</td><td>2</td><td>2</td><td>NIRI/2006</td></tr><tr><td>WW Vul</td><td>19 25 58.750</td><td>+21 12 31.28</td><td>A2</td><td>9000</td><td>485<sup>481</sup><sub>489</sub></td><td>ALE13/GAIA3</td><td>1</td><td>0</td><td>NIRI/2006</td></tr><tr><td>PX Vul</td><td>19 26 40.25</td><td>+23 53 50.8</td><td>F3</td><td>6740*</td><td>636<sup>616</sup><sub>657</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HBC 687</td><td>19 29 00.7</td><td>+09 38 39</td><td>A5:ea</td><td>8200*</td><td>300</td><td>THE94/CON08</td><td>10</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V409 Vul</td><td>19 40 13.6</td><td>+22 31 34</td><td>B8[e]</td><td>11,900*</td><td>2339<sup>2220</sup><sub>2471</sub></td><td>MIR99/GAIA3</td><td>2</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 338916</td><td>19 45 42.110</td><td>+25 21 16.43</td><td>O8e</td><td>35,900*</td><td>2171<sup>2107</sup><sub>2240</sub></td><td>THE94/GAIA3</td><td>6</td><td>0</td><td>NIRI/2007</td></tr><tr><td>MWC 623</td><td>19 56 31.8</td><td>+31 06 16</td><td>B4III</td><td>17,000*</td><td>3700<sup>3504</sup><sub>3918</sub></td><td>ZIC01/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 190073</td><td>20 03 02.5099</td><td>+05 44 16.676</td><td>A0</td><td>9750</td><td>848<sup>826</sup><sub>871</sub></td><td>WIC20/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V1685 Cyg</td><td>20 20 28.2473</td><td>+41 21 51.586</td><td>B2</td><td>23,000</td><td>913<sup>897</sup><sub>929</sub></td><td>WIC20/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>LkHA 224</td><td>20 20 29.26</td><td>+41 21 28.6</td><td>F9:</td><td>6115*</td><td>980</td><td>HER04/SHE91</td><td>3</td><td>1</td><td>NIRI/2007</td></tr><tr><td>BD+41 3731</td><td>20 24 15.7155</td><td>+42 18 01.377</td><td>B4</td><td>17,000</td><td>991<sup>974</sup><sub>1008</sub></td><td>ALE13/GAIA3</td><td>1</td><td>1</td><td>NIRI/2007</td></tr><tr><td>HBC 694</td><td>20 24 29.49</td><td>+42 14 03.7</td><td>A5eV</td><td>8200*</td><td>1200</td><td>THE94/CC78</td><td>2</td><td>2</td><td>ADONIS/1996</td></tr><tr><td>MWC 1021</td><td>20 29 27.3</td><td>+41 40 45</td><td>Be</td><td>None</td><td>3650<sup>3344</sup><sub>4016</sub></td><td>THE94/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>MWC 349</td><td>20 32 45.44</td><td>+40 39 36.8</td><td>B[e] LBV?</td><td>None</td><td>1400</td><td>GVA12/GVA12</td><td>1</td><td>1</td><td>NIRI/2007</td></tr><tr><td>PV Cep</td><td>20 45 53.96</td><td>+67 57 38.9</td><td>A5:</td><td>8200*</td><td>357<sup>352</sup><sub>362</sub></td><td>THE94/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>AS 442</td><td>20 47 37.47</td><td>+43 47 24.9</td><td>B8Ve</td><td>11,900*</td><td>834<sup>826</sup><sub>843</sub></td><td>MOR01/GAIA3</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>AS 443</td><td>20 48 04.78</td><td>+43 47 25.8</td><td>B9</td><td>11,000</td><td>853<sup>842</sup><sub>863</sub></td><td>WIC20/GAIA3</td><td>5</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 147</td><td>20 51 02.71</td><td>+43 49 32.0</td><td>B2</td><td>22,000*</td><td>2352<sup>2386</sup><sub>2421</sub></td><td>HER04/GAIA3</td><td>2</td><td>1</td><td>NIRI/2006</td></tr><tr><td>LkHA 167</td><td>20 52 04.65</td><td>+44 37 30.4</td><td>A2:</td><td>8970*</td><td>1148<sup>1091</sup><sub>1211</sub></td><td>THE94/GAIA3</td><td>3</td><td>1</td><td>NIRI/2006</td></tr></tbody></table>
<table><caption>**Table 1**
(Continued)</caption><thead><tr><th>Name</th><th>R.A. (J2000)</th><th>Decl. (J2000)</th><th>SpecType</th><th>Teff (K)</th><th>Distance (pc)</th><th>Spt Ref/Dist Ref</th><th>Ndet</th><th>Ncomp</th><th>Instrument</th></tr></thead><tbody><tr><td>LkHA 168</td><td>20 52 06.05</td><td>+44 17 16.1</td><td>F2:</td><td>6890*</td><td>838<sup>770</sup><sub>918</sub></td><td>THE94/GAIA3</td><td>2</td><td>1</td><td>NIRI/2006</td></tr><tr><td>LkHA 170</td><td>20 52 12.76</td><td>+44 19 26.0</td><td>A0</td><td>9520*</td><td>764<sup>254</sup><sub>774</sub></td><td>HER04/GAIA3</td><td>6</td><td>1</td><td>NIRI/2006</td></tr><tr><td>DV Aqr</td><td>20 58 41.8401</td><td>-14 28 59.260</td><td>A3/9V</td><td>8720*</td><td>89<sup>89</sup><sub>90</sub></td><td>THE94/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 200775</td><td>21 01 36.9198</td><td>+68 09 47.763</td><td>B3</td><td>19,000</td><td>355<sup>350</sup><sub>360</sub></td><td>WIC20/GAIA3</td><td>1</td><td>1</td><td>ADONIS/1996</td></tr><tr><td>LkHA 324</td><td>21 03 54.14</td><td>+50 15 10.4</td><td>B7</td><td>12,500</td><td>622<sup>619</sup><sub>626</sub></td><td>WIC20/GAIA3</td><td>3</td><td>2</td><td>NIRI/2006</td></tr><tr><td>HD 203024</td><td>21 16 03.025</td><td>+68 54 52.13</td><td>A4</td><td>8500</td><td>420<sup>470</sup><sub>470</sub></td><td>WIC20/KUN00</td><td>1</td><td>1</td><td>NIRI/2006</td></tr><tr><td>HD 235495</td><td>21 21 27.500</td><td>+50 59 47.64</td><td>A0e</td><td>9520*</td><td>516<sup>512</sup><sub>520</sub></td><td>THE94/GAIA3</td><td>4</td><td>2</td><td>NIRI/2006</td></tr><tr><td>LkHA 349</td><td>21 36 50.72</td><td>+57 31 10.8</td><td>F9</td><td>6115*</td><td>986<sup>974</sup><sub>999</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>V645 Cyg</td><td>21 39 58.24</td><td>+50 14 21.2</td><td>B0</td><td>30,000</td><td>3500<sup>4000</sup><sub>4000</sub></td><td>WIC20/GOO86</td><td>2</td><td>1</td><td>NIRI/2007</td></tr><tr><td>BD+65 1637</td><td>21 42 50.18</td><td>+66 06 35.2</td><td>B4</td><td>16,750</td><td>894<sup>883</sup><sub>905</sub></td><td>WIC20/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 234</td><td>21 43 06.68</td><td>+66 06 54.6</td><td>B8</td><td>11,500</td><td>877<sup>862</sup><sub>893</sub></td><td>WIC20/GAIA3</td><td>2</td><td>2</td><td>NIRI/2007</td></tr><tr><td>BD+46 3471</td><td>21 52 34.0993</td><td>+47 13 43.612</td><td>B9</td><td>10,500</td><td>769<sup>762</sup><sub>777</sub></td><td>WIC20/GAIA3</td><td>4</td><td>4</td><td>NIRI/2006</td></tr><tr><td>LkHA 257</td><td>21 54 18.78</td><td>+47 12 09.7</td><td>A1</td><td>9250</td><td>801<sup>793</sup><sub>810</sub></td><td>WIC20/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>BH Cep</td><td>22 01 42.867</td><td>+69 44 36.53</td><td>F5</td><td>6440*</td><td>328<sup>326</sup><sub>329</sub></td><td>HER04/GAIA3</td><td>3</td><td>2</td><td>NIRI/2007</td></tr><tr><td>MWC 1055</td><td>22 08 25.3</td><td>+54 13 25</td><td>B[e]</td><td>None</td><td>6345<sup>5896</sup><sub>6868</sub></td><td>THE94/GAIA3</td><td>2</td><td>0</td><td>NIRI/2007</td></tr><tr><td>BO Cep</td><td>22 16 54.06</td><td>+70 03 45.0</td><td>F4</td><td>6590*</td><td>374<sup>372</sup><sub>376</sub></td><td>HER04/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>SV Cep °</td><td>22 21 33.19</td><td>+73 40 27.1</td><td>A7</td><td>8000</td><td>342<sup>340</sup><sub>343</sub></td><td>WIC20/GAIA3</td><td>1</td><td>1</td><td>ADONIS/1996</td></tr><tr><td>LkHA 233</td><td>22 34 40.98</td><td>+40 40 04.3</td><td>A7</td><td>8000</td><td>880</td><td>WIC20/TES98</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>HD 240010</td><td>22 38 31.8311</td><td>+55 50 05.387</td><td>B1:Vnnep</td><td>25,400*</td><td>1954<sup>1906</sup><sub>2004</sub></td><td>THE94/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>MWC 657</td><td>22 42 41.91</td><td>+60 24 00.8</td><td>Be</td><td>None</td><td>3338<sup>4199</sup><sub>4189</sub></td><td>THE94/GAIA3</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>BD+57 2615</td><td>22 47 49.5709</td><td>+58 08 49.522</td><td>B4e</td><td>17,000*</td><td>1534<sup>1499</sup><sub>1569</sub></td><td>THE94/GAIA3</td><td>2</td><td>0</td><td>NIRI/2006</td></tr><tr><td>LkHA 350</td><td>22 49 07.23</td><td>+62 11 08.4</td><td>B8</td><td>11,900*</td><td>2907<sup>2768</sup><sub>3061</sub></td><td>HER04/GAIA3</td><td>2</td><td>2</td><td>NIRI/2006</td></tr><tr><td>HD 216629</td><td>22 53 15.6047</td><td>+62 08 44.986</td><td>B2</td><td>21,500</td><td>811<sup>802</sup><sub>820</sub></td><td>WIC20/GAIA3</td><td>3</td><td>2</td><td>NIRI/2006</td></tr><tr><td>V374 Cep</td><td>23 05 07.457</td><td>+62 15 36.54</td><td>B5</td><td>15,500</td><td>841<sup>832</sup><sub>850</sub></td><td>WIC20/GAIA3</td><td>1</td><td>0</td><td>NIRI/2006</td></tr><tr><td>MWC 1080</td><td>23 17 25.5744</td><td>+60 50 43.340</td><td>B0</td><td>31,000</td><td>1490<sup>1426</sup><sub>1560</sub></td><td>WIC20/GAIA3</td><td>7</td><td>7</td><td>NIRI/2006</td></tr><tr><td>HBC 742</td><td>23 52 33.10</td><td>+68 25 55.3</td><td>B8:</td><td>11,900*</td><td>850</td><td>THE94/TES98</td><td>0</td><td>0</td><td>NIRI/2007</td></tr><tr><td>LkHA 259</td><td>23 58 41.54</td><td>+66 26 12.9</td><td>A9:</td><td>7390*</td><td>724<sup>716</sup><sub>731</sub></td><td>THE94/GAIA3</td><td>1</td><td>1</td><td>NIRI/2007</td></tr></tbody></table>

Notes. In the “Teff” column, the symbol “*” indicates the spectral type that was used to derive the effective temperature. °—HIP 592 is often confused with HBC 324 in the literature; HD 283817 is identified as a G3+K spectroscopic binary by Martin (1993); VY Mon has a large uncertainty in Teff; R Mon is classified as a continuum star by HER04; and SV Cep is classified as A0 by HER04

References. MAC68: MacConnell (1968); GAR77: Garrison et al. (1977); CC78: Calvet & Cohen (1978); RYD80: Rydgren (1980); GOO86: Goodrich (1986); HOU88: Houk & Smith-Moore (1988); WAL90: Walter et al. (1990); SHE91: Shevchenko et al. (1991); HIL92: Hillenbrand et al. (1992); THE94: Thé et al. (1994); NES95: Nesterov et al. (1995); SUN97: Sung et al. (1997); TES98: Testi et al. (1998); MIR99: Miroshnichenko et al. (1999); SHE99: Shevchenko et al. (1999); KUN00: Kun et al. (2000); MOR01: Mora et al. (2001); ZIC01: Zickgraf (2001), VIE03: Vieira et al. (2003); HER04: Hernández et al. (2004); LEV06: Levenhagen & Leister (2006); TUT07: Tuthill & Lloyd (2007); CON08: Connelley et al. (2008); BIK10: Bik et al. (2010); CAR10: Carmona et al. (2010); GVA12: Gvaramadze & Menten (2012); ALE13: Alecian et al. (2013); FAL15: Fairlamb et al. (2015); WIC20: Wichittanakom et al. (2020); and GAIA3: Gaia Collaboration et al. (2022). (This table is available in machine-readable form.)

gives us access to an area in the parameter space {resolution, magnitude difference} that is not available with some other techniques. Our results show that we are probing both more deeply and more tightly (that is, closer in) than previous studies in the literature. Using the Near-Infrared Imager (NIRI) with Altair on Gemini North, for example, for separations greater than 2", we detect stars up to 9 mag fainter than the primary star; sources 2 mag fainter are detected as close as 0.1"1 to the primary star (see Section 3.3). Because of the extinction that is associated with objects in star-forming regions, the NIRI also offers a less obscured wavelength region than the optical, through which to study these objects.

The survey presented here is the most extensive and complete database of multiplicity among HAEBEs that we are aware of, spanning nearly three decades. It provides statistically significant answers regarding the frequency and degree of multiplicity as a function of the primary star mass, as well as an indication of the types of companions that are found in HAEBE systems. The recent release of accurate distance and proper-motion data from GAIA (Gaia Collaboration et al.

2016, 2018) provides the opportunity to determine the physical parameters of these systems with higher accuracy than was previously possible.

In Section 2, the target sample is introduced. Section 3 describes the observations and data reductions for each survey, including a discussion of the detection limits as a function of the separation from the sample stars. Section 4 describes the detections and the statistical probability analysis used to identify those that are likely physical companions. In Section 5, we analyze the results, considering the multiplicity frequency, HAEBE systems in particular, and high-order multiple systems. Finally, a multiepoch analysis for common proper motion is presented in Section 6, with conclusions in Section 7.

## 2. The Sample

The class of HAEBE stars is heterogeneous, spanning a large range of spectral types—from B0 to F9 (~1.2 to ≥15 $M_\odot$)—as well as distances, especially the Be stars (Herbig 1960).
<table><caption>**Table 2**
Details of the Observing Surveys</caption><thead><tr><th>Telescope</th><th>Diameter</th><th>Instrument</th><th>Plate Scale</th><th>FOV</th><th>High-sensitivity FOV</th><th>Year Observed</th></tr></thead><tbody><tr><td>La Silla</td><td>3.6 m</td><td>Adonis</td><td>51 mas</td><td>16"</td><td>6"</td><td>1993</td></tr><tr><td>CFHT</td><td>3.6 m</td><td>PUEO</td><td>34.4 mas</td><td>16"</td><td>10"</td><td>1995/1996</td></tr><tr><td>Gemini North</td><td>8 m</td><td>NIRI</td><td>22 mas</td><td>11"</td><td>5"/5</td><td>2005/2006</td></tr><tr><td>Gemini North</td><td>8 m</td><td>NIRI</td><td>22 mas</td><td>22"</td><td>8"/5</td><td>2007</td></tr><tr><td>VLT</td><td>8 m</td><td>NACO</td><td>13.21 mas</td><td>14"</td><td>7"</td><td>2007</td></tr></tbody></table>

Therefore, to be able to draw statistically significant conclusions, and to substantially increase the known pool of multiple systems, a large sample is required.

We started with all the tables of Thé et al. (1994; hereafter, “Thé”), including Table 6, which lists stars that may not be HAEBE stars. This list was supplemented with HAEBE stars from the later literature (primarily Hillenbrand 1997; Testi et al. 1997; Malfait et al. 1998; Vieira et al. 2003; Acke et al. 2005). From this compilation, we selected optically bright stars ($R < 15$) that can serve as their own AO guide stars, which turned out to be more than 95% of the list. A sample of over 300 stars was compiled, roughly half of which are presented here, predominantly from the northern hemisphere. Of the stars reported here, 10 originate from Table 6 of Thé, and 16 are from other sources; the remaining 117 are from Tables 1 through 5 of Thé. Observations of this sample were conducted during 2005 and 2007, and are hereafter referred to as the “2005 Survey.”

In addition, we report the results of another earlier campaign conducted with AO at the Canada-France-Hawaii Telescope (CFHT) and European Southern Observatory (ESO), between 1993 December and 1997 October. This sample of 62 stars was compiled from only Table 1 of Thé, and is limited to a magnitude range of $R = 4$ to $R = 14$, due to the AO wave-front sensor sensibility and the dynamic range of the science camera. These data are hereafter referred to as the “1995 Survey.” There are 45 stars in common between the two surveys, for a total of 143 unique sample stars in our sample.

The observed stars are listed in Table 1, with the following information. Column (1): common name (typically from SIMBAD; Wenger et al. 2000). Columns (2) and (3): R.A. and decl. Columns (4)–(7): spectral type; effective temperature; distance; and references for these (see the following). Column (8): the number of other stars detected (Ndet) within the radius of the sample star, as defined by the high-resolution field of view (FOV) given in Table 2. Column (9): the number of these that are likely companions (Ncomp; see Section 4). Column (10): the instrument used and the year of observation. For the targets in common between the 2005 and 1995 surveys, the 2005 observations are listed. The 1995 survey observations that are not listed in Table 1 are provided in the Appendix; we will return to these in Section 6.

## 2.1. Distances and Proper Motions

The GAIA mission has greatly improved the distance information for our sample. While less than 20% of the stars have reliable HIPPARCOS parallaxes, 142 stars are included in GAIA Data Release 3 (Gaia Collaboration et al. 2022; hereafter, “GAIA3”). However, not all of these stars have reported parallaxes, and some reported parallaxes are not yet reliable. So, for 119 stars, the distance is directly calculated

from GAIA3 as an inverse parallax, and the distance errors are similarly calculated from the parallax errors given (while noting the more sophisticated treatment by Bailer-Jones et al. 2018 for GAIA Data Release 2). Of the remaining, 10 stars have no parallaxes in GAIA3, and 14 stars are rejected, based on the relative parallax errors and other validity tests, following Appendix C of Lindegren et al. (2018).

Overall, we accepted GAIA distances with percentage errors in parallaxes of ~9% or less, with one exception (HD 37357 had a parallax error of 10.5%, but a derived distance consistent with the literature; Wade et al. 2007). For most stars, the error was much less (average error ~2%); those with parallax errors of 5%–9% were typically at larger distances (>1000 pc), and in a few cases had noisier GAIA3 results, but the derived distances were generally consistent with the literature, or no other distance was available. Noteworthy among these are MWC 1021, MWC 1055, and BD+14 3887, with distances of 3650, 6345 and 4496 parsecs, respectively (the latter is listed at 1500 pc by Carmona et al. 2010); although these stars passed all the sanity tests, we consider the GAIA3 distances to be uncertain.

Nearly 90% percent of the updated distances from GAIA3 are within a factor of 2 of the distances that are quoted in the literature. When this is not the case, the GAIA3 distances nearly always place the stars farther away—often more than 1000 pc farther than the literature estimates (e.g., HD 95881, BD+57 2615, BD-13 5061, HD 240010, LkHa 147, LkHa 201, MWC 953, and LkHa 350). There are two interesting exceptions, however: the GAIA3 data confirm the closer distance of 810 pc for RR TAU, consistent with Manoj et al. (2006), but not Montesinos et al. (2009); and the GAIA3 parallax tentatively places HBC 694 at around 430 pc (but with a 12% relative parallax error), as opposed to 1200 pc, assumed according to its reflection nebula (Parsamian 22) and surrounding clouds (Calvet & Cohen 1978). For the latter case, we find both sources to be insufficiently reliable, and await GAIA Data Release 4 for this interesting multiple system.

For the stars without reliable GAIA3 distances, we have carefully gathered the distances from the literature, citing original sources in Table 1 whenever possible, and accompanying error data if available. Several distances are from Testi et al. (1998), which are primarily based on proximity to star-forming regions. All but two of the stars in our sample have some estimated distance listed in Table 1.

The GAIA survey also provides proper-motion data, which are used in this paper in Section 6. We used the same method described above to validate the GAIA3 proper-motion values, and in most cases the results align. That is, we typically use the GAIA3 proper-motion data when the GAIA3 parallax is used, as the uncertainties in proper motion were also less than 10%; and where the parallax is not used, the proper-motion data are also absent or unusable. The two exceptions are MWC
<figure><img src="image_4.png" /><figcaption>**Figure 1.** Distribution of the sample by spectral type and distance. The second bar, labeled “Be,” shows B-type stars of uncertain spectral type, while the last bar is for a continuum star. Further details are given in Section 2.</figcaption></figure>

349 and LkHa 224. MWC 349 has a parallax error of 12%, but a proper-motion error of just 5.2%, which is significantly lower than the previously published data. LkHa 224 has a parallax error of 10.7%, but the proper-motion error is 5.4% and no other proper-motion data are available.

## 2.2. Spectral Types

HAEBE stars are known to be variable, and their spectral types, or effective temperatures, must be compiled with care. For more than half the sample, we have taken effective temperatures from recent sources that provide those values directly (Levenhagen & Leister 2006; Alecian et al. 2013; Fairlamb et al. 2015; Wichittanakom et al. 2020). The typical errors quoted in these sources are of order 10% or less. We have translated these temperatures to spectral type, for the convenience of using spectral type, following Kenyon & Hartmann (1995). This accounts for 81 of the stars in our sample.

