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The same frequency of planets inside and outside open clusters of stars

Meibom, Søren and Torres, Guillermo and Fressin, Francois and Latham, David W. and Rowe, Jason F. and Ciardi, David R. and Bryson, Steven T. and Rogers, Leslie A. and Henze, Christopher E. and Janes, Kenneth and Barnes, Sydney A. and Marcy, Geoffrey W. and Isaacson, Howard and Fischer, Debra A. and Howell, Steve B. and Horch, Elliott P. and Jenkins, Jon M. and Schuler, Simon C. and Crepp, Justin (2013) The same frequency of planets inside and outside open clusters of stars. Nature, 499 (7456). pp. 55-58. ISSN 0028-0836. https://resolver.caltech.edu/CaltechAUTHORS:20130805-101335123

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Abstract

Most stars and their planets form in open clusters. Over 95 per cent of such clusters have stellar densities too low (less than a hundred stars per cubic parsec) to withstand internal and external dynamical stresses and fall apart within a few hundred million years. Older open clusters have survived by virtue of being richer and denser in stars (1,000 to 10,000 per cubic parsec) when they formed. Such clusters represent a stellar environment very different from the birthplace of the Sun and other planet-hosting field stars. So far more than 800 planets have been found around Sun-like stars in the field. The field planets are usually the size of Neptune or smaller. In contrast, only four planets have been found orbiting stars in open clusters, all with masses similar to or greater than that of Jupiter. Here we report observations of the transits of two Sun-like stars by planets smaller than Neptune in the billion-year-old open cluster NGC6811. This demonstrates that small planets can form and survive in a dense cluster environment, and implies that the frequency and properties of planets in open clusters are consistent with those of planets around field stars in the Galaxy.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1038/nature12279DOIArticle
http://www.nature.com/nature/journal/v499/n7456/full/nature12279.htmlPublisherArticle
http://arxiv.org/abs/1307.5842arXivDiscussion Paper
http://rdcu.be/cm3SPublisherFree ReadCube access
ORCID:
AuthorORCID
Torres, Guillermo0000-0002-5286-0251
Latham, David W.0000-0001-9911-7388
Rowe, Jason F.0000-0002-5904-1865
Ciardi, David R.0000-0002-5741-3047
Rogers, Leslie A.0000-0003-0638-3455
Marcy, Geoffrey W.0000-0002-2909-0113
Isaacson, Howard0000-0002-0531-1073
Fischer, Debra A.0000-0003-2221-0861
Howell, Steve B.0000-0002-2532-2853
Horch, Elliott P.0000-0003-2159-1463
Jenkins, Jon M.0000-0002-4715-9460
Crepp, Justin0000-0003-0800-0593
Additional Information:© 2013 Macmillan Publishers Limited. Received 6 November 2012; accepted 2 May 2013; Published online 26 June 2013. Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA’s Science Mission Directorate. S.M. acknowledges support through NASA grant NNX09AH18A (The Kepler Cluster Study) and from the Kepler mission via NASA Cooperative Agreement NCC2-1390. G.T. acknowledges support through NASA’s Kepler Participating Scientist Program grant NNX12AC75G. L.A.R. acknowledges NASA support through Hubble Fellowship grant HF-51313.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Author Contributions: S.M. is the Principal Investigator of The Kepler Cluster Study and led the writing of the paper and the effort to identify members of NGC6811. He worked with G.T. and F.F. on characterization and validation of Kepler-66b and Kepler-67b, and with K.J. and S.A.B. on determination of the properties of NGC6811. G.T. developed the BLENDER software used to validate the planets, and determined the stellar properties of the host stars. F.F. worked on the BLENDER validation of the two planets and the Monte-Carlo simulation of the cluster yield. D.W.L. contributed follow-up spectroscopy of host stars. J.F.R. performed the light-curve analysis to extract the planet characteristics. D.R.C. provided constraints on angular separation of potential background blends fromadaptive optics imaging. S.T.B. performed pixel-level centroid analysis. C.E.H. assisted in running BLENDER on the NASA Pleiades supercomputer. L.A.R.modelled the planets’ interior structure to constrain the range of possible masses and compositions. K.J. led the supporting photometric study from which the bulk properties of NGC6811 are derived. S.A.B. participated in the acquisition of ground-based spectroscopic and photometric data on NGC6811. G.W.M. and H.I. obtained and analysed high-resolution Keck HIRES spectra of the host stars used for the BLENDER analysis. D.A.F. analysed HIRES spectra using the Spectroscopy Made Easy software. S.B.H. andE.P.H. obtained andanalysed speckle observations of the host stars. J.M.J. led the efforts of data collection, data processing and data review that yielded the Kepler time series photometry. S.C.S. did spectroscopic analysis of stellar members of NGC6811 to aid in the determination of cluster parameters including metallicity. J.C. obtained adaptive optics imaging observations.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANNX09AH18A
NASANCC2-1390
NASANNX12AC75G
NASA Hubble FellowshipHF-51313.01-A
NASANAS 5-26555
Subject Keywords:Exoplanets
Issue or Number:7456
Record Number:CaltechAUTHORS:20130805-101335123
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130805-101335123
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39760
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:06 Aug 2013 14:31
Last Modified:09 Mar 2020 13:18

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