A terrestrial planet in a ~1-AU orbit around one member of a ∼15-AU binary

Gould, Andrew; Udalski, A.; Shin, In-Gu; Porritt, I.; Skowron, J.; Han, Cheongho; Yee, Jennifer C.; Kozłowski, S.; Choi, J.-Y.; Poleski, R.; Wyrzykowski, Ł.; Ulaczyk, K.; Pietrukowicz, P.; Mróz, P.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Gaudi, B. Scott; Christie, Grant; Drummond, J.; McCormick, J.; Natusch, T.; Ngan, H.; Tan, T. G.; Albrow, M. D.; DePoy, D. L.; Hwang, Kyu-Ha; Jung, Youn Kil; Lee, Chung-Uk; Park, H.; Pogge, Richard W.; Abe, F.; Bennett, D. P.; Bond, I. A.; Botzler, C. S.; Freeman, Matthew; Fukui, A.; Fukunaga, D.; Itow, Y.; Koshimoto, Naoki; Larsen, Patricia; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Namba, Susumu; Ohnishi, Kouhei; Philpott, L.; Rattenbury, N. J.; Saito, To.; Sullivan, D. J.; Sumi, T.; Suzuki, D.; Tristram, P. J.; Tsurumi, Naoki; Wada, K.; Yamai, N.; Yock, P. C. M.; Yonehara, A.; Shvartzvald, Yossi; Maoz, Dan; Kaspi, S.; Friedmann, M.

doi:10.1126/science.1251527

Cited by 107 publications

(50 citation statements)

References 45 publications

(59 reference statements)

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“…Planets exist in binaries with a wide range of separations, but it is clear that the majority of them show semi-major axes greater than a B ∼ 100 au. HD 59686 AB is, together with ν Octantis (Ramm et al 2009) and OGLE-2013-BLG-0341LB (Gould et al 2014), the binary with the closest separation of its stellar components known to harbor a planet. Semi-major axis of planet [AU] Fig.…”

Section: Discussionmentioning

confidence: 99%

Precise radial velocities of giant stars

Ortiz

Reffert

Trifonov

et al. 2016

A&A

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Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G-and K-giant stars using the Hamilton Échelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m p sin i = 6.92 +0.18 −0.24 M Jup orbiting at a p = 1.0860 +0.0006 −0.0007 au from the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e B = 0.729 +0.004 −0.003 ) binary companion with a mass of m B sin i = 0.5296 +0.0011 −0.0008 M orbiting at a close separation from the giant primary with a semi-major axis of a B = 13.56 +0.18 −0.14 au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.

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Section: Discussionmentioning

confidence: 99%

Precise radial velocities of giant stars

Ortiz

Reffert

Trifonov

et al. 2016

A&A

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“…However, because the planetary deviation was sparsely covered, the uncertainties on the planet's mass and separation are large. Gould et al (2014) discovered a ∼2 M ⊕ planet at ∼0.8AU from a 0.1-0.15 M M dwarf, which is one member of a binary system with a slightly heavier companion (0.12-0.18 M ). This planet had the lowest securely-measured mass found by microlensing previous to the one presented here.…”

Section: Introductionmentioning

confidence: 99%

An Earth-mass Planet in a 1 au Orbit around an Ultracool Dwarf

Shvartzvald

Yee

Novati

et al. 2017

ApJL

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We combine Spitzer and ground-based KMTNet microlensing observations to identify and precisely measure an Earth-mass (1.43 −0.46 kpc, it is the third consecutive case among the Spitzer "Galactic distribution" planets toward the Galactic bulge that lies in the Galactic disk as opposed to the bulge itself, hinting at a skewed distribution of planets. Together with previous microlensing discoveries, the seven Earth-size planets orbiting the ultracool dwarf TRAPPIST-1, and the detection of disks around young brown dwarfs, OGLE-2016-BLG-1195Lb suggests that such planets might be common around ultracool dwarfs. It therefore sheds light on the formation of both ultracool dwarfs and planetary systems at the limit of low-mass protoplanetary disks.

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“…In order not to include the affected data in the fit, we restricted the MOA dataset to the fourteen epochs that are closest to the anomaly, i.e., from HJD = 5961.1 to 5969.2. Similar issues with a nearby star contaminating photometry of the microlensing event were faced by Gould et al (2014) who analyzed the event OGLE-2013-BLG-0341. We note that the remaining MOA data will not improve accuracy of the fitted event properties, because with the exception of the anomaly, the event was of a low magnification and during bulge observing season the OGLE cadence of 20 min is more than sufficient to characterize the light curve.…”

Section: Photometric Observationsmentioning

confidence: 96%

A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

Poleski

Udalski

Bond

et al. 2017

A&A

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We present the discovery of a substellar companion to the primary host lens in the microlensing event MOA-2012-BLG-006. The companion-to-host mass ratio is 0.016, corresponding to a companion mass ofThus, the companion is either a high-mass giant planet or a low-mass brown dwarf, depending on the mass of the primary M * . The companion signal was separated from the peak of the primary event by a time that was as much as four times longer than the event timescale. We therefore infer a relatively large projected separation of the companion from its host of ≈ 10 a.u.(M * /0.5M ) 1/2 for a wide range (3-7 kpc) of host star distances from the Earth. We also challenge a previous claim of a planetary companion to the lens star in microlensing event OGLE-2002-BLG-045.

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A terrestrial planet in a ~1-AU orbit around one member of a ∼15-AU binary

Cited by 107 publications

References 45 publications

Precise radial velocities of giant stars

Precise radial velocities of giant stars

An Earth-mass Planet in a 1 au Orbit around an Ultracool Dwarf

A companion on the planet/brown dwarf mass boundary on a wide orbit discovered by gravitational microlensing

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