K2-231 b: A Sub-Neptune Exoplanet Transiting a Solar Twin in Ruprecht 147

Curtis, Jason L.; Vanderburg, Andrew; Torres, Guillermo; Kraus, Adam L.; Huber, Daniel; Mann, Andrew W.; Rizzuto, Aaron C.; Isaacson, Howard; Howard, Andrew W.; Henze, Christopher E.; Fulton, Benjamin J.; Wright, Jason T.

doi:10.3847/1538-3881/aab49c

Cited by 56 publications

(30 citation statements)

References 139 publications

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“…The cluster metallicity is Z/Z = 0.017 (Bragaglia et al 2018). As mentioned before, this value is in agreement with the previous determinations of Curtis et al (2013Curtis et al ( , 2018.…”

Section: In the Resultssupporting

confidence: 93%

“…Later on, Torres et al (2018) determine and age of 2.65 ± 0.25 Gyr (with an extra ±0.13 Gyr uncertainty due to metallicity), and an extinction of 0.347 ± 0.09 mag for the eclipsing binary (hereafter EB) and cluster member (Curtis et al 2013) EPIC 219394517. In addition, Curtis et al (2018) determined the metallicity ([Fe/H] = +0.14 ± 0.04 dex) of the cluster member and solar twin EPIC 21980081. The previous metallicity values (Curtis et al 2013 are in agreement with the latest determination of the cluster metallicity ([Fe/H] = +0.08 ± 0.07 dex) done by Bragaglia et al (2018) based on 21 high probability cluster members.…”

Section: Introductionmentioning

confidence: 99%

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Ruprecht 147 DANCe

Olivares

Bouy

Sarro

et al. 2019

A&A

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Context. Ruprecht 147 is the oldest (2.5 Gyr) open cluster in the solar vicinity (<300 pc), making it an important target for stellar evolution studies and exoplanet searches. Aims. We aim to derive a census of members and the luminosity, mass, and spatial distributions of the cluster. Methods. We used an astro-photometric data set including all available information from the literature together with our own observations. We processed the data with an updated version of an existent membership selection methodology. Results. We identify 259 high-probability candidate members, including 58 previously unreported. All these candidates cover the luminosity interval between G 6 mag and i 21 mag. The cluster luminosity and mass distributions are derived with an unprecedented level of details allowing us to recognize, among other features, the Wielen dip. The mass distribution in the low-mass regime drops sharply at 0.4 M even though our data are sensitive to stellar masses down to 0.1 M , suggesting that most very-low-mass members left the cluster as the result of its dynamical evolution. In addition, the cluster is highly elongated (ellipticity ∼0.5) towards the galactic plane, and mass segregated. Conclusions. Our combined Gaia+DANCe data set allows us to obtain an extended list of cluster candidate members, and to derive luminosity, mass, and projected spatial distributions in the oldest open cluster of the solar vicinity.

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“…The cluster metallicity is Z/Z = 0.017 (Bragaglia et al 2018). As mentioned before, this value is in agreement with the previous determinations of Curtis et al (2013Curtis et al ( , 2018.…”

Section: In the Resultssupporting

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Ruprecht 147 DANCe

Olivares

Bouy

Sarro

et al. 2019

A&A

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“…There are too few planets in the vicinity of NGC 6819 to draw any conclusions. The exoplanet frequency in the inner and outer cylinders around NGC 6811 and NGC 6866 indicate no variation within current error bars, which is in agreement with the observations (Meibom et al 2013;Curtis et al 2018) and theoretical predictions (Bonnell et al 2001;Fujii & Hori 2018). We assumed that enhanced crowding in the clusters did not im- 1.5 × 10 −5 4.6 × 10 −5 4.1 × 10 −3 4.7 × 10 −3 −9.6 × 10 −3 6.5 × 10 −3 G » 169 2.3 × 10 −4 1.4 × 10 −4 5.3 × 10 −3 6.5 × 10 −3 1.9 × 10 −3 9.1 × 10 −3 K » 6 Number of objects is too low for statistics Table 2.…”

Section: Relative Exoplanet Frequency and Metallicity In The Vicinitysupporting

confidence: 88%

“…They concluded that the frequency of planets in this cluster is approximately equal to the field one. Curtis et al (2018) identified a sub-Neptune exoplanet transiting a solar twin EPIC 219800881(K2-231) in the Ruprecht 147 stellar cluster. This indicates an exoplanet frequency of the same order of magnitude as in NGC 6811.…”

