OGLE-2017-BLG-1049: Another giant planet microlensing event

Autor: Kim, Yun Hak, Chung, Sun-Ju, Udalski, A., Bond, Ian A., Jung, Youn Kil, Gould, Andrew, Albrow, Michael D., Han, Cheongho, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C., Zang, Weicheng, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Poleski, Radek, Mroz, Przemek, Skowron, Jan, Szymanski, Michal K., Soszynski, Igor, Pietrukowicz, Pawel, Kozlowski, Syzmon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fujii, Hirosane, Fukui, Akihiko, Itow, Yoshitaka, Hirao, Yuki, Kirikawa, Rintaro, Kondo, Iona, Koshimoto, Naoki, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Ranc, Clement, Rattenbury, Nicholas J., Satoh, Yuki, Shoji, Hikaru, Sumi, Takahiro, Suzuki, Daisuke, Tristram, Paul J., Tanaka, Yuzuru, Yamawaki, Tsubasa, Yonehara, Atsunori
Rok vydání: 2020
Předmět:
Zdroj: JKAS, 53:161~168, 2020 December
Druh dokumentu: Working Paper
DOI: 10.5303/JKAS.2020.53.6.161
Popis: We report a giant exoplanet discovery in the microlensing event OGLE-2017-BLG-1049, which is a planet-host star mass ratio of $q=9.53\pm0.39\times10^{-3}$ and has a caustic crossing feature in the Korea Microlensing Telescope Network (KMTNet) observations. The caustic crossing feature yields an angular Einstein radius of $\theta_{\rm E}=0.52 \pm 0.11\ {\rm mas}$. However, the microlens parallax is not measured because of the time scale of the event $t_{\rm E}\simeq 29\ {\rm days}$, which is not long enough in this case to determine the microlens parallax. Thus, we perform a Bayesian analysis to estimate physical quantities of the lens system. From this, we find that the lens system has a star with mass $M_{\rm h}=0.55^{+0.36}_{-0.29} \ M_{\odot}$ hosting a giant planet with $M_{\rm p}=5.53^{+3.62}_{-2.87} \ M_{\rm Jup}$, at a distance of $D_{\rm L}=5.67^{+1.11}_{-1.52}\ {\rm kpc}$. The projected star-planet separation in units of the Einstein radius $(\theta_{\rm E})$ corresponding to the total mass of the lens system is $a_{\perp}=3.92^{+1.10}_{-1.32}\ \rm{au}$. This means that the planet is located beyond the snow line of the host. The relative lens-source proper motion is $\mu_{\rm rel}\sim 7 \ \rm{mas \ yr^{-1}}$, thus the lens and source will be separated from each other within 10 years. Then the flux of the host star can be measured by a 30m class telescope with high-resolution imaging in the future, and thus its mass can be determined.
Comment: 7 figures, Published in Journal of the Korean Astronomical Society(JKAS)
Databáze: arXiv
Externí odkaz: