Planets in binaries, additional information

NOTES ON SOME INDIVIDUAL SYSTEMS:

- Gamma Ceph A is a post-main-sequence star (sub-giant). Recent astrometry analysis (Benedict et al., 2018) shows that there is a 70 degrees mutual inclination between the binary and planetary orbits and that the planet probably has a much higher mass than previously expected (9 MJup).

- 30Ari B is actually part of a wide triple system (component Ari A, see Kane et al., 2015). What we show here is the BC binary. The orbit of the Ari C companion is poorly constrained: with a separation of 21.9AU, the constraint is that e<0.75. I took e=0.75/2 as a reference value. (And the component Ari Aa is actually also a very tight binary)

- Kepler 410 is maybe a triple system with a star "C" between A and B (Gajdos et al., 2017) / Binary revised by Mugrauer(2019)

- Kepler 420: The binary companion was inferred by Santerne et al.(2014) based on joint analysis of RV, bisector and FWHM variations. It should be confirmed by other independent constraints.

- Kepler 444: it is a triple star, so the data corresponds to the merged B+C M-stars (Dupuy et al., 2016).

- HD8673: The "planet" is at the brown dwarf limit. The projected separation is actually 11AU only. The given orbit is the closest stable one as computed by Roberts et al.(2015)

- HD87646: the 2nd "planet" is potentially a brown dwarf

- HD131399: DISCARDED. It is a hierarchical triple (the companion star is in fact a tight binary, see Wagner et al., 2016): Nielsen et al.(2017) discard the imaged planet as a being a background star

- HD106515: The binary orbit corresponds to that with lowest possible e and a, but there is a wide range of other possibilities (see Fig.9 of Desidera et al., 2012). Better (but still loose) constraints on the orbit given by Rica et al.(2017). Refined projected distance in Mugrauer(2019)

- Kepler 132 possesses at least 3 planets, and we know that 2 of them (b and c) cannot orbit the same star. But we don't know which planet orbits which star. There is also a 4th planet that is still a KOI. (Lissauer, et al., 2014, Everett et al., 2015)

- HD132563B: The distant A component is itself a binary of separation 15AU (Desidera et al., 2011)

- Gliese667: Triple System. The planet-hosting C star is linked to the A-B binary at a projected distance of 230AU. The AB binary has an orbit with a =12.6AU and e=0.58. The stability has been calculated for a merged AB component

- Kelt 4: Kelt-4A is orbited, at a projected separation of 328AU, by a binary (B-C), composed of 2 identical K stars separated by 10.3AU. The stability has been calculated for a merged BC component (Eastman et al., 2015)

- HD65216: The B component is in fact a B-C tight binary of separation 6AU (Mugrauer et aL, 2007)

- Kepler 21, 68 , HD197037, HD217786: binarity discovered by Ginski et al.(2016)

- HD28254: listed as binary in Moutou et al. and Lodieu et al.(2014).

- HD30856, HD116029, HD207382, HD86081, HD43691. All objects described in Ngo et al.(2017). HD30856, 86051, 207382: companions presented for the first time in this paper. HD43691 & 116029: companions confirmed by Ngo.

-Kepler693: 150Mjup companion inferred by Masuda by modelling the transit timing&duration variations. Planet and Binary planes should have a mutual inclination of 53 deg.

-Kepler13: the B component is in fact a binary (separation 0.410UA)

-HD126614 is a triple star, the third component is beyond 1000AU (Gould and Chamané, 2004)

-HD2638 is a triple star. The planet is actually orbiting HD2628B, the companion being HD2638C. But there is a third, more massive star (called HD2567, not HD2638A) at a projected separation of 839" (45000AU, see Roberts et al., 2015)

-TauBootis: refined investigation of the binary by Justesen&Albrecht(2019). Finds a larger semi-major axis than before (221 instead of 118, but with a large uncertainty). And constrains q to 28.3au+-3. Planetary and Binary orbits should be aligned.

