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Table 3:

Close companions to solar-type stars with (projected) masses between 10 $M_{\rm J}$and 80 $M_{\rm J}$.
Object $M_{\rm c}\sin i$ Period a e i $M_{\rm c}$ SpT Mstar [Fe/H] Remarks and references
  $M_{\rm J}$ d AU   deg $M_{\rm J}$   $M_{\odot }$    
Probable substellar objects with mass $M_{\rm c} > 10 M_{\rm J}$and a<7 AU around solar-type stars
HD 29587b 41 1474.9   0.356   41 (27) G2V 1.00 -0.61 Halbwachs et al. (2000), Bensby et al. (2005)a
HD 29587b 12.7 2174.3 3.68 0.36 160 37+36-19 G4IV 1.46 +0.45 Butler et al. (2006), Reffert & Quirrenbach (2006),
                    Valenti & Fischer (2005), PL, MULT, HIPG
HD 29587b 59 297.708   0.952   64 (19) G1V 1.05 -0.42 Halbwachs et al. (2000), Edvardsson et al. (1993)b
HD 29587b 36 2599   0.716   45 (21) K3V 0.75 +0.06 Halbwachs et al. (2000), Han et al. (2001)
HD 29587b 18.15 1951 3.17 0.638 $55\pm12$ 23+26-5 G3V 1.10 +0.32 this paper, HIPG
HD 29587b 18.1 1765.8 2.91 0.2125 150 $34\pm12$ G5 1.08 +0.08 Reffert & Quirrenbach (2006), PL
            <82       Zucker & Mazeh (2001)
HD 29587b   4.2568 0.057 0.0 85.9 $21.7\pm1.0$ F3V 1.37 -0.02 Deleuil et al. (2008), transitc
HD 29587b   3.19152 0.0454 0.26 84.20 $11.79\pm0.59$ F5V 1.21 -0.18 Winn et al. (2008), transitd
Objects with projected mass $10 < M_{\rm c} \sin i< 80 $ $M_{\rm J}$and a<7 AU around solar-type stars
HD 29587b 42.3 6832.0 6.70 0.64       0.82 -0.22 Nidever et al. (2002), Valenti & Fischer (2005)
HD 29587b 52 3000 4.3 0.14     G0 1.00 +0.03 Perrier et al. (2003), Valenti & Fischer (2005)e
HD 29587b 13.13 466.47 1.084 0.084     G5V 0.78 +0.07 Sato et al. (2009), Bouchy et al. (2009), MULT
HD 29587b 77.8 15.0778 0.13 0.25     F8 1.39 +0.26 Nidever et al. (2002), Valenti & Fischer (2005)
HD 29587b 10.35 2063.818 3.29 0.62     G1IV 1.10 +0.05 Butler et al. (2006), Valenti & Fischer (2005)
HD 29587b 67.8 3138.0 4.00 0.32       0.83 -0.12 Nidever et al. (2002), Valenti & Fischer (2005)
HD 29587b 30.6 497.5 1.205 0.448       0.91 +0.31 Wittenmyer et al. (2009),
HD 29587b 35 3.9805   0.0       0.86 -0.35 Fuhrmann (2008), MULTf
HD 29587b 11.02 83.90 0.3 0.34     F9V 0.93 -0.65 Halbwachs et al. (2000), MULTg
HD 29587b 11.9 1209 2.3 0.37     F9V 1.25 -0.05 Butler et al. (2006), Valenti & Fischer (2005)
HD 29587b 26 798.2 1.85 0.402 >16 <94 G0IV 1.41 +0.37 Endl et al. (2004), Valenti & Fischer (2005)
HD 29587b 10.45 359.51 0.99 0.8472     G0V 1.43 +0.22 Tamuz et al. (2008), MULT
HD 29587b 13.75 8.428198 0.072 0.277     K2V 0.78 +0.11 Udry et al. (2002)h
HD 29587b 50.3 4385 5.47 0.337     G0V 1.11 -0.17 Patel et al. (2007), Valenti & Fischer (2005)
HD 29587b 65.8 840.800 1.90 0.23       1.07 -0.18 Nidever et al. (2002), Valenti & Fischer (2005)
HD 29587b 32.0 693 1.4 0.67     K2V 0.77 -0.04 Vogt et al. (2002), Valenti & Fischer (2005), MULT
HD 29587b 38.17 505.65 1.35 0.63     G3IV/V 1.28 +0.29 Jenkins et al. (2009)
HD 29587b 17.4 255.87 0.83 0.435   <149 G6V 1.17 +0.35 Correia et al. (2005), Zucker & Mazeh (2001), PL
HD 29587b 51 1.788   0.002     dK5 0.67 +0.03 Halbwachs et al. (2000), MULTi
HD 29587b 39.7 103.698 0.44 0.385     G2V 1.00 -0.25 Kane et al. (2009)
HD 29587b 15.2 428.5 1.19 0.691     G4V 1.22 +0.43 Bakos et al. (2009), PL
Probable stellar companions with projected mass in the substellar range
HD 29587b 45 554.6   0.558   187 (20) K2V 0.78 0.00 Halbwachs et al. (2000), Valenti & Fischer (2005), MULTj
          -16.1 $178\pm20$       Zucker & Mazeh (2001)
HD 29587b 9.3 2128   0.48 $4.1\pm0.1$ 142+3.3-1.8   1.02 -0.13 Bean et al. (2007)
HD 29587b 25 2371 3.4 0.69 $55\pm12$ 120+167-43 G0V 0.89 -0.03 this paper, HIPG
HD 29587b 17 271.17   0.784   146 (12) K3V 0.72 0.00 Halbwachs et al. (2000), Mishenina et al. (2004)k
          7.76 $143\pm12$       Zucker & Mazeh (2001)
HD 29587b 34 103.258   0.139   212 (44) K0V 0.79 -0.56 Halbwachs et al. (2000), Mishenina et al. (2004)
          10.4 $213\pm43$       Zucker & Mazeh (2001)
HD 29587b 43.2 147.968 0.55 0.54   177 (73)   1.17 +0.13 Nidever et al. (2002), Halbwachs et al. (2000)
          16.3 $181\pm74$       Zucker & Mazeh (2001), Valenti & Fischer (2005)l
HD 29587b 46 108.55 0.46 0.55 8.5 372+106-85   1.18 +0.13 Zucker & Mazeh (2001)
            <190       Tinney et al. (2001)
HD 29587b 27.2 293.1 0.84 0.48 175 320 G5V 0.91 -0.12 Vogt et al. (2002), MULTm
HD 29587b 68 454.66   0.520   171 (14) K4V 0.69 -0.06 Halbwachs et al. (2000), Gray et al. (2003)n
          25.2 $172\pm15$       Zucker & Mazeh (2001)
HD 29587b 48 716.68   0.074   261 (15) K5V 0.67 +0.05 Halbwachs et al. (2000), Heiter & Luck (2003)o
          12.77 $257\pm16$       Zucker & Mazeh (2001)

