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)

- OGLE2013BLG0341: Planet and binary by Gould+(2014). Companion star's mass only constrained to be "slightly more massive" than the primary

- HD59686: Planet and binary by Ortiz+(2016)

- HD7449: Planet by Dumusque+(2011) / Binary by Rodigas+(2016), of excentricity <0.5 / Debate whether 2 planets or just 1

- 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. The binary's orbit is inclined by 18 deg.

- Kepler 444: it is a triple star, so the data corresponds to the merged B+C M-stars (Dupuy et al., 2016) / Planets by Campante+(2015) / Binary by Lillobox+(2014) / Mugrauer2019 finds a proj. distance of 61.2au between the stars, still compatible with Lillobox orbit

- 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) / Planet by Moutou+(2005) / binary by Roberts+(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). Simonetti+(2020) give 0.54 for the binary's eccentricity
 
- 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)

- 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

- Kepler449, 450, 632, 884, 907 & 1339: Common proper motions companions found by Colton et al.(2021), would maybe need additional confirmation.

- HD23472: Planets by Trifonov(2018), Binarity by Michel&Mugrauer(2021)

- HIP 65 (TOI218): Planet by Nielsen+(2020)/Binarity by Mugrauer&Michel(2020)

- HD5278(TOI130): Planets by Sozetti+(2021)/Binarity by Mugrauer&Michel(2020)

- TOI1634 : Planet by Hirano+(2021) / Binarity by Mugrauer&Michel(2020)

- HR858: Planets by Vanderburg+(2019) / Binarity by Michel&Mugrauer(2021)

- HD39855: Planet by Feng+(2019) / Binarity by Michel&Mugrauer(2021)

- NGTS10: Planet by McCormac+(2020) / Binarity by Michel&Mugrauer(2021)

- HD79211: Planet by Gonzales-Alvares+(2020) / Binary long known, orbit refined by Gonzales-Alvares

- HD93148 (MASCARA-3 or KELT-24): Planet by Hjorth+(2019) / Binarity by Rodriguez+(2019)

- HD233832: Planet & binarity by Barbato+(2019), latest binary measurement by Michel&Mugrauer(2021)

- TOI-905: Planet by Davis+(2021) / Binarity by Michel&Mugrauer(2021): possible higher hierarchy for the system because diff.proper motion exceeds the system's escape velocity

- HD181234: Planet by Rickman+(2019) / Binarity by Michel&Mugrauer(2021)

- HD4113: Triple system / Planet by Tamuz(2007) / B companion at 2000au by Mugrauer / C companion (this one) by Cheetham(2018). The companion is actually a BD of mass 65Mjup