Ensemble Analysis of Open Cluster Transit Surveys: Upper Limits on the Frequency of Short-Period Planets Consistent With the Field

Saders, Jennifer L. van; Gaudi, B. Scott

doi:10.1088/0004-637x/729/1/63

Cited by 56 publications

(18 citation statements)

References 84 publications

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“…Bramich et al ; Mochejska et al , ; Bramich & Horne ; Burke et al ; Rosvick & Robb ; Montalto et al , ; Miller et al ; Hartman et al ). Nevertheless, these null results from ground based surveys do not yet constrain the planet occurrence rate in open clusters to be lower than that expected from observations in the field (van Saders & Gaudi ). Hence, it would be very interesting to identify a promising candidate cluster where planets are expected to be detected.…”

Section: Introductioncontrasting

confidence: 59%

Planets in open clusters detectable byKepler

Chatterjee

Geller

Rasio

2012

Monthly Notices of the Royal Astronomical Society

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While hundreds of planets have been discovered around field stars, only a few are known in star clusters. To explain the lack of short‐period giant planets in globular clusters (GCs), such as 47 Tucane and ω Centauri, it has been suggested that their low metallicities may have prevented planet formation. Alternatively, the high rates of close stellar encounters in these clusters may have influenced the formation and subsequent evolution of planetary systems. How common are planets in clusters around normal main‐sequence stars? Here we consider whether this question can be addressed using data from the Kepler mission. The Kepler field of view contains four low‐density (relative to GCs) open clusters where the metallicities are about solar (or even higher) and stellar encounters are much less frequent than in typical GCs. We provide detailed N‐body models and show that most planets in Kepler‐detectable orbits are not significantly perturbed by stellar encounters in these open clusters. We focus on the most massive cluster, NGC 6791, which has supersolar metallicity, and find that if planets formed in this cluster at the same frequency as observed in the field, Kepler could detect 1–20 transiting planets depending on the planet‐size distribution and the duration of data collection. Due to the large distance to NGC 6791 Kepler will have to search relatively faint (Kp < 20) stars for the full extended mission to achieve such a yield.

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Section: Introductioncontrasting

confidence: 59%

Planets in open clusters detectable byKepler

Chatterjee

Geller

Rasio

2012

Monthly Notices of the Royal Astronomical Society

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“…We supply the algorithm with all of our determined constraints, including stellar photometry from 2MASS and WISE, contrast curves from high-angular resolution imaging and the light curve from K2. Furthermore, we also extract the photometric light curve from Vanderburg & Johnson (2014), remove the periodic modulations, recover the signal with the Pan-Planets signal detection pipeline (Obermeier et al 2016) and then perform the same analysis. This way, we end up with an independent confirmation based on a different data reduction and signal detection routine.…”

Section: False Positive Probabilitymentioning

confidence: 99%

K2 Discovers a Busy Bee: An Unusual Transiting Neptune Found in the Beehive Cluster

et al. 2016

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Open clusters have been the focus of several exoplanet surveys, but only a few planets have so far been discovered. The Kepler spacecraft revealed an abundance of small planets around small cool stars, therefore, such cluster members are prime targets for exoplanet transit searches. Keplerʼs new mission, K2, is targeting several open clusters and star-forming regions around the ecliptic to search for transiting planets around their low-mass constituents. Here, we report the discovery of the first transiting planet in the intermediate-age ( and an orbital period of 10.134 days. We combined photometry, medium/high-resolution spectroscopy, adaptive optics/speckle imaging, and archival survey images to rule out any false-positive detection scenarios, validate the planet, and further characterize the system. The planet's radius is very unusual as M-dwarf field stars rarely have Neptune-sized transiting planets. The comparatively large radius of K2-95b is consistent with the other recently discovered cluster planets K2-25b (Hyades) and K2-33b (Upper Scorpius), indicating systematic differences in their evolutionary states or formation. These discoveries from K2 provide a snapshot of planet formation and evolution in cluster environments and thus make excellent laboratories to test differences between field-star and cluster planet populations.

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“…In Section 4, we discuss the uniqueness of the candidate around HD 283869 and explore the path towards confirming the 12 The lack of detections from transit surveys of clusters was not entirely expected (see, e.g. van Saders & Gaudi 2011;Masuda & Winn 2017).…”

Section: Introductionmentioning

confidence: 99%

Zodiacal Exoplanets in Time (ZEIT). VII. A Temperate Candidate Super-Earth in the Hyades Cluster

Vanderburg

Mann

Rizzuto

et al. 2018

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Transiting exoplanets in young open clusters present opportunities to study how exoplanets evolve over their lifetimes. Recently, significant progress detecting transiting planets in young open clusters has been made with the K2 mission, but so far all of these transiting cluster planets orbit close to their host stars, so planet evolution can only be studied in a high-irradiation regime. Here, we report the discovery of a long-period planet candidate, called HD 283869 b, orbiting a member of the Hyades cluster. Using data from the K2 mission, we detected a single transit of a super-Earth-sized (1.96 ± 0.12 R ⊕ ) planet candidate orbiting the K-dwarf HD 283869 with a period longer than 72 days. Since we only detected a single transit event, we cannot validate HD 283869 b with high confidence, but our analysis of the K2 images, archival data, and follow-up observations suggests that the source of the event is indeed a transiting planet. We estimated the candidate's orbital parameters and find that if real, it has a period P≈100 days and receives approximately Earth-like incident flux, giving the candidate a 71% chance of falling within the circumstellar habitable zone. If confirmed, HD 283869 b would have the longest orbital period, lowest incident flux, and brightest host star of any known transiting planet in an open cluster, making it uniquely important to future studies of how stellar irradiation affects planetary evolution.

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Ensemble Analysis of Open Cluster Transit Surveys: Upper Limits on the Frequency of Short-Period Planets Consistent With the Field

Cited by 56 publications

References 84 publications

Planets in open clusters detectable byKepler

Planets in open clusters detectable byKepler

K2 Discovers a Busy Bee: An Unusual Transiting Neptune Found in the Beehive Cluster

Zodiacal Exoplanets in Time (ZEIT). VII. A Temperate Candidate Super-Earth in the Hyades Cluster

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