Zodiacal Exoplanets in Time (Zeit). Iii. A Short-Period Planet Orbiting a Pre-Main-Sequence Star in the Upper Scorpius Ob Association

Mann, Andrew W.; Newton, Elisabeth R.; Rizzuto, Aaron C.; Irwin, Jonathan; Feiden, Gregory A.; Gaidos, Eric; Mace, Gregory N.; Kraus, Adam L.; James, D. J.; Ansdell, Megan; Charbonneau, David; Covey, Kevin R.; Ireland, Michael; Jaffe, D. T.; Johnson, Marshall C.; Kidder, Benjamin; Vanderburg, Andrew

doi:10.3847/0004-6256/152/3/61

Cited by 201 publications

(145 citation statements)

References 117 publications

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“…K2 has led to the discovery of numerous candidate and confirmed planets Foreman-Mackey et al 2015;Montet et al 2015;Vanderburg et al 2015bVanderburg et al , 2016bAdams et al 2016;Barros et al 2016;Crossfield et al 2016;Schlieder et al 2016;Sinukoff et al 2016;Pope et al 2016;Dressing et al 2017b;Hirano et al 2017;Martinez et al 2017), as well as to the identification of planets orbiting rare types of stars, including particularly bright nearby dwarf stars Vanderburg et al 2016a;Christiansen et al 2017;Crossfield et al 2017;Niraula et al 2017;Rodriguez et al 2017aRodriguez et al , 2017b, young, pre-main-sequence stars (Mann et al 2016;David et al 2016), and disintegrating planetary material transiting a white dwarf (Vanderburg et al 2015a).…”

Section: Introductionmentioning

confidence: 99%

275 Candidates and 149 Validated Planets Orbiting Bright Stars in K2 Campaigns 0–10

Mayo

Vanderburg

Latham

et al. 2018

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Since 2014, NASA's K2 mission has observed large portions of the ecliptic plane in search of transiting planets and has detected hundreds of planet candidates. With observations planned until at least early 2018, K2 will continue to identify more planet candidates. We present here 275 planet candidates observed during Campaigns 0-10 of the K2 mission that are orbiting stars brighter than 13 mag (in Kepler band) and for which we have obtained highresolution spectra (R = 44,000). These candidates are analyzed using the vespa package in order to calculate their false-positive probabilities (FPP). We find that 149 candidates are validated with an FPP lower than 0.1%, 39 of which were previously only candidates and 56 of which were previously undetected. The processes of data reduction, candidate identification, and statistical validation are described, and the demographics of the candidates and newly validated planets are explored. We show tentative evidence of a gap in the planet radius distribution of our candidate sample. Comparing our sample to the Kepler candidate sample investigated by Fulton et al., we conclude that more planets are required to quantitatively confirm the gap with K2 candidates or validated planets. This work, in addition to increasing the population of validated K2 planets by nearly 50% and providing new targets for follow-up observations, will also serve as a framework for validating candidates from upcoming K2 campaigns and the Transiting Exoplanet Survey Satellite, expected to launch in 2018.

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Section: Introductionmentioning

confidence: 99%

275 Candidates and 149 Validated Planets Orbiting Bright Stars in K2 Campaigns 0–10

Mayo

Vanderburg

Latham

et al. 2018

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177

235

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“…Since the radio flux scales directly with the power of the incident stellar wind, targeting young systems that host dense, strong stellar winds may offer an exciting opportunity to make a definitive detection of radio emission from exoplanets. Indeed, there are now a number of planets known around young stars, including CI Tau b (Johns-Krull et al 2016), V830 Tau b (Donati et al 2016), K2-33 b (David et al 2016;Mann et al 2016), and TAP 26 b (Yu et al 2017). Vidotto & Donati (2017) carried out a theoretical study to predict the radio emission from V830 Tau b, a ∼2 Myr old hot Jupiter orbiting a pre-main sequence star.…”

Section: Introductionmentioning

confidence: 99%

Simulating Radio Emission from Low-mass Stars

Llama

Jardine

Wood

et al. 2018

ApJ

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Understanding the origins of stellar radio emission can provide invaluable insight into the strength and geometry of stellar magnetic fields and the resultant space weather environment experienced by exoplanets. Here, we present the first model capable of predicting radio emission through the electron cyclotron maser instability using observed stellar magnetic maps of low-mass stars. We determine the structure of the coronal magnetic field and plasma using spectropolarimetric observations of the surface magnetic fields and the X-ray emission measure. We then model the emission of photons from the locations within the corona that satisfy the conditions for electron cyclotron maser emission. Our model predicts the frequency and intensity of radio photons from within the stellar corona. We have benchmarked our model against the low-mass star V374 Peg. This star has both radio observations from the Very Large Array and a nearly simultaneous magnetic map. Using our model we are able to fit the radio observations of V374 Peg, providing additional evidence that the radio emission observed from low-mass stars may originate from the electron cyclotron maser instability. Our model can now be extended to all stars with observed magnetic maps to predict the expected frequency and variability of stellar radio emission in an effort to understand and guide future radio observations of low-mass stars.

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“…The Kepler era of discovery was instead expected to give way to a new era in which the K2 mission would largely find more of the same kinds of planets that had been previously discovered, just orbiting brighter stars or in different environments. While K2 has certainly delivered in that regard, finding small planets around nearby stars well-suited to detailed characterization (Vanderburg et al , 2016aSinukoff et al 2016;Crossfield et al 2017; Rodriguez et al 2017), temperate planets around M-dwarfs Petigura et al 2015;Dressing et al 2017aDressing et al , 2017bMartinez et al 2017), and planets in open clusters (David et al 2016;Libralato et al 2016;Mann et al 2016aMann et al , 2016bObermeier et al 2016;Mann et al 2017), K2 is still delivering new and unexpected discoveries, like the unique architecture of the WASP-47 system, that are yielding fundamental insights about the formation and evolution of planetary systems.…”

Section: Introductionmentioning

confidence: 99%

Precise Masses in the WASP-47 System

Vanderburg

Becker

Buchhave

et al. 2017

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We present precise radial velocity observations of WASP-47, a star known to host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional transiting planets in short-period orbits: a super-Earth in a ≈19 hr orbit, and a Neptune in a ≈9 day orbit. We analyze our observations from the HARPS-N spectrograph along with previously published data to measure the most precise planet masses yet for this system. When combined with new stellar parameters and reanalyzed transit photometry, our mass measurements place strong constraints on the compositions of the two small planets. We find that, unlike most other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83 ± 0.66 Å M ) and a radius (1.810 ± 0.027 Å R ) that are inconsistent with an Earth-like composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding an Earth-like core and mantle. We also perform a dynamical analysis to constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This planet likely orbits close to the plane of the inner three planets, suggesting a quiet dynamical history for the system. Our dynamical constraints also imply that WASP-47 c is much more likely to transit than a geometric calculation would suggest. We calculate a transit probability for WASP-47 c of about 10%, more than an order of magnitude larger than the geometric transit probability of 0.6%.

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Zodiacal Exoplanets in Time (Zeit). Iii. A Short-Period Planet Orbiting a Pre-Main-Sequence Star in the Upper Scorpius Ob Association

Cited by 201 publications

References 117 publications

275 Candidates and 149 Validated Planets Orbiting Bright Stars in K2 Campaigns 0–10

275 Candidates and 149 Validated Planets Orbiting Bright Stars in K2 Campaigns 0–10

Simulating Radio Emission from Low-mass Stars

Precise Masses in the WASP-47 System

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