Characterizing microlensing planetary system OGLE-2014-BLG-0676Lb with adaptive optics imaging

Creators: Xie, Xiao-Jia; Dong, Subo; Shvartzvald, Yossi; Gould, Andrew; Udalski, Andrzej; Beaulieu, Jean-Philippe; Beichman, Charles; Close, Laird Miller; Henderson, Calen B.; Males, Jared R.; Marquette, Jean-Baptiste; Morzinski, Katie M.; Gelino, Christopher R.

Abstract

We constrain the host-star flux of the microlensing planet OGLE-2014-BLG-0676Lb using adaptive optics (AO) images taken by the Magellan and Keck telescopes. We measure the flux of the light blended with the microlensed source to be K = 16.79 ± 0.04 mag and J = 17.76 ± 0.03 mag. Assuming that the blend is the lens star, we find that the host is a 0.73^(+0.14)_(−0.29) M⊙ star at a distance of 2.67^(+0.77)_(−1.41) kpc, where the relatively large uncertainty in angular Einstein radius measurement is the major source of uncertainty. With mass of M_p = 3.68^(+0.69)_(−1.44) M_J, the planet is likely a "super Jupiter" at a projected separation of r_⊥ = 4.53^(+1.49)_(−2.50) AU, and a degenerate model yields a similar M_p = 3.73^(+0.73)_(−1.47) M_J at a closer separation of r_⊥ = 2.56^(+0.84)_(−1.41) AU. Our estimates are consistent with the previous Bayesian analysis based on a Galactic model. OGLE-2014-BLG-0676Lb belongs to a sample of planets discovered in a "second-generation" planetary microlensing survey and we attempt to systematically constrain host properties of this sample with high-resolution imaging to study the distribution of planets.

Additional Information

© 2021 National Astronomical Observatories, CAS and IOP Publishing Ltd. Received 2 June 2021; Accepted 23 September 2021. We acknowledge the support by National Key R&D Program of China (No. 2019YFA0405100), the China Manned Space Project with NO. CMS-CSST-2021-A11 and Project 11573003 supported by the National Natural Science Foundation of China (NSFC). This research uses data obtained through the Telescope Access Program (TAP). This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. JPB and JBM acknowledge the financial support of the ANR COLD WORLDS (ANR-18-CE31-0002). KMM's work is supported by the NASA Exoplanets Research Program (XRP) by cooperative agreement NNX16AD44G. JPB is supported by the University of Tasmania through the UTAS Foundation and the endowed Warren Chair in Astronomy.

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