MOA 2011-BLG-028Lb: a Neptune-mass Microlensing Planet in the Galactic Bulge

We present the discovery of a Neptune-mass planet orbiting a 0.8 +- 0.3 M_Sun star in the Galactic bulge. The planet manifested itself during the microlensing event MOA 2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement...

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Bibliographic Details
Published in:arXiv.org 2015-12
Main Authors: Skowron, J, Udalski, A, Poleski, R, Kozłowski, S, Szymański, M K, Wyrzykowski, Ł, Ulaczyk, K, Pietrukowicz, P, Pietrzyński, G, Soszyński, I, The OGLE Collaboration, Abe, F, Bennett, D P, Bhattacharya, A, Bond, I A, Freeman, M, Fukui, A, Hirao, Y, Itow, Y, Koshimoto, N, Ling, C H, Masuda, K, Matsubara, Y, Muraki, Y, Nagakane, M, Ohnishi, K, Rattenbury, N, Saito, To, Sullivan, D J, Sumi, T, Suzuki, D, Tristram, P J, Yonehara, A, The MOA Collaboration, Dominik, M, Jørgensen, U G, Bozza, V, Harpsøe, K, Hundertmark, M, Skottfelt, J, The MiNDSTEp Collaboration
Format: Article
Language:English
Subjects:
Galactic bulge
Light curve
Microlenses
Motion effects
Parallax
Parameter estimation
Physical properties
Planetary mass
Windows (intervals)
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Summary:We present the discovery of a Neptune-mass planet orbiting a 0.8 +- 0.3 M_Sun star in the Galactic bulge. The planet manifested itself during the microlensing event MOA 2011-BLG-028/OGLE-2011-BLG-0203 as a low-mass companion to the lens star. The analysis of the light curve provides the measurement of the mass ratio: (1.2 +- 0.2) x 10^-4, which indicates the mass of the planet to be 12-60 Earth masses. The lensing system is located at 7.3 +- 0.7 kpc away from the Earth near the direction to Baade's Window. The projected separation of the planet, at the time of the microlensing event, was 3.1-5.2 AU. Although the "microlens parallax" effect is not detected in the light curve of this event, preventing the actual mass measurement, the uncertainties of mass and distance estimation are narrowed by the measurement of the source star proper motion on the OGLE-III images spanning eight years, and by the low amount of blended light seen, proving that the host star cannot be too bright and massive. We also discuss the inclusion of undetected parallax and orbital motion effects into the models, and their influence onto the final physical parameters estimates.
ISSN:2331-8422
DOI:10.48550/arxiv.1512.03422