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Table A.1

Parameters for young systems with companions/planets.

With Gap
Separation Gap Size
Name Mass ratio (AU) Method1 Eccentricity (AU) Method2 Reference
CoKu Tau/4 0.85 7.8 Image – 12.6 SED Fit 1, 2
T Cha – 6.7 Image – 12 Mid-IR Int 3, 4
V4046 Sgr 0.96 0.04a Spec, D <0.01 29 MM Int 5, 6
AK Sco 0.987 0.14 Spec, D 0.47 0.4 SED Fit 7
GG Tau A 0.9 35b Image 0.3 ± 0.2 180 MM Int 8, 9, 10
CS Cha – ~3.6c Spec, S – 43 SED Fit 11, 12, 13
HD 98800 B 0.83 0.98 Spec, D 0.78 3.5 SED Fit 14, 15, 16
DQ Tau 0.97 0.13 Spec, D 0.556 ≲0.4 SED Fit 17, 18
162814–2427 0.92 0.28 Spec, D 0.48 0.4 SED Fit 19, 20
162819–2423S ≳0.26 0.1 Spec, S 0.41 0.24 SED Fit 19, 20
FL Cha – 2.4/6 Image – 8.3 SED Fit 21
LkHα 330 – 10–13 Image – 68 MM Int 22, 23
T21 – 22.4 Image – 146.7 SED Fit 24, 25
DF Tau 0.75 12.5d Image 0.51 17 SED Fit 26, 27, 28
MHO 3 0.5 4.5 Image – 6.9 SED Fit 29, 30
CHX22 – 39.5 Image – 37.1 SED Fit 24, 30
ST 34 ~1 ~0.2e Spec, D – 0.7 SED Fit 31, 32
Sz Cha ~0.07f Spec, S – 29.5 SED Fit 33, 30
LkCa 15 ~0.006 ~15.9 Image – 50 MM Int 34, 35
Without Gap
Separation R in
Name Mass ratio (AU) Method1 Eccentricity (AU) Method2 Reference
HD 104237 0.64 0.22g Spec, S 0.66 0.5 SED Fit 36, 37, 38
UZ Tau E 0.30 0.124 Spec, D 0.33 ~0.02 R sub 39, 40
DP Tau 0.74 15.5 Image – ~0.01 R sub 29, 41
TOs without known companions and their detection limit
Separation Gap Size
Name Mass ratio (Detection limit, AU) Method1 Eccentricity (AU) Method2 Reference
GM Aur 0.01 5.7 Image – 28 MM Int 29, 22
UX Tau A 0.01 6 Image – 25 MM Int 29, 22
RY Tau 0.01 2.9 Image – 27.6 SED Fit 29, 30
DM Tau 0.02 5.7 Image – 19 MM Int 29, 22
GK Tau 0.02 5.6 Image – 9.7 SED Fit 29, 22
HK Tau 0.02 6.1 Image – 16.1 SED Fit 29, 30
RX J1604.3–2130 0.02 3 Image – 72 MM Int 42, 43
IP Tau 0.03 5.5 Image – 12.6 SED Fit 29, 30
RX J1633.9–2442 ~0.02 2.4 Image – ~25 MMT Int 44
TW Hya – 2.3 Image – 4 SED Fit 45, 46

Notes. Column 3: if it is not specified, the separation is projected distance between two stellar components when the binary is detected with imaging, and is minimum semi-major of the orbit when it is detected with spectroscopy. Column 4: the methods with which the binaries are detected: Image for imaging, Spec for spectroscopy, D for double lines, and S for single line. Column 4: the methods with which the gap sizes are estimated, including fitting the SED (SED Fit), mid-infrared interferometry (Mid-IR Int), millimeter interferometry (MM Int). For the full disks (UZ Tau E and DP Tau), the inner radius of the disks are determined by the evaporation of dust (Rsub).

(a)

sum of semi-majors of the orbits for the two stellar components with an assumption of inclination 35°;

(b,d)

the orbital semi-major from fitting the orbit.

c

roughly estimated using the orbit period 2482 day;

(e)

roughly estimated assuming the system is edge-on;

(f)

roughly estimated using the orbit period of 5 days;

(g)

the semi-major of the orbit assuming an inclination 17°.

Reference. 1). Ireland & Kraus (2008); 2). Nagel et al. (2010); 3). Huélamo et al. (2011); 4). Olofsson et al. (2013); 5). Stempels & Gahm (2004); 6). Rosenfeld et al. (2013); 7). Alencar et al. (2003); 8). White et al. (1999); 9). McCabe et al. (2002); 10). Guilloteau et al. (1999); 11). Guenther et al. (2007); 12). Espaillat et al. (2007); 13). Nagel et al. (2012); 14). Torres et al. (1995); 15). Boden et al. (2005); 16). Andrews et al. (2010); 17). Mathieu et al. (1997); 18). Boden et al. (2009); 19). Mathieu et al. (1989); 20). Jensen & Mathieu (1997); 21). Cieza et al. (2013); 22). Andrews et al. (2011); 23). Isella et al. (2013); 24). Lafrenière et al. (2008); 25). Kim et al. (2009); 26). White & Ghez (2001); 27). Marsh & Mahoney (1993); 28). Tamazian et al. (2002); 29). Kraus et al. (2011) 30). Kim et al. (2013); 31). White & Hillenbrand (2005); 32). Hartmann et al. (2005); 33). Reipurth et al. (2002); 34). Kraus & Ireland (2012); 35). Piétu et al. (2006); 36). Böhm et al. (2004); 37). Tatulli et al. (2007); 38). Garcia et al. (2013); 39). Jensen et al. (2007); 40). Jensen et al. (1996); 41). Furlan et al. (2006); 42). Kraus et al. (2008); 43). Mathews et al. (2012); 44). Cieza et al. (2012); 45). Calvet et al. (2002); 46). Brandeker et al. (2003).

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