2010
DOI: 10.1088/0004-637x/720/2/1073
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Abstract: We present the first measurement of the planet frequency beyond the "snow line," for the planet-to-star mass-ratio interval −4.5 < log q < −2, corresponding to the range of ice giants to gas giants. We find d 2 N pl d log q d log s = (0.36 ± 0.15) dex −2 at the mean mass ratio q = 5 × 10 −4 with no discernible deviation from a flat (Öpik's law) distribution in logprojected separation s. The determination is based on a sample of six planets detected from intensive follow-up observations of high-magnification (A… Show more

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Cited by 318 publications
(443 citation statements)
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References 58 publications
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“…10 Jup and separation 0.5-10 AU, including constraints obtained by the two previous works by Sumi et al (2010) and Gould et al (2010), and found that there is one planet per star in the Galaxy. Clanton & Gaudi (2014) found that the planet abundances estimated by microlensing are consistent with those found by radial velocity.…”
Section: Introductionmentioning
confidence: 69%
See 1 more Smart Citation
“…10 Jup and separation 0.5-10 AU, including constraints obtained by the two previous works by Sumi et al (2010) and Gould et al (2010), and found that there is one planet per star in the Galaxy. Clanton & Gaudi (2014) found that the planet abundances estimated by microlensing are consistent with those found by radial velocity.…”
Section: Introductionmentioning
confidence: 69%
“…Sumi et al (2010) constructed the planet mass function beyond the snow line and found that Neptune-mass planets are ∼3 times more common than Jupiter-mass planets based on 10 microlensing planets. Gould et al (2010) estimated the planet abundance beyond the snow line based on six events and found that they are 7 times more likely than that at close orbits of 1 AU. Cassan et al (2012) used 6 yr of PLANET collaboration data to constrain the cool planetary mass function for masses -…”
Section: Introductionmentioning
confidence: 99%
“…However, if the method for measuring complete Kepler orbits can be extended from binaries to planets (as we begin to do here), then it will permit much stricter comparison between RV and microlensing samples, which has so far been possible only statistically, (e.g., Gould et al 2010;Clanton & Gaudi 2014a, 2014b. In particular, we provide here the first evidence for a non-circular orbit of a microlensing planet.…”
Section: Full Kepler Orbits In Microlensingmentioning
confidence: 80%
“…The statistical analysis of Suzuki et al (2016) shows that the planet detection efficiency weighted median t E value is »42 days, while the efficiency-corrected median is t E . This effect occurs for high-magnification events (Gould et al 2010b) because high magnification is much easier to predict when t E is large, and for low-magnification events (Suzuki et al 2016) because the planetary signal duration (for fixed q) is proportional to t E . This effect can be accounted for with accurate detection efficiency calculations, but Penny et al (2016) use a detection efficiency calculation for an advance ground-based survey that is much more sensitive than any ground-based survey undertaken to date.…”
Section: Lens Properties and Discussionmentioning
confidence: 99%
“…Higher density of solids speeds the planet formation process in the protoplanetary disk, hence forming cold planets quickly beyond the snow line. The planets, discovered by microlensing, provide the statistics needed to understand the architecture of cold planets beyond the snow line (Gould et al 2010b;Cassan et al 2012;Shvartzvald et al 2016;Suzuki et al 2016). Since this method does not rely on the light from the host stars, it can detect planets, even when the host stars cannot be detected (Mao & Paczyński 1991).…”
Section: Introductionmentioning
confidence: 99%