Section: Introductionmentioning

confidence: 99%

Spatial distribution of exoplanet candidates based on Kepler and Gaia data

Maliuk

Budaj

2020

A&A

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Context. Surveying the spatial distribution of exoplanets in the Galaxy is important for improving our understanding of planet formation and evolution. Aims. We aim to determine the spatial gradients of exoplanet occurrence in the Solar neighbourhood and in the vicinity of open clusters. Methods. We combined Kepler and Gaia DR2 data for this purpose, splitting the volume sampled by the Kepler mission into certain spatial bins. We determined an uncorrected and bias-corrected exoplanet frequency and metallicity for each bin.Results. There is a clear drop in the uncorrected exoplanet frequency with distance for F-type stars (mainly for smaller planets), a decline with increasing distance along the Galactic longitude l = 90 • , and a drop with height above the Galactic plane. We find that the metallicity behaviour cannot be the reason for the drop of the exoplanet frequency around F stars with increasing distance. This might have only contributed to the drop in uncorrected exoplanet frequency with the height above the Galactic plane. We argue that the above-mentioned gradients of uncorrected exoplanet frequency are a manifestation of a single bias of undetected smaller planets around fainter stars. When we correct for observational biases, most of these gradients in exoplanet frequency become statistically insignificant. Only a slight decline of the planet occurrence with distance for F stars remains significant at the 3σ level. Apart from that, the spatial distribution of exoplanets in the Kepler field of view is compatible with a homogeneous one. At the same time, we do not find a significant change in the exoplanet frequency with increasing distance from open clusters. In terms of byproducts, we identified six exoplanet host star candidates that are members of open clusters. Four of them are in the NGC 6811 (KIC 9655005, KIC 9533489, Kepler-66, Kepler-67) and two belong to NGC 6866 (KIC 8396288, KIC 8331612). Two out of the six had already been known to be cluster members.

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“…With Kepler and K2 missions, a handful of planets were newly detected in four star clusters: Kepler-66b and 67b in NGC 6811 (Meibom et al 2013), five planets (K2-25 b, K2-136 b,c,d, and HD 283869 b) in the Hyades Livingston et al 2018;Ciardi et al 2018), eight planets (K2-95 b, K2-100 b,101 b,102 b,103 b,104 b, and K2-264 b,c) and one planetary candidate (EPIC 211901114 b) in the Preasepe (Obermeier et al 2016;Mann et al 2017;Pepper et al 2017; A&A 624, A110 (2019) Rizzuto et al 2018;Livingston et al 2019), and K2-231 b in Ruprecht 147 (Curtis et al 2018).…”

Section: Introductionmentioning

confidence: 98%

Survival rates of planets in open clusters: the Pleiades, Hyades, and Praesepe clusters

Fujii

Hori

2019

A&A

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Context. In clustered environments, stellar encounters can liberate planets from their host stars via close encounters. Although the detection probability of planets suggests that the planet population in open clusters resembles that in the field, only a few dozen planethosting stars have been discovered in open clusters. Aims. We explore the survival rates of planets against stellar encounters in open clusters similar to the Pleiades, Hyades, and Praesepe and embedded clusters. Methods. We performed a series of N-body simulations of high-density and low-density open clusters, open clusters that grow via mergers of subclusters, and embedded clusters. We semi-analytically calculated the survival rate of planets in star clusters up to ∼1 Gyr using relative velocities, masses, and impact parameters of intruding stars. Results. Less than 1.5% of close-in planets within 1 AU and at most 7% of planets with 1-10 AU are ejected by stellar encounters in clustered environments after the dynamical evolution of star clusters. If a planet population from 0.01-100 AU in an open cluster initially follows the probability distribution function of exoplanets with semi-major axis (a p ) between 0.03 and 3 AU in the field discovered by RV surveys (∝ a −0.6 p ), the PDF of surviving planets beyond ∼10 AU in open clusters can be slightly modified to ∝ a −0.76 p . The production rate of free-floating planets (FFPs) per star is 0.0096-0.18, where we have assumed that all the stars initially have one giant planet with a mass of 1-13 M Jup in a circular orbit. The expected frequency of FFPs is compatible with the upper limit on that of FFPs indicated by recent microlensing surveys. Our survival rates of planets in open clusters suggest that planets within 10 AU around FGKM-type stars are rich in relatively-young ( 10-100 Myr for open clusters and ∼1-10 Myr for embedded clusters), less massive open clusters, which are promising targets for planet searches.

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K2-231 b: A Sub-Neptune Exoplanet Transiting a Solar Twin in Ruprecht 147

Cited by 56 publications

References 139 publications

Ruprecht 147 DANCe

Ruprecht 147 DANCe

Spatial distribution of exoplanet candidates based on Kepler and Gaia data

Survival rates of planets in open clusters: the Pleiades, Hyades, and Praesepe clusters

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