Precise Masses in the WASP-47 System

Vanderburg, Andrew; Becker, Juliette; Buchhave, Lars A.; Mortier, A.; Lopez, Eric; Malavolta, L.; Haywood, R. D.; Latham, David W.; Charbonneau, David; López‐Morales, Mercedes; Adams, Fred C.; Bonomo, A. S.; Bouchy, F.; Cameron, A. Collier; Cosentino, R.; Fabrizio, L. Di; Dumusque, X.; Fiorenzano, A. F. Martínez; Harutyunyan, A.; Johnson, John Asher; Lorenzi, V.; Lovis, C.; Mayor, M.; Micela, G.; Molinari, E.; Pedani, M.; Pepe, F.; Piotto, G.; Phillips, David F.; Rice, Ken; Sasselov, Dimitar; Ségransan, D.; Sozzetti, A.; Udry, S.; Watson, Chris

doi:10.3847/1538-3881/aa918b

Cited by 78 publications

(62 citation statements)

References 120 publications

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“…Notably, the three complementary methods all yielded the same conclusions, resulting in a mass measurement for the innermost planet that is not only precise but also robust. Demory et al 2011Demory et al , 2016Winn et al 2011;Nelson et al 2014), CoRoT-7b (Léger et al 2009;Queloz et al 2009;Haywood et al 2014), WASP-47e (Becker et al 2015;Dai et al 2015;Sinukoff et al 2017b;Vanderburg et al 2017), Kepler-78b (Howard et al 2013;Pepe et al 2013;Sanchis-Ojeda et al 2013;Hatzes 2014;Grunblatt et al 2015), Kepler-10b (Batalha et al 2011;Dumusque et al 2014;Weiss et al 2016;Rajpaul et al 2017), K2-131b , HD 3167b (Vanderburg et al 2016a;Christiansen et al 2017;Gandolfi et al 2017, respectively labeled as C17 and G17 in the plot), K2-106b (Guenther et al 2017;Sinukoff et al 2017a, G17 and S17 respectively). Notably, the last two planets have two independent density measurements that are not consistent with each other, resulting in a disagreement in the interpretation of the internal composition.…”

Section: Discussionmentioning

confidence: 99%

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Malavolta

Mayo

Louden

et al. 2018

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133

119

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Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51±0.05R Å and a mass of 5.08±0.41M Å , consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.

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Section: Discussionmentioning

confidence: 99%

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Malavolta

Mayo

Louden

et al. 2018

Self Cite

133

119

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“…The system includes three inner transiting planets and an outer non-transiting planet in an eccentric (e ∼ 0.3) orbit. The most recent system parameters, provided by Vanderburg et al (2017), are shown in Table 1 and for each planet include the orbital period (P ), semi-major axis (a), eccentricity (e), and periastron argument (ω), orbital inclination (i), radius (R p ), and mass (M p ). Note that we have assumed a Jupiter radius for the non-transiting giant planet WASP-47c.…”

Section: System Architecture and Habitable Zonementioning

confidence: 99%

“…Note that we have assumed a Jupiter radius for the non-transiting giant planet WASP-47c. WASP-47 is a star that is similar to the Sun, with a mass of M ⋆ = 1.040 ± 0.031 M ⊙ , radius of R ⋆ = 1.137 ± 0.013 R ⊙ , and effective temperature of T eff = 5552 ± 75 K (Vanderburg et al 2017). A topdown representation of the orbital architecture for the WASP-47 system is shown in Figure 1.…”

Section: System Architecture and Habitable Zonementioning

confidence: 99%

“…Furthermore, the uncertainties in the HZ boundaries depend on the robustness of the stellar property values (Kane 2014). As pointed out by Vanderburg et al (2017), the WASP-47 stellar properties are quite accurately determined, aided substantially by the vast number of measurements and similarity to the Sun. The representation of the orbital architecture shown in Figure 1 includes a green region that indicates the extent of the HZ in the system (Kane & Gelino 2012b).…”

Section: System Architecture and Habitable Zonementioning

confidence: 99%

“…Radial velocity (RV) monitoring of the system revealed a non-transiting giant planet in an eccentric orbit (Neveu-VanMalle et al 2016). The masses of the transiting planets have been determined through a combination of RVs (Dai et al 2015;Sinukoff et al 2017;Vanderburg et al 2017;Weiss et al 2017), TTVs (Dai et al 2015;Weiss et al 2017), and photodynamical constraints (Almenara et al 2016). The system is fascinating for numerous reasons, including the diverse architecture, the potential for atmospheric detection of the planets via phase variations as a function of planet orbital phase, and the presence of an eccentric giant planet interior to the snow line.…”

Section: Introductionmentioning

confidence: 99%

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The Dark Planets of the WASP-47 Planetary System

Kane

Fetherolf

Hill

2020

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Exoplanet discoveries have demonstrated a vast range of planetary system architectures. The demographic of compact planetary systems are especially interesting from the perspective of planetary formation and the evolution of orbital dynamics. Another interesting demographic is that of giant planets in eccentric orbits, since these planets have likely had a dynamical history involving planetplanet scattering events. The WASP-47 system is particularly fascinating since it combines these two demographics, having both compact planetary orbits and a giant planet on an eccentric orbit within the system Habitable Zone. Here we provide an analysis of the WASP-47 system from the perspective of atmospheric detection and characterization. We discuss the system architecture and the potential for additional long-period planets. We simulate expected phase variations as a function of planet orbital phase for the system due to the combined effect of the planets. We present an analysis of precision photometry of WASP-47 from the K2 mission, phased on each of the planets. The analysis rules out the detection of phase signatures for the two inner-most planets, enabling constraints upon their albedos and atmospheric properties. Our study concludes that WASP-47b is an example of a "dark" planet with a tentative geometric albedo of 0.016 and a 1σ upper limit of 0.17. The WASP-47e data are consistent with a broad range of albedos, but also show early evidence of having a relatively low albedo. The growing number of dark, short-period giant planets provide the framework of an ideal sample for studying low albedo dependence on atmospheric composition.

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Exoplanet mass estimation for a sample of targets for the Ariel mission

Barnes

Haswell

2021

Exp Astron

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Ariel’s ambitious goal to survey a quarter of known exoplanets will transform our knowledge of planetary atmospheres. Masses measured directly with the radial velocity technique are essential for well determined planetary bulk properties. Radial velocity masses will provide important checks of masses derived from atmospheric fits or alternatively can be treated as a fixed input parameter to reduce possible degeneracies in atmospheric retrievals. We quantify the impact of stellar activity on planet mass recovery for the Ariel mission sample using Sun-like spot models scaled for active stars combined with other noise sources. Planets with necessarily well-determined ephemerides will be selected for characterisation with Ariel. With this prior requirement, we simulate the derived planet mass precision as a function of the number of observations for a prospective sample of Ariel targets. We find that quadrature sampling can significantly reduce the time commitment required for follow-up RVs, and is most effective when the planetary RV signature is larger than the RV noise. For a typical radial velocity instrument operating on a 4 m class telescope and achieving 1 m s−1 precision, between ~17% and ~ 37% of the time commitment is spent on the 7% of planets with mass Mp < 10 M⊕. In many low activity cases, the time required is limited by asteroseismic and photon noise. For low mass or faint systems, we can recover masses with the same precision up to ~3 times more quickly with an instrumental precision of ~10 cm s−1.

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Precise Masses in the WASP-47 System

Cited by 78 publications

References 120 publications

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

The Dark Planets of the WASP-47 Planetary System

Exoplanet mass estimation for a sample of targets for the Ariel mission

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