(a) For spectroscopic binaries with brown dwarf candidates observed by Hipparcos and with an actual mass estimate derived by Halbwachs et al. (2000), the error distribution of the secondary masses is not Gaussian and not symmetric. We list here the values of $M_{\rm c}$ and the accompanying one-sided errors as defined by Eq. (5) in Halbwachs et al. (2000). The star has both chemical abundances and kinematics of thick disk. (b) Thick disk population. c Transiting system. Triaud et al. (2009) found a significant misalignment between the planetary orbital axis and d Transiting system. Winn et al. (2009) found a significant misalignment between the planetary orbital axis and the stellar rotation axis ( $37.3\pm3.7$ deg). the stellar rotation axis ( 37.6+10.0-22.3 deg). (e) The orbit in Perrier et al. (2003) is preliminary, with only limited phase coverage. Perrier et al. (2003) also report no detection with AO. (f) Assuming synchronous rotation and orbit aligment Fuhrmann (2008) derive i=15 and $M_{\rm c}=0.14_{-0.05}^{+0.09}~M_{\odot}$for the companion. The system is a quadruple with another SB at a=2.53 arcsec (21 AU) with e=0.41 from HD 29587b. g The possibility that the star is seen nearly pole-on because of its very low projected rotational velocity is widely debated in the literature. Halbwachs et al. (2000) derive a very uncertain astrometric mass $112~M_{\rm J}$with an error of $103~M_{\rm J}$. An additional low-mass companion close to the substellar boundary detected at 130 AU by Patience et al. (2002). The star is a member of the thick disk population. (h) Zucker & Mazeh (2001) derive an astromeric solution that gives a companion mass of $3.0\pm0.94~M_{\odot}$, not compatible with the stellar properties of the primary. Probably a spurious result due to the short orbital period. (i) Halbwachs et al. (2000) derive an astrometric mass of $182~M_{\rm J}$with a large error of $470~M_{\rm J}$. Glebocki & Stawikowski (1995) estimate $i=22\pm10$ and then $M=136\pm39~M_{\rm J}$ from the rotation period (synchronous with the orbit) and projected rotational velocity, assuming the rotation axis is perpendicular to the orbital plane. However, misalignements can not be ruled out, especially considering that the system has a wide WD companion. The system is probably associated with the Hyades (Catalan et al. 2008). Metallicity from Catalan et al. (2008). (j) Also resolved with direct imaging by Beuzit et al. (2004). Quintuple system (see Bonavita & Desidera (2007) and references therein). (k) Purely astrometric orbital solution in Hipparcos. (l) The significance of the orbital solution in Zucker & Mazeh (2001) is about 0.92. (m) Triple system, see Bonavita & Desidera (2007). Flagged as stochastic solution in Hipparcos. (n) Purely astrometric orbital solution in Hipparcos. (o) Flagged as stochastic solution in Hipparcos.

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