Where effective temperatures are not directly available, we have taken spectral types from the literature. Many sources, including Thé, provide HAEBE spectral types without reference, or citing SIMBAD, which in many cases also lacks references. Where possible, we have avoided these sources, in favor of works that derive spectral type directly, such as Hernández et al. (2004), Carmona et al. (2010), Mora et al. (2001), and Vieira et al. (2003). Of the remaining, 19 spectral types are from Thé, and 11 have been traced to a variety of mostly older sources. For consistency, we have used Kenyon & Hartmann (1995) to translate the spectral types to their corresponding effective temperatures (which may differ slightly from the effective temperatures given in those sources). These derived effective temperatures are necessarily a bit coarser than those that are modeled directly. In Table 1, the effective temperatures derived from spectral types are signaled by an asterisk (*).

Only eight stars have no effective temperature listed in the table—seven Be stars and one continuum star. For these stars, the spectral type is too uncertain to derive a useful effective temperature. For all other stars, an effective temperature is given; however, less certain spectral types (as identified either by the source, due to discrepancies between sources, or by the

age of the original source) show a “:” in the spectral type given in Table 1.

The distribution of our sample as a function of spectral type and distance is shown in Figure 1. This figure and Table 1 present all the stars observed. However, any large compilation of HAEBE stars has a risk of including post-main-sequence stars (see the discussion by Sartori et al. 2010) and other interlopers, and the table shows that ours is no exception. We note two late O stars, three G stars, and at least three that are identified by their luminosity class as likely evolved stars, in addition to the eight stars with no assigned effective temperatures. All of these stars are included in the results through Section 4, but are excluded from the HAEBE analysis in Section 5.

## 3. Observations and Data Reductions

In this paper, we present the results of two independent imaging surveys that were carried out approximately 10 yr apart. The two surveys used different telescopes and instruments, and we refer to the two surveys as the “1995 survey” (Bouvier & Corporon 2001) and the “2005 survey” (Thomas et al. 2007). Both surveys used the AO technique to enhance resolution and sensitivity. The 2005 survey improves on the 1995 survey in terms of the resolution and the faintness limit, because telescopes with larger diameters were used as well as more modern AO techniques. As a result, of the 45 stars in common between the two surveys, 11 have more detections in the 2005 survey.

Table 2 provides the observation details for each survey, with the following information. Columns (1) and (2): the name and diameter of the telescope used. Column (3): the instrument used. Column (4): the plate scale. Columns (5) and (6): two FOVs. Column (7): the observation year(s). The 1995 survey observed 62 targets between the two telescopes, while the 2005 survey observed 126 targets, 118 of those with NIRI. The high-sensitivity FOV is the common area of individual dithered exposures (usually around five exposures) that make up a final image. At Gemini North, we changed the observed FOV from 2006 to 2007, to increase the number of detections of binaries with larger separation.
### 3.1. 1995 Survey

The 1995 survey was conducted from 1993 to 1996 at the 3.6 m telescope on La Silla, Chile, and at the CFHT on Maunakea, USA.

**Observations.** Observations at visual and NIR wavelengths were obtained for the northern part of the sample with CFHT's AO system PUEO (Rigaut et al. 1998), equipped with the NIR camera MONICA (Nadeau et al. 1994). For the southern targets, ESO's AO system ADONIS (Beuzit et al. 1997) was used, with the NIR camera SHARP (Hofmann et al. 1995). Both systems deliver nearly diffraction-limited images at *K*, with an FWHM of ≈0.1" and a pixel sampling of 0.0344 at CFHT and 0.051 at ESO. All targets were first observed with either the *K* or *H* filter, depending on their magnitude, in order to optimize the adaptive correction. Whenever a companion was detected in real time, additional images were obtained in complementary filters to obtain *JHK* measurements. Some of the systems that were first detected in the NIR were later reobserved at visual wavelengths, using PUEO, equipped with a CCD detector. However, this paper focuses on discovery only, and therefore does not include the follow-up *J* and *H* data.

**Data Reduction.** Each target was successively observed in at least three different positions on the IR camera, in order to optimize the sky subtraction. The exposure times typically ranged between 60 and 180 s in each filter. To produce the final images, individual exposures were first dark- and flat-corrected, then registered to subpixel accuracy, and eventually coadded. The area common to the individual exposures, over which the full dynamic range is achieved, is about 5" in radius around the primary for the PUEO observations (1996 May, 1996 June, and 1996 September) and 3" for the ADONIS observations (1993 December). Our ability to detect faint companions, down to 6.5 mag fainter than the primary, is restricted to within this area. We therefore adopt the lower value of 3" as defining the radius over which our survey reaches its maximum sensitivity, although the actual FOV of the final images is 16" on the side.

The detection limit curve for PUEO can be found in Figure 3 of Bouvier et al. (1997). The one for ADONIS can be found in Figure 4 of Le Mignant et al. (1999).

### 3.2. 2005 Survey

**Observations.** The 2005 Survey used high-resolution AO *K*-band imaging with Altair-NIRI, at Gemini North (programs GN-2005B-Q-81 and GN-2007A-Q-107), and NAOS CONICA (NACO), on the Very Large Telescope (VLT) in Chile (program 076.C-0708(A)).

The data from ALTAIR were taken in queue mode, in scientific ranking band 3, which usually means nonideal conditions for optimal AO performance. However, because of the quick exposures needed, most of our targets were observed. The observations span multiple semesters, from 2005 September until 2006 March, and from 2007 April until 2007 September. Depending on the brightness of the source and the observing conditions impacting the seeing, and thus the AO performance, the stars were observed either with the broadband *K*-short filter centered at 2.12 µm or with a narrowband *B*γ filter, to avoid saturation. We used NIRI (Hodapp et al. 2003) with the f/32 configuration, which has a plate scale of 21.77 mas per pixel and an FOV of 11" or 17", depending on the size of the full array used. For some very bright targets, a smaller FOV was chosen, in order to enable shorter exposure

times, to avoid saturation, reducing the discovery area in some cases. We estimated our average resolution for this set of data to be about 5.5 mas, based on centroiding errors of a quarter of a pixel. This is in line with other AO surveys around that time.

In the southern hemisphere, NACO at the VLT offers similar capabilities to ALTAIR on Gemini North. Observations of eight targets were conducted with this facility during 2006 February and March, in similar conditions as for Altair. The filter choice between the narrowband NB_2.17 and the regular *Ks* depended on the conditions and the brightness of the star. The FOV was 14", with a pixel size of 13.30 mas (Lenzen et al. 2003; Rousset et al. 2003). In addition, NACO allowed us to use neutral density filters to avoid saturation with brighter stars ($R=3$). In addition, for these brighter stars, a different dichroic was used, sending 90% of the light to a visible wave-front sensor and 10% of the light to the camera.

The primary objective of these observations was the discovery of companions, with a small investment in telescope time. Therefore, only *K*-band images of the targets were taken. Moreover, we did not observe point-spread function (PSF) references or known companions for plate-scale reestimation. For the PSF estimation, the sample is large enough to use stars without close secondary detections. To optimize the sky subtraction, each target was successively observed in at least four different jittered positions on the IR camera. Each image is the accumulation of 100 images of less than 2 s each. We decreased the number of coadds when the exposure time was long, to optimize the time on the telescope. The resulting exposure times typically ranged between 60 and 180 s. The total exposure times were set by the primary star magnitude, so that the detection sensitivities are roughly constant in $\Delta K$.

**Data Reduction.** The data were reduced in a standard way for dark subtraction, flat-fielding, and sky subtraction, using the IRAF Gemini package NIRI for the Gemini data and Eclipse for the VLT data. In the case of relatively wide companions, the astrometry and relative photometry were obtained by PSF fitting of a reference star, using an IDL version of the DAOPHOT PSF fitting procedure. For closer companions, we used the method described in Tokovinin et al. (2006) for PSF reconstruction and fitting. HAEBE stars are young, and therefore likely have circumstellar disks, which in most cases are unresolved. Thus, the routine for detecting the companions used a threshold higher than the expected flux coming from the disk at 2.2 µm.

The error bars were estimated based on the centroiding uncertainty of a quarter of pixel, due to the higher error caused by the band 3 conditions. This led to a 5.5 mas error, which is on the higher end of the uncertainties for AO surveys (e.g., 1 mas—Levenhagen & Leister 2006; 7 and 3 mas—Smith et al. 2005).

### 3.3. Sensitivity and Detection Limits for the 2005 Survey

Instrument limitations and observing conditions impact a survey's sensitivity and, therefore, the detection limits of the results. To be precise, we define the detection limit as the minimum difference in $\Delta K$ magnitude observable at a given angular distance from the primary, which incorporates the dependence on the telescope and instrument.

As expected, this detection limit varies significantly between the 1995 survey and the 2005 survey, given the significant differences in the telescope diameters and the instruments used. Within the 2005 survey, the detection limits between NACO
<figure><img src="image_5.png" /><figcaption>**Figure 2.** The detection limit for Altair—the dashed line is the lower limit and the dotted-dashed line is the upper limit. The star points correspond to all the discovered candidates, during all the surveys (including the NIRI, NACO, ADONIS, and PUEO data). The detection limit was calculated from the NIRI data, assuming that the VLT was similar. The two lines correspond to the lowest and highest detection limits. This varies significantly, due to the conditions during the different observing nights. All discoveries fall under the lowest detection limit (the dashed line).</figcaption></figure>

and NIRI are comparable, with a slight difference mostly due to the generally better observing conditions for the VLT/NACO observations. To determine the detection limit in the 2005 survey, we first calculate the intensity radial variance $\sigma_{\text{var}}$ of the images centered on the sample stars for cases of no detections. The detection limit is then set such that the minimum detectable intensity increase at a specific angular separation, due to the presence of a companion, is greater than $5\sigma_{\text{var}}$. In Figure 2, we show both the sensitivity (lines) and the detections (stars) up to the 10" radius FOV. Because the observing conditions vary from night to night, we calculate a detection limit for each night of the observations. The two lines in Figure 2 show the envelope of these variations (for clarity, not all of the curves are plotted on the graph); the dashed line shows the maximum sensitivity that we reached (during good seeing nights, for instance), while the dotted-dashed line shows the minimum sensitivity that we reached. Figure 2 only uses data from the NIRI observing runs (2005 September–2006 March as well as 2007 March–2007 August); the stars on the plot correspond to the $\Delta K$ magnitude as a function of the angular separation of all the companion detections (from NIRI, NACO, ADONIS, and PUEO). The model will only vary slightly for NACO, but will be worse for ADONIS and PUEO. As expected, all the discoveries fall under the dashed curve, validating our detection limit.

Thanks to the 8 m class telescopes and the use of AO systems, these observations go significantly deeper and closer to the sample stars than previous surveys. On average, for separations greater than 2", we detect stars that are up to 9 mag fainter, and companions that are 2 mag fainter are detected as close as 0"/1 from the sample star. This suggests that the limited range of 3–5 mag fainter, found by Leinert et al. (1997) and Testi et al. (1997), was biased by instrumentation.

Note that in Figure 2, we show the sensitivity and the detections up to the 10" radius FOV. Indeed, we considered all candidates, meaning the candidates discovered within the high-

sensitivity FOV described, as well as within the full FOV, as given in Table 2. The signal-to-noise ratio for the detections outside the high-sensitivity FOV was lower, because fewer dithered images were taken into account in the reconstruction of the final image.

### 3.4. Detections

A detection is defined as any object near the main target that meets the criteria for shape and symmetry and any other criteria included in DAOphot (Stetson 1987). The parameter space also includes the available FOV for each observation presented in Table 2. Of the 143 targets observed, we report 250 detections around 88 stars. Near the other 55 stars in our sample, we did not detect anything.

Of the sample stars with potential companions (detections), one object was detected near 42 sample stars, two objects were detected near 19 sample stars, and three or more objects were detected near 27 sample stars. The maximum number of objects detected, near the B1 star AS310, was 12.

The numbers of detections around each of the targets are given in Table 1, and more information on the actual detections is given later, in Tables 3 and 9 (in the Appendix). Figure 3 provides examples of these detections, including the newly discovered apparent tertiary systems HD 37411 and HBC 334.

