$Spitzer$ Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M-dwarf
| Autor: | Jung, Youn Kil, Gould, Andrew, Udalski, Andrzej, Sumi, Takahiro, Yee, Jennifer C., Shvartzvald, Yossi, Zang, Weicheng, Han, Cheongho, Albrow, Michael D., Chung, Sun Ju, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Zhu, Wei, 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., Mróz, Przemek, Szymański, Michał K., Skowron, Jan, Poleski, Radek, Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzystof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Beichman, Charles A., Bryden, Geoffery, Novati, Sebastiano Calchi, Carey, Sean, Gaudi, B. Scott, Henderson, Calen B., Abe, Fumio, Barry, Richard, Bennett, David P., Bond, Ian A., Bhattacharya, Aparna, Donachie, Martin, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Miyazaki, Shota, Muraki, Yasushi, Nagakane, Masayuki, Ranc, Clément, Rattenbury, Nicholas J., Suematsu, Haruno, Sullivan, Denis J., Suzuki, Daisuke, Tristram, Paul J., Yonehara, Atsunori, Jacklin, Savannah, Penny, Matthew T., Stassun, Keivan G. |
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| Rok vydání: | 2019 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.3847/1538-3881/ab237f |
| Popis: | We report the discovery of a $Spitzer$ microlensing planet OGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio $q \sim 2\times10^{-4}$. The planetary signal, which is characterized by a short $(\sim 1~{\rm day})$ "bump" on the rising side of the lensing light curve, was densely covered by ground-based surveys. We find that the signal can be explained by a bright source that fully envelops the planetary caustic, i.e., a "Hollywood" geometry. Combined with the source proper motion measured from $Gaia$, the $Spitzer$ satellite parallax measurement makes it possible to precisely constrain the lens physical parameters. The preferred solution, in which the planet perturbs the minor image due to lensing by the host, yields a Uranus-mass planet with a mass of $M_{\rm p} = 13.9\pm1.6~M_{\oplus}$ orbiting a mid M-dwarf with a mass of $M_{\rm h} = 0.23\pm0.03~M_{\odot}$. There is also a second possible solution that is substantially disfavored but cannot be ruled out, for which the planet perturbs the major image. The latter solution yields $M_{\rm p} = 1.2\pm0.2~M_{\oplus}$ and $M_{\rm h} = 0.15\pm0.02~M_{\odot}$. By combining the microlensing and $Gaia$ data together with a Galactic model, we find in either case that the lens lies on the near side of the Galactic bulge at a distance $D_{\rm L} \sim 6\pm1~{\rm kpc}$. Future adaptive optics observations may decisively resolve the major image/minor image degeneracy. Comment: 34 pages, 8 figures, Submitted to AAS journal |
| Databáze: | arXiv |
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