Discovery of a Transiting Adolescent Sub-Neptune Exoplanet with K2

David, Trevor J.; Mamajek, Eric E.; Vanderburg, Andrew; Schlieder, Joshua E.; Bristow, Makennah; Petigura, Erik A.; Ciardi, David R.; Crossfield, Ian J. M.; Isaacson, Howard; Cody, Ann Marie; Stauffer, J. R.; Hillenbrand, Lynne A.; Bieryla, Allyson; Latham, David W.; Fulton, Benjamin J.; Rebull, L. M.; Beichman, C. A.; Gonzales, Erica J.; Hirsch, Lea A.; Howard, Andrew W.; Vasisht, Gautam; Ygouf, Marie

doi:10.3847/1538-3881/aaeed7

Cited by 29 publications

(18 citation statements)

References 154 publications

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“…Many of these targets are listed in Luhman (2018) as Group 29 members (see also Oh et al 2018). Some appear in the literature as possible members of Mu Tau (M. Gagne et al 2020, in preparation;Liu et al 2020) or possibly Cas-Tau (e.g., Hartmann et al 1991;de Zeeuw et al 1999;Luhman 2018; also see appendix of David et al 2018). Analyses to date of this population in the literature suggest that they are ∼30 Myr (e.g., Kraus et al 2017).…”

Section: A1 Membersmentioning

confidence: 99%

Rotation of Low-mass Stars in Taurus with K2

Rebull

Stauffer

Cody

et al. 2020

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We present an analysis of K2 light curves (LCs) from Campaigns 4 and 13 for members of the young (∼3 Myr) Taurus association, in addition to an older (∼30 Myr) population of stars that is largely in the foreground of the Taurus molecular clouds. Out of 156 of the highest-confidence Taurus members, we find that 81% are periodic. Our sample of young foreground stars is biased and incomplete, but nearly all stars (37/38) are periodic. The overall distribution of rotation rates as a function of color (a proxy for mass) is similar to that found in other clusters: the slowest rotators are among the early M spectral types, with faster rotation toward both earlier FGK and later M types. The relationship between period and color/mass exhibited by older clusters such as the Pleiades is already in place by Taurus age. The foreground population has very few stars but is consistent with the USco and Pleiades period distributions. As found in other young clusters, stars with disks rotate on average slower, and few with disks are found rotating faster than ∼2 days. The overall amplitude of the LCs decreases with age, and highermass stars have generally lower amplitudes than lower-mass stars. Stars with disks have on average larger amplitudes than stars without disks, though the physical mechanisms driving the variability and the resulting LC morphologies are also different between these two classes.

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Section: A1 Membersmentioning

confidence: 99%

Rotation of Low-mass Stars in Taurus with K2

Rebull

Stauffer

Cody

et al. 2020

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“…Despite these difficulties, Sanchis-Ojeda et al (2013) identified Kepler-63 b as a giant planet around a ∼ 300 Myr young field star, and made use of the spot activity to infer its orbital obliquity via transit spot-crossing events. The small planets around K2-233 (David et al 2018b) and EPIC 247267267 (David et al 2018a) are additional examples of young field stars with ages of 100-700 Myr discovered by the K2 mission.…”

Section: Introductionmentioning

confidence: 99%

Two Young Planetary Systems around Field Stars with Ages between 20 and 320 Myr from TESS

Zhou

Quinn

Irwin

et al. 2020

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Zhou et al. Planets around young stars trace the early evolution of planetary systems. We report the discovery and validation of two planetary systems with ages 300 Myr from observations by the Transiting Exoplanet Survey Satellite. TOI-251 is a 40 − 320 Myr old G star hosting a 2.74 +0.18 −0.18 R ⊕ mini-Neptune with a 4.94 day period. TOI-942 is a 20−160 Myr old K star hosting a system of inflated Neptune-sized planets, with TOI-942b orbiting with a period of 4.32 days, with a radius of 4.81 +0.20 −0.20 R ⊕ , and TOI-942c orbiting in a period of 10.16 days with a radius of 5.79 +0.19 −0.18 R ⊕. Though we cannot place either host star into a known stellar association or cluster, we can estimate their ages via their photometric and spectroscopic properties. Both stars exhibit significant photometric variability due to spot modulation, with measured rotation periods of ∼ 3.5 days. These stars also exhibit significant chromospheric activity, with age estimates from the chromospheric calcium emission lines and X-ray fluxes matching that estimated from gyrochronology. Both stars also exhibit significant lithium absorption, similar in equivalent width to well-characterized young cluster members. TESS has the potential to deliver a population of young planet-bearing field stars, contributing significantly to tracing the properties of planets as a function of their age.

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“…Other age indicators include stellar rotation periods, the abundance of photospheric lithium, and chromospheric diagnostics such as calcium emission and broadband UV emission. Studies by, for instance, Sanchis-Ojeda et al (2013) and David et al (2018) have combined these methods to age-date individual field stars hosting transiting planets. Many of these latter methods were summarized by Mamajek & Hillenbrand (2008) and have since been calibrated by, e.g., Irwin & Bouvier (2009), Barnes et al (2015), Meibom et al (2015), Angus et al (2015), and Curtis et al (2019b) for stellar rotation, Žerjal et al (2017) for chromospheric activity, and Berger et al (2018) and Žerjal et al (2019) for lithium abundance.…”

Section: Introductionmentioning

confidence: 99%

Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602

Bouma

Hartman

Brahm

et al. 2020

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We report the discovery of TOI 837b and its validation as a transiting planet. We characterize the system using data from the NASA Transiting Exoplanet Survey Satellite mission, the ESA Gaia mission, ground-based photometry from El Sauce and ASTEP400, and spectroscopy from CHIRON, FEROS, and Veloce. We find that TOI 837 is a T=9.9 mag G0/F9 dwarf in the southern open cluster IC 2602. The star and planet are therefore -+ Unified Astronomy Thesaurus concepts: Exoplanets (498); Transits (1711); Exoplanet evolution (491); Stellar ages (1581); Young star clusters (1833)

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Discovery of a Transiting Adolescent Sub-Neptune Exoplanet with K2

Cited by 29 publications

References 154 publications

Rotation of Low-mass Stars in Taurus with K2

Rotation of Low-mass Stars in Taurus with K2

Two Young Planetary Systems around Field Stars with Ages between 20 and 320 Myr from TESS

Cluster Difference Imaging Photometric Survey. II. TOI 837: A Young Validated Planet in IC 2602

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