Title

Kmt-2018-blg-0029lb: A very low mass-ratio spitzer microlens planet

Authors

Andrew Gould, Max Planck Institute for Astronomy
Yoon Hyun Ryu, Korea Astronomy and Space Science Institute
Sebastiano Calchi Novati, Infrared Processing & Analysis Center
Weicheng Zang, Tsinghua University
Michael D. Albrow, University of Canterbury
Sun Ju Chung, Korea Astronomy and Space Science Institute
Cheongho Han, Chungbuk National University
Kyu Ha Hwang, Korea Astronomy and Space Science Institute
Youn Kil Jung, Korea Astronomy and Space Science Institute
In Gu Shin, Korea Astronomy and Space Science Institute
Yossi Shvartzvald, Infrared Processing & Analysis Center
Jennifer C. Yee, Harvard-Smithsonian Center for Astrophysics
Sang Mok Cha, Korea Astronomy and Space Science Institute
Dong Jin Kim, Korea Astronomy and Space Science Institute
Hyoun Woo Kim, Korea Astronomy and Space Science Institute
Seung Lee Kim, Korea Astronomy and Space Science Institute
Chung Uk Lee, Korea Astronomy and Space Science Institute
Dong Joo Lee, Korea Astronomy and Space Science Institute
Yongseok Lee, Korea Astronomy and Space Science Institute
Byeong Gon Park, Korea Astronomy and Space Science Institute
Richard W. Pogge, The Ohio State University
Charles Beichman, California Institute of Technology
Geoff Bryden, Infrared Processing & Analysis Center
Sean Carey, Spitzer Science Center
B. Scott Gaudi, The Ohio State University
Calen B. Henderson, Infrared Processing & Analysis Center
Wei Zhu, L’Institut Canadien d’Astrophysique Théorique
Pascal Fouqué, Télescope Canada-France-Hawaii
Matthew T. Penny, The Ohio State University
Andreea Petric, Télescope Canada-France-Hawaii
Todd Burdullis, Télescope Canada-France-Hawaii
Shude Mao, Tsinghua University

Document Type

Article

Publication Date

2-1-2020

Abstract

At q = 1.81 ± 0.20 × 10−5, KMT-2018-BLG-0029Lb has the lowest planet-host mass ratio q of any microlensing planet to date by more than a factor of two. Hence, it is the first planet that probes below the apparent “pile-up” at q = 5–10 ×10−5. The event was observed by Spitzer, yielding a microlens-parallax πE measurement. Combined with a measurement of the Einstein radius θE from finite-source effects during the caustic crossings, these measurements imply masses of the host Mhost = 1.14+0.10 −0.12M⊙ and planet Mplanet = 7.59−0.69+0.75M⊕, system distance DL = 3.38+0.22 −0.26kpc and projected separationa⊥ = 4.27+0.21 −0.23AU. The blended light, which is substantially brighter than the microlensed source, is plausibly due to the lens and could be observed at high resolution immediately.

Publication Source (Journal or Book title)

Journal of the Korean Astronomical Society

First Page

9

Last Page

26

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