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OGLE-2017-BLG-1434Lb: Eighth q < 1 x 10(-4) Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function
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Number of Authors: 582018 (English)In: Acta Astronomica, ISSN 0001-5237, Vol. 68, no 1, p. 1-42Article in journal (Refereed) Published
Abstract [en]

We report the discovery of a cold Super-Earth planet (m(p) = 4.4 +/- 0.5 M-circle plus) orbiting a low-mass (M = 0.23 +/- 0.03 M-circle dot) M dwarf at projected separation a(perpendicular to) l = 1.18 +/- 0.10 a.u., i.e., about 1.9 times the distance the snow line. The system is quite nearby for a microlensing planet, D-L = 0.86 +/- 0.09 kpc. Indeed, it was the large lens-source relative parallax pi(rel) = 1.0 mas (combined with the low mass M) that gave rise to the large, and thus well-measured, microlens parallax pi(E) proportional to (pi(rel)/M)(1)(/2) that enabled these precise measurements. OGLE-2017-BLG-1434Lb is the eighth microlensing planet with planet-host mass ratio q < 1 x 10(-4). We apply a new planet-detection sensitivity method, which is a variant of V/V-max, to seven of these eight planets to derive the mass-ratio function in this regime. We find dN/ d lnq proportional to q(P) , with p =1.05(-0.68)(+0.78), which confirms the turnover in the mass function found by Suzuki et al. relative to the power law of opposite sign n = -0.93 +/- 0.13 at higher mass ratios q greater than or similar to 2 x 10(-4). We combine our result with that of Suzuki et al. to obtain p = 0.73(-0.34)(+0.42.)

Place, publisher, year, edition, pages
2018. Vol. 68, no 1, p. 1-42
Keywords [en]
Gravitational lensing: micro, Planetary systems
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-156703ISI: 000432182200001OAI: oai:DiVA.org:su-156703DiVA, id: diva2:1210965
Available from: 2018-05-30 Created: 2018-05-30 Last updated: 2018-05-30Bibliographically approved

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OGLE-2017-BLG-1434Lb: Eighth q < 1 x 10(-4) Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function

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Ciceri, Simona
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