## 4. Determining Physical Companions

In this section, we discuss different methods of determining whether a detection is likely to be a physical companion of the primary star or whether it is more likely to be a background star. Several previous multiplicity studies of young stars have based companionship on linear separations and other observational parameters, such as magnitude difference and colors. Other studies have based companionship on the statistical probability of detections not being background stars. This is the method that we have adopted to identify the likely physical
<table><caption>**Table 3**
Statistically Likely Companions</caption><thead><tr><th>Companion</th><th>Ang. Sep. (arcsec)</th><th>PA (deg)</th><th>Linear Sep. (au)</th><th>K Sample Star</th><th>ΔK</th><th>P</th><th>Likelihood</th><th>Date Observed</th></tr></thead><tbody><tr><td>LkHA 198 B</td><td>5.78</td><td>4.40</td><td>3468.0</td><td>6.29</td><td>5.50</td><td>8.92E-03</td><td>Very likely</td><td>13/09/05</td></tr><tr><td>VX Cas B</td><td>5.34</td><td>165.30</td><td>2880.7</td><td>8.21</td><td>4.80</td><td>2.54E-02</td><td>Likely</td><td>13/10/05</td></tr><tr><td>LkHA 201 B</td><td>2.34</td><td>325.80</td><td>6255.0</td><td>9.85</td><td>6.20</td><td>4.29E-02</td><td>Likely</td><td>13/10/05</td></tr><tr><td>HBC 334 B</td><td>0.44</td><td>347.00</td><td>704.0</td><td>11.42</td><td>4.00</td><td>6.10E-04</td><td>Very likely</td><td>16/11/05</td></tr><tr><td>HBC 334 C *</td><td>3.9</td><td>305.60</td><td>6240.0</td><td>11.42</td><td>1.90</td><td>9.02E-03</td><td>Very likely</td><td>16/11/05</td></tr><tr><td>XY Per B</td><td>1.33</td><td>256.70</td><td>565.1</td><td>6.09</td><td>0.10</td><td>2.18E-06</td><td>Very likely</td><td>17/10/05</td></tr><tr><td>V892 Tau B</td><td>3.91</td><td>23.00</td><td>525.9</td><td>5.79</td><td>7.60</td><td>3.16E-03</td><td>Very likely</td><td>15/11/05</td></tr><tr><td>CO Ori B</td><td>2.04</td><td>276.00</td><td>814.4</td><td>6.51</td><td>3.04</td><td>5.78E-05</td><td>Very likely</td><td>01/12/93</td></tr><tr><td>HD 36112 B *</td><td>2.28</td><td>311.30</td><td>355.4</td><td>5.80</td><td>8.30</td><td>4.41E-03</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>HK Ori B</td><td>0.35</td><td>40.80</td><td>161.0</td><td>7.34</td><td>1.80</td><td>1.70E-06</td><td>Very likely</td><td>15/11/05</td></tr><tr><td>HK Ori C</td><td>4.04</td><td>353.10</td><td>1858.4</td><td>7.34</td><td>7.30</td><td>1.45E-02</td><td>Likely</td><td>15/11/05</td></tr><tr><td>HD 245185 B *</td><td>8.38</td><td>294.70</td><td>3479.1</td><td>8.02</td><td>6.70</td><td>6.54E-02</td><td>Likely</td><td>30/10/05</td></tr><tr><td>CQ Tau B</td><td>2.09</td><td>55.50</td><td>312.2</td><td>6.17</td><td>8.50</td><td>6.19E-03</td><td>Very likely</td><td>15/11/05</td></tr><tr><td>BD-06 1253 B</td><td>0.12</td><td>232.80</td><td>45.4</td><td>5.95</td><td>1.40</td><td>3.11E-08</td><td>Very likely</td><td>16/02/06</td></tr><tr><td>HD 37258 B *</td><td>0.99</td><td>30.30</td><td>376.2</td><td>7.69</td><td>2.80</td><td>4.78E-05</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>BF Ori B</td><td>2.04</td><td>46.70</td><td>779.4</td><td>7.90</td><td>4.00</td><td>4.85E-04</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>HD 37357 B #</td><td>0.14</td><td>226.30</td><td>65.2</td><td>7.37</td><td>1.70</td><td>2.18E-07</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>HD 37411 B *</td><td>0.46</td><td>357.50</td><td>161.2</td><td>7.58</td><td>3.30</td><td>7.97E-06</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>HD 37411 C *</td><td>0.58</td><td>348.30</td><td>203.3</td><td>7.58</td><td>3.80</td><td>1.90E-05</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>HD 245906 B *</td><td>0.13</td><td>77.10</td><td>260.0</td><td>7.98</td><td>1.50</td><td>4.69E-07</td><td>Very likely</td><td>30/09/05</td></tr><tr><td>V350 Ori B *</td><td>0.29</td><td>206.80</td><td>115.0</td><td>8.37</td><td>3.20</td><td>4.33E-06</td><td>Very likely</td><td>12/02/06</td></tr><tr><td>LkHA 215 B *</td><td>8.5</td><td>226.60</td><td>6278.2</td><td>7.03</td><td>4.80</td><td>1.67E-02</td><td>Likely</td><td>18/10/05</td></tr><tr><td>HD 259431 B *</td><td>0.15</td><td>55.60</td><td>98.0</td><td>5.73</td><td>3.80</td><td>7.64E-07</td><td>Very likely</td><td>14/10/05</td></tr><tr><td>HD 259431 C *</td><td>3.15</td><td>345.30</td><td>2058.3</td><td>5.73</td><td>5.70</td><td>1.55E-03</td><td>Very likely</td><td>14/10/05</td></tr><tr><td>R Mon B</td><td>0.71</td><td>293.60</td><td>568.0</td><td>6.38</td><td>4.90</td><td>6.95E-05</td><td>Very likely</td><td>16/11/05</td></tr><tr><td>S Mon B</td><td>2.91</td><td>112.80</td><td>2211.6</td><td>5.34</td><td>3.46</td><td>1.54E-04</td><td>Very likely</td><td>01/03/95</td></tr><tr><td>HD 52721 B</td><td>0.65</td><td>194.40</td><td>747.5</td><td>6.04</td><td>1.41</td><td>2.35E-06</td><td>Very likely</td><td>01/12/93</td></tr><tr><td>Z CMa B</td><td>0.1</td><td>118.20</td><td>105.0</td><td>3.77</td><td>2.14</td><td>9.26E-09</td><td>Very likely</td><td>04/04/06</td></tr><tr><td>HD 53367 B</td><td>0.64</td><td>296.90</td><td>736.0</td><td>6.12</td><td>1.77</td><td>4.68E-06</td><td>Very likely</td><td>"12/93, 09/96"</td></tr><tr><td>NX Pup B</td><td>0.13</td><td>69.10</td><td>58.5</td><td>6.08</td><td>1.43</td><td>2.61E-08</td><td>Very likely</td><td>01/12/93</td></tr><tr><td>NX Pup C #</td><td>6.98</td><td>45.30</td><td>3141.0</td><td>6.08</td><td>3.95</td><td>1.49E-03</td><td>Very likely</td><td>01/12/93</td></tr><tr><td>HD 76534 B</td><td>2.09</td><td>303.00</td><td>1849.7</td><td>7.80</td><td>1.46</td><td>1.90E-04</td><td>Very likely</td><td>"12/93, 03/95"</td></tr><tr><td>RCW 34 B</td><td>1.55</td><td>193.00</td><td>3205.1</td><td>8.61</td><td>1.64</td><td>2.03E-04</td><td>Very likely</td><td>01/03/95</td></tr><tr><td>RCW 34 C</td><td>2.21</td><td>292.90</td><td>4569.9</td><td>8.61</td><td>4.45</td><td>4.37E-03</td><td>Very likely</td><td>01/03/95</td></tr><tr><td>RCW 34 D</td><td>2.89</td><td>165.60</td><td>5976.0</td><td>8.61</td><td>3.13</td><td>2.51E-03</td><td>Very likely</td><td>01/03/95</td></tr><tr><td>RCW 34 E</td><td>4.6</td><td>92.10</td><td>9512.0</td><td>8.61</td><td>5.74</td><td>4.85E-02</td><td>Likely</td><td>01/03/95</td></tr><tr><td>RCW 34 F</td><td>5.26</td><td>65.90</td><td>10,876.8</td><td>8.61</td><td>5.23</td><td>4.38E-02</td><td>Likely</td><td>01/03/95</td></tr><tr><td>HD 97300 B</td><td>0.79</td><td>327.10</td><td>149.4</td><td>7.15</td><td>3.08</td><td>3.14E-05</td><td>Very likely</td><td>28/02/06</td></tr><tr><td>HD 101412 B *</td><td>3.06</td><td>226.30</td><td>1261.2</td><td>7.47</td><td>7.00</td><td>8.24E-02</td><td>Likely</td><td>01/03/95</td></tr><tr><td>HD 141569 B</td><td>7.61</td><td>-48.00</td><td>849.4</td><td>6.82</td><td>2.58</td><td>4.65E-04</td><td>Very likely</td><td>04/04/07</td></tr><tr><td>HD 141569 C</td><td>8.96</td><td>-49.00</td><td>1000.0</td><td>6.82</td><td>3.20</td><td>1.11E-03</td><td>Very likely</td><td>04/04/07</td></tr><tr><td>HD 144432 B</td><td>1.45</td><td>4.40</td><td>224.5</td><td>5.89</td><td>2.49</td><td>1.95E-05</td><td>Very likely</td><td>"03/95, 05/96"</td></tr><tr><td>V856 Sco B</td><td>1.46</td><td>109.70</td><td>231.5</td><td>4.39</td><td>3.44</td><td>3.42E-05</td><td>Very likely</td><td>01/03/95</td></tr><tr><td>PDS415 B</td><td>4.494</td><td>-0.21</td><td>700.1</td><td>7.49</td><td>0.38</td><td>1.50E-04</td><td>Very likely</td><td>01/07/07</td></tr><tr><td>HD 150193 B</td><td>1.103</td><td>-134.18</td><td>166.3</td><td>5.48</td><td>2.64</td><td>1.13E-05</td><td>Very likely</td><td>19/07/07</td></tr><tr><td>KK Oph B</td><td>1.61</td><td>245.50</td><td>268.8</td><td>5.80</td><td>1.61</td><td>4.64E-05</td><td>Very likely</td><td>01/03/06</td></tr><tr><td>Hen 3-1475 B</td><td>2.36</td><td>195.20</td><td>UNKNOWN</td><td>6.81</td><td>6.52</td><td>3.72E-02</td><td>Likely</td><td>19/07/07</td></tr><tr><td>PDS469 B</td><td>1.692</td><td>16.63</td><td>1707.9</td><td>10.35</td><td>4.49</td><td>2.72E-02</td><td>Likely</td><td>02/08/07</td></tr><tr><td>HD 168607 B *</td><td>5.978</td><td>-22.72</td><td>10,995.0</td><td>3.51</td><td>1.84</td><td>2.43E-04</td><td>Very likely</td><td>13/07/07</td></tr><tr><td>MWC 922 B *</td><td>4.366</td><td>-172.44</td><td>7422.2</td><td>5.70</td><td>5.06</td><td>5.15E-02</td><td>Likely</td><td>25/07/07</td></tr><tr><td>MWC 922 C *</td><td>4.483</td><td>62.28</td><td>7621.1</td><td>5.70</td><td>2.90</td><td>7.96E-03</td><td>Very likely</td><td>25/07/07</td></tr><tr><td>MWC 922 D *</td><td>5.854</td><td>158.01</td><td>9951.8</td><td>5.70</td><td>2.02</td><td>4.61E-03</td><td>Very likely</td><td>25/07/07</td></tr><tr><td>MWC 922 E *</td><td>7.348</td><td>75.65</td><td>12,491.6</td><td>5.70</td><td>4.50</td><td>8.99E-02</td><td>Likely</td><td>25/07/07</td></tr><tr><td>MWC 297 B</td><td>3.381</td><td>-47.06</td><td>1412.8</td><td>3.04</td><td>7.27</td><td>3.54E-03</td><td>Very likely</td><td>04/04/07</td></tr><tr><td>AS 310 B</td><td>1.298</td><td>79.13</td><td>3194.7</td><td>11.71</td><td>2.94</td><td>3.80E-02</td><td>Likely</td><td>09/04/07</td></tr><tr><td>AS 310 C</td><td>4.377</td><td>122.43</td><td>10,772.8</td><td>11.71</td><td>0.34</td><td>6.86E-02</td><td>Likely</td><td>09/04/07</td></tr><tr><td>PDS530 B</td><td>1.774</td><td>39.86</td><td>1774.0</td><td>9.14</td><td>6.81</td><td>4.30E-02</td><td>Likely</td><td>13/07/07</td></tr><tr><td>PDS530 C</td><td>2.22</td><td>174.91</td><td>2220.0</td><td>9.14</td><td>5.21</td><td>1.97E-02</td><td>Likely</td><td>13/07/07</td></tr><tr><td>PDS530 D</td><td>2.253</td><td>101.36</td><td>2253.0</td><td>9.14</td><td>4.85</td><td>1.49E-02</td><td>Likely</td><td>13/07/07</td></tr><tr><td>MWC 953 B *</td><td>1.885</td><td>55.98</td><td>4053.8</td><td>7.77</td><td>4.03</td><td>1.84E-02</td><td>Likely</td><td>04/04/07</td></tr><tr><td>MWC 953 C *</td><td>2.206</td><td>-82.62</td><td>4744.1</td><td>7.77</td><td>5.11</td><td>5.88E-02</td><td>Likely</td><td>04/04/07</td></tr></tbody></table>
<table><caption>**Table 3**
(Continued)</caption><thead><tr><th>Companion</th><th>Ang. Sep. (arcsec)</th><th>PA (deg)</th><th>Linear Sep. (au)</th><th>K Sample Star</th><th>ΔK</th><th>P</th><th>Likelihood</th><th>Date Observed</th></tr></thead><tbody><tr><td>MWC 953 D *</td><td>2.99</td><td>92.36</td><td>6430.1</td><td>7.77</td><td>1.61</td><td>5.98E-03</td><td>Very likely</td><td>04/04/07</td></tr><tr><td>AS 321 B *</td><td>6.18</td><td>-9.96</td><td>1915.8</td><td>9.06</td><td>2.74</td><td>5.42E-02</td><td>Likely</td><td>04/04/07</td></tr><tr><td>HD 179218 B</td><td>2.54</td><td>140.50</td><td>660.6</td><td>6.00</td><td>6.60</td><td>1.53E-02</td><td>Likely</td><td>13/10/05</td></tr><tr><td>HD 179218 C</td><td>6.39</td><td>300.20</td><td>1662.0</td><td>6.00</td><td>5.30</td><td>3.38E-02</td><td>Likely</td><td>13/10/05</td></tr><tr><td>BD+14 3887 B</td><td>1.19</td><td>319.30</td><td>5350.7</td><td>5.02</td><td>7.40</td><td>5.63E-03</td><td>Very likely</td><td>19/09/05</td></tr><tr><td>BD+14 3887 C</td><td>7.28</td><td>313.70</td><td>32,733.8</td><td>5.02</td><td>4.40</td><td>1.79E-02</td><td>Likely</td><td>19/09/05</td></tr><tr><td>V1685 Cyg B #</td><td>0.72</td><td>175.10</td><td>657.2</td><td>5.77</td><td>5.40</td><td>1.85E-04</td><td>Very likely</td><td>19/09/05</td></tr><tr><td>LkHA 224 B</td><td>4.724</td><td>-67.47</td><td>4629.5</td><td>6.35</td><td>7.87</td><td>8.61E-02</td><td>Likely</td><td>08/04/07</td></tr><tr><td>BD+41 3731 B *</td><td>5.87</td><td>-82.76</td><td>5816.5</td><td>9.63</td><td>3.57</td><td>5.62E-02</td><td>Likely</td><td>12/04/07</td></tr><tr><td>HBC 694 B</td><td>1.39</td><td>259.90</td><td>1668.0</td><td>11.73</td><td>0.60</td><td>1.62E-03</td><td>Very likely</td><td>01/07/96</td></tr><tr><td>HBC 694 C</td><td>1.85</td><td>250.50</td><td>2220.0</td><td>11.73</td><td>2.50</td><td>1.30E-02</td><td>Likely</td><td>01/07/96</td></tr><tr><td>MWC 349 B</td><td>2.763</td><td>-73.73</td><td>3868.2</td><td>3.15</td><td>3.69</td><td>1.11E-04</td><td>Very likely</td><td>12/04/07</td></tr><tr><td>AS 442 B</td><td>4.75</td><td>54.50</td><td>3962.6</td><td>6.62</td><td>6.60</td><td>4.92E-02</td><td>Likely</td><td>20/09/05</td></tr><tr><td>LkHA 147 B</td><td>1.63</td><td>340.70</td><td>3833.5</td><td>9.48</td><td>3.00</td><td>2.91E-03</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>LkHA 167 B *</td><td>0.58</td><td>294.80</td><td>665.8</td><td>8.12</td><td>3.20</td><td>1.36E-04</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>LkHA 168 B *</td><td>0.31</td><td>208.90</td><td>259.7</td><td>8.34</td><td>2.60</td><td>2.73E-05</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>LkHA 170 B *</td><td>0.67</td><td>295.00</td><td>511.8</td><td>13.24</td><td>2.70</td><td>5.73E-03</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>HD 200775 B</td><td>2.55</td><td>167.20</td><td>905.1</td><td>4.65</td><td>4.64</td><td>8.23E-05</td><td>Very likely</td><td>01/06/96</td></tr><tr><td>LkHA 324 B #</td><td>2.01</td><td>302.14</td><td>1250.8</td><td>9.57</td><td>7.70</td><td>9.66E-02</td><td>Likely</td><td>20/09/05</td></tr><tr><td>LkHA 324 C</td><td>5.67</td><td>325.80</td><td>3528.3</td><td>9.57</td><td>3.70</td><td>5.51E-02</td><td>Likely</td><td>20/09/05</td></tr><tr><td>HD 203024 B</td><td>0.25</td><td>153.10</td><td>105.0</td><td>8.12</td><td>0.07</td><td>4.63E-07</td><td>Very likely</td><td>01/05/07</td></tr><tr><td>HD 235495 B *</td><td>2.08</td><td>297.02</td><td>1072.4</td><td>6.97</td><td>4.60</td><td>2.29E-03</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>HD 235495 C *</td><td>4.15</td><td>27.30</td><td>2139.6</td><td>6.97</td><td>6.00</td><td>2.76E-02</td><td>Likely</td><td>20/09/05</td></tr><tr><td>V645 Cyg B *</td><td>3.226</td><td>151.58</td><td>11,291.0</td><td>6.85</td><td>8.33</td><td>7.32E-02</td><td>Likely</td><td>01/05/07</td></tr><tr><td>LkHA 234 B</td><td>1.895</td><td>97.32</td><td>1661.8</td><td>7.08</td><td>5.57</td><td>1.17E-03</td><td>Very likely</td><td>01/05/07</td></tr><tr><td>LkHA 234 C</td><td>8.377</td><td>11.11</td><td>7346.3</td><td>7.08</td><td>6.52</td><td>4.60E-02</td><td>Likely</td><td>01/05/07</td></tr><tr><td>BD+46 3471 B</td><td>1.31</td><td>309.60</td><td>1007.6</td><td>7.22</td><td>4.60</td><td>5.67E-04</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>BD+46 3471 C</td><td>4.69</td><td>40.50</td><td>3607.4</td><td>7.22</td><td>4.40</td><td>6.14E-03</td><td>Very likely</td><td>20/09/05</td></tr><tr><td>BD+46 3471 D</td><td>5.8</td><td>206.20</td><td>4461.2</td><td>7.22</td><td>5.30</td><td>1.91E-02</td><td>Likely</td><td>20/09/05</td></tr><tr><td>BD+46 3471 E</td><td>6.1</td><td>200.70</td><td>4691.9</td><td>7.22</td><td>5.00</td><td>1.68E-02</td><td>Likely</td><td>20/09/05</td></tr><tr><td>BH Cep B</td><td>2.121</td><td>103.66</td><td>694.8</td><td>8.31</td><td>7.46</td><td>1.30E-02</td><td>Likely</td><td>01/05/07</td></tr><tr><td>BH Cep C</td><td>3.25</td><td>-92.73</td><td>1064.7</td><td>8.31</td><td>5.99</td><td>9.06E-03</td><td>Very likely</td><td>01/05/07</td></tr><tr><td>SV Cep B *</td><td>1.09</td><td>311.60</td><td>372.6</td><td>7.74</td><td>5.50</td><td>3.55E-04</td><td>Very likely</td><td>"07/96, 09/96"</td></tr><tr><td>LkHA 350 B *</td><td>2.84</td><td>229.90</td><td>8255.8</td><td>8.32</td><td>7.90</td><td>7.21E-02</td><td>Likely</td><td>13/10/05</td></tr><tr><td>LkHA 350 C *</td><td>10.38</td><td>49.30</td><td>30,174.4</td><td>8.32</td><td>3.60</td><td>4.46E-02</td><td>Likely</td><td>13/10/05</td></tr><tr><td>HD 216629 B *</td><td>7.41</td><td>197.40</td><td>6010.7</td><td>7.10</td><td>6.50</td><td>8.70E-02</td><td>Likely</td><td>25/09/05</td></tr><tr><td>HD 216629 C</td><td>7.8</td><td>329.20</td><td>6327.1</td><td>7.10</td><td>0.07</td><td>6.76E-04</td><td>Very likely</td><td>25/09/05</td></tr><tr><td>MWC 1080 B</td><td>0.76</td><td>269.60</td><td>1132.1</td><td>4.83</td><td>2.80</td><td>7.84E-06</td><td>Very likely</td><td>13/09/05</td></tr><tr><td>MWC 1080 C *</td><td>2.54</td><td>147.50</td><td>3783.7</td><td>4.83</td><td>8.60</td><td>9.31E-03</td><td>Very likely</td><td>13/09/05</td></tr><tr><td>MWC 1080 D *</td><td>3.92</td><td>-138.70</td><td>5839.4</td><td>4.83</td><td>8.30</td><td>1.74E-02</td><td>Likely</td><td>13/09/05</td></tr><tr><td>MWC 1080 E *</td><td>4.93</td><td>-161.30</td><td>7344.0</td><td>4.83</td><td>7.70</td><td>1.69E-02</td><td>Likely</td><td>13/09/05</td></tr><tr><td>MWC 1080 F</td><td>5.17</td><td>89.30</td><td>7701.5</td><td>4.83</td><td>5.00</td><td>1.99E-03</td><td>Very likely</td><td>13/09/05</td></tr><tr><td>MWC 1080 G *</td><td>6.72</td><td>76.20</td><td>10,010.4</td><td>4.83</td><td>8.60</td><td>6.34E-02</td><td>Likely</td><td>13/09/05</td></tr><tr><td>MWC 1080 H *</td><td>6.99</td><td>79.50</td><td>10,412.6</td><td>4.83</td><td>6.40</td><td>1.20E-02</td><td>Likely</td><td>13/09/05</td></tr><tr><td>LkHA 259 B *</td><td>1.43</td><td>149.67</td><td>1034.7</td><td>9.27</td><td>4.23</td><td>2.02E-03</td><td>Very likely</td><td>11/06/07</td></tr></tbody></table>

Note. New detections are marked with an "*".

(This table is available in machine-readable form.)

companions among the 250 detections in our study. We discuss this method in Section 4.2, and we present the sample of the companions that we have found in our survey in Section 4.3. Where possible, we have also investigated proper-motion companions, the only method that is able to identify physically bound companions with near certainty; this is discussed in Section 6.

## 4.1. Circumstantial Evidence for Companionship

Over the last 25 yr, several studies on binary and multiplicity frequency among young stars have been published. An

overview of the upper limits that are used for parameters such as linear separation, magnitude difference, and others is given in Connelley et al. (2008).

The most widely used parameter for identifying likely companions is linear separation. For instance, Duchene et al. (2004) adopt an upper limit for the linear separation of 1400 au for a detection to be a companion as opposed to a background star. 1400 au was chosen based on a study by Duquennoy & Mayor (1991), who found that less than 10% of solar field stars have separations wider than 1400 au. In addition, 1400 au is significantly smaller than the typical core sizes in the Taurus
<figure><img src="image_6.png" /><figcaption>**Figure 3.** Examples of detections: HBC 334, HD 37411, HK Ori, and XY Per. HBC 334 and HD 37411 are apparent triple systems. The orientation in each image is north to the top, east to the left.</figcaption></figure>

and Ophiuchus clouds, the regions in the study of Duchene et al. (2004), and thus is a reasonable upper limit in this particular study. Another study discussed by Connelley et al. (2008), the binarity study of pre-main-sequence stars by Reipurth & Zinnecker (1993), uses a cutoff for detections of 12". This corresponds to an upper limit for the linear separation of about 1800 au for the regions observed. However, Reipurth & Zinnecker (1993) argue that the typical star-star distance in high-density regions is about 10,000 au, and even larger in low-density regions, about 20,000 au. And more recently, Joncour et al. (2017) find “ultra-wide pairs” in Taurus, with separations ranging from 1000 to 60,000 au.

Based on the findings of Duquennoy & Mayor (1991) that most binaries with a solar-type primary have a mass ratio of 10:1, and taking into account the understanding that the primary will exhibit NIR excess, Connelley et al. (2008) adopt a limit to the brightness difference of $\Delta L' = 4$. These authors also adopt an upper limit for the linear separation of 5000 au, which, they argue, will keep the background contamination below 5%, in regions with a low star count. In dense regions, they determine the upper limit for the linear separation to be such that the probability of contamination by background stars is less than 5%.

However, in their discussion on the choice of the upper limit for the linear separation, Connelley et al. (2008) note that several wide binaries are known, the earliest recognized one being β Capricorni (Michell 1767), with a separation of 9400 au, and η Lyrae, with a separation of 13,000 au (Burnham 1978). In fact, in a more comprehensive study on the upper limit for the linear separation in young binaries, Kraus & Hillenbrand (2009) find that, in general, there is no evidence for an upper limit for linear separation.

For specific star-forming regions, imposing an upper limit on the linear separation might be valid, as in the examples of the studies described above. However, in our study of the multiplicity of HAEBE stars, which is not limited to a specific star-forming region, but rather aims to include all known HAEBE stars, a statistical approach is more appropriate.

## 4.2. A Statistical Approach to Determining Companionship

The statistical method (e.g., Kohler & Leinert 1998; Brandner et al. 2000; Correia et al. 2006) is based on the assumption that the probability of finding a background star, i.e., a source unrelated to the sample star, can be calculated using a Poisson distribution. In this case, the probability $P$ of finding $k=0$ occurrences of an event $\lambda$ is defined by

$$P(k = 0, \lambda) = \frac{e^{-\lambda}\lambda^0}{0!} = e^{-\lambda}. \qquad (1)$$

The probability of finding at least one occurrence of an event $\lambda$ is

$$P(k > 0, \lambda) = 1 - P(k = 0, \lambda) = 1 - e^{-\lambda}. \qquad (2)$$

For our purposes, the event $\lambda$ is the presence of a background star within a radius of $\theta$, given by $\lambda = \pi\Sigma\theta^2$, where $\Sigma$ is the surface density of the stars in that region.

Therefore, the probability of finding at least one background star within this radius is

$$P(k > 0, \pi\Sigma\theta^2) = 1 - e^{-\pi\Sigma\theta^2}. \qquad (3)$$

To account for the uneven distribution of stars in the galaxy, we use the Two Micron All Sky Survey (2MASS) Point Source Catalog (PSC) to calculate the stellar density in the area of each
<figure><img src="image_7.png" /><figcaption>**Figure 4.** Brightness distribution of the stars within 30' of HD 101412. The potential companion that was detected near HD 101412 has a magnitude $K = 14.466$. To determine the surface density for stars with $K \ge 14.466$, the distribution was extrapolated out to $K = 18$, using a polynomial fit.</figcaption></figure>

sample star. We determine the number of stars found in the 2MASS PSC within 30' of the sample star with a magnitude in the $K$ band equal to or smaller than the magnitude $K_{\text{companion}}$ of the detection: $N_{K \le K_{\text{companion}}}$. For areas in which the 2MASS PSC is not complete<fnref n="9" /> up to the $K$ magnitude of the detection, we have extrapolated the number of 2MASS detections within the 30' radius, to estimate the actual surface density in that area. Figure 4 presents an example of such an extrapolation. Extrapolation was needed for 57% of the detections; about 90% of these were not found to be likely companions.

Setting $\theta$ equal to the angular separation between the candidate companion and the sample star, we use Equation (3) to calculate the probability of finding at least one unrelated source within the radius at which the candidate companion is located, with $K \le K_{\text{companion}}$. Tables 3 and 9 (in the Appendix) list these probabilities for each detection in our survey.

### 4.3. Likely and Very Likely Companions

A probability of being unrelated that is less than 10% means that the probability of being related is 90% or more. We consider these to be likely physical companions. A total of 106 detections meet this criterion, and these are listed in Table 3. The remaining 144 detections have an unrelated probability $P > 10\%$. These are considered background objects and are listed in Table 9 in the Appendix. The tables list all the detections found near each star, along with some of their properties, with columns (2) to (9) giving the angular separation, position angle (PA), the linear separation, the magnitude of the sample star, the magnitude difference between the detection and the sample star $\Delta K$, the probability of being unrelated, the likelihood of being related (see Section 4.2), and, finally the date observed, respectively.

Within the 10% cutoff, we further differentiate between very likely and likely companions. We consider detections with a probability of being unrelated that is less than or equal to 1%, $P \le 1\%$, as very likely to be a physical companion of the primary, while those with a probability of being unrelated of

$1\% < P \le 10\%$ are considered as likely to be physical companions. There are 64 very likely companions and 42 likely companions. Throughout this paper, we maintain the distinction between the two groups, and refer to them collectively as “(very) likely” companions.

Regarding the cutoff choices of 1% and 10%, the literature generally agrees that a probability of being unrelated of <1% makes a companion very likely to be related (see Duchene et al. 2004; Correia et al. 2006). However, there is less consistency in the choice of a lower limit. Our choice of a <10% chance of being unrelated may be somewhat less conservative compared to other studies (Duchene et al. 2004), but it is consistent with our goal of detecting all likely physical companions, regardless of separation and contrast. Of the likely companions, 27 have unrelated probabilities of less than 5%, 10 have probabilities between 5% and 8%, and the remaining five likely detections have probabilities between 8% and 10%.

In cases of double or multiple companions, we have labeled the companions “A,” “B,” “C,” etc., with a hierarchy based on the angular separation from the primary. We choose separation rather than brightness, as separation is a wavelength-independent parameter and the NIR colors of young stars are known to be variable. While orbital motion may also change the angular separation, it is likely to change slowly in all but the closest binaries.

Figure 5 shows the results of all of the detections, plotted by the angular separation $\theta$ and $\Delta K$. The figure demonstrates that, for the sample at hand, with primaries in a broad range of environments, there are no clear cutoffs in $\Delta K$ or in angular separation. Although the majority of the companions are within 4" and have $\Delta K$ of less than 5, there are several very likely companions that are fainter and at larger angular separations.

In Table 4, we consider the probability results by comparing the number of sample stars with zero or more detections to the number with zero or more (very) likely companions. What is remarkable is that although more than half of the detections are considered background stars (144 of 250 detections), the number of primaries with companions (70) is not that much smaller than the number with one or more detections (88). However, the number of primaries with more than two companions is significantly smaller than the number of primaries with three or more detections. This implies that the majority of the sources that are labeled as background objects are found in high surface-density areas, suggesting that the probability approach is effective in weeding out background objects in crowded fields.

Figure 6 shows the distribution of the targets in the survey in galactic coordinates. Not surprisingly, the majority of the target sample is located along the galactic plane—in areas of high stellar density, in many cases. The symbols in the top panel differentiate those sample stars without companions from those with one, two, and more companions. There is no clear correlation between the location, with respect to the galactic plane, and the number of companions found, although the higher-order multiples, i.e., those sample stars with more than two companions, are mostly located closer to or in the galactic plane.

