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dc.contributor.author | Zang, Weicheng | |
dc.contributor.author | Shvartzvald, Yossi | |
dc.contributor.author | Udalski, Andrzej | |
dc.contributor.author | Yee, Jennifer C. | |
dc.contributor.author | Lee, Chung Uk | |
dc.contributor.author | Sumi, Takahiro | |
dc.contributor.author | Zhang, Xiangyu | |
dc.contributor.author | Yang, Hongjing | |
dc.contributor.author | Mao, Shude | |
dc.contributor.author | Novati, Sebastiano Calchi | |
dc.contributor.author | Gould, Andrew | |
dc.contributor.author | Zhu, Wei | |
dc.contributor.author | Beichman, Charles A. | |
dc.contributor.author | Bryden, Geoffery | |
dc.contributor.author | Carey, Sean | |
dc.contributor.author | Gaudi, B. Scott | |
dc.contributor.author | Henderson, Calen B. | |
dc.contributor.author | Mróz, Przemek | |
dc.contributor.author | Skowron, Jan | |
dc.contributor.author | Poleski, Radoslaw | |
dc.contributor.author | Szymański, Michał K. | |
dc.contributor.author | Soszyński, Igor | |
dc.contributor.author | Pietrukowicz, Paweł | |
dc.contributor.author | Kozłowski, Szymon | |
dc.contributor.author | Ulaczyk, Krzysztof | |
dc.contributor.author | Rybicki, Krzysztof A. | |
dc.contributor.author | Iwanek, Patryk | |
dc.contributor.author | Wrona, Marcin | |
dc.contributor.author | Albrow, Michael D. | |
dc.contributor.author | Chung, Sun Ju | |
dc.contributor.author | Han, Cheongho | |
dc.contributor.author | Hwang, Kyu Ha | |
dc.contributor.author | Jung, Youn Kil | |
dc.contributor.author | Ryu, Yoon Hyun | |
dc.contributor.author | Shin, In Gu | |
dc.contributor.author | Cha, Sang Mok | |
dc.contributor.author | Kim, Dong Jin | |
dc.contributor.author | Kim, Hyoun Woo | |
dc.contributor.author | Kim, Seung Lee | |
dc.contributor.author | Lee, Dong Joo | |
dc.contributor.author | Lee, Yongseok | |
dc.contributor.author | Park, Byeong Gon | |
dc.contributor.author | Pogge, Richard W. | |
dc.contributor.author | Bond, Ian A. | |
dc.contributor.author | Abe, Fumio | |
dc.contributor.author | Barry, Richard | |
dc.contributor.author | Bennett, David P. | |
dc.contributor.author | Bhattacharya, Aparna | |
dc.contributor.author | Donachie, Martin | |
dc.contributor.author | Fujii, Hirosane | |
dc.contributor.author | Fukui, Akihiko | |
dc