EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Nowak, G.; Πάλλη, Ε.; Gandolfi, D.; Dai, Fei; Lanza, A. F.; Hirano, Teruyuki; Barragán, Oscar; Fukui, A.; Bruntt, H.; Endl, Michael; Cochran, William D.; Moroni, Pier Giorgio Prada; Prieto-Arranz, J.; Kiilerich, Amanda; Nespral, D.; Hatzes, A. P.; Albrecht, S.; Deeg, H. J.; Winn, Joshua N.; Yu, Li; Kuzuhara, Masayuki; Grziwa, S.; Smith, A. M. S.; Guenther, E. W.; Eylen, Vincent Van; Csizmadia, Szilárd; Fridlund, M.; Cabrera, J.; Eigmüller, Philipp; Erikson, A.; Korth, J.; Narita, Norio; Pätzold, M.; Rauer, H.; Ribas, I.

doi:10.3847/1538-3881/aa5cb6

Cited by 43 publications

(48 citation statements)

References 77 publications

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“…The resulting probabilities are listed in Table 5 for each candidate. The two faint candidates identified beyond 7 from EPIC 219388192 by Nowak et al (2017) were found to likely be background sources, with probabilities <15% of being physically associated. With the exception of the wider candidate around 70 Vir, most other candidates were found to have very high probabilities of being bonafide companions: the close candidates around 70 Vir, EPIC 219388192, HD 89744 and KELT-1 have >99% probabilities of being bound.…”

Section: Literature Search and Imaging Surveysmentioning

confidence: 95%

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

Fontanive

Rice

Bonavita

et al. 2019

Monthly Notices of the Royal Astronomical Society

119

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Stellar multiplicity is believed to influence planetary formation and evolution, although the precise nature and extent of this role remain ambiguous. We present a study aimed at testing the role of stellar multiplicity in the formation and/or evolution of the most massive, closein planetary and substellar companions. Using past and new direct imaging observations, as well as the Gaia DR2 catalogue, we searched for wide binary companions to 38 stars hosting massive giant planets or brown dwarfs (M > 7 M Jup ) on orbits shorter than ∼1 AU. We report the discovery of a new component in the WASP-14 system, and present an independent confirmation of a comoving companion to WASP-18. From a robust Bayesian statistical analysis, we derived a binary fraction of 79.0 +13.2 −14.7 % between 20−10,000 AU for our sample, twice as high as for field stars with a 3-σ significance. This binary frequency was found to be larger than for lower-mass planets on similar orbits, and we observed a marginally higher binary rate for inner companions with periods shorter than 10 days. These results demonstrate that stellar companions greatly influence the formation and/or evolution of these systems, suggesting that the role played by binary companions becomes more important for higher-mass planets, and that this trend may be enhanced for systems with tighter orbits. Our analysis also revealed a peak in binary separation at 250 AU, highlighting a shortfall of close binaries among our sample. This indicates that the mechanisms affecting planet and brown dwarf formation or evolution in binaries must operate from wide separations, although we found that the Kozai-Lidov mechanism is unlikely to be the dominant underlying process. We conclude that binarity plays a crucial role in the existence of very massive short-period giant planets and brown dwarf desert inhabitants, which are almost exclusively observed in multiple systems.

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Section: Literature Search and Imaging Surveysmentioning

confidence: 95%

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

Fontanive

Rice

Bonavita

et al. 2019

Monthly Notices of the Royal Astronomical Society

119

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“…In fact, the recently discovered transiting brown dwarf in the significantly older Ruprecht 147 cluster similarly exhibits a relatively high eccentricity and short orbital period (Nowak et al 2017).…”

Section: Tidal Circularizationmentioning

confidence: 99%

“…Figure 13 shows the phase-folded and GPdetrended light curve: the primary eclipse is well-fit, although there is a modest increase in the residual scatter, which is larger than in AD 2615 but smaller than in AD 3814. The RV data suggest a moderately eccentric orbit (ẽ 0.15; see Figure 14) with a systemic velocity of = Nowak et al 2017;Bayliss et al 2017) and the primary component is one of only three M-dwarfs known to host a transiting brown dwarf. Furthermore, this is only the second known transiting brown dwarf in an open cluster (i.e., where the age is well-constrained), and the first younger than a Gyr.…”

