Table 1: Properties of planets in multiple systems, of their host stars and their companions: planet $m \sin i$, period, semimajor axis, eccentricity, radial velocity semi-amplitude, metallicity and mass of the planet host (from B06); projected separation, semimajor axis and eccentricity (when available) and mass of the companions, and critical semiaxis for dynamical stability of planets. The asterisks in the last column mark systems discussed individually in Appendix C.

Object		 Object $m \sin i$ P ap ep Kp [Fe/H] $M_{\rm star}$ $\rho$ $a_{\rm bin}$ $e_{\rm bin}$ $M_{\rm comp}$ $a_{\rm crit}$ Rem.
HD other $M_{\rm J}$ d AU   m/s   $M_{\odot}$ AU AU   $M_{\odot}$ AU  

142		   1.31 350.3 1.045 0.26 33.9 0.100 1.24 138     0.56 35  
1237 GJ 3021 3.37 133.71 0.495 0.511 167.0 0.120 0.90 70     0.13 21  
3651 54 Psc 0.227 62.206 0.296 0.618 16.0 0.164 0.89 480     0.06 151 *
9826 $\upsilon$ And 0.687 4.617 0.0595 0.023 69.8 0.120 1.32 750     0.19 223  
    1.98 241.23 0.832 0.262 55.6 0.120 1.32 750     0.19 223  
    3.95 1290.1 2.54 0.258 63.4 0.153 1.32 750     0.19 223  
11964   0.61 2110.0 3.34 0.06 9.0 0.122 1.12 1379     0.67 325  
13445 GL 86 3.91 15.7649 0.113 0.0416 376.7 -0.268 0.77   18.4 0.40 0.49 3.1 a
16141 79 Cet 0.26 75.523 0.363 0.252 11.99 0.170 1.12 223     0.29 62  
19994 94 Cet 1.69 535.7 1.428 0.30 36.2 0.186 1.35   120 0.26 0.35 31 *
20782   1.78 585.86 1.364 0.925 115.0 -0.051 0.98 9080     0.84 1940  
27442 $\epsilon $ Ret 1.56 428.1 1.27 0.06 32.2 0.420 1.49 251     0.60 62 a
38529   0.852 14.3093 0.1313 0.248 56.8 0.445 1.47 12000     0.50 3190 *
    13.2 2165.0 3.74 0.3506 170.3 0.445 1.47 12000     0.50 3190  
40979   3.83 263.84 0.855 0.269 112.0 0.168 1.19 6400     0.75 1488  
41004A   2.60 963.0 1.70 0.74 99.0 0.160 0.70 23     0.40 5.5 *
41004B   18.4 1.3283 0.0177 0.081 6114.0 0.160 0.40 23     0.70 3.9 *
46375   0.226 3.0235 0.0398 0.063 33.65 0.240 0.92 346     0.60 80  
75289   0.467 3.5092 0.0482 0.034 54.9 0.217 1.21 621     0.14 188  
75732 55 Cnc 0.0377 2.7955 0.0377 0.09 5.8 0.315 0.91 1062     0.26 291  
    0.833 14.652 0.1138 0.01 73.38 0.315 0.91 1062     0.26 291  
    0.157 44.36 0.238 0.071 9.6 0.315 0.91 1062     0.26 291  
    3.90 5552.0 5.97 0.091 47.5 0.315 0.91 1062     0.26 291  
80606   4.31 111.449 0.468 0.935 481.9 0.343 1.10 1200     0.90 260  
89744   8.58 256.80 0.934 0.677 267.3 0.265 1.64 2456     0.079 780  
99492 83 Leo B 0.109 17.0431 0.1232 0.254 9.8 0.362 0.86 515     1.01 100  
109749   0.277 5.23947 0.0629 0 28.58 0.250 1.21 490     0.78 113  
114729   0.95 1114.0 2.11 0.167 18.8 -0.262 1.00 282     0.25 79  
114762   11.68 83.8881 0.363 0.336 615.2 -0.653 0.89 130     0.07 40  
120136 $\tau$ Boo 4.13 3.3125 0.048 0.023 461.1 0.234 1.35   245 0.91 0.40 2.8 *
142022   4.50 1928.0 2.93 0.53 92.0 0.190 0.90 820     0.60 188  
147513   1.18 528.4 1.31 0.26 29.3 0.089 1.07 4451     0.65 1044 a
178911   7.35 71.511 0.345 0.139 346.9 0.285 1.06 640     1.89 108 b
186427 16 CygB 1.68 798.5 1.681 0.681 50.5 0.038 0.99 850     1.19 164 b
188015   1.50 461.2 1.203 0.137 37.6 0.289 1.09 684     0.21 198  
189733   1.15 2.219 0.0312 0 205.0 -0.030 0.82 216     0.19 61 *
190360 GJ 777 A 0.0587 17.1 0.1303 0.01 4.6 0.213 1.01 3000     0.20 864  
    1.55 2891.0 3.99 0.36 23.5 0.213 1.01 3000     0.20 864  
195019   3.69 18.2013 0.1388 0.0138 271.5 0.068 1.07 150     0.70 35  
196050   2.90 1378.0 2.454 0.228 49.7 0.229 1.15 511     0.36 138  
213240   4.72 882.7 1.92 0.421 96.6 0.139 1.22 3898     0.15 1177  
222404 $\gamma$ Cep 1.77 905.0 2.14 0.12 27.5 0.180 1.59   18.5 0.36 0.40 4.0  
222582   7.75 572.38 1.347 0.725 276.3 -0.029 0.99 4746     0.36 1246  
Binary references: HD 142: R06; HD 1237: Chauvin et al. (2006); HD 3651: Mugrauer et al. (2006b); HD 9826: Lowrance et al. (2002), E04; HD 11964: R06; HD 13445: Lagrange et al. (2006), Mugrauer & Neuhauser (2005); HD 16141: Mugrauer et al. (2005); HD 19994: Hale (1994), E04; HD 20782: this paper; HD 27442: Chauvin et al. (2006), R06; HD 38529: R06; HD 40979: E04; HD 41404: E04; HD 46375: Mugrauer et al. (2006a); HD 75289: Mugrauer et al. (2004b); HD 75732: E04, Mugrauer et al. (2006a); HD 80606: E04; HD 89744: Mugrauer et al. (2004a); HD 99492: R06; HD 109749: this paper; HD 114729: Mugrauer et al. (2005); HD 114762: Patience et al. (2002), E04; HD 120136: Hale (1994), E04; HD 142022: Eggenberger et al. (2006b); HD 147513: Mayor et al. (2004), R06, Silvestri et al. (2001); HD 178911: Tokovinin et al. (2000), E04; HD 186427: Hauser & Marcy (1999), Patience et al. (2002), E04; HD 188015: R06; HD 189733: Bakos et al. (2006a); HD 190360: E04; HD 195019: E04; HD 196050: Mugrauer et al. (2005); HD 213240: Mugrauer et al. (2005); HD 222404: Hatzes et al. (2003); HD 222582: R06.

a
The secondary is a white dwarf; the original mass was larger and the separation smaller. See Appendix B for details.
b
Hierarchical triple system, the sum of the masses of the two companions is listed here. See Appendix C for details.

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