Skip to main content

Research Repository

Advanced Search

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

Udalski, A.; Ryu, Y.-H.; Sajadian, S.; Gould, A.; Mróz, P.; Poleski, R.; Szymański, M.K.; Skowron, J.; Soszyński, I.; Kozłowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Pawlak, M.; Rybicki, K.; Iwanek, P.; Albrow, M.D.; Chung, S.-J.; Han, C.; Hwang, K.-H.; Jung, Y.K.; Shin, I.-G.; Shvartzvald, Y.; Yee, J.C.; Zang, W.; Zhu, W.; Cha, S.-M.; Kim, D.-J.; Kim, H.-W.; Kim, S.-L.; Lee, C.-U.; Lee, D.-J.; Lee, Y.; Park, B.-G.; Pogge, R.W.; Bozza, V.; Dominik, M.; Helling, C.; Hundertmark, M.; Jørgensen, U.G.; Longa-Peña, P.; Lowry, S.; Burgdorf, M.; Campbell-White, J.; Ciceri, S.; Evans, D.; Figuera Jaimes, R.; Fujii, Y.I.; Haikala, L.K.; Henning, T.; Hinse, T.C.; Mancini, L.; Peixinho, N.; Rahvar, S.; Rabus, M.; Skottfelt, J.; Snodgrass, C.; Southworth, J.; von Essen, C.

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


Authors

A. Udalski

Y.-H. Ryu

S. Sajadian

A. Gould

P. Mróz

R. Poleski

M.K. Szymański

J. Skowron

I. Soszyński

S. Kozłowski

P. Pietrukowicz

K. Ulaczyk

M. Pawlak

K. Rybicki

P. Iwanek

M.D. Albrow

S.-J. Chung

C. Han

K.-H. Hwang

Y.K. Jung

I.-G. Shin

Y. Shvartzvald

J.C. Yee

W. Zang

W. Zhu

S.-M. Cha

D.-J. Kim

H.-W. Kim

S.-L. Kim

C.-U. Lee

D.-J. Lee

Y. Lee

B.-G. Park

R.W. Pogge

V. Bozza

M. Dominik

C. Helling

M. Hundertmark

U.G. Jørgensen

P. Longa-Peña

S. Lowry

M. Burgdorf

J. Campbell-White

S. Ciceri

D. Evans

R. Figuera Jaimes

Y.I. Fujii

L.K. Haikala

T. Henning

T.C. Hinse

L. Mancini

N. Peixinho

S. Rahvar

M. Rabus

J. Skottfelt

C. Snodgrass

C. von Essen



Abstract

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.)

Journal Article Type Article
Acceptance Date Feb 8, 2018
Publication Date Mar 1, 2018
Journal Acta Astronomica
Print ISSN 0001-5237
Publisher Copernicus Foundation for Polish Astronomy
Peer Reviewed Peer Reviewed
Volume 68
Issue 1
Pages 1 -42
DOI https://doi.org/10.32023/0001-5237/68.1.1
Keywords gravitational lensing, planetary systems
Publisher URL http://acta.astrouw.edu.pl/

Files




You might also like



Downloadable Citations