The frequency of low-mass exoplanets. II. The "period valley"

Robert A. Wittenmyer, Simon J. O'Toole, H. R A Jones, C. G. Tinney, R. P. Butler, B. D. Carter, J. Bailey

Research output: Contribution to journalArticle

20 Citations (Scopus)

Abstract

Radial-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 17M (P = 50 days). Our results indicate that the observed "period valley," a lack of giant planets (M > 100M ) 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.

Original languageEnglish
Pages (from-to)1854-1863
Number of pages10
JournalAstrophysical Journal
Volume722
Issue number2
DOIs
Publication statusPublished - 20 Oct 2010

Keywords

  • Planetary systems
  • Techniques: radial velocities

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