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OGLE-2019-BLG-0362Lb: A Super-Jovian-Mass Planet around A Low-Mass Star
정선주,Jennifer C. Yee,Andrej Udalski,Andrew Gould,Michael D. Albrow,정연길,황규하,CHEONGHOHAN,Yoon-Hyun Ryu,신인구,Yossi Shvartzvald,Weicheng Zang,차상목,Dong Jin Kim,김승리,이충욱,Dong-Joo Lee,이용석,Byeong-Gon Park,Richar 한국천문학회 2022 Journal of The Korean Astronomical Society Vol.55 No.4
We present the analysis of a planetary microlensing event OGLE-2019-BLG-0362 with a short-duration anomaly (~0.4 days) near the peak of the light curve, which is caused by the resonant caustic. The event has a severe degeneracy with $\delcs = 0.9$ between the close and the wide binary lens models both with planet-host mass ratio $q \simeq 0.007$. We measure the angular Einstein radius but not the microlens parallax, and thus we perform a Bayesian analysis to estimate the physical parameters of the lens. We find that the OGLE-2019-BLG-0362L system is a super-Jovian-mass planet $M_{\rm p}=3.26^{+0.83}_{-0.58}~M_{\rm J}$ orbiting an M dwarf $M_{\rm h}=0.42^{+0.34}_{-0.23}~M_{\odot}$ at a distance $D_{\rm L} =5.83^{+1.04}_{-1.55}$ kpc. The projected star-planet separation is $a_{\perp} = 2.18^{+0.58}_{-0.72}~{\rm AU}$, which indicates that the planet lies beyond the snow line of the host star.
OGLE-2011-BLG-0417: A RADIAL VELOCITY TESTBED FOR MICROLENSING
Gould, Andrew,Shin, In-Gu,Han, Cheongho,Udalski, Andrzej,Yee, Jennifer C. IOP Publishing 2013 The Astrophysical journal Vol.768 No.2
<P>Microlensing experiments are returning increasingly detailed information about the planetary and binary systems that are being detected, far beyond what was originally expected. In several cases the lens mass and distance are measured, and a few very special cases have yielded complete eight-parameter Kepler solutions, i.e., the masses of both components, five Kepler invariants, and the phase. We identify one such case that is suitable for a precision test that could be carried out by comparing Doppler radial velocity (RV) measurements with the predictions from the microlensing solution. The lens primary is reasonably bright (I = 16.3, V = 18.2) and is expected to have a relatively large RV semi-amplitude (K similar to 6.35 km s(-1)).</P>
KMT-2017-BLG-0165Lb: A Super-Neptune-mass Planet Orbiting a Sun-like Host Star
Kil Jung, Youn,Gould, Andrew,Zang, Weicheng,Hwang, Kyu-Ha,Ryu, Yoon-Hyun,Han, Cheongho,Yee, Jennifer C.,Albrow, Michael D.,Chung, Sun-Ju,Shin, In-Gu,Shvartzvald, Yossi,Zhu, Wei,Cha, Sang-Mok,Kim, Dong American Astronomical Society 2019 The Astronomical journal Vol.157 No.2
KMT-2018-BLG-0029LB: A VERY LOW MASS-RATIO Spitzer MICROLENS PLANET
Andrew Gould,류윤현,Sebastiano Calchi Novati,Weicheng Zang,Michael D. Albrow,정선주,CHEONGHOHAN,황규하,정연길,신인구,Yossi Shvartzvald,Jennifer C. Yee,차상목,Dong-Jin Kim,김현우,김승리,이정욱,Dong-Joo Lee,이용석,Byeong-Gon Park,Ri 한국천문학회 2020 Journal of The Korean Astronomical Society Vol.53 No.1
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 pi_E measurement. Combined with a measurement of the Einstein radius theta_E from finite-source effects during the caustic crossings, these measurements imply masses of the host M_host = 1.14+0.10-0.12 M_sun and planet M_planet = 7.59+0.75-0.69 M_Earth, system distance D_L = 3.38+0.22-0.26 kpc and projected separation a_p = 4.27+0.21-0.23 au. 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.
FREE-FLOATING PLANETS, THE EINSTEIN DESERT, AND 'OUMUAMUA
Gould, Andrew,Jung, Youn Kil,Hwang, Kyu-Ha,Dong, Subo,Albrow, Michael D.,Chung, Sun-Ju,Han, Cheongho,Ryu, Yoon-Hyun,Shin, In-Gu,Shvartzvald, Yossi,Yang, Hongjing,Yee, Jennifer C.,Zang, Weicheng,Cha, S The Korean Astronomical Society 2022 Journal of The Korean Astronomical Society Vol.55 No.5
We complete the survey for finite-source/point-lens (FSPL) giant-source events in 2016-2019 KMTNet microlensing data. The 30 FSPL events show a clear gap in Einstein radius, 9 𝜇as < 𝜃<sub>E</sub> < 26 𝜇as, which is consistent with the gap in Einstein timescales near t<sub>E</sub> ~ 0.5 days found by Mróz et al. (2017) in an independent sample of point-source/point-lens (PSPL) events. We demonstrate that the two surveys are consistent. We estimate that the 4 events below this gap are due to a power-law distribution of free-floating planet candidates (FFPs) dN<sub>FFP</sub>/d log M = (0.4 ± 0.2) (M/38 M<sub>⊕</sub>)<sup>-p</sup>/star, with 0.9 ≲ p ≲ 1.2. There are substantially more FFPs than known bound planets, implying that the bound planet power-law index 𝛾 = 0.6 is likely shaped by the ejection process at least as much as by formation. The mass density per decade of FFPs in the Solar neighborhood is of the same order as that of 'Oumuamua-like objects. In particular, if we assume that 'Oumuamua is part of the same process that ejected the FFPs to very wide or unbound orbits, the power-law index is p = 0.89 ± 0.06. If the Solar System's endowment of Neptune-mass objects in Neptune-like orbits is typical, which is consistent with the results of Poleski et al. (2021), then these could account for a substantial fraction of the FFPs in the Neptune-mass range.