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dc.contributor.authorWittenmyer, R.
dc.contributor.authorO'Toole, S.
dc.contributor.authorJones, H.R.A.
dc.contributor.authorTinney, C.G.
dc.contributor.authorButler, R.P.
dc.contributor.authorCarter, B.D.
dc.contributor.authorBailey, J.
dc.identifier.citationWittenmyer , R , O'Toole , S , Jones , H R A , Tinney , C G , Butler , R P , Carter , B D & Bailey , J 2010 , ' The frequency of low-mass exoplanets. II. The "Period Valley" ' , The Astrophysical Journal , vol. 722 , no. 2 , pp. 1854-1863 .
dc.identifier.otherPURE: 158860
dc.identifier.otherPURE UUID: 02dc50e8-aa10-418b-ba62-fed62051cada
dc.identifier.otherdspace: 2299/5057
dc.identifier.otherScopus: 78149246299
dc.descriptionOriginal article can be found at: Copyright American Astronomical Society [Full text of this article is not available in the UHRA]
dc.description.abstractRadial-velocity planet search campaigns are now beginning to detect low-mass "Super-Earth" planets, with minimum masses M sin i 10 M ⊕. Using two independently developed methods, we have derived detection limits from nearly four years of the highest-precision data on 24 bright, stable stars from the Anglo-Australian Planet Search. Both methods are more conservative than a human analyzing an individual observed data set, as is demonstrated by the fact that both techniques would detect the radial-velocity signals announced as exoplanets for the 61 Vir system in 50% of trials. There are modest differences between the methods which can be recognized as arising from particular criteria that they adopt. What both processes deliver is a quantitative selection process such that one can use them to draw quantitative conclusions about planetary frequency and orbital parameter distribution from a given data set. Averaging over all 24 stars, in the period range P< 300 days and the eccentricity range 0.0 < e < 0.6, we could detect 99% of planets with velocity amplitudes K 7.1 m s–1. For the best stars in the sample, we are able to detect or exclude planets with K 3 m s–1, corresponding to minimum masses of 8 M ⊕ (P = 5 days) or 17 M ⊕ (P = 50 days). Our results indicate that the observed "period valley," a lack of giant planets (M > 100 M ⊕) with periods between 10 and 100 days, is indeed real. However, for planets in the mass range 10-100 M ⊕, our results suggest that the deficit of such planets may be a result of selection effects. [please see online version for correct notation]en
dc.relation.ispartofThe Astrophysical Journal
dc.titleThe frequency of low-mass exoplanets. II. The "Period Valley"en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review

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