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dc.creatorBorucki, William J.en_US
dc.creatorKoch, David G.en_US
dc.creatorBasri, Giboren_US
dc.creatorBatalha, Natalieen_US
dc.creatorBrown, Timothy M.en_US
dc.creatorBryson, Stephen T.en_US
dc.creatorCaldwell, Douglasen_US
dc.creatorChristensen-Dalsgaard, Jorgenen_US
dc.creatorCochran, William D.en_US
dc.creatorDeVore, Ednaen_US
dc.creatorDunham, Edward W.en_US
dc.creatorGautier, Thomas N., IIIen_US
dc.creatorGeary, John C.en_US
dc.creatorGilliland, Ronalden_US
dc.creatorGould, Alanen_US
dc.creatorHowell, Steve B.en_US
dc.creatorJenkins, Jon M.en_US
dc.creatorLatham, David W.en_US
dc.creatorLissauer, Jack J.en_US
dc.creatorMarcy, Geoffrey W.en_US
dc.creatorRowe, Jasonen_US
dc.creatorSasselov, Dimitaren_US
dc.creatorBoss, Alanen_US
dc.creatorCharbonneau, Daviden_US
dc.creatorCiardi, Daviden_US
dc.creatorDoyle, Lauranceen_US
dc.creatorDupree, Andrea K.en_US
dc.creatorFord, Eric B.en_US
dc.creatorFortney, Jonathanen_US
dc.creatorHolman, Matthew J.en_US
dc.creatorSeager, Saraen_US
dc.creatorSteffen, Jason H.en_US
dc.creatorTarter, Jillen_US
dc.creatorWelsh, William F.en_US
dc.creatorAllen, Christopheren_US
dc.creatorBuchhave, Lars A.en_US
dc.creatorChristiansen, Jessie L.en_US
dc.creatorClarke, Bruce D.en_US
dc.creatorDas, Santanuen_US
dc.creatorDesert, Jean-Michelen_US
dc.creatorEndl, Michaelen_US
dc.creatorFabrycky, Danielen_US
dc.creatorFressin, Francoisen_US
dc.creatorHaas, Michaelen_US
dc.creatorHorch, Elliotten_US
dc.creatorHoward, Andrewen_US
dc.creatorIsaacson, Howarden_US
dc.creatorKjeldsen, Hansen_US
dc.creatorKolodziejczak, Jefferyen_US
dc.creatorKulesa, Craigen_US
dc.creatorLi, Jieen_US
dc.creatorLucas, Philip W.en_US
dc.creatorMachalek, Pavelen_US
dc.creatorMcCarthy, Donalden_US
dc.creatorMacQueen, Phillipen_US
dc.creatorMeibom, Sorenen_US
dc.creatorMiquel, Thibauten_US
dc.creatorPrsa, Andrejen_US
dc.creatorQuinn, Samuel N.en_US
dc.creatorQuintana, Elisa V.en_US
dc.creatorRagozzine, Darinen_US
dc.creatorSherry, Williamen_US
dc.creatorShporer, Avien_US
dc.creatorTenenbaum, Peteren_US
dc.creatorTorres, Guillermoen_US
dc.creatorTwicken, Joseph D.en_US
dc.creatorVan Cleve, Jeffreyen_US
dc.creatorWalkowicz, Lucianneen_US
dc.creatorWitteborn, Fred C.en_US
dc.creatorStill, Martinen_US
dc.date.accessioned2016-04-28T19:42:42Z
dc.date.available2016-04-28T19:42:42Z
dc.date.issued2011-07en
dc.identifierdoi:10.15781/T22V56
dc.identifier.citationBorucki, William J., David G. Koch, Gibor Basri, Natalie Batalha, Timothy M. Brown, Stephen T. Bryson, Douglas Caldwell et al. "Characteristics of planetary candidates observed by Kepler. II. Analysis of the first four months of data." The Astrophysical Journal, Vol. 736, No. 1 (Jul., 2011): 19.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35151
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.en_US
dc.description.sponsorshipNASA's Science Mission Directorateen_US
dc.description.sponsorshipW. M. Keck Foundationen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectplanetary systemsen_US
dc.subjectstars: statisticsen_US
dc.subjectplanets and satellites: detectionen_US
dc.subjectsurveysen_US
dc.subjectterrestrial planetsen_US
dc.subjectinitial characteristicsen_US
dc.subjecttransiting planeten_US
dc.subjecttargeten_US
dc.subjectstarsen_US
dc.subjectcadence dataen_US
dc.subjectdwarf starsen_US
dc.subjectlow-densityen_US
dc.subjecthabitabilityen_US
dc.subjectsystemen_US
dc.subjectfielden_US
dc.subjectastronomy & astrophysicsen_US
dc.titleCharacteristics Of Planetary Candidates Observed By Kepler. II. Analysis Of The First Four Months Of Dataen_US
dc.typeArticleen_US
dc.description.departmentMcDonald Observatoryen_US
dc.identifier.Filename2011_07_planetarycandidates.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/736/1/19en_US
dc.contributor.utaustinauthorCochran, William D.en_US
dc.contributor.utaustinauthorEndl, Michaelen_US
dc.relation.ispartofserialAstrophysical Journalen_US


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