The bottom half of the figure distinguishes between those sample stars for which the number of detections is greater than the number of companions and those for which all detections are found to be companions. As expected, the former are primarily located in the galactic plane, where, due to the high

<footnote n="9">⁹ As discussed in the Level 1 Science Specifications of 2MASS, the 2MASS PSC is in general complete to $K < 15.1$. For high-density regions, such as the Galactic plane, the completeness limit is only $K = 13.1$.</footnote>
<figure><img src="image_8.png" /><figcaption>**Figure 5.** Angular separation vs. $\Delta K$ for all detections. The squares are the “very likely” physical companions; the triangles are the “likely” companions; and the small circles are “unlikely” to be companions. See the text for the definitions.</figcaption></figure>

<table><caption>**Table 4**
Number of Primaries with Detections vs. Number of Primaries with Very Likely and Likely Companions</caption><thead><tr><th></th><th>N Detections</th><th>N Very Likely/Likely Companions</th></tr></thead><tbody><tr><td>None</td><td>55</td><td>73</td></tr><tr><td>One or more</td><td>88</td><td>70</td></tr><tr><td>One</td><td>42</td><td>48</td></tr><tr><td>Two</td><td>19</td><td>16</td></tr><tr><td>Three or more</td><td>27</td><td>6</td></tr></tbody></table>

surface density, more detections fall into the category of being unrelated. Detections near primaries outside the galactic plane are almost all statistically found to be physical companions.

### 4.4. New Detections

This survey is, to the best of our knowledge, the largest multiplicity study of HAEBE stars to date. Not surprisingly, then, a large number of new multiple systems, as well as additional companions to known binary systems, have been detected.

Using the study of Vioque et al. (2018, and references therein; hereafter, Vioque) as well as our own literature search for multiepoch observations (see Section 6), we looked at the likely and very likely candidates from our statistical study in order to identify new discoveries. Altogether, we have identified 23 systems that have not previously been recognized as multiple, as well as additional companions around six systems that have previously been identified as multiple. Of the 106 companions listed in Table 3, 42 are new discoveries. These are identified with an asterisk in the table.

Examining the 70 multiple systems reported in this paper, 36 are marked “binary” by Vioque, 19 are not, and 15 are not part of the Vioque sample. In addition, 18 stars are listed as

binary by Vioque for which we did not find companions. The details of each of these categories are as follows:

1. There are 36 systems that are identified as multiples both by our survey and by Vioque. We note that the candidates around nine of these systems were in fact first detected by the Thomas et al. (2007) survey, which is referenced as Wheelwright et al. (2010) and Wheelwright et al. (2011) in the Vioque paper. Of the remaining 27 systems, nine have multiepoch and proper-motion data, listed in Table 8.

2. We have found candidates around 19 primaries that Vioque does not identify as binaries. Seven of these systems are apparently new discoveries. All but one of the remaining 12 have multiepoch observations from the literature, listed in Table 8. The remaining one (PDS530; Perrin 2006) does not have proper-motion data.

3. Of the 15 multiple systems that are not included in Vioque, six are apparently new discoveries, while the other nine are identified as multiple systems in other literature. Multiepoch observations (and references) for five of these targets are listed in Table 8. The remaining four are LkHA 198 (Leinert et al. 1997; Perrin 2006), Hen 3-1475 (Perrin 2006), RCW 34 (SIMBAD), and R Mon (Close et al. 1997).

4. Conversely, Vioque reports 18 systems from our sample for which we did not find companions as binaries. However, we find that two of the detections from the survey (LkHa 25 and V374 Cep; referencing Thomas et al. 2007, via Wheelwright et al. 2010) are unlikely to be companions (see Table 9 in the Appendix). The remaining stars are wide binaries beyond our FOV, spectro-astrometric binaries, or unresolved spectroscopic or eclipsing binaries. None of these would be detectable by us.
<figure><img src="image_9.png" /><figcaption>**Figure 6.** Galactic distribution of the target sample. Top: the number of companions for each sample star. Bottom: distinction between the stars for which all detections are (very) likely companions (pluses) and those for which a number of detections have been rejected, i.e., with more detections than (very) likely companions (squares). Note: sample stars with detections but no companions appear as squares in the lower panel, while stars without any detections are not plotted.</figcaption></figure>

<figure><img src="image_10.png" /><figcaption>**Figure 7.** The probability of detecting a companion as a function of separation and magnitude difference.</figcaption></figure>

We mention that six systems are known binaries, for which we have increased the degree of multiplicity. These targets are MWC 1080, HD 216629, LkHA 324, NX Pup, V1685 Cyg, and HD 37357.

We also note that 15 of the new detections are marked as likely companions, with probabilities of being unrelated to the primary greater than 5%. These would benefit from further observations, to confirm their status as physical companions, as most of the primaries have proper-motion data.

## 5. Multiplicity Analysis

Having identified the (very) likely companions, we now investigate the nature of the multiplicity among HAEBE stars. In this section, we consider the statistical multiplicity frequency, the multiplicity, and the companion characteristics as a function of the primary star's effective temperature; finally, we briefly comment on higher-order multiple systems.

<table><caption>**Table 5**
Summary of HAEBE Companions Binned by Effective Temperature</caption><thead><tr><th></th><th>Low</th><th>Medium</th><th>High</th></tr></thead><tbody><tr><td>Effective Temp (K)</td><td>6000-8700</td><td>8800-12,000</td><td>12,500-32,000</td></tr><tr><td>Spectral Type Range</td><td>(F9-A3)</td><td>(A2-B8)</td><td>(B7-B0)</td></tr><tr><td>Sample stars observed</td><td>43</td><td>51</td><td>32</td></tr><tr><td>Primaries w/comp (% of bin)</td><td>20(47%)</td><td>26(51%)</td><td>19(60%)</td></tr><tr><td>Binaries (% of bin)</td><td>15(35%)</td><td>19(37%)</td><td>12(38%)</td></tr><tr><td>Higher-order multiples</td><td>5(12%)</td><td>7(14%)</td><td>7(22%)</td></tr></tbody></table>

### 5.1. Multiplicity Frequency

The multiplicity frequency is often biased by the detection limit and contamination from visual (nonphysical) binaries. These biases cause the multiplicity frequency to be underestimated and overestimated, respectively. The probability analysis described in the previous section reduces the biases due to nonphysical contamination. Including both the likely and very likely companions from Section 4.2, the fraction of primary stars having at least one companion is 49%. This frequency decreases to 34% if only the very likely companions are included.

It is now also possible to compensate for incompleteness by using the detection limit information for the binarity frequency. We define the detection limit for a given target as the lowest magnitude of a companion that is detectable above a $5\sigma$ noise variance, as a function of separation. While we cannot create data for the space of an $\{\Delta K, \text{separation}\}$ graph that does not have any detections, we can compensate for those parts where we do have occasional detections. To do so, we use the method described in Tokovinin et al. (2006). First, the detection limits
<figure><img src="image_11.png" /><figcaption>**Figure 8.** Multiplicity as a function of spectral type for the 126 HAEBE primary stars.</figcaption></figure>

<figure><img src="image_12.png" /><figcaption>**Figure 9.** Multiplicity plotted by effective temperature and distance for the HAEBE Sample.</figcaption></figure>

for each of the individual stars without detections in the region of interest are calculated up to the noise floor (around $\Delta K = 9$), using 25 NIRI targets from 2007 and 56 from 2006 (i.e., 57% of the sample).

The probability of detection is then calculated from the individual detection limits. We define bins in {$\Delta K$, separation} data space. For this particular case, we choose $\Delta K$ ranging from 0 to 12, and sample it in 40 bins with $\Delta K = 0.3$ per bin. For the separation, we use the pixel size as a bin, therefore we have 21.90 mas per bin (note that the NIRI observations have a K-band diffraction limit of 79 mas). For each bin {$\Delta K$, separation}, we calculate the percentage of primary stars for which we could have detected at least one companion. For each entry bin {$\Delta K$, separation}, this percentage is the probability of a companion detection for one target and a bin, $D_{i,k}$. We repeat this measurement for each {$\Delta K$, separation} couple, to determine the detection probability as a function of separation and magnitude difference, as shown in Figure 7.

Once the detection probability has been defined, the binarity frequency needs to be corrected for incompleteness. This method only allows the adjustment of the probability of stars

with at least one companion. We calculate how many detections are found in each bin {$\Delta K$, separation} defined above. The binarity fraction for each bin is then corrected by the average probability of detection $\sum_i D_{i,k}/N$, where the final frequency of the binaries is the sum of the frequencies found in each bin. The corrected frequency is thus 39%, to find a sample star with at least one companion in only the very likely category, and 56%, counting both the very likely and likely categories. Note that this is still a lower limit, as the detection limit used here is calculated from the NIRI data only, which is comparable to NACO, but better than ADONIS/PUEO.

## 5.2. Companions as a Function of Primary Spectral Type

To investigate the multiplicity in HAEBE stars, we are only interested in sample stars with spectral types B0 to F9, for which we have reliable estimates of the spectral type and distance (see Section 2 and Table 1). We therefore exclude three G stars, and two O stars, as well as eight stars lacking effective temperatures (nearly all hot ~B stars) and two at unknown distances. Two of these excluded stars are Hen 3-
<figure><img src="image_13.png" /></figure>

<figure><img src="image_14.png" /><figcaption>**Figure 10.** Companions as a function of primary effective temperature. Top: $\Delta K$ relative to the primary star. Bottom: linear separation. The symbols distinguish binary, triple, and higher-order multiple systems, while the shading indicates the very likely (black) and the likely (gray) companions. Note: there are two triangles per primary star, and the 17 diamond symbols are associated with four systems at 7200, 10,500, 22,000, and 31,000 K.</figcaption></figure>

1475 and MWC 349, which have been identified as post-main-sequence stars, along with BD+14 3887 and V409 Vul (Rodrigues et al. 2003; Carmona et al. 2010; Gvaramadze & Menten 2012; Miroshnichenko et al. 1999, respectively). Table 1 reveals that several of these excluded stars have detections, and that five have likely companions, including two high-order multiple systems that we revisit in the next section.

This leaves 126 HAEBE primary stars in the following analysis. Based on the probability results, 61 of these stars have

no likely companions, 46 are binary systems, and 19 have multiple companions. More than two companions are rare, found around only four stars, three of them being B-type stars. These results are shown by spectral type in Figure 8 and are summarized in Table 5, where the sample is divided into three similarly populated temperature bins.

Table 5 shows a weak trend toward increasing multiples with temperature, and specifically a higher percentage of higher-order multiples in the hottest bin. The percentages of primaries
$T_{eff} \le 12500K$

<figure><img src="image_15.png" /><figcaption>**Figure 11.** Companion sample by distance and linear separation. Left: the companions found around 45 cool stars (≤12,500 K). Right: the companions found around 16 hot stars (>12,500 K). The dashed lines indicate the detection limits, as discussed in the text.</figcaption></figure>

$T_{eff} > 12500K$

<figure><img src="image_16.png" /></figure>

<figure><img src="image_17.png" /><figcaption>**Figure 12.** Linear separation and $\Delta K$ of all the companions. The symbols are as in Figure 11; the dashed lines indicate the detection limits, as discussed in the text.</figcaption></figure>

<table><caption>**Table 6**
Locations of the High-Order Multiple Systems in the Galactic Plane</caption><thead><tr><th>Target Name</th><th>Detections</th><th>Companions</th><th><i>l</i></th><th><i>b</i></th><th>In/Out Plane</th></tr></thead><tbody><tr><td>RCW 34</td><td>5</td><td>5</td><td>264.28</td><td>1.47</td><td>Out</td></tr><tr><td>MWC 922</td><td>6</td><td>4</td><td>17.93</td><td>0.63</td><td>In plane</td></tr><tr><td>PDS 530</td><td>11</td><td>3</td><td>39.08</td><td>5.88</td><td>Out</td></tr><tr><td>MWC 953</td><td>9</td><td>3</td><td>28.67</td><td>0.05</td><td>In plane</td></tr><tr><td>BD+46 3471</td><td>4</td><td>4</td><td>94.25</td><td>-5.44</td><td>Out</td></tr><tr><td>MWC 1080</td><td>7</td><td>7</td><td>111.72</td><td>0.04</td><td>In plane</td></tr></tbody></table>

with companions in each bin are consistent with the “wide binary fraction” reported by Offner et al. (2022), for both

HAEBE and main-sequence stars of these spectral types (see their Figure 4). However, a correlation between the effective temperature and the likelihood of harboring companions is not apparent in Figure 9, which plots the number of companions found for all the HAEBE sample stars by effective temperature and distance. Figure 9 also shows no apparent correlation between the distance and the number of companions for a given temperature range (an indication that the results do not suffer from a spatial resolution bias), although a dearth of nearby hot stars in the sample is apparent in the figure.

The linear separations and $\Delta K$ magnitudes of the companions as a function of primary temperature are plotted in Figure 10. Higher-order multiples are separated from triple systems, for clarity, as there are 17 companions that are associated with four systems, and likely companions are
<table><caption>**Table 7**
Imaging Surveys for the Multiplicity of HAEBE Stars Included in the Multiepoch Analysis</caption><thead><tr><th>Our Surveys</th><th>Legend</th><th>Epoch</th><th>Ntot (Candidates)</th><th>Pix Scale (mas)</th><th>Res (mas)</th><th>Telescope</th><th>Method</th></tr></thead><tbody><tr><td>1995 Survey</td><td>♦ or •<sup>a</sup></td><td>1984–95</td><td>34</td><td>50</td><td>120</td><td>3.6 m</td><td>AO</td></tr><tr><td>2005 Survey</td><td>•</td><td>2005–07</td><td>53</td><td>22</td><td>50</td><td>8 m Gemini<br>VLT</td><td>AO</td></tr><tr><th>Survey</th><th>Legend</th><th>Epoch</th><th>Ntot</th><th>Pix Scale (mas)</th><th>Res (mas)</th><th>Telescope</th><th>Method</th></tr><tr><td>Perrin (2006)</td><td>▷</td><td>2003–06</td><td>41</td><td>80</td><td>150</td><td>3 m Lick</td><td>AO</td></tr><tr><td>Pirzkal et al. (1997)</td><td>△</td><td>1996</td><td>11</td><td>120</td><td>400</td><td>2.3 m<br>Wyoming</td><td>Imaging</td></tr><tr><td>Leinert et al. (1997)</td><td>▽</td><td>1985–95</td><td>7</td><td>50</td><td>50</td><td>Multiple</td><td>SI</td></tr><tr><td>Ageorges et al. (1997)</td><td>□</td><td>1994</td><td>5</td><td>50</td><td>150</td><td>ESO–NTT</td><td>Speckle Nulling</td></tr><tr><td>Correia et al. (2006)</td><td>x</td><td>2002–04</td><td>3</td><td>13.26/27.01</td><td>77.8</td><td>VLT</td><td>AO</td></tr><tr><td>Ghez et al. (1997)</td><td>*</td><td>1994</td><td>2</td><td>460</td><td>2000</td><td>CTIO</td><td>Imaging</td></tr></tbody></table>

Notes. The error on the PA for Perrin (2006) is ~1°. SI = speckle interferometry. (The symbols of the legend are used in all following graphs).

distinguished from the very likely companions. The top panel shows a wide range in $\Delta K$, from near zero to 9 mag, but with the majority of the likely companions having $\Delta K < 4$; the average and median $\Delta K$ are 3.4 and 3, respectively, for the very likely companions. Very small $\Delta K$ is rare, and we find no apparent correlation with primary effective temperature.

In contrast, the lower panel clearly shows that all but one of the closer companions, between 45 and 500 au, are exclusively around cooler primary stars, $T_{eff} < 10,000$ K. With one exception, all the companions around higher-temperature primaries in our survey have separations of 700 au or more. Altogether, only four companions are found within 100 au (BD-06 1253B, NX PupB, HD 37357B, and HD 259431B). Companions at larger separations are found across all temperatures, and nearly all of the likely companions have large separations (>1000 au), while most (but not all) of the very likely companions are closer, not surprisingly.

Noting the lack of nearby hot stars in our sample, Figure 11 investigates whether the dearth of nearby companions around hot stars could be due to observational bias. The figure divides the sample into low- and high-temperature bins and plots the primary star distance versus companion linear separation. The detection limits of the survey for $\Delta K = 0$ and $\Delta K = 5$ are shown with the dashed lines. A comparison of the two panels shows relatively fewer—and preferentially more distant—hot stars in our sample, as already noted, and therefore fewer total companions in the right panel. Faint companions close to these hot primaries would be harder to detect. However, the dashed lines show that companions with $\Delta K < 5$ would have been easily detected closer than 700 au among the hotter stars, and even within 100 au, in some cases. Only one was found. Among the cooler stars, our detection limits indicate that $\Delta K < 5$ companions within 100 au would have been found for most of the sample. We conclude that companions within ~700 au are more common among cooler Herbig Ae stars compared to Herbig Be stars, and that very close companions, within 100 au, are quite rare for all HAEBE stars (at least with a magnitude difference $\Delta K < 5$).

Finally, Figure 12 plots the linear separations and $\Delta K$ magnitudes of all the companion stars together, along with dashed lines that indicate the detection limits based on sample star distances of 100 and 500 pc. The preponderance of

likely companions toward the upper right of the figure is expected given our algorithm, as discussed, and the detection limits may explain the absence of points in the upper left of the graph. However, the dashed lines show that our observations are quite sensitive, even very close to the primary, and considering that nearly half of the primaries with companions are within 500 pc, the absence of faint companions with separations up to 300 au is still somewhat surprising.

Deriving $K$ magnitudes for the companions from $\Delta K$ is problematic, given the IR excesses of young stars, presumably both of the primaries as well as the companions. The $K$ excesses of HAEBE stars range from 0 to more than 5 mag (Vioque). Using the $K$ magnitude as a proxy for the mass of the companions, or the mass ratio $q$, is similarly problematic. Nevertheless, we can assume that the smaller $\Delta K$ companions are more likely to be companions with similar mass, while the companions with $\Delta K > 5$ are surely low-mass companions, presumably T Tauri stars, and possibly young brown dwarfs (Siess et al. 2000; Baraffe et al. 2002). Therefore, the very likely companions with large $\Delta K$ shown in Figure 12 are interesting cases for further study.

### 5.3. High-order Multiples

Of the 70 likely or very likely multiple systems, six were found to have three or more companions. These are listed in Table 6, with the number of companions and their locations in the galactic plane. In this small sample, half are located in the galactic plane. For BD+46 3471 and MWC 1080, we also have proper-motion and other epoch data, as discussed in the next section. Here, we look briefly at each of these systems individually.

RCW 34, aka VdBH 25a, is an O8/8.5V star similar to HAEBE stars (Vittone et al. 1987; Bik et al. 2010). This star was observed in 1996 with Adonis, which had a brighter detection limit than either NACO or Altair. RCW 34 is located close to the galactic plane, but away from the center; it is in a star-forming region, making it a fairly crowded field. All five detections are found to be likely physical companions; the three very likely ones, however, are all quite far from the primary (linear separations of 3000–11,000 au) and faint (all but one having $\Delta K > 3$).

