KPF:  Keck Planet Finder

Gibson, Steven R.; Howard, Andrew W.; Marcy, Geoffrey W.; Edelstein, Jerry; Wishnow, Edward H.; Poppett, Claire

doi:10.1117/12.2233334

Cited by 49 publications

(12 citation statements)

References 19 publications

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“…The mid-transit time of the 2028 August transit is almost perfectly timed with Kepler-1704 crossing the meridian, and the full transit (plus post-transit baseline) is observable. However, in the coming years, new precise RV facilities with the capability of achieving a few meters per second precision on faint (V = 13.4) stars, such as MAROON-X (Seifahrt et al 2018) or the Keck Planet Finder (Gibson et al 2016), should consider conducting RM measurements of long-period Kepler planets like Kepler-1704 b.…”

Section: Stellar Obliquitymentioning

confidence: 99%

Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. II. Discovery of a Failed Hot Jupiter on a 2.7 Yr, Highly Eccentric Orbit*

Dalba

Kane

et al. 2021

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Radial velocity (RV) surveys have discovered giant exoplanets on au-scale orbits with a broad distribution of eccentricities. Those with the most eccentric orbits are valuable laboratories for testing theories of high-eccentricity migration. However, few such exoplanets transit their host stars, thus removing the ability to apply constraints on formation from their bulk internal compositions. We report the discovery of Kepler-1704 b, a transiting 4.15 M J giant planet on a 988.88 day orbit with an extreme eccentricity of -+ 0.921 0.015 0.010 . Our decade-long RV baseline from the Keck I telescope allows us to measure the orbit and bulk heavy-element composition of Kepler-1704 b and place limits on the existence of undiscovered companions. A failed hot Jupiter, Kepler-1704 b was likely excited to high eccentricity by scattering events that possibly began during its gas accretion phase. Its final periastron distance was too large to allow for tidal circularization, so now it orbits its host from distances spanning 0.16-3.9 au. The maximum difference in planetary equilibrium temperature resulting from this elongated orbit is over 700 K. A simulation of the thermal phase curve of Kepler-1704 b during periastron passage demonstrates that it is a remarkable target for atmospheric characterization from the James Webb Space Telescope, which could potentially also measure the planet's rotational period as the hot spot from periastron rotates in and out of view. Continued characterization of the Kepler-1704 system promises to refine theories explaining the formation of hot Jupiters and cool giant planets like those in the solar system.

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Section: Stellar Obliquitymentioning

confidence: 99%

Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. II. Discovery of a Failed Hot Jupiter on a 2.7 Yr, Highly Eccentric Orbit*

Dalba

Kane

et al. 2021

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“…Future advances in the exoplanet census and RV instruments will expand the number of systems amenable to similar studies. Next-generation RV facilities at large telescopes such as VLT/ ESPRESSO (González Hernández et al 2017), Keck/KPF (Gibson et al 2016), and GMT/GCLEF (Szentgyorgyi et al 2016) will enable RV measurements of a large sample of faint Kepler planet hosts, including many TTV-active systems. Also, ESA's PLATO mission (Rauer 2013) will conduct a transit survey over ≈2000deg 2 for 2-3 years and add to the sample of planets with long baseline photometry.…”

Section: Discussionmentioning

confidence: 99%

Dynamics and Formation of the Near-resonant K2-24 System: Insights from Transit-timing Variations and Radial Velocities

Petigura

Benneke

Batygin

et al. 2018

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While planets between the size of Uranus and Saturn are absent within the solar system, the star K2-24 hosts two such planets, K2-24b and c, with radii equal to 5.4 Å R and 7.5 Å R , respectively. The two planets have orbital periods of 20.9days and 42.4days, residing only 1% outside the nominal 2:1 mean-motion resonance. In this work, we present results from a coordinated observing campaign to measure planet masses and eccentricities that combines radial velocity measurements from Keck/HIRES and transit-timing measurements from K2 and Spitzer. K2-24b and c have low, but nonzero, eccentricities of~ẽ e 0.08 1 2. The low observed eccentricities provide clues to the formation and dynamical evolution of K2-24b and K2-24c, suggesting that they could be the result of stochastic gravitational interactions with a turbulent protoplanetary disk, among other mechanisms. K2-24b and c are M , respectively; K2-24c is 20% less massive than K2-24b, despite being 40% larger. Their large sizes and low masses imply large envelope fractions, which we estimate at -+ 26 3 3 % and -+ 52 3 5 %. In particular, K2-24c's large envelope presents an intriguing challenge to the standard model of core-nucleated accretion that predicts the onset of runaway accretion when f env ≈50%.

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“…By further studying the orbital architectures of M dwarf systems, which have a lower occurrence of massive planets, we can gain further insight into the role massive planets play in sculpting the orbital architectures across different exoplanet host stars. The advent of precise NIR spectrographs, such as HPF (Mahadevan et al 2012(Mahadevan et al , 2014, the Infrared Doppler Instrument (IRD; Kotani et al 2018), CARMENES (Quirrenbach et al 2018), SPIROU (Artigau et al 2014), NIRPS (Wildi et al 2017), and GIANO-B (Claudi et al 2018), and red-optical spectrographs on large telescopes, such as MAROON-X (Seifahrt et al 2016), ESPRESSO (González Hernández et al 2018), and KPF (Gibson et al 2016), is opening the doors to the ensemble study of the obliquities of M dwarfs.…”

Section: Obliquity and Orbital Alignmentmentioning

confidence: 99%

The Habitable Zone Planet Finder Reveals a High Mass and Low Obliquity for the Young Neptune K2-25b

Stefánsson

Mahadevan

Maney

et al. 2020

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Using radial velocity data from the Habitable Zone Planet Finder, we have measured the mass of the Neptune-sized planet K2-25b, as well as the obliquity of its M4.5 dwarf host star in the 600-800 Myr Hyades cluster. This is one of the youngest planetary systems for which both of these quantities have been measured and one of the very few M dwarfs with a measured obliquity. Based on a joint analysis of the radial velocity data, time-series photometry from the K2 mission, and new transit light curves obtained with diffuser-assisted photometry, the planet's radius and mass are 3.44±0.12 R ⊕ and -+ Å M 24.5 5.2 5.7. These properties are compatible with a rocky core enshrouded by a thin hydrogen-helium atmosphere (5% by mass). We measure an orbital eccentricity of e=0.43±0.05. The skyprojected stellar obliquity is λ=3°±16°, compatible with spin-orbit alignment, in contrast to other "hot Neptunes" that have been studied around older stars.

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KPF: Keck Planet Finder

Cited by 49 publications

References 19 publications

Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. II. Discovery of a Failed Hot Jupiter on a 2.7 Yr, Highly Eccentric Orbit*

Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. II. Discovery of a Failed Hot Jupiter on a 2.7 Yr, Highly Eccentric Orbit*

Dynamics and Formation of the Near-resonant K2-24 System: Insights from Transit-timing Variations and Radial Velocities

The Habitable Zone Planet Finder Reveals a High Mass and Low Obliquity for the Young Neptune K2-25b

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