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dc.contributor.authorBorucki, William J.
dc.contributor.authorKoch, David G.
dc.contributor.authorBasri, Gibor
dc.contributor.authorBatalha, Natalie
dc.contributor.authorBrown, Timothy M.
dc.contributor.authorBryson, Stephen T.
dc.contributor.authorCaldwell, Douglas
dc.contributor.authorChristensen-Dalsgaard, Jørgen
dc.contributor.authorCochran, William D.
dc.contributor.authorDeVore, Edna
dc.contributor.authorDunham, Edward W.
dc.contributor.authorGautier, Thomas N.
dc.contributor.authorGeary, John C.
dc.contributor.authorGilliland, Ronald
dc.contributor.authorGould, Alan
dc.contributor.authorHowell, Steve B.
dc.contributor.authorJenkins, Jon M.
dc.contributor.authorLatham, David W.
dc.contributor.authorLissauer, Jack J.
dc.contributor.authorMarcy, Geoffrey W.
dc.contributor.authorRowe, Jason
dc.contributor.authorSasselov, Dimitar
dc.contributor.authorBoss, Alan
dc.contributor.authorCharbonneau, David
dc.contributor.authorCiardi, David
dc.contributor.authorDoyle, Laurance
dc.contributor.authorDupree, Andrea K.
dc.contributor.authorFord, Eric B.
dc.contributor.authorFortney, Jonathan
dc.contributor.authorHolman, Matthew J.
dc.contributor.authorSeager, Sara
dc.contributor.authorSteffen, Jason H.
dc.contributor.authorTarter, Jill
dc.contributor.authorWelsh, William F.
dc.contributor.authorAllen, Christopher
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorChristiansen, Jessie L.
dc.contributor.authorClarke, Bruce D.
dc.contributor.authorDas, Santanu
dc.contributor.authorDésert, Jean-Michel
dc.contributor.authorEndl, Michael
dc.contributor.authorFabrycky, Daniel
dc.contributor.authorFressin, Francois
dc.contributor.authorHaas, Michael
dc.contributor.authorHorch, Elliott
dc.contributor.authorHoward, Andrew
dc.contributor.authorIsaacson, Howard
dc.contributor.authorKjeldsen, Hans
dc.contributor.authorKolodziejczak, Jeffery
dc.contributor.authorKulesa, Craig
dc.contributor.authorLi, Jie
dc.contributor.authorLucas, Philip W.
dc.contributor.authorMachalek, Pavel
dc.contributor.authorMcCarthy, Donald
dc.contributor.authorMacQueen, Phillip
dc.contributor.authorMeibom, Søren
dc.contributor.authorMiquel, Thibaut
dc.contributor.authorPrsa, Andrej
dc.contributor.authorQuinn, Samuel N.
dc.contributor.authorQuintana, Elisa V.
dc.contributor.authorRagozzine, Darin
dc.contributor.authorSherry, William
dc.contributor.authorShporer, Avi
dc.contributor.authorTenenbaum, Peter
dc.contributor.authorTorres, Guillermo
dc.contributor.authorTwicken, Joseph D.
dc.contributor.authorVan Cleve, Jeffrey
dc.contributor.authorWalkowicz, Lucianne
dc.contributor.authorWitteborn, Fred C.
dc.contributor.authorStill, Martin
dc.date.accessioned2019-09-24T17:25:19Z
dc.date.issued2011
dc.identifier.citationBorucki, William J., David G. Koch, Gibor Basri, Natalie Batalha, Timothy M. Brown, Stephen T. Bryson, Douglas Caldwell, et al. 2011. “CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BYKEPLER. II. ANALYSIS OF THE FIRST FOUR MONTHS OF DATA.” The Astrophysical Journal 736 (1): 19. https://doi.org/10.1088/0004-637x/736/1/19.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41397421*
dc.description.abstractOn 2011 February 1 the Kepler mission released data for 156,453 stars observed from the beginning of the science observations on 2009 May 2 through September 16. There are 1235 planetary candidates with transit-like signatures detected in this period. These are associated with 997 host stars. Distributions of the characteristics of the planetary candidates are separated into five class sizes: 68 candidates of approximately Earth-size (R-p < 1.25 R-circle plus), 288 super-Earth-size (1.25 R-circle plus <= R-p < 2 R-circle plus), 662 Neptune-size (2 R-circle plus <= R-p < 6 R-circle plus), 165 Jupiter-size (6 R-circle plus <= R-p < 15 R-circle plus), and 19 up to twice the size of Jupiter (15 R-circle plus <= R-p < 22 R-circle plus). In the temperature range appropriate for the habitable zone, 54 candidates are found with sizes ranging from Earth-size to larger than that of Jupiter. Six are less than twice the size of the Earth. Over 74% of the planetary candidates are smaller than Neptune. The observed number versus size distribution of planetary candidates increases to a peak at two to three times the Earth-size and then declines inversely proportional to the area of the candidate. Our current best estimates of the intrinsic frequencies of planetary candidates, after correcting for geometric and sensitivity biases, are 5% for Earth-size candidates, 8% for super-Earth-size candidates, 18% for Neptune-size candidates, 2% for Jupiter-size candidates, and 0.1% for very large candidates; a total of 0.34 candidates per star. Multi-candidate, transiting systems are frequent; 17% of the host stars have multi-candidate systems, and 34% of all the candidates are part of multi-candidate systems.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleCharacteristics of Planetary Candidates Observed by Kepler . Ii. Analysis of the First Four Months of Data
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorCharbonneau, David::a0e3ca75d3fb8511f2f554ed69428108::600
dc.date.available2019-09-24T17:25:19Z
dash.workflow.comments1Science Serial ID 98727
dc.identifier.doi10.1088/0004-637X/736/1/19
dash.source.volume736;1
dash.source.page19


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