<footnote><sup>a</sup> If there is no 2005 Survey data.</footnote>
<table><caption>**Table 8**

Multiepoch Observations</caption><thead><tr><th>Detection/Companion</th><th>Sep. (arcsec)</th><th>Sep. Err. (arcsec)</th><th>PA (degrees)</th><th>PA Err. (degrees)</th><th>ΔK</th><th>Date Observed</th><th>Min. Time Needed (yr)</th><th>Survey</th><th>PM Res.</th><th>Statistical Res.</th></tr></thead><tbody><tr><td>HIP 592-1 (***)</td><td>7.28</td><td>0.0055</td><td>352.3</td><td>...</td><td>6.2</td><td>2006.04</td><td>3.16</td><td>2005 Survey</td><td>Yes</td><td>Not likely</td></tr><tr><td>HIP 592-1</td><td>7.33</td><td>0.02</td><td>351.7</td><td>2.0</td><td>...</td><td>2004.68</td><td>3.16</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HIP 592-2</td><td>8.01</td><td>0.0055</td><td>354.0</td><td>...</td><td>3.9</td><td>2006.04</td><td>3.16</td><td>2005 Survey</td><td>Inconclusive</td><td>Not likely</td></tr><tr><td>HIP 592-2</td><td>8.03</td><td>0.02</td><td>353.3</td><td>2.0</td><td>...</td><td>2004.68</td><td>3.16</td><td>Perrin06</td><td></td><td></td></tr><tr><td>VX Cas-1</td><td>5.01</td><td>0.0055</td><td>344.4</td><td>...</td><td>8.2</td><td>2005.78</td><td>2.59</td><td>2005 Survey</td><td>Inconclusive</td><td>Not likely</td></tr><tr><td>VX Cas-1</td><td>5.04</td><td>0.02</td><td>343.9</td><td>2.0</td><td>8.88</td><td>2004.68</td><td>2.59</td><td>Perrin06</td><td></td><td></td></tr><tr><td>VX Cas-B</td><td>5.34</td><td>0.0055</td><td>165.3</td><td>...</td><td>4.8</td><td>2005.78</td><td>2.59</td><td>2005 Survey</td><td>Inconclusive</td><td>Likely</td></tr><tr><td>VX Cas-B</td><td>5.34</td><td>0.02</td><td>164.6</td><td>2.0</td><td>5.51</td><td>2004.68</td><td>2.59</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 201-B</td><td>2.34</td><td>0.0055</td><td>326.0</td><td>...</td><td>6.2</td><td>2005.78</td><td>5.37</td><td>2005 Survey</td><td>Inconclusive</td><td>Likely</td></tr><tr><td>LkHA 201-B</td><td>2.34</td><td>0.02</td><td>326.2</td><td>2.0</td><td>...</td><td>2005.57</td><td>5.37</td><td>Perrin06</td><td></td><td></td></tr><tr><td>XY Per-B (**)</td><td>1.33</td><td>0.0055</td><td>256.7</td><td>...</td><td>0.1</td><td>2006.79</td><td>0.97</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>XY Per-B</td><td>1.29</td><td>0.02</td><td>256.1</td><td>2.0</td><td>0.6</td><td>2002.90</td><td>0.97</td><td>Perrin06</td><td></td><td></td></tr><tr><td>XY Per-B</td><td>1.20</td><td>0.1</td><td>255.0</td><td>1.0</td><td>...</td><td>1996.00</td><td>0.97</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>V892 Tau-B (**)</td><td>3.91</td><td>0.0055</td><td>23.0</td><td>...</td><td>7.6</td><td>2005.87</td><td>0.38</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>V892 Tau-B</td><td>4.07</td><td>0.02</td><td>23.7</td><td>2.0</td><td>3.79</td><td>2005.89</td><td>0.38</td><td>Perrin06</td><td></td><td></td></tr><tr><td>V892 Tau-B</td><td>3.72</td><td>0.1</td><td>19.0</td><td>1.0</td><td>4.2</td><td>1996.00</td><td>0.38</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>V892 Tau-B</td><td>4.10</td><td>0.04</td><td>23.4</td><td>0.5</td><td>4.01</td><td>1993.75</td><td>0.38</td><td>Leinert97</td><td></td><td></td></tr><tr><td>CO Ori-B</td><td>2.04</td><td>0.05</td><td>276.0</td><td>1.0</td><td>3.04</td><td>1993.95</td><td>3.57</td><td>1995 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>CO Ori-B</td><td>1.90</td><td>0.02</td><td>274.9</td><td>2.0</td><td>4.25</td><td>2005.88</td><td>3.57</td><td>Perrin06</td><td></td><td></td></tr><tr><td>CO Ori-B</td><td>2.00</td><td>0.007</td><td>280.0</td><td>2.0</td><td>0</td><td>1991.00</td><td>3.57</td><td>Reipurth91</td><td></td><td></td></tr><tr><td>CO Ori-B</td><td>2.06</td><td>0.005</td><td>274.7</td><td>0.5</td><td>0.07</td><td>2003.50</td><td>3.57</td><td>Correia06</td><td></td><td></td></tr><tr><td>HK Ori-B</td><td>0.35</td><td>0.0055</td><td>40.8</td><td>...</td><td>1.8</td><td>2005.87</td><td>4.47</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>HK Ori-B</td><td>0.34</td><td>0.02</td><td>36.5</td><td>2.0</td><td>...</td><td>2004.92</td><td>4.47</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HK Ori-B</td><td>0.34</td><td>0.05</td><td>47.9</td><td>1.0</td><td>2.19</td><td>1994.00</td><td>4.47</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HK Ori-B</td><td>0.34</td><td>0.2</td><td>41.7</td><td>0.5</td><td>2.3</td><td>1995.77</td><td>4.47</td><td>Leinert97</td><td></td><td></td></tr><tr><td>HK Ori-B</td><td>0.34</td><td>0.007</td><td>44.2</td><td>0.5</td><td>...</td><td>1997.80</td><td>4.47</td><td>Smith05a</td><td></td><td></td></tr><tr><td>HK Ori-B</td><td>0.35</td><td>0.003</td><td>41.8</td><td>0.7</td><td>...</td><td>2003.78</td><td>4.47</td><td>Smith05b</td><td></td><td></td></tr><tr><td>HK Ori-C</td><td>4.04</td><td>0.0055</td><td>353.1</td><td>...</td><td>7.3</td><td>2005.87</td><td>4.47</td><td>2005 Survey</td><td>Yes?</td><td>Likely</td></tr><tr><td>HK Ori-C</td><td>3.89</td><td>0.02</td><td>353.1</td><td>2.0</td><td>...</td><td>2004.92</td><td>4.47</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HK Ori-C</td><td>3.98</td><td>0.05</td><td>354.4</td><td>1.0</td><td>7.36</td><td>1994.00</td><td>4.47</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>CQ Tau-B</td><td>2.09</td><td>0.0055</td><td>55.5</td><td>...</td><td>8.5</td><td>2005.87</td><td>0.41</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>CQ Tau-B</td><td>2.10</td><td>0.02</td><td>56.4</td><td>2.0</td><td>8.19</td><td>2005.89</td><td>0.41</td><td>Perrin06</td><td></td><td></td></tr><tr><td>CQ Tau-B</td><td>2.16</td><td>0.02</td><td>53.1</td><td>0.5</td><td>...</td><td>2012.00</td><td>0.41</td><td>Uyama12</td><td></td><td></td></tr><tr><td>BD-06 1253-B</td><td>0.12</td><td>0.0055</td><td>232.8</td><td>...</td><td>1.4</td><td>2006.13</td><td>4.40</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>BD-06 1253-B</td><td>0.14</td><td>0.05</td><td>205.0</td><td>1.0</td><td>1.36</td><td>1993.95</td><td>4.40</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>BD-06 1253-B</td><td>0.15</td><td>0.002</td><td>204.2</td><td>0.9</td><td>1.14</td><td>1993.75</td><td>4.40</td><td>Leinert97</td><td></td><td></td></tr><tr><td>BD-06 1253-B</td><td>0.12</td><td>0.003</td><td>224.0</td><td>0.7</td><td>...</td><td>2003.78</td><td>4.40</td><td>Smith05b</td><td></td><td></td></tr><tr><td>HD 37258-B</td><td>0.99</td><td>0.0055</td><td>30.3</td><td>...</td><td>2.8</td><td>2006.13</td><td>5.83</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>HD 37258-B</td><td>0.99</td><td>0.05</td><td>31.6</td><td>1.0</td><td>2.34</td><td>1994.00</td><td>5.83</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>BF Ori-B</td><td>2.04</td><td>0.0055</td><td>46.7</td><td>...</td><td>4</td><td>2006.12</td><td>10.08</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>BF Ori-B</td><td>2.05</td><td>0.02</td><td>47.5</td><td>2.0</td><td>4.09</td><td>2005.89</td><td>10.08</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BF Ori-B</td><td>2.03</td><td>0.05</td><td>48.0</td><td>1.0</td><td>3.68</td><td>1994.00</td><td>10.08</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HD 259431-C</td><td>3.15</td><td>0.0055</td><td>345.3</td><td>...</td><td>5.7</td><td>2005.79</td><td>2.91</td><td>2005 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>HD 259431-C</td><td>3.12</td><td>0.05</td><td>346.5</td><td>1.0</td><td>5.67</td><td>1993.95</td><td>2.91</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>S Mon-B</td><td>2.91</td><td>0.05</td><td>112.8</td><td>1.0</td><td>3.46</td><td>1995.16</td><td>3.59</td><td>1995 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>S Mon-B</td><td>2.88</td><td>0.04</td><td>202.0</td><td>2.0</td><td>3.31</td><td>2001.75</td><td>3.59</td><td>Turner08</td><td></td><td></td></tr><tr><td>HD 52721-B</td><td>0.65</td><td>0.05</td><td>194.4</td><td>1.0</td><td>1.41</td><td>1993.95</td><td>1.61</td><td>1995 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>HD 52721-B</td><td>0.65</td><td>0.02</td><td>196.6</td><td>2.0</td><td>1.51</td><td>2003.88</td><td>1.61</td><td>Perrin06</td><td></td><td></td></tr><tr><td>Z CMa-B</td><td>0.10</td><td>0.0055</td><td>118.2</td><td>...</td><td>2.14</td><td>2006.25</td><td>2.26</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>Z CMa-B</td><td>0.10</td><td>0.007</td><td>122.5</td><td>0.2</td><td>0.86</td><td>1994.08</td><td>2.26</td><td>Leinert97</td><td></td><td></td></tr><tr><td>Z CMa-B</td><td>0.10</td><td>0.01</td><td>120.0</td><td>4.0</td><td>3.79</td><td>1990.82</td><td>2.26</td><td>Koresko91</td><td></td><td></td></tr><tr><td>NX Pup-B (**)</td><td>0.13</td><td>0.0055</td><td>69.1</td><td>...</td><td>1.43</td><td>2006.16</td><td>0.62</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>NX Pup-B</td><td>0.13</td><td>0.05</td><td>62.4</td><td>1.0</td><td>1.75</td><td>1993.99</td><td>0.62</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>NX Pup-B</td><td>0.13</td><td>0.007</td><td>63.4</td><td>1.0</td><td>0.64</td><td>1993.00</td><td>0.62</td><td>Bernacca93</td><td></td><td></td></tr><tr><td>HD 76534-B (**)</td><td>2.09</td><td>0.05</td><td>303.0</td><td>1.0</td><td>1.46</td><td>1994.50</td><td>1.41</td><td>1995 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>HD 76534-B</td><td>2.07</td><td>0.005</td><td>303.6</td><td>0.5</td><td>0.33</td><td>2003.50</td><td>1.41</td><td>Correia06</td><td></td><td></td></tr><tr><td>HD 97300-B</td><td>0.79</td><td>0.0055</td><td>327.1</td><td>...</td><td>3.08</td><td>2006.16</td><td>0.51</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>HD 97300-B</td><td>0.79</td><td>0.001</td><td>326.7</td><td>0.6</td><td>3.05</td><td>2004.23</td><td>0.51</td><td>Lafreniere08</td><td></td><td></td></tr><tr><td>HD 97300-B</td><td>0.84</td><td>0.04</td><td>327.0</td><td>2.0</td><td>...</td><td>1994.32</td><td>0.51</td><td>Ghez97</td><td></td><td></td></tr><tr><td>HD 141569-B</td><td>7.61</td><td>0.0055</td><td>312.0</td><td>...</td><td>2.58</td><td>2007.26</td><td>0.43</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>HD 141569-B</td><td>6.80</td><td>0.1</td><td>312.0</td><td>1.0</td><td>2.7</td><td>1996.00</td><td>0.43</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>HD 141569-C</td><td>8.96</td><td>0.0055</td><td>311.0</td><td>...</td><td>3.2</td><td>2007.26</td><td>0.43</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>HD 141569-C</td><td>8.00</td><td>0.1</td><td>314.0</td><td>1.0</td><td>2</td><td>1996.00</td><td>0.43</td><td>Pirzkal97</td><td></td><td></td></tr></tbody></table>
<table><caption>**Table 8**
(Continued)</caption><thead><tr><th>Detection/Companion</th><th>Sep. (arcsec)</th><th>Sep. Err. (arcsec)</th><th>PA (degrees)</th><th>PA Err. (degrees)</th><th>ΔK</th><th>Date Observed</th><th>Min. Time Needed (yr)</th><th>Survey</th><th>PM Res.</th><th>Statistical Res.</th></tr></thead><tbody><tr><td>HD 144432-B (**)</td><td>1.45</td><td>0.05</td><td>4.4</td><td>1.0</td><td>2.49</td><td>1995.25</td><td>0.40</td><td>1995 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>HD 144432-B</td><td>1.47</td><td>0.02</td><td>4.3</td><td>2.0</td><td>2.23</td><td>2004.51</td><td>0.40</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 144432-B</td><td>1.40</td><td>0.1</td><td>-7.0</td><td>1.0</td><td>2.4</td><td>2002.50</td><td>0.40</td><td>Perez04</td><td></td><td></td></tr><tr><td>V856 Sco-B (**)</td><td>1.46</td><td>0.05</td><td>109.7</td><td>1.0</td><td>3.44</td><td>1995.25</td><td>0.44</td><td>1995 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>V856 Sco-B</td><td>1.46</td><td>0.05</td><td>110.8</td><td>1.0</td><td>3.41</td><td>1993.93</td><td>0.44</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>V856 Sco-B</td><td>1.45</td><td>0.05</td><td>111.2</td><td>1.0</td><td>3.36</td><td>1994.59</td><td>0.44</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>V856 Sco-B</td><td>1.43</td><td>0.01</td><td>114.6</td><td>0.5</td><td>3.58</td><td>1993.58</td><td>0.44</td><td>Leinert97</td><td></td><td></td></tr><tr><td>V856 Sco-B</td><td>1.53</td><td>0.07</td><td>114.0</td><td>2.0</td><td>...</td><td>1996.41</td><td>0.44</td><td>Ghez97</td><td></td><td></td></tr><tr><td>PDS415-B</td><td>4.49</td><td>0.0055</td><td>179.8</td><td>...</td><td>0.38</td><td>2007.50</td><td>0.47</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>PDS415-B</td><td>4.51</td><td>0.02</td><td>180.6</td><td>2.0</td><td>...</td><td>2005.57</td><td>0.47</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 150193-B</td><td>1.10</td><td>0.0055</td><td>225.8</td><td>...</td><td>2.638</td><td>2006.55</td><td>0.56</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>HD 150193-B</td><td>1.09</td><td>0.02</td><td>224.8</td><td>2.0</td><td>1.12</td><td>2004.51</td><td>0.56</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 150193-B</td><td>1.07</td><td>0.05</td><td>224.6</td><td>1.0</td><td>2.72</td><td>1995.08</td><td>0.56</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HD 150193-B</td><td>1.10</td><td>0.1</td><td>236.0</td><td>1.0</td><td>2.2</td><td>1996.00</td><td>0.56</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>HD 150193-B</td><td>1.10</td><td>0.005</td><td>224.9</td><td>0.5</td><td>0.2</td><td>2003.50</td><td>0.56</td><td>Correia06</td><td></td><td></td></tr><tr><td>KK Oph-B</td><td>1.61</td><td>0.0055</td><td>245.5</td><td>...</td><td>1.61</td><td>2006.16</td><td>0.56</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>KK Oph-B</td><td>1.61</td><td>0.02</td><td>247.2</td><td>0.5</td><td>1.96</td><td>1992.63</td><td>0.56</td><td>Leinert97</td><td></td><td></td></tr><tr><td>KK Oph-B</td><td>1.61</td><td>0.02</td><td>245.2</td><td>2.0</td><td>1.37</td><td>2004.51</td><td>0.56</td><td>Perrin06</td><td></td><td></td></tr><tr><td>KK Oph-B</td><td>1.50</td><td>0.1</td><td>257.0</td><td>1.0</td><td>2.5</td><td>1996.00</td><td>0.56</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>PDS453-7</td><td>6.01</td><td>0.0055</td><td>139.9</td><td>...</td><td>3.382</td><td>2007.59</td><td>0.36</td><td>2005 Survey</td><td>Inconclusive</td><td>Not likely</td></tr><tr><td>PDS453-7</td><td>6.01</td><td>0.02</td><td>141.4</td><td>2.0</td><td>...</td><td>2005.57</td><td>0.36</td><td>Perrin06</td><td></td><td></td></tr><tr><td>PDS453-9</td><td>6.98</td><td>0.0055</td><td>2.7</td><td>...</td><td>6.55</td><td>2007.59</td><td>0.36</td><td>2005 Survey</td><td>Inconclusive</td><td>Not likely</td></tr><tr><td>PDS453-9</td><td>7.01</td><td>0.02</td><td>3.8</td><td>2.0</td><td>...</td><td>2005.57</td><td>0.36</td><td>Perrin06</td><td></td><td></td></tr><tr><td>PDS469-B</td><td>1.69</td><td>0.0055</td><td>16.6</td><td>...</td><td>4.49</td><td>2007.59</td><td>16.32</td><td>2005 Survey</td><td>Inconclusive</td><td>Likely</td></tr><tr><td>PDS469-B</td><td>1.68</td><td>0.02</td><td>16.4</td><td>2.0</td><td>4.63</td><td>2004.69</td><td>16.32</td><td>Perrin06</td><td></td><td></td></tr><tr><td>PDS469-9 (***)</td><td>7.74</td><td>0.0055</td><td>339.0</td><td>...</td><td>3.195</td><td>2007.59</td><td>16.32</td><td>2005 Survey</td><td>Yes?</td><td>Not likely</td></tr><tr><td>PDS469-9</td><td>7.76</td><td>0.02</td><td>334.0</td><td>2.0</td><td>2.3</td><td>2004.69</td><td>16.32</td><td>Perrin06</td><td></td><td></td></tr><tr><td>MWC 297-B (*)(**)</td><td>3.38</td><td>0.0055</td><td>312.9</td><td>...</td><td>7.27</td><td>2007.26</td><td>1.27</td><td>2005 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>MWC 297-B</td><td>3.39</td><td>0.02</td><td>313.2</td><td>2.0</td><td>6.61</td><td>2004.69</td><td>1.27</td><td>Perrin06</td><td></td><td></td></tr><tr><td>MWC 297-B</td><td>3.39</td><td>0.2</td><td>313.0</td><td>2.0</td><td>8.5</td><td>2004.58</td><td>1.27</td><td>Vink05</td><td></td><td></td></tr><tr><td>AS 310-B</td><td>1.30</td><td>0.0055</td><td>79.1</td><td>...</td><td>2.944</td><td>2007.27</td><td>3.71</td><td>2005 Survey</td><td>Yes?</td><td>Likely</td></tr><tr><td>AS 310-B</td><td>1.31</td><td>0.05</td><td>78.3</td><td>1.0</td><td>3.69</td><td>1996.54</td><td>3.71</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>AS 310-B</td><td>1.30</td><td>0.15</td><td>81.3</td><td>0.3</td><td>3.53</td><td>1994.00</td><td>3.71</td><td>Ageorges94</td><td></td><td></td></tr><tr><td>AS 310-C (**)</td><td>4.38</td><td>0.0055</td><td>122.4</td><td>...</td><td>0.343</td><td>2007.27</td><td>3.71</td><td>2005 Survey</td><td>Yes?</td><td>Likely</td></tr><tr><td>AS 310-C</td><td>4.34</td><td>0.05</td><td>122.0</td><td>1.0</td><td>1.1</td><td>1996.54</td><td>3.71</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>AS 310-C</td><td>4.40</td><td>0.15</td><td>153.9</td><td>0.3</td><td>0.94</td><td>1994.00</td><td>3.71</td><td>Ageorges94</td><td></td><td></td></tr><tr><td>AS 310-2 (***)</td><td>2.23</td><td>0.0055</td><td>240.7</td><td>...</td><td>3.115</td><td>2007.27</td><td>3.71</td><td>2005 Survey</td><td>Yes?</td><td>Not likely</td></tr><tr><td>AS 310-2</td><td>2.30</td><td>0.15</td><td>242.3</td><td>0.3</td><td>3.87</td><td>1994.00</td><td>3.71</td><td>Ageorges94</td><td></td><td></td></tr><tr><td>AS 310-2</td><td>2.22</td><td>0.05</td><td>240.5</td><td>1.0</td><td>3.42</td><td>1996.54</td><td>3.71</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>AS 310-3 (***)</td><td>3.73</td><td>0.0055</td><td>233.6</td><td>...</td><td>2.929</td><td>2007.27</td><td>3.71</td><td>2005 Survey</td><td>Yes?</td><td>Not likely</td></tr><tr><td>AS 310-3</td><td>3.80</td><td>0.15</td><td>235.7</td><td>0.3</td><td>4.1</td><td>1994.00</td><td>3.71</td><td>Ageorges94</td><td></td><td></td></tr><tr><td>AS 310-3</td><td>3.74</td><td>0.05</td><td>233.4</td><td>1.0</td><td>3.7</td><td>1996.54</td><td>3.71</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>AS 310-6 (***)</td><td>4.91</td><td>0.0055</td><td>1.0</td><td>...</td><td>2.61</td><td>2007.27</td><td>3.71</td><td>2005 Survey</td><td>Yes?</td><td>Not likely</td></tr><tr><td>AS 310-6</td><td>4.88</td><td>0.05</td><td>0.9</td><td>1.0</td><td>2.7</td><td>1996.54</td><td>3.71</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>AS 310-6</td><td>4.90</td><td>0.15</td><td>2.9</td><td>0.3</td><td>2.58</td><td>1994.00</td><td>3.71</td><td>Ageorges94</td><td></td><td></td></tr><tr><td>AS 310-8</td><td>5.02</td><td>0.0055</td><td>6.3</td><td>...</td><td>4.293</td><td>2007.27</td><td>3.71</td><td>2005 Survey</td><td>Inconclusive</td><td>Not likely</td></tr><tr><td>AS 310-8</td><td>5.00</td><td>0.05</td><td>6.1</td><td>1.0</td><td>4.65</td><td>1996.54</td><td>3.71</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HD 179218-B</td><td>2.54</td><td>0.0055</td><td>140.5</td><td>...</td><td>6.6</td><td>2005.78</td><td>0.51</td><td>2005 Survey</td><td>Yes</td><td>Likely</td></tr><tr><td>HD 179218-B</td><td>2.55</td><td>0.02</td><td>139.9</td><td>2.0</td><td>5.31</td><td>2004.51</td><td>0.51</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 179218-1</td><td>3.67</td><td>0.0055</td><td>339.3</td><td>...</td><td>8.7</td><td>2005.78</td><td>0.51</td><td>2005 Survey</td><td>Yes</td><td>Not likely</td></tr><tr><td>HD 179218-1</td><td>3.66</td><td>0.02</td><td>338.7</td><td>2.0</td><td>6.56</td><td>2004.51</td><td>0.51</td><td>Perrin06</td><td></td><td></td></tr><tr><td>V1685 Cyg-B</td><td>0.72</td><td>0.0055</td><td>240.0</td><td>...</td><td>5.4</td><td>2005.72</td><td>1.75</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>V1685 Cyg-B</td><td>0.72</td><td>0.05</td><td>239.1</td><td>1.0</td><td>5.5</td><td>1996.41</td><td>1.75</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>LkHA 224-B</td><td>4.72</td><td>0.0055</td><td>292.5</td><td>...</td><td>7.867</td><td>2007.27</td><td>2.27</td><td>2005 Survey</td><td>Yes</td><td>Likely</td></tr><tr><td>LkHA 224-B</td><td>4.76</td><td>0.02</td><td>293.8</td><td>2.0</td><td>...</td><td>2004.56</td><td>2.27</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 224-2</td><td>9.16</td><td>0.0055</td><td>331.0</td><td>...</td><td>7.481</td><td>2007.27</td><td>2.27</td><td>2005 Survey</td><td>Inconclusive</td><td>Not likely</td></tr><tr><td>LkHA 224-2</td><td>9.17</td><td>0.02</td><td>332.9</td><td>2.0</td><td>...</td><td>2004.56</td><td>2.27</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 224-3 (***)</td><td>8.96</td><td>0.0055</td><td>332.7</td><td>...</td><td>7.064</td><td>2007.27</td><td>2.27</td><td>2005 Survey</td><td>Yes</td><td>Not likely</td></tr><tr><td>LkHA 224-3</td><td>9.07</td><td>0.02</td><td>333.6</td><td>2.0</td><td>...</td><td>2004.56</td><td>2.27</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HBC 694-B</td><td>1.39</td><td>0.05</td><td>259.9</td><td>1.0</td><td>0.6</td><td>1996.67</td><td>2.00</td><td>1995 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>HBC 694-B</td><td>1.46</td><td>0.08</td><td>261.9</td><td>2.0</td><td>1.14</td><td>2004.27</td><td>2.00</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HBC 694-C</td><td>1.85</td><td>0.05</td><td>250.5</td><td>1.0</td><td>2.5</td><td>1996.67</td><td>2.00</td><td>1995 Survey</td><td>Inconclusive</td><td>Likely</td></tr></tbody></table>
<table><caption>**Table 8**
(Continued)</caption><thead><tr><th>Detection/Companion</th><th>Sep. (arcsec)</th><th>Sep. Err. (arcsec)</th><th>PA (degrees)</th><th>PA Err. (degrees)</th><th>ΔK</th><th>Date Observed</th><th>Min. Time Needed (yr)</th><th>Survey</th><th>PM Res.</th><th>Statistical Res.</th></tr></thead><tbody><tr><td>HBC 694-C</td><td>1.86</td><td>0.08</td><td>251.8</td><td>2.0</td><td>0</td><td>2004.27</td><td>2.00</td><td>Perrin06</td><td></td><td></td></tr><tr><td>MWC 349-B (**)</td><td>2.76</td><td>0.0055</td><td>286.3</td><td>...</td><td>3.686</td><td>2007.28</td><td>2.02</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>MWC 349-B</td><td>2.77</td><td>0.02</td><td>286.0</td><td>2.0</td><td>4.27</td><td>2004.68</td><td>2.02</td><td>Perrin06</td><td></td><td></td></tr><tr><td>MWC 349-B</td><td>2.40</td><td>0.2</td><td>280.0</td><td>2.0</td><td>...</td><td>1983.56</td><td>2.02</td><td>Cohen85</td><td></td><td></td></tr><tr><td>AS 442-B</td><td>4.75</td><td>0.0055</td><td>54.5</td><td>...</td><td>6.6</td><td>2005.72</td><td>4.36</td><td>2005 Survey</td><td>Inconclusive</td><td>Likely</td></tr><tr><td>AS 442-B</td><td>4.75</td><td>0.02</td><td>54.0</td><td>2.0</td><td>6.19</td><td>2004.68</td><td>4.36</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 147-B</td><td>1.63</td><td>0.0055</td><td>340.7</td><td>...</td><td>3</td><td>2005.72</td><td>3.87</td><td>2005 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>LkHA 147-B</td><td>1.63</td><td>0.02</td><td>341.7</td><td>2.0</td><td>3.13</td><td>2005.57</td><td>3.87</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 147-B</td><td>1.62</td><td>0.05</td><td>341.7</td><td>1.0</td><td>3.04</td><td>1996.49</td><td>3.87</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HD 200775-B</td><td>2.55</td><td>0.05</td><td>167.2</td><td>1.0</td><td>4.64</td><td>1996.49</td><td>1.36</td><td>1995 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>HD 200775-B</td><td>2.57</td><td>0.02</td><td>168.3</td><td>2.0</td><td>3.95</td><td>2003.88</td><td>1.36</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 200775-B</td><td>2.25</td><td>0.1</td><td>164.0</td><td>1.0</td><td>4.9</td><td>1996.00</td><td>1.36</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>LkHA 324-C</td><td>5.67</td><td>0.0055</td><td>325.8</td><td>...</td><td>3.7</td><td>2005.72</td><td>2.87</td><td>2005 Survey</td><td>Yes</td><td>Likely</td></tr><tr><td>LkHA 324-C</td><td>5.62</td><td>0.05</td><td>325.3</td><td>1.0</td><td>3.79</td><td>1996.54</td><td>2.87</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>LkHA 324-C</td><td>5.68</td><td>0.02</td><td>325.2</td><td>2.0</td><td>3</td><td>2004.57</td><td>2.87</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 203024-B (**)</td><td>0.25</td><td>0.0055</td><td>153.1</td><td>...</td><td>0.07</td><td>2007.33</td><td>1.03</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>HD 203024-B</td><td>0.23</td><td>0.05</td><td>160.6</td><td>1.0</td><td>0.04</td><td>1996.49</td><td>1.03</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HD 203024-B</td><td>0.14</td><td>0.02</td><td>151.5</td><td>2.0</td><td>0.19</td><td>2004.83</td><td>1.03</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 234-B</td><td>1.90</td><td>0.0055</td><td>97.3</td><td>...</td><td>5.568</td><td>2005.33</td><td>2.87</td><td>2005 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>LkHA 234-B</td><td>1.89</td><td>0.02</td><td>97.9</td><td>2.0</td><td>...</td><td>2005.57</td><td>2.87</td><td>Perrin06</td><td></td><td></td></tr><tr><td>LkHA 234-B</td><td>1.87</td><td>0.05</td><td>96.6</td><td>1.0</td><td>5.5</td><td>1996.54</td><td>2.87</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>LkHA 234-C</td><td>8.38</td><td>0.0055</td><td>11.1</td><td>...</td><td>6.519</td><td>2005.33</td><td>2.87</td><td>2005 Survey</td><td>Yes?</td><td>Likely</td></tr><tr><td>LkHA 234-C</td><td>8.45</td><td>0.02</td><td>12.3</td><td>2.0</td><td>...</td><td>2005.57</td><td>2.87</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BD+46 3471-B</td><td>1.31</td><td>0.0055</td><td>309.6</td><td>...</td><td>4.6</td><td>2005.72</td><td>2.41</td><td>2005 Survey</td><td>Yes</td><td>Very likely</td></tr><tr><td>BD+46 3471-B</td><td>1.31</td><td>0.02</td><td>311.4</td><td>2.0</td><td>4.27</td><td>2003.88</td><td>2.41</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BD+46 3471-B</td><td>1.31</td><td>0.05</td><td>308.7</td><td>1.0</td><td>4.48</td><td>1996.49</td><td>2.41</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>BD+46 3471-C</td><td>4.69</td><td>0.0055</td><td>40.5</td><td>...</td><td>4.4</td><td>2005.72</td><td>2.41</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>BD+46 3471-C</td><td>4.71</td><td>0.02</td><td>41.4</td><td>2.0</td><td>3.2</td><td>2003.88</td><td>2.41</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BD+46 3471-C</td><td>4.67</td><td>0.05</td><td>40.0</td><td>1.0</td><td>4.48</td><td>1996.49</td><td>2.41</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>BD+46 3471-C</td><td>4.18</td><td>0.1</td><td>45.0</td><td>1.0</td><td>4.7</td><td>1996.00</td><td>2.41</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>BD+46 3471-D</td><td>5.80</td><td>0.0055</td><td>206.2</td><td>...</td><td>5.3</td><td>2005.72</td><td>2.41</td><td>2005 Survey</td><td>Yes?</td><td>Likely</td></tr><tr><td>BD+46 3471-D</td><td>5.85</td><td>0.02</td><td>206.7</td><td>2.0</td><td>4.26</td><td>2003.88</td><td>2.41</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BD+46 3471-D</td><td>5.82</td><td>0.05</td><td>205.7</td><td>1.0</td><td>4.48</td><td>1996.49</td><td>2.41</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>BD+46 3471-E (**)</td><td>6.10</td><td>0.0055</td><td>200.7</td><td>...</td><td>5</td><td>2005.72</td><td>2.41</td><td>2005 Survey</td><td>Inconclusive</td><td>Likely</td></tr><tr><td>BD+46 3471-E</td><td>6.09</td><td>0.02</td><td>201.6</td><td>2.0</td><td>4.76</td><td>2003.88</td><td>2.41</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BD+46 3471-E</td><td>6.01</td><td>0.05</td><td>199.9</td><td>1.0</td><td>0</td><td>1996.49</td><td>2.41</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>BH Cep-B (**)</td><td>2.12</td><td>0.0055</td><td>103.7</td><td>...</td><td>7.464</td><td>2006.33</td><td>1.11</td><td>2005 Survey</td><td>Inconclusive</td><td>Likely</td></tr><tr><td>BH Cep-B</td><td>2.14</td><td>0.02</td><td>103.6</td><td>2.0</td><td>6.72</td><td>2004.68</td><td>1.11</td><td>Perrin06</td><td></td><td></td></tr><tr><td>BH Cep-C (**)</td><td>3.25</td><td>0.0055</td><td>267.3</td><td>...</td><td>5.985</td><td>2006.33</td><td>1.11</td><td>2005 Survey</td><td>Inconclusive</td><td>Very likely</td></tr><tr><td>BH Cep-C</td><td>3.26</td><td>0.02</td><td>266.3</td><td>2.0</td><td>6.48</td><td>2004.68</td><td>1.11</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 216629-C</td><td>7.80</td><td>0.0055</td><td>329.2</td><td>...</td><td>0.071</td><td>2005.73</td><td>5.05</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>HD 216629-C</td><td>7.81</td><td>0.02</td><td>328.5</td><td>2.0</td><td>-0.11</td><td>2004.68</td><td>5.05</td><td>Perrin06</td><td></td><td></td></tr><tr><td>HD 216629-C</td><td>7.71</td><td>0.05</td><td>328.6</td><td>1.0</td><td>0.12</td><td>1996.49</td><td>5.05</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>HD 216629-C</td><td>6.96</td><td>0.1</td><td>327.0</td><td>1.0</td><td>0</td><td>1996.00</td><td>5.05</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>MWC 1080-B</td><td>0.76</td><td>0.0055</td><td>269.6</td><td>...</td><td>2.8</td><td>2005.70</td><td>2.47</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>MWC 1080-B</td><td>0.77</td><td>0.05</td><td>268.2</td><td>1.0</td><td>2.84</td><td>1996.49</td><td>2.47</td><td>1995 Survey</td><td></td><td></td></tr><tr><td>MWC 1080-B</td><td>0.60</td><td>0.1</td><td>270.0</td><td>1.0</td><td>3.1</td><td>1996.00</td><td>2.47</td><td>Pirzkal97</td><td></td><td></td></tr><tr><td>MWC 1080-B</td><td>0.76</td><td>0.02</td><td>267.0</td><td>1.0</td><td>3.25</td><td>1995.77</td><td>2.47</td><td>Leinert97</td><td></td><td></td></tr><tr><td>MWC 1080-F</td><td>5.17</td><td>0.0055</td><td>89.3</td><td>...</td><td>5</td><td>2005.70</td><td>2.47</td><td>2005 Survey</td><td>Yes?</td><td>Very likely</td></tr><tr><td>MWC 1080-F</td><td>4.69</td><td>0.1</td><td>86.0</td><td>1.0</td><td>6.2</td><td>1995.54</td><td>2.47</td><td>Pirzkal97</td><td></td><td></td></tr></tbody></table>

