Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

Christiansen, Jessie L.; Vanderburg, Andrew; Burt, Jennifer; Fulton, Benjamin J.; Batygin, Konstantin; Benneke, Björn; Brewer, John M.; Charbonneau, David; Ciardi, David R.; Cameron, A. Collier; Coughlin, Jeffrey L.; Crossfield, Ian J. M.; Dressing, Courtney D.; Greene, Thomas P.; Howard, Andrew W.; Latham, David W.; Molinari, E.; Mortier, A.; Mullally, Fergal; Pepe, F.; Rice, Ken; Sinukoff, Evan; Sozzetti, A.; Thompson, Susan E.; Udry, S.; Vogt, Steven S.; Barman, Travis; Batalha, Natasha E.; Bouchy, F.; Buchhave, Lars A.; Butler, R. Paul; Cosentino, R.; Dupuy, Trent J.; Ehrenreich, D.; Fiorenzano, A. F. Martínez; Hansen, Brad M. S.; Henning, Thomas; Hirsch, Lea A.; Holden, B.; Isaacson, Howard; Johnson, John Asher; Knutson, Heather A.; Kosiarek, Molly R.; López‐Morales, Mercedes; Lovis, C.; Malavolta, L.; Mayor, M.; Micela, G.; Motalebi, F.; Petigura, Erik A.; Phillips, David F.; Piotto, G.; Rogers, Leslie; Sasselov, Dimitar; Schlieder, Joshua E.; Ségransan, D.; Watson, C. A.; Weiss, Lauren M.

doi:10.3847/1538-3881/aa832d

Cited by 97 publications

(47 citation statements)

References 108 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The empirical relation of Weiss & Marcy (2014) disguises a large scatter in the measured masses for planets ranging from 2-3 R Å , spanning nearly an order of magnitude from roughly 2-20 M ⊕ (see Figure 11 of Christiansen et al 2017). This diversity is due to a wide, degenerate mix of rock, volatile, and gas compositions that can comprise this size of planet.…”

Section: Discussionmentioning

confidence: 99%

The K2-138 System: A Near-resonant Chain of Five Sub-Neptune Planets Discovered by Citizen Scientists

Christiansen

Crossfield

Barentsen

et al. 2018

Self Cite

View full text Add to dashboard Cite

K2-138 is a moderately bright (V=12.2, K=10.3) main-sequence K star observed in Campaign 12 of the NASA K2 mission. It hosts five small (1.6-3.3 R Å ) transiting planets in a compact architecture. The periods of the five planets are 2. 35, 3.56, 5.40, 8.26, and 12.76 days, forming an unbroken chain of near 3:2 resonances. Although we do not detect the predicted 2-5 minute transit timing variations (TTVs) with the K2 timing precision, they may be observable by higher-cadence observations with, for example, Spitzer or CHEOPS. The planets are amenable to mass measurement by precision radial velocity measurements, and therefore K2-138 could represent a new benchmark system for comparing radial velocity and TTV masses. K2-138 is the first exoplanet discovery by citizen scientists participating in the Exoplanet Explorers project on the Zooniverse platform.

show abstract

Section: Discussionmentioning

confidence: 99%

The K2-138 System: A Near-resonant Chain of Five Sub-Neptune Planets Discovered by Citizen Scientists

Christiansen

Crossfield

Barentsen

et al. 2018

Self Cite

View full text Add to dashboard Cite

show abstract

“…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

Self Cite

133

119

View full text Add to dashboard Cite

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.

show abstract

“…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

Self Cite

176

235

View full text Add to dashboard Cite

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.

show abstract

Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets

Cited by 97 publications

References 108 publications

The K2-138 System: A Near-resonant Chain of Five Sub-Neptune Planets Discovered by Citizen Scientists

The K2-138 System: A Near-resonant Chain of Five Sub-Neptune Planets Discovered by Citizen Scientists

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

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

Contact Info

Product

Resources

About