Section: Ad 3116mentioning

confidence: 99%

New Low-mass Eclipsing Binary Systems in Praesepe Discovered by K2

Gillen

Hillenbrand

David

et al. 2017

ApJ

107

112

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We present the discovery and characterization of four low-mass ( < M 0.6  M ) eclipsing binary (EB) systems in the sub-Gyr old Praesepe open cluster using Kepler/K2 time series photometry and Keck/HIRES spectroscopy. We present a new Gaussian process EB model, GP-EBOP, as well as a method of simultaneously determining effective temperatures and distances for EBs. Three of the reported systems (AD 3814, AD 2615 and AD 1508) are detached and double-lined, and precise solutions are presented for the first two. We determine masses and radii to 1%-3% precision for AD 3814 and to 5%-6% for AD 2615. Together with effective temperatures determined to ∼50 K precision, we test the PARSEC v1.2 and BHAC15 stellar evolution models. Our EB parameters are more consistent with the PARSEC models, primarily because the BHAC15 temperature scale is hotter than our data over the mid-M-dwarf mass range probed. Both ADs 3814 and 2615, which have orbital periods of 6.0 and 11.6 days, are circularized but not synchronized. This suggests that either synchronization proceeds more slowly in fully convective stars than the theory of equilibrium tides predicts, or magnetic braking is currently playing a more important role than tidal forces in the spin evolution of these binaries. The fourth system (AD 3116) comprises a brown dwarf transiting a mid-M-dwarf, which is the first such system discovered in a sub-Gyr open cluster. Finally, these new discoveries increase the number of characterized EBs in sub-Gyr open clusters by 20% (40%) below < M 1.5 M e ( < M 0.6 M e ).

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“…As part of the ongoing RV follow-up program of K2 transiting planets successfully carried out by our consortium KESPRINT (e.g., Sanchis-Ojeda et al 2015;Grziwa et al 2016;Van Eylen et al 2016;Fridlund et al 2017;Guenther et al 2017;Nowak et al 2017), we herein present the results of an intensive RV campaign we conducted with the FIES, HARPS, and HARPS-N spectrographs to accurately measure the masses of the two small planets transiting HD 3167. The paper is organized as follows.…”

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confidence: 99%

The Transiting Multi-planet System HD 3167: A 5.7 M_⊕ Super-Earth and an 8.3 M_⊕ Mini-Neptune

Gandolfi

Barragán

Hatzes

et al. 2017

Self Cite

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HD 3167 is a bright (V = 8.9 mag) K0 V star observed by NASA's K2 space mission during its Campaign8. It has recently been found to host two small transiting planets, namely, HD 3167b, an ultra-short-period (0.96 days) superEarth, and HD 3167c, a mini-Neptune on a relatively long-period orbit (29.85 days). Here we present an intensive radial velocity (RV) follow-up of HD 3167 performed with the FIES@NOT, HARPS@ESO-3.6 m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69±0.44 M ⊕ , a radius of 1.574±0.054 R ⊕ , and a mean density of 8.00 0.98-, HD 3167b joins the small group of ultra-short-period planets known to have rocky terrestrial compositions. HD 3167c has a mass of 8. -, indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (∼350 km) and the brightness of the host star make HD 3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the RV measurements but the currently available data set does not allow us to draw any firm conclusions on the origin of the observed variation.

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EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Cited by 43 publications

References 77 publications

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

New Low-mass Eclipsing Binary Systems in Praesepe Discovered by K2

The Transiting Multi-planet System HD 3167: A 5.7 M_⊕ Super-Earth and an 8.3 M_⊕ Mini-Neptune

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EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Cited by 43 publications

References 77 publications

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

New Low-mass Eclipsing Binary Systems in Praesepe Discovered by K2

The Transiting Multi-planet System HD 3167: A 5.7 M⊕ Super-Earth and an 8.3 M⊕ Mini-Neptune

Contact Info

Product

Resources

About

The Transiting Multi-planet System HD 3167: A 5.7 M_⊕ Super-Earth and an 8.3 M_⊕ Mini-Neptune