- LTT 1445: Triple system with 3 M stars. The A component is orbited by the BC pair, whose  orbit has been constrained to be a=8,00au and e=0.5 (Winters et al., 2019). The A-BC orbit is unconstrained.

- HD202772: first hot-Jupiter discovered by TESS. The A star is mildly evolved. The bound nature of the AB pair has been confirmed by Mugrauer(2019).

- HD4732: Planets by Sato et al.(2013)

- HD19994: also known as 94 Cet / planet by Queloz2001 / binary parameters by Hale1994, revised by Roberts(2011) / B is itself a compact binary (BC)  (Röll et al.2011)/ proj.separation (50au) by Mugrauer2019. This system is highly inclined with respect to the line of sight (104degres), with a « real » orbit of a=220 & e=0.26 (Roberts2011).

- WASP-49: Planet by Lendl(2012) /   Binary in Mugrauer(2019)

- omi Uma: Planet by Sato(2012)/   Binary in Mugrauer2019

- HD93385: planets by Harris2012 /   Binary in Mugrauer2019

- HD98736: planet by Ment(2018) / binary in Vogt(2015)

- HD102365: planet by Tinney(2011) / Binary well known

- HD103774: Planet by Lo Curto(2013) / Binary identified by Mugrauer(2019)

- HD108341: Planet by Moutou(2014) /   binary in Mugrauer2019

- Qatar 6 : Planet by Alsubai(2018) / Binary by Mugrauer(2019)

- HD133131: each star of this wide binary possesses planets (Teske, 2016).

- HD142245: Planet by Johnson(2011)/ Binary and binarity of the BC component in Mugrauer2015 

- Kepler1651: Planet by Fischer(2012)/ Binary by Mann(2017), revised by Mugrauer(2019)

- HD176051: Planet detected by astrometry by Muterspaugh(2010) / Not sure which star the planet is orbiting (I’ve put A by default) / binary well known, orbit by Muterspaugh(2010)
 
- Kepler1319: Planet by Morton(2016) / binary by Mann(2017), revised by Mugrauer(2019) /  not sure around which star the planet is orbiting

- Kepler333: Planets by Rowe(2014) / Binary in Mugrauer(2019)

- HD185269: Planet by Moutou(2006)/ The B component is itself a tight binary (BC)

- WASP145: Planet by Hellier(2018) / Bound nature of the AB pair confirmed by Mugrauer(2019)

- HD220842: Planet by Hebrard(2016 / Binary by Mugrauer(2019)

- WASP-8: Triple system, with a distant (14500au) C component / Planet b in transit by Queloz(2010), Planet c in RV by Knutson(2014)

- HD114762: DISCARDED: The study by Kiefer et al.(2019) shows that the « planetary » companion has a mass of more than 100 MJup.

- WASP-108: triple system: wide companion (>2000au) detected by Evans(2018), closer companion by Bohn(2020). Possibly a 4th object at 5" (Bohn2020)

- HD42936: planet and binary by Barnes(2019)

- HR858: planets by Vanderburg(2019). Mass of HR858B not given, extrapolated from its radius

- DS Tuc: Planet and binary by Newton(2019) / Young (40Myr) system in the Tucana-Horologium association

- HD1666: Planet by Harakawa(2015 / binary by Ginski(2020)

- HD109271: planets by Lo Curto(2013) / binary by Ginski(2020)

- HIP68468: planets by Melendez(2017) / binary by Ginski(2020)

- HIP107773: planet by Jones(2015) / binary by Ginski(2020)

- LTT3780(TOI-732): planets by Nowak et al.(2020, CARMENES) & Cloutier et al.(2020, TESS) / binarity well known

- HD238090(GJ458): Planet by Stock et al.(2020) / binary parameters in Cortes-Contrars et al.(2016)

- GJ414: Planets by Dedrick et al.(2020) / binary well known

- HD26965(40Eri): Planet by Ma et al.(2018) / triple system: primary orbited by binary of separation 32AU, B component is a white dwarf