Notes. (*) Thomas was saturated. (**) Pirzkal data. (***) Candidates for which the statistical and multiepoch studies give different conclusions. The PA errors from the 2005 Survey are calculated directly from the position error bars for each target.

(This table is available in machine-readable form.)

MWC 922 is a Be star surrounded by a beautiful nebula (Tuthill & Lloyd 2007). It is located in the galactic plane in a very high-density region. Of the six detections, two are considered very likely companions, having ΔK of 2 to 3, and two are likely companions, with ΔK greater than 5; again, all four are at large distances from the primary (~7000 to ~12,000 au). Tuthill & Lloyd (2007) reconstructed the structure of

MWC 922 using a lower-quality AO image taken with Palomar and CFHT, showing a very crowded field as well. This is an interesting system, which would benefit from additional observations.

PDS 530 is of uncertain spectral type, reported as “F0V?” by Vieira et al. (2003) and as “A5” in Sartori et al. (2010), without a source or explanation for the change; it is out of the galactic
<figure><img src="image_18.png" /><figcaption>**Figure 13.** Examples of a common proper-motion star (left) and a potential background star that remains inconclusive (right). Indeed, on the right graph, the error bars are such that the candidate could either be a background star or a common proper-motion star. The legends are as follows. For HD 97300: • = 2005 Survey; ▷ = Perrin (2006); and ◦ = Lafrenière et al. (2008). For MWC 297: • = 2005 Survey; ★ = Ghez et al. (1997); and ◦ = Vink et al. (2005).</figcaption></figure>

<figure><img src="image_19.png" /></figure>

plane, but still in a high-density field. Of the 11 detections, we find three likely companions, all ~2000 au from the primary star and ~5–7 mag fainter in K. However, as noted by Vieira et al. (2011), this star has not been well studied. It has a large parallax error in GAIA3 and the Vioque paper includes it as a “low quality” source, without identifying it as a binary.

MWC 953 is a B2Ve star (Carmona et al. 2010) at a distance of 2150 pc (GAIA3; previously reported at 800 pc, by Carmona et al. 2010). Of the nine detections, we identify one very likely companion, with a $\Delta K$ of 1.6 at 6400 au, and two fainter likely companions ($\Delta K$ ~ 4–5), which are slightly closer. This star is located in the galactic plane, also in a very high-density field, which explains the large number of additional nonlikely candidates. Vioque does not identify MWC 953 as a binary system.

BD+46 3471, aka V1578 Cyg, is a well-studied B9/A0 star (Hernández et al. 2004; Wichittanakom et al. 2020) in the Cygnus Constellation. The GAIA3 distance is well defined at 770 pc, and it is outside the galactic plane. The statistical survey finds that all four candidates are likely (two) or very likely (two) to be physical companions. The separations range from ~1000 to 5000 au, with $\Delta K$ from ~4 to 5. There are multiepoch data for all candidates, but only one shows convincing proper motion (see Section 6). Vioque also lists it as a multiple, citing Maheswar et al. (2002).

MWC 1080, aka V628 Cas, is also a well-studied HAEBE star, with a spectral type of B0 (Wichittanakom et al. 2020) at a distance of 1490 pc (GAIA3), being part of a complex region. Li et al. (2014) state that it is a triple system, in which the primary (MWC 1080A) is also an eclipsing binary. The companion (MWC 1080B) is located 0.7676 west of MWC 1080A (Leinert et al. 1997; Wang et al. 2008). Although this system is in the galactic plane, and part of a cluster, our analysis finds a high probability that all seven detections are physical companions. The close companion (MWC 1080B) at 0.7676 is identified as very likely, in our statistical survey. The other ones are quite faint, but are still found to be related. Two at 2.52 and 2.55 are very likely, while the other four are likely, although all have large $\Delta K$ ~ 5–9. This is in agreement with the mid-IR observations of the close environment of MWC 1080 from Li et al. (2014). Even though the wavelength difference makes it challenging to directly compare the

positions of the candidates, they also conclude that the surrounding detections are members of the MWC 1080 young cluster. Our multiepoch results for two of the detections (described in Section 6) show that both MWC 1080B and MWC 1080F have a common proper motion with the primary, but that more observations are required in order to understand the orbital motion.

## 6. Multiepoch Observations and Common Proper-motion Pairs

Several of the detections from the 2005 survey were also detected in the 1995 survey, as well as in other surveys that have been reported in the literature. Since almost all of the associated primaries have proper-motion data, we can use these observations to search for common proper motions, to help identify false companions. Indeed, since several of the observed targets are within high-density star-forming regions, common proper motions are not always a proof of physical companionship, but noncommon proper motions do rule out background objects. Multiepoch data can also be used to study the photometric variability of the companions, which will not be presented in this paper. The majority of the proper-motion values come from GAIA3, and are listed in Table 10 in the Appendix.

Of the 88 primary stars for which detections are reported here, multiple observations in conjunction with proper-motion data are available for 53 of them. Table 7 gathers useful observational information for the references that have more than one common primary source. This includes the epoch of the observations, the techniques that were used, and the resolutions. In addition, only one primary is associated with each of the following references: Cohen et al. (1985), Koresko et al. (1991), Bernacca et al. (1993), Reipurth & Zinnecker (1993), Perez et al. (2004), Smith et al. (2005), Vink et al. (2005), Lafrenière et al. (2008), Turner et al. (2008), and Uyama et al. (2017).

Altogether, we compare multiepoch data for 64 detections around 53 primary stars, with epochs ranging from 1983 to 2012. Table 8 lists all the detections for primary stars that have measured proper motions, measured distances, and multiple observations. This table also gives the results of the
<figure><img src="image_20.png" /></figure>

<figure><img src="image_21.png" /></figure>

<figure><img src="image_22.png" /></figure>

<figure><img src="image_23.png" /></figure>

<figure><img src="image_24.png" /></figure>

<figure><img src="image_25.png" /></figure>

<figure><img src="image_26.png" /><figcaption>**Figure 14.** Proper-motion graphs for the targets for which our statistical and proper-motion studies do not match. The legend is as given in Table 7.</figcaption></figure>
<figure><img src="image_27.png" /><figcaption>**Figure 15.** Comparison of the statistical (squares, triangles, and crosses) and proper-motion (circles) results for all the detections that are common to both studies. The symbols without circles have inconclusive proper-motion results, while the dotted circles indicate that the common proper-motion results are questionable.</figcaption></figure>

proper-motion study described in this section, and its comparison with the statistical study described in Section 4.3.

In order to estimate whether a candidate is related to the primary, we looked at the evolution of the candidate position in separation and PA relative to the primary over a few years. Whether or not the primary/companion pair can be identified as a common proper-motion pair depends on the following parameters:

1. *The proper motion of the star.* As mentioned above, the proper-motion data come primarily from GAIA3.

2. *The length of time between the different observations.* The time difference between observations has to be large enough relative to the resolution of the images in order to determine by proper motion whether the candidate companion is a background star. For example, if the proper motion is $0''_{-1}01$ yr$^{-1}$ and the resolution of the data is $0''_{-1}1$, one needs at least 10 yr between observations to declare that a potential candidate is a background star. On the contrary, if the candidate position is outside the “background start” trajectory before the minimum time, it is possible to determine whether they are related. For this purpose, we twice used our centroiding error as the minimum detectable motion, i.e., 11 mas.

3. *The astrometric error bars of the different detections.* All but one of the references list the error bars for both the separations and the PAs of their observations (see Table 8). For the 2005 survey, we used the error bars as described in Section 3.2.

4. *The observation time error bars.* Similarly, the references list the times of the observations with various precisions, from 1 day to 1 yr. We used these to create horizontal error bars.

5. *The potential orbital period of the candidate.* In addition, for some of the companions, the different multiepoch data

would lead to nonrealistic orbital motions. This is mostly true for the results that show big swings in PA. In order to verify a PA change that is not explained by proper motion, we looked at crude estimations of the potential orbital motions of the candidates. We were looking at the upper-case scenario of a circular orbit for which we would see the most PA variations. The orbital motion was calculated using Kepler's third law, from the linear separation in astronomical units (au) and the estimated stellar mass of the primary, based on spectral type.

We then classified the different candidates into four categories:

1. “Yes”—the candidate is a common proper-motion pair with the primary;

2. “Yes?”—the separation and PA versus time graphs indicate that the candidate is not a background object, suggesting common proper motion, but the implied orbital motion is not realistic (most likely due to measurement errors);

3. “No”—the candidate is clearly behaving as a background star, and the time elapsed between the earliest and latest observations is greater than the required minimum time; due to the sample and the uncertainties, we have not found any “No” instances in our results; and

4. “Inconclusive”—either because the candidate behaves as a background star, but the time elapsed is too short, or because the error bars (astrometric and time) are large enough that the separation or PA measurement is ambiguous as to whether the candidate falls on the background track or not.

Figure 13 presents two examples of how the PA and the separations for different epochs were used to determine the
relationship, showing the angular separations (at the bottom) and the PAs (at the top) as a function of time.

On each graph, the points show the different measurements that have been made for each observation, over the time of the candidate's separation and the PA. The dotted line shows what would be a constant separation and PA for our observations, which is taken as a reference. The solid line shows the motion of a background star relative to the primary. Finally, the dashed-dotted lines parallel to the solid line are the error bars, including proper-motion error bars as well as error bars from our observations (either Survey05 or Survey95, if there is no entry for Survey05).

If the companion separation or PA for epochs other than ours are located away from the solid line, this indicates that the object is not a background star, and so is most likely physically bound. Note that the points will not necessarily appear on the dotted line for all epochs, due to orbital motion.

Figure 13 shows the results for two typical scenarios: a common proper-motion companion (left) and a likely background star, which remains inconclusive due to the error bars and the small expected change in the background star motion over the elapsed time (right). Interestingly, there were no cases for which the candidate was definitely a background star; this is mostly explained by the large measurement error bars relative to the expected motion and the long times needed between observations. The rest of the plots are shown in the Appendix (Figures 16–19).

We find that 24 of all detections show common proper motions, 20 are inconclusive, and 20 have unrealistic orbital motions, even though the graphs show common proper motions.

Note that the multiepoch data from 10 of these targets come from the survey from Perrin (2006), with observations that are less than 1 yr away from our observations, meaning that these second-epoch observations are only informative in cases of the high orbital motion of the companions.

Since this method of determination of the relationship between the companion and the primary is independent from the statistical study conducted in Section 4.2, it is informative to compare the results, as shown in Table 10. Of the 64 detections studied in this section, 21 of the confirmed proper-motion companions are statistically found to be very likely or likely. On the other hand, three have common proper-motion companions where the statistical method finds them unlikely to be related: HIP 592, HD 179218, and LkHa 224. In the first two cases, the separations are barely off the background track, and it is possible that the error bars are underestimated; for the last case, the proper-motion data from GAIA3 are of marginal quality (but none other are available). Similarly, four detections around two additional primaries are categorized as a “Yes?” due to their unrealistic orbital motions calling into question the multiepoch results: GSC 05673-00127 (PDS 469) and three candidates for AS310 (HBC 284). In addition, the GAIA data were questionable and were only taken into account due to the lack of earlier data. In all of these cases, more data would be helpful for solving the ambiguity. Figure 14 shows the corresponding proper-motion graphs for these seven cases.

Note that finding candidates and primaries with common proper motions is only an indication of the physical relationship. The objects could either be physically bound or be part of the same comoving group. Finally, in addition to position

errors, the fact that the brightnesses of both the primary and the companion may vary introduces an uncertainty, particularly if there are multiple companions.

A few objects with interesting or peculiar results are noted here (see the figures in the Appendix):

1. CO Ori-B, CQ Tau-B, HD 141569-C, and MWC 349-B. Both the statistical and the proper-motion studies match, but the candidate motion relative to the primary, for the PA and/or the separation, is larger than the expected orbital motion. Additional observations could help to better determine the actual orbit of the companion.

2. Z CMa-B. This is borderline inconclusive, as the PA has a large error, due to the close separation, while the separation is constant and has low error bars.

3. SMon-B. There seems to be a 90° error in the PA measurement from the previous study.

4. BD06 1253-B. There is a hint of an orbit, reinforcing its belonging to a multiple system.

Figure 15 presents a visual summary of the proper-motion study compared to the statistical study, plotting the proper-motion results on the data from Figure 5 for the 64 stars in the proper-motion study. All three of the not likely detections with common proper motions have separations of ~4" or more and $\Delta K > 6$. The four not likely detections that have potential common proper motions (“Yes?”) have $\Delta K \sim 3$ (which we assume is a coincidence) and separations ranging from 2" to 8". These cases are discussed earlier in this section. Of the results in common, we see that most of the very likely companions with common proper motions are located, as expected, toward the lower left. Including the likely companions, this dependency weakens, and there are several with large separations or large $\Delta K$.

We found that establishing common proper motions for more than 50% of the (very) likely candidates was premature at this stage (inconclusive or questionable), indicating that the study would benefit from further observations. As a result, while the comparison of the studies is useful for identifying specific targets of interest, it does not change the multiplicity frequency results that are presented in Section 5.1.

## 7. Conclusions/Summary

We present the results of a sensitive AO-assisted imaging survey of 143 mainly pre-main-sequence stars, of spectral types from late O to early G, to identify companions to HAEBE stars. These data are a compilation of two distinct surveys conducted ~10 yr apart, and represent the most extensive and most sensitive survey of HAEBE multiplicity to date. A total of 250 nearby objects were detected around 88 primary stars. To identify the likely physical companions, we employed a statistical likelihood analysis.

Most of the primary stars that were rejected as multiples from the statistical analysis were found in crowded fields in and around the galactic plane, emphasizing the difficulty in reliably identifying multiple systems in these regions. In addition, many apparent high-order multiples were reduced to binaries or triples, as other detections were rejected as unlikely companions. Nevertheless, we found likely (≥90%) or very likely (≥99%) companions around 70 systems: 48 binaries, 16 triples, and 6 higher-order multiples. The majority of the very likely companions have angular separations <3" and $\Delta K < 4$, but several were found at large angular (and linear) separations and
large Δ*K* magnitudes, highlighting the advantage of a statistical method over arbitrary cutoffs in either of these parameters.

Discarding the nonlikely candidates, and correcting for completeness, we found multiplicity frequencies (the likelihood of finding at least one companion) of at least 39% (very likely) and possibly higher than 56% (likely and very likely). Among the 126 established HAEBE stars in our sample, we found no strong correlation between multiplicity and primary star temperature, although higher-order (greater than two) multiples appeared to be more common among the early B stars.

The majority of the very likely companions around cooler stars ($T_{eff} < 13,000$ K) had separations of ~100 to ~1000 au, while the companions of higher-mass stars were predominantly found at distances from 800 au to several thousand astronomical units. Even considering the detection limits of the survey, we found that companions within ~700 au are more common among Herbig Ae stars compared to Herbig Be stars, and very close companions, within 100 au, are quite rare for all HAEBE stars (at least, with $\Delta K < 5$). The difference in *K* magnitude between the primaries and the companions spanned a wide range, from near zero to >8; however, $\Delta K < 1.5$ was relatively rare. This suggests that similar mass companions are not common, and many of the companion stars are likely T Tauri or young brown dwarf stars.

Finally, GAIA3 has provided improved distances and proper motions for most of our sample, allowing us to study the nature of these systems in more detail. Using GAIA3 proper-motion data and multiepoch observations from our studies and the literature, we were able to search for common proper motions among 53 stars in our sample. We found that 24 of all the detections showed common proper motions, 20 were inconclusive, and 20 had unrealistic orbital motions, even though the graphs showed common proper motions. The high number of inconclusive results was due to the large measurement error bars in the older data, which also contributed to the unrealistic orbital motions, in some cases. Of the statistically very likely companions included in the proper-motion analysis, 53% were confirmed to have common proper motion, with the remaining being inconclusive or unclear. The comparison revealed several interesting targets for further study.

We have presented a broad sample of intermediate-mass young stars and substantially increased the known pool of multiple systems within this group. The data are not specific to particular regions or stellar environments, but rather provide statistical results based on a relatively large sample, identifying a number of intriguing individual systems, and adding to the historical database of multiepoch observations of intermediate-mass multiple systems.

We acknowledge with gratitude the CTIO REU-PIA program and the many students who have assisted with various aspects of this program over several years, including Lara Pierpoint, Maria-Jose Cordero, Anne Sweet, Ben Brandvig, Jacqueline Serron, and Will Flanagan, as well as Portland State University students Camille Pierson, Austin Tant, and David Post. We thank the Gemini staff observers who collected these data over many nights of queue observations at Gemini North, and the ESO staff who did the same at Paranal.

This research has made extensive use of the SIMBAD database, operated at CDS, Strasbourg, France, as well as 2MASS data.

This work was enabled by observations made from the Gemini North telescope, located within the Maunakea Science Reserve and adjacent to the summit of Maunakea. We are grateful for the privilege of observing the universe from a place that is unique in both its astronomical quality and its cultural significance.

Based on observations obtained at the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA), under a cooperative agreement with the National Science Foundation, on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), the National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and the Korea Astronomy and Space Science Institute (Republic of Korea).

Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 076.C-0708.

Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. The observations at CFHT were performed with care and respect from the summit of Maunakea, which is a significant cultural and historic site.

This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC: https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Facilities: Gemini, VLT, La Silla, CFHT, Gaia.

## Appendix

### Appendix Material

#### A.1. Unlikely Detections from the 2005 Survey

The following table (Table 9) provides data on the remaining detections from the 2005 survey that were rejected from the companion sample, as a result of the statistical probability analysis. The majority of these are additional detections around the primary stars listed in Table 3.

#### A.2. Proper-motion Data for the Multiepoch Study

Table 10 gathers the proper-motion information for all the sample stars with multiepoch data. Most of the data come from Gaia DR3.

#### A.3. Additional Data from the 1995 Survey

The observations from the 1995 Survey also included several bands that allowed the gathering of additional information about the colors of both the primary and the candidates, which are presented in Table 11. We have not used these data in this particular paper, but we publish them as they could be useful for any follow-up work on determinations of spectral energy distributions or excess characterizations.
<table><caption>**Table 9**
Data for the Nonlikely Candidates</caption><thead><tr><th>Companion</th><th>Ang. Sep. (arcsec)</th><th>PA (deg)</th><th>Linear Sep. (au)</th><th>K Sample</th><th>Star</th><th>ΔK</th><th>P</th><th>Likelihood</th><th>Date Observed</th></tr></thead><tbody><tr><td>HIP 592-1</td><td>7.28</td><td>352.30</td><td>5285.3</td><td>11.00</td><td></td><td>6.20</td><td>5.07E-01</td><td>Not likely</td><td>16/01/06</td></tr><tr><td>HIP 592-2</td><td>8.01</td><td>354.00</td><td>5815.3</td><td>11.00</td><td></td><td>3.90</td><td>1.81E-01</td><td>Not likely</td><td>16/01/06</td></tr><tr><td>VX Cas-1</td><td>5.01</td><td>344.40</td><td>2702.7</td><td>8.21</td><td></td><td>8.20</td><td>2.51E-01</td><td>Not likely</td><td>13/10/05</td></tr><tr><td>LkHA 201-2</td><td>9.69</td><td>35.20</td><td>25902.2</td><td>9.85</td><td></td><td>7.20</td><td>7.52E-01</td><td>Not likely</td><td>13/10/05</td></tr><tr><td>HBC 334-2</td><td>3.4</td><td>177.00</td><td>5440.0</td><td>11.42</td><td></td><td>6.10</td><td>1.33E-01</td><td>Not likely</td><td>16/11/05</td></tr><tr><td>HBC 334-4</td><td>6.27</td><td>294.20</td><td>10032.0</td><td>11.42</td><td></td><td>5.70</td><td>3.22E-01</td><td>Not likely</td><td>16/11/05</td></tr><tr><td>HBC 334-5</td><td>8.1</td><td>50.40</td><td>12960.0</td><td>11.42</td><td></td><td>6.70</td><td>6.71E-01</td><td>Not likely</td><td>16/11/05</td></tr><tr><td>HBC 531-1</td><td>6.61</td><td>163.00</td><td>4697.3</td><td>11.32</td><td></td><td>5.70</td><td>3.08E-01</td><td>Not likely</td><td>18/01/06</td></tr><tr><td>HBC 531-2</td><td>7.9</td><td>332.20</td><td>5614.0</td><td>11.32</td><td></td><td>7.60</td><td>7.03E-01</td><td>Not likely</td><td>18/01/06</td></tr><tr><td>HBC 531-3</td><td>8.99</td><td>317.50</td><td>6388.6</td><td>11.32</td><td></td><td>6.90</td><td>7.07E-01</td><td>Not likely</td><td>18/01/06</td></tr><tr><td>LkHA 25-1</td><td>5.07</td><td>97.10</td><td>3586.1</td><td>9.33</td><td></td><td>6.60</td><td>1.05E-01</td><td>Not likely</td><td>24/12/05</td></tr><tr><td>HBC 535-1</td><td>3.67</td><td>221.30</td><td>2638.0</td><td>10.21</td><td></td><td>7.10</td><td>1.15E-01</td><td>Not likely</td><td>01/11/05</td></tr><tr><td>HBC 535-2</td><td>5.42</td><td>172.40</td><td>3895.9</td><td>10.21</td><td></td><td>8.30</td><td>3.65E-01</td><td>Not likely</td><td>01/11/05</td></tr><tr><td>HBC 535-3</td><td>5.9</td><td>301.21</td><td>4240.9</td><td>10.21</td><td></td><td>5.60</td><td>1.28E-01</td><td>Not likely</td><td>01/11/05</td></tr><tr><td>PDS453-1</td><td>1.698</td><td>-146.51</td><td>219.1</td><td>9.17</td><td></td><td>7.98</td><td>2.28E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-2</td><td>2.078</td><td>34.43</td><td>268.2</td><td>9.17</td><td></td><td>7.26</td><td>2.36E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-3</td><td>3.56</td><td>-13.55</td><td>459.4</td><td>9.17</td><td></td><td>8.02</td><td>6.87E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-4</td><td>3.947</td><td>48.59</td><td>509.3</td><td>9.17</td><td></td><td>7.65</td><td>6.95E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-5</td><td>3.984</td><td>108.94</td><td>514.1</td><td>9.17</td><td></td><td>7.04</td><td>5.86E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-6</td><td>5.855</td><td>139.27</td><td>755.6</td><td>9.17</td><td></td><td>7.33</td><td>8.90E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-7</td><td>6.012</td><td>139.94</td><td>775.8</td><td>9.17</td><td></td><td>3.38</td><td>1.30E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-8</td><td>6.061</td><td>52.64</td><td>782.1</td><td>9.17</td><td></td><td>8.02</td><td>9.65E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-9</td><td>6.976</td><td>2.69</td><td>900.2</td><td>9.17</td><td></td><td>6.55</td><td>8.72E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>PDS453-10</td><td>7.264</td><td>52.46</td><td>937.4</td><td>9.17</td><td></td><td>5.48</td><td>6.83E-01</td><td>Not likely</td><td>03/08/07</td></tr><tr><td>BD-22 4400-1</td><td>3.139</td><td>-44.18</td><td>4846.4</td><td>8.50</td><td></td><td>8.13</td><td>7.12E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-2</td><td>3.465</td><td>-111.82</td><td>5349.7</td><td>8.50</td><td></td><td>8.13</td><td>7.81E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-3</td><td>3.568</td><td>173.68</td><td>5508.7</td><td>8.50</td><td></td><td>4.34</td><td>1.33E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-4</td><td>4.366</td><td>32.24</td><td>6740.8</td><td>8.50</td><td></td><td>8.09</td><td>9.05E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-5</td><td>4.55</td><td>48.36</td><td>7024.9</td><td>8.50</td><td></td><td>8.18</td><td>9.32E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-6</td><td>4.657</td><td>125.90</td><td>7190.1</td><td>8.50</td><td></td><td>6.08</td><td>5.83E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-7</td><td>5.479</td><td>-14.74</td><td>8459.2</td><td>8.50</td><td></td><td>7.69</td><td>9.52E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-8</td><td>7.031</td><td>-168.71</td><td>10855.3</td><td>8.50</td><td></td><td>5.21</td><td>6.75E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400-9</td><td>8.283</td><td>29.32</td><td>12788.3</td><td>8.50</td><td></td><td>6.83</td><td>9.87E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>BD-22 4400 10</td><td>8.348</td><td>-115.62</td><td>12888.7</td><td>8.50</td><td></td><td>7.69</td><td>9.99E-01</td><td>Not likely</td><td>20/07/07</td></tr><tr><td>PDS469-1</td><td>1.686</td><td>-119.89</td><td>1701.8</td><td>10.35</td><td></td><td>7.54</td><td>1.39E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-3</td><td>3.389</td><td>46.97</td><td>3420.8</td><td>10.35</td><td></td><td>7.72</td><td>4.79E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-4</td><td>4.165</td><td>-168.11</td><td>4204.1</td><td>10.35</td><td></td><td>7.72</td><td>6.27E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-5</td><td>4.262</td><td>80.02</td><td>4302.0</td><td>10.35</td><td></td><td>7.37</td><td>5.87E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-6</td><td>5.566</td><td>-172.73</td><td>5618.2</td><td>10.35</td><td></td><td>7.87</td><td>8.45E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-7</td><td>6.416</td><td>34.68</td><td>6476.2</td><td>10.35</td><td></td><td>7.53</td><td>8.84E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-8</td><td>7.192</td><td>52.59</td><td>7259.5</td><td>10.35</td><td></td><td>5.61</td><td>6.31E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-9</td><td>7.744</td><td>-25.95</td><td>7816.7</td><td>10.35</td><td></td><td>3.20</td><td>2.19E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>PDS469-10</td><td>8.282</td><td>-174.35</td><td>8359.7</td><td>10.35</td><td></td><td>6.83</td><td>9.22E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-1</td><td>2.331</td><td>38.83</td><td>3129.3</td><td>8.99</td><td></td><td>7.42</td><td>4.86E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-2</td><td>2.406</td><td>-21.90</td><td>3230.0</td><td>8.99</td><td></td><td>7.76</td><td>5.64E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-3</td><td>3.049</td><td>64.30</td><td>4093.2</td><td>8.99</td><td></td><td>5.17</td><td>2.95E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-4</td><td>4.231</td><td>-43.95</td><td>5680.0</td><td>8.99</td><td></td><td>3.07</td><td>1.43E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-5</td><td>4.545</td><td>119.78</td><td>6101.5</td><td>8.99</td><td></td><td>7.66</td><td>9.41E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-6</td><td>6.452</td><td>116.41</td><td>8661.6</td><td>8.99</td><td></td><td>7.59</td><td>9.96E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-7</td><td>7.231</td><td>-155.68</td><td>9707.3</td><td>8.99</td><td></td><td>6.56</td><td>9.85E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-8</td><td>8.386</td><td>-39.21</td><td>11257.9</td><td>8.99</td><td></td><td>6.38</td><td>9.94E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133-9</td><td>8.525</td><td>51.49</td><td>11444.5</td><td>8.99</td><td></td><td>6.79</td><td>9.99E-01</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 165133 10</td><td>8.743</td><td>128.22</td><td>11737.1</td><td>8.99</td><td></td><td>7.55</td><td>1.00E+00</td><td>Not likely</td><td>02/08/07</td></tr><tr><td>HD 312787-1</td><td>1.736</td><td>38.43</td><td>353.7</td><td>13.33</td><td></td><td>6.69</td><td>7.08E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-2</td><td>3.598</td><td>25.64</td><td>733.1</td><td>13.33</td><td></td><td>5.58</td><td>9.82E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-3</td><td>6.76</td><td>-157.36</td><td>1377.3</td><td>13.33</td><td></td><td>6.88</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-4</td><td>7.657</td><td>-75.01</td><td>1560.1</td><td>13.33</td><td></td><td>7.57</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-5</td><td>8.017</td><td>-79.23</td><td>1633.5</td><td>13.33</td><td></td><td>7.08</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-6</td><td>8.532</td><td>107.16</td><td>1738.4</td><td>13.33</td><td></td><td>7.00</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-7</td><td>8.63</td><td>-161.09</td><td>1758.4</td><td>13.33</td><td></td><td>5.67</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HD 312787-8</td><td>9.499</td><td>146.68</td><td>1935.4</td><td>13.33</td><td></td><td>7.29</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr></tbody></table>
<table><caption>**Table 9**
(Continued)</caption><thead><tr><th>Companion</th><th>Ang. Sep. (arcsec)</th><th>PA (deg)</th><th>Linear Sep. (au)</th><th>K Sample Star</th><th>ΔK</th><th>P</th><th>Likelihood</th><th>Date Observed</th></tr></thead><tbody><tr><td>HD 312787-9</td><td>9.693</td><td>-41.79</td><td>1974.9</td><td>13.33</td><td>7.21</td><td>1.00E+00</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>MWC 922-5</td><td>7.532</td><td>-138.55</td><td>12804.4</td><td>5.70</td><td>5.13</td><td>1.53E-01</td><td>Not likely</td><td>25/07/07</td></tr><tr><td>MWC 922-6</td><td>7.816</td><td>17.73</td><td>13287.2</td><td>5.70</td><td>5.40</td><td>2.02E-01</td><td>Not likely</td><td>25/07/07</td></tr><tr><td>VV Ser-1</td><td>7.47</td><td>249.60</td><td>3053.1</td><td>6.32</td><td>7.10</td><td>1.05E-01</td><td>Not likely</td><td>13/10/05</td></tr><tr><td>AS 310-2</td><td>2.231</td><td>-119.34</td><td>5491.0</td><td>11.71</td><td>3.12</td><td>1.18E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-3</td><td>3.731</td><td>-126.38</td><td>9182.9</td><td>11.71</td><td>2.93</td><td>2.72E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-4</td><td>3.852</td><td>-78.13</td><td>9480.7</td><td>11.71</td><td>3.67</td><td>3.91E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-6</td><td>4.908</td><td>1.04</td><td>12079.7</td><td>11.71</td><td>2.61</td><td>3.69E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-7</td><td>4.931</td><td>-61.57</td><td>12136.4</td><td>11.71</td><td>6.30</td><td>9.26E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-8</td><td>5.024</td><td>6.29</td><td>12365.2</td><td>11.71</td><td>4.29</td><td>6.80E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-9</td><td>5.614</td><td>139.14</td><td>13817.4</td><td>11.71</td><td>3.40</td><td>6.01E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-10</td><td>6.327</td><td>-145.13</td><td>15572.2</td><td>11.71</td><td>3.89</td><td>7.76E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-11</td><td>7.575</td><td>-56.91</td><td>18643.9</td><td>11.71</td><td>4.10</td><td>9.07E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>AS 310-12</td><td>9.51</td><td>-141.72</td><td>23406.3</td><td>11.71</td><td>3.12</td><td>8.98E-01</td><td>Not likely</td><td>09/04/07</td></tr><tr><td>BD-13 5061-1</td><td>4.379</td><td>-139.49</td><td>7480.4</td><td>7.36</td><td>7.93</td><td>3.45E-01</td><td>Not likely</td><td>25/07/07</td></tr><tr><td>BD-13 5061-2</td><td>5.517</td><td>145.50</td><td>9424.3</td><td>7.36</td><td>8.32</td><td>5.64E-01</td><td>Not likely</td><td>25/07/07</td></tr><tr><td>PDS530-4</td><td>3.41</td><td>-50.46</td><td>3410.0</td><td>9.14</td><td>6.31</td><td>1.09E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-5</td><td>3.679</td><td>26.82</td><td>3679.0</td><td>9.14</td><td>7.40</td><td>2.39E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-6</td><td>3.803</td><td>-15.78</td><td>3803.0</td><td>9.14</td><td>7.18</td><td>2.26E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-7</td><td>4.636</td><td>-37.61</td><td>4636.0</td><td>9.14</td><td>6.08</td><td>1.67E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-8</td><td>5.593</td><td>142.36</td><td>5593.0</td><td>9.14</td><td>6.29</td><td>2.65E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-9</td><td>5.76</td><td>17.51</td><td>5760.0</td><td>9.14</td><td>7.06</td><td>4.21E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-10</td><td>6.576</td><td>1.32</td><td>6576.0</td><td>9.14</td><td>6.55</td><td>4.01E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>PDS530-11</td><td>6.593</td><td>-4.40</td><td>6593.0</td><td>9.14</td><td>5.71</td><td>2.41E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>MWC 953-4</td><td>4.327</td><td>7.26</td><td>9305.4</td><td>7.77</td><td>4.67</td><td>1.48E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>MWC 953-5</td><td>4.442</td><td>-156.21</td><td>9552.7</td><td>7.77</td><td>6.73</td><td>5.34E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>MWC 953-6</td><td>5.414</td><td>102.81</td><td>11643.0</td><td>7.77</td><td>4.33</td><td>1.75E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>MWC 953-7</td><td>6.543</td><td>-115.51</td><td>14071.0</td><td>7.77</td><td>5.99</td><td>6.45E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>MWC 953-8</td><td>7.646</td><td>109.84</td><td>16443.0</td><td>7.77</td><td>7.25</td><td>9.55E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>MWC 953-9</td><td>8.462</td><td>-154.11</td><td>18197.8</td><td>7.77</td><td>6.70</td><td>9.34E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>AS 321-1</td><td>2.708</td><td>54.03</td><td>839.5</td><td>9.06</td><td>7.59</td><td>2.46E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>AS 321-2</td><td>4.406</td><td>30.80</td><td>1365.9</td><td>9.06</td><td>5.79</td><td>2.25E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>AS 321-3</td><td>5.541</td><td>-17.77</td><td>1717.7</td><td>9.06</td><td>8.02</td><td>7.70E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>AS 321-5</td><td>7.497</td><td>-57.91</td><td>2324.1</td><td>9.06</td><td>6.71</td><td>7.32E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>AS 321-6</td><td>8.308</td><td>8.31</td><td>2575.5</td><td>9.06</td><td>7.55</td><td>9.25E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>AS 321-7</td><td>10.178</td><td>-51.40</td><td>3155.2</td><td>9.06</td><td>7.83</td><td>9.89E-01</td><td>Not likely</td><td>04/04/07</td></tr><tr><td>HD 179218-2</td><td>3.67</td><td>339.30</td><td>954.5</td><td>6.00</td><td>8.70</td><td>1.45E-01</td><td>Not likely</td><td>13/10/05</td></tr><tr><td>WW Vul-1</td><td>7.29</td><td>239.70</td><td>3535.4</td><td>7.28</td><td>6.50</td><td>2.79E-01</td><td>Not likely</td><td>25/09/05</td></tr><tr><td>HBC 687-1</td><td>3.303</td><td>-49.59</td><td>990.9</td><td>9.76</td><td>6.17</td><td>1.86E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-2</td><td>4.258</td><td>142.24</td><td>1277.4</td><td>9.76</td><td>7.18</td><td>4.59E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-3</td><td>4.321</td><td>-158.29</td><td>1296.3</td><td>9.76</td><td>7.14</td><td>4.63E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-4</td><td>4.937</td><td>-22.60</td><td>1481.1</td><td>9.76</td><td>6.92</td><td>5.13E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-5</td><td>5.97</td><td>-96.48</td><td>1791.0</td><td>9.76</td><td>4.77</td><td>2.14E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-6</td><td>6.754</td><td>-80.05</td><td>2026.2</td><td>9.76</td><td>5.90</td><td>5.17E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-7</td><td>6.905</td><td>-27.37</td><td>2071.5</td><td>9.76</td><td>8.46</td><td>9.53E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-8</td><td>6.958</td><td>-61.79</td><td>2087.4</td><td>9.76</td><td>6.65</td><td>7.04E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-9</td><td>8.273</td><td>93.73</td><td>2481.9</td><td>9.76</td><td>6.79</td><td>8.45E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>HBC 687-10</td><td>10.176</td><td>43.85</td><td>3052.8</td><td>9.76</td><td>6.51</td><td>9.10E-01</td><td>Not likely</td><td>13/07/07</td></tr><tr><td>V409 Vul-1</td><td>5.582</td><td>53.64</td><td>13054.3</td><td>9.43</td><td>5.24</td><td>3.62E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>V409 Vul-2</td><td>8.211</td><td>117.67</td><td>19202.5</td><td>9.43</td><td>3.61</td><td>2.51E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>HD 338916-1</td><td>4.523</td><td>-149.04</td><td>9819.8</td><td>8.71</td><td>6.80</td><td>3.97E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>HD 338916-2</td><td>5.09</td><td>15.20</td><td>11050.8</td><td>8.71</td><td>9.10</td><td>8.75E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>HD 338916-3</td><td>6.461</td><td>143.16</td><td>14027.4</td><td>8.71</td><td>7.29</td><td>7.42E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>HD 338916-4</td><td>7.343</td><td>111.17</td><td>15942.2</td><td>8.71</td><td>8.90</td><td>9.81E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>HD 338916-5</td><td>8.427</td><td>121.89</td><td>18295.7</td><td>8.71</td><td>9.22</td><td>9.98E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>HD 338916-6</td><td>9.971</td><td>34.54</td><td>21647.9</td><td>8.71</td><td>7.79</td><td>9.85E-01</td><td>Not likely</td><td>25/06/07</td></tr><tr><td>LkHA 224-2</td><td>9.164</td><td>-28.98</td><td>8980.7</td><td>6.35</td><td>7.48</td><td>2.23E-01</td><td>Not likely</td><td>08/04/07</td></tr><tr><td>LkHA 224-3</td><td>8.964</td><td>-27.34</td><td>8784.7</td><td>6.35</td><td>7.06</td><td>1.61E-01</td><td>Not likely</td><td>01/01/04</td></tr><tr><td>AS 443-1</td><td>3.389</td><td>25.26</td><td>2889.2</td><td>8.24</td><td>6.81</td><td>1.01E-01</td><td>Not likely</td><td>12/04/07</td></tr><tr><td>AS 443-2</td><td>3.913</td><td>-104.99</td><td>3335.9</td><td>8.24</td><td>6.47</td><td>1.06E-01</td><td>Not likely</td><td>12/04/07</td></tr><tr><td>AS 443-3</td><td>4.481</td><td>46.80</td><td>3820.1</td><td>8.24</td><td>8.86</td><td>4.77E-01</td><td>Not likely</td><td>12/04/07</td></tr></tbody></table>
<table><caption>**Table 9**
(Continued)</caption><thead><tr><th>Companion</th><th>Ang. Sep. (arcsec)</th><th>PA (deg)</th><th>Linear Sep. (au)</th><th>K Sample Star</th><th>ΔK</th><th>P</th><th>Likelihood</th><th>Date Observed</th></tr></thead><tbody><tr><td>AS 443-4</td><td>6.93</td><td>141.08</td><td>5907.9</td><td>8.24</td><td>8.41</td><td>7.03E-01</td><td>Not likely</td><td>12/04/07</td></tr><tr><td>AS 443-5</td><td>8.901</td><td>-113.52</td><td>7588.2</td><td>8.24</td><td>8.92</td><td>9.29E-01</td><td>Not likely</td><td>12/04/07</td></tr><tr><td>LkHA 147-2</td><td>2.2</td><td>1.30</td><td>5174.0</td><td>9.48</td><td>8.40</td><td>1.76E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 167-2</td><td>4.24</td><td>85.90</td><td>4867.4</td><td>8.12</td><td>8.40</td><td>2.82E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 167-3</td><td>8.17</td><td>151.10</td><td>9378.9</td><td>8.12</td><td>8.10</td><td>6.48E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 168-2</td><td>9.44</td><td>222.10</td><td>7907.5</td><td>8.34</td><td>8.10</td><td>7.84E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 170-2</td><td>1.69</td><td>309.80</td><td>1291.1</td><td>13.24</td><td>6.10</td><td>1.55E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 170-3</td><td>4.87</td><td>187.30</td><td>3720.4</td><td>13.24</td><td>3.80</td><td>4.27E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 170-4</td><td>5.11</td><td>349.10</td><td>3903.7</td><td>13.24</td><td>4.39</td><td>5.63E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 170-5</td><td>6.07</td><td>131.80</td><td>4637.1</td><td>13.24</td><td>3.00</td><td>4.31E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 170-6</td><td>6.84</td><td>268.50</td><td>5225.4</td><td>13.24</td><td>4.00</td><td>7.06E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>LkHA 324-2</td><td>5.36</td><td>325.50</td><td>3335.4</td><td>9.57</td><td>5.88</td><td>2.23E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>HD 235495-3</td><td>5.18</td><td>323.90</td><td>2670.7</td><td>6.97</td><td>7.90</td><td>1.72E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>HD 235495-4</td><td>6.36</td><td>112.10</td><td>3279.0</td><td>6.97</td><td>8.10</td><td>2.78E-01</td><td>Not likely</td><td>20/09/05</td></tr><tr><td>V645 Cyg-2</td><td>6.616</td><td>27.38</td><td>23156.0</td><td>6.85</td><td>8.45</td><td>2.95E-01</td><td>Not likely</td><td>01/05/07</td></tr><tr><td>BH Cep-3</td><td>9.519</td><td>-38.09</td><td>3118.3</td><td>8.31</td><td>8.81</td><td>4.69E-01</td><td>Not likely</td><td>01/05/07</td></tr><tr><td>MWC 1055-1</td><td>2.719</td><td>167.35</td><td>17252.5</td><td>8.60</td><td>8.23</td><td>1.49E-01</td><td>Not likely</td><td>18/06/07</td></tr><tr><td>MWC 1055-2</td><td>4.704</td><td>-142.70</td><td>29847.7</td><td>8.60</td><td>7.23</td><td>2.24E-01</td><td>Not likely</td><td>18/06/07</td></tr><tr><td>BD+57 2615-1</td><td>6.66</td><td>310.10</td><td>10213.2</td><td>8.99</td><td>7.90</td><td>5.82E-01</td><td>Not likely</td><td>13/09/05</td></tr><tr><td>BD+57 2615-2</td><td>7.41</td><td>228.40</td><td>11363.3</td><td>8.99</td><td>5.90</td><td>2.41E-01</td><td>Not likely</td><td>13/09/05</td></tr><tr><td>HD 216629-3</td><td>8.04</td><td>10.90</td><td>6521.7</td><td>7.10</td><td>6.60</td><td>1.09E-01</td><td>Not likely</td><td>25/09/05</td></tr><tr><td>V374 Cep-1</td><td>6.17</td><td>29.20</td><td>5187.9</td><td>7.09</td><td>8.30</td><td>1.67E-01</td><td>Not likely</td><td>14/10/05</td></tr></tbody></table>

(This table is available in machine-readable form.)
<table><caption>**Table 10**

Proper-motion Information for all Sample Stars with Multiepoch Data</caption><thead><tr><th>Sample Star<br>Name<br>(Reference)</th><th>PM ra<br>(mas yr<sup>-1</sup>)</th><th>PM dec<br>(mas yr<sup>-1</sup>)</th><th>DPM ra</th><th>DPM dec</th></tr></thead><tbody><tr><td>HIP 592 (1)</td><td>2.63</td><td>-2.28</td><td>0.01</td><td>0.01</td></tr><tr><td>VX Cas (1)</td><td>3.32</td><td>-2.65</td><td>0.02</td><td>0.02</td></tr><tr><td>LkHA 201 (1)</td><td>-1.49</td><td>-1.40</td><td>0.01</td><td>0.02</td></tr><tr><td>XY Per (1)</td><td>8.34</td><td>-7.62</td><td>0.03</td><td>0.03</td></tr><tr><td>V892 Tau (1)</td><td>3.52</td><td>-28.81</td><td>0.10</td><td>0.07</td></tr><tr><td>CO Ori (1)</td><td>2.22</td><td>-2.13</td><td>0.03</td><td>0.02</td></tr><tr><td>HK Ori (3)</td><td>-2.20</td><td>1.10</td><td>2.20</td><td>2.10</td></tr><tr><td>CQ Tau (1)</td><td>2.99</td><td>-26.36</td><td>0.06</td><td>0.04</td></tr><tr><td>BD-06 1253 (1)</td><td>-0.67</td><td>-2.41</td><td>0.11</td><td>0.08</td></tr><tr><td>HD 37258 (1)</td><td>1.75</td><td>-0.72</td><td>0.03</td><td>0.02</td></tr><tr><td>BF Ori (1)</td><td>0.87</td><td>0.65</td><td>0.03</td><td>0.02</td></tr><tr><td>HD 259431 (1)</td><td>-2.41</td><td>-2.91</td><td>0.03</td><td>0.03</td></tr><tr><td>S Mon (2)</td><td>-2.61</td><td>-1.61</td><td>0.56</td><td>0.39</td></tr><tr><td>HD 52721 (2)</td><td>-5.08</td><td>4.59</td><td>2.23</td><td>1.93</td></tr><tr><td>Z CMa (2)</td><td>-4.44</td><td>2.00</td><td>2.53</td><td>2.07</td></tr><tr><td>NX Pup (2)</td><td>-7.88</td><td>16.00</td><td>2.21</td><td>2.25</td></tr><tr><td>HD 76534 (1)</td><td>-5.55</td><td>5.47</td><td>0.03</td><td>0.03</td></tr><tr><td>HD 97300 (1)</td><td>-21.50</td><td>-0.17</td><td>0.03</td><td>0.04</td></tr><tr><td>HD 141569 (1)</td><td>-17.42</td><td>-19.11</td><td>0.03</td><td>0.03</td></tr><tr><td>HD 144432 (1)</td><td>-12.84</td><td>-24.24</td><td>0.03</td><td>0.02</td></tr><tr><td>V856 Sco (1)</td><td>-9.07</td><td>-23.03</td><td>0.03</td><td>0.02</td></tr><tr><td>PDS415 (1)</td><td>-11.86</td><td>-20.04</td><td>0.02</td><td>0.02</td></tr><tr><td>HD 150193 (1)</td><td>-4.94</td><td>-19.05</td><td>0.02</td><td>0.02</td></tr><tr><td>KK Oph (1)</td><td>0.47</td><td>-19.69</td><td>0.15</td><td>0.10</td></tr><tr><td>PDS453 (1)</td><td>-11.59</td><td>-27.92</td><td>0.57</td><td>0.41</td></tr><tr><td>PDS469 (1)</td><td>0.48</td><td>-0.48</td><td>0.05</td><td>0.04</td></tr><tr><td>MWC 297 (1)</td><td>1.51</td><td>-8.55</td><td>0.03</td><td>0.03</td></tr><tr><td>AS 310 (1)</td><td>-0.15</td><td>-2.97</td><td>0.01</td><td>0.01</td></tr><tr><td>HD 179218 (1)</td><td>5.34</td><td>-21.09</td><td>0.03</td><td>0.03</td></tr><tr><td>V1685 Cyg (1)</td><td>-2.27</td><td>-5.87</td><td>0.02</td><td>0.02</td></tr><tr><td>LkHA 224 (1)</td><td>-1.90</td><td>-4.47</td><td>0.17</td><td>0.20</td></tr><tr><td>HBC 694 (1)</td><td>-1.28</td><td>-5.35</td><td>0.34</td><td>0.33</td></tr><tr><td>MWC 349 (1)</td><td>-3.14</td><td>-4.44</td><td>0.07</td><td>0.08</td></tr><tr><td>AS 442 (1)</td><td>-1.66</td><td>-1.90</td><td>0.01</td><td>0.01</td></tr><tr><td>LkHA 147 (1)</td><td>-0.83</td><td>-2.72</td><td>0.01</td><td>0.01</td></tr><tr><td>HD 200775 (1)</td><td>7.60</td><td>-2.82</td><td>0.05</td><td>0.05</td></tr><tr><td>LkHA 324 (1)</td><td>1.05</td><td>-3.69</td><td>0.01</td><td>0.01</td></tr><tr><td>HD 203024 (3)</td><td>10.50</td><td>-2.20</td><td>1.40</td><td>1.40</td></tr><tr><td>LkHA 234 (1)</td><td>-1.68</td><td>-3.44</td><td>0.02</td><td>0.02</td></tr><tr><td>BD+46 3471 (1)</td><td>-3.19</td><td>-3.26</td><td>0.01</td><td>0.01</td></tr><tr><td>BH Cep (1)</td><td>9.74</td><td>-1.82</td><td>0.01</td><td>0.01</td></tr><tr><td>HD 216629 (1)</td><td>-0.68</td><td>-2.07</td><td>0.02</td><td>0.01</td></tr><tr><td>MWC 1080 (1)</td><td>-3.96</td><td>-2.05</td><td>0.03</td><td>0.03</td></tr></tbody></table>

**References.** (1) Gaia Collaboration et al. (2022); (2) van Leeuwen (2007); (3) Ducourant et al. (2005); (4) Zacharias et al. (2003); and (5) Hog et al. (2000).
<table><caption>Table 11
Astrometry and Photometry Data for the 1995 Survey</caption><thead><tr><th>Name</th><th></th><th>Sep (")</th><th>PA (°)</th><th>ΔU</th><th>ΔB</th><th>ΔV</th><th>ΔR</th><th>ΔI</th><th>ΔJ</th><th>ΔH</th><th>ΔK</th><th>ΔL</th><th>ΔM</th><th>Date Obs.</th></tr></thead><tbody><tr><td>CO Ori</td><td></td><td>2.04</td><td>276</td><td></td><td></td><td></td><td></td><td>3.2</td><td></td><td>3.17</td><td>3.08</td><td>3.04</td><td></td><td>1993 Dec</td></tr><tr><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>1996 Dec</td></tr><tr><td>HK Ori</td><td>AB</td><td>0.34<br>0.37</td><td>47.9<br>220<br>230</td><td></td><td></td><td>0.22:</td><td>0.24:</td><td></td><td></td><td>0.43</td><td>1.15</td><td>2.19</td><td></td><td>1993 Dec</td></tr><tr><td></td><td>AC</td><td>3.98</td><td>354.4</td><td></td><td></td><td></td><td></td><td></td><td></td><td>6.14</td><td>6.66</td><td>7.36</td><td></td><td>1996 Mar<br>1997 Oct<br>1993 Dec</td></tr><tr><td>V380 Ori</td><td></td><td>0.14<br>0.16</td><td>205<br>22</td><td></td><td></td><td></td><td>0.10:</td><td></td><td></td><td>0.11</td><td>0.94</td><td>1.36</td><td></td><td>1993 Dec<br>1996 Mar</td></tr><tr><td>V586 Ori</td><td></td><td>0.98<br>0.99</td><td>29.7<br>31.6</td><td></td><td></td><td>3.23</td><td>2.78</td><td>2.39</td><td></td><td>1.76</td><td>1.71</td><td>2.34</td><td></td><td>1996 Sep<br>1993 Dec</td></tr><tr><td>BF Ori</td><td></td><td>2.03<br>2.03</td><td>46.2<br>48</td><td></td><td></td><td>6.63</td><td>5.94</td><td>4.33</td><td></td><td>2.7<br>4.20<sup>g</sup></td><td>2.97<br>3.60<sup>g</sup></td><td></td><td></td><td>1996 Sep<br>1993 Dec<br>1994 Jan</td></tr><tr><td>MWC 147</td><td></td><td>3.11<br>3.12</td><td>344.4<br>346.5</td><td></td><td></td><td>7.22</td><td>6.82</td><td>6.02</td><td></td><td>4.81</td><td>5.05</td><td>5.67</td><td></td><td>1996 Sep, 1997 Jan<br>1993 Dec</td></tr><tr><td>S Mon</td><td></td><td>2.91</td><td>112.8</td><td></td><td></td><td></td><td></td><td></td><td></td><td>2.62</td><td>2.29</td><td>3.46</td><td></td><td>1995 Mar</td></tr><tr><td>GU CMa</td><td></td><td>0.65<br>0.66</td><td>194.4<br>196.2</td><td></td><td></td><td></td><td>1.30:</td><td>1.40:</td><td></td><td>1.1<br>1.2</td><td>1.27<br>1.2</td><td>1.41<br>1.5</td><td></td><td>1996 Dec<br>1993 Dec<br>1996 Mar</td></tr><tr><td>MWC 166</td><td></td><td>0.64<br>0.65<br>0.65</td><td>296.9<br>299.2<br>297.3</td><td></td><td></td><td></td><td></td><td>1.43<br>1.12</td><td>1.61<br>1.15</td><td>1.64<br>1.7<br>1.8</td><td>1.4<br>1.73<br>2.14</td><td>1.77<br>2.3</td><td></td><td>1996 Dec<br>1993 Dec<br>1996 Sep<br>1993 Dec<br>1996 Mar</td></tr><tr><td>NX Pup</td><td>AB<br>AC</td><td>0.13<br>6.98</td><td>62.4<br>45.3</td><td></td><td></td><td></td><td></td><td></td><td>1.15</td><td>1.2</td><td>1.2</td><td>1.13<sup>g</sup></td><td></td><td>1993 Dec<br>1993 Dec</td></tr><tr><td>Hen 3-225</td><td></td><td>2.06<br>2.07<br>2.09</td><td>302.9<br>305<br>303</td><td></td><td></td><td></td><td></td><td></td><td></td><td>1.14<br>0.85<br>1.17<br>1.36<br>1.13<sup>g</sup></td><td>1.15<br>0.9<br>1.3<br>1.49</td><td>1.16<br>0.95<br>1.46</td><td></td><td>1996 Dec<br>1993 Dec<br>1995 Mar<br>Apr 1996<br>1994 Jan<br>1996 May</td></tr><tr><td></td><td></td><td></td><td></td><td>1.01<br>1.15</td><td>1</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>RCW 34</td><td>AB<br>AC<br>AD<br>AE<br>AF</td><td>1.55<br>2.89<br>2.21<br>5.26<br>4.6</td><td>193<br>165.6<br>292.9<br>65.9<br>92.1</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>1993 Dec<br>1993 Dec<br>1993 Dec<br>1993 Dec<br>1993 Dec</td></tr><tr><td>Hen 3-692</td><td></td><td>3.06<br>3.07</td><td>226.3<br>227.8</td><td></td><td></td><td></td><td></td><td></td><td></td><td>6.63<br>5.98</td><td>6.38<br>6.2</td><td>7<br>6.47</td><td></td><td>1996 Dec<br>1995 Mar</td></tr><tr><td>Hen 3-1141</td><td></td><td>1.45<br>1.45<br>1.46</td><td>4.4<br>3<br>2.6</td><td></td><td></td><td></td><td></td><td></td><td></td><td>2.13<br>2.2</td><td>2.05<br>2.1</td><td>2.49<br>2.55</td><td></td><td>1995 Mar<br>1996 May<br>1996 May<br>1995 Aug</td></tr><tr><td>V856 Sco</td><td></td><td>1.45<br>1.46<br>2.99</td><td>111.2<br>110.8<br>3.36</td><td></td><td></td><td></td><td></td><td>4.2</td><td>3.65</td><td>2.86</td><td></td><td></td><td></td><td>1994 Jul</td></tr><tr><td>3.04</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td>1993 Dec</td></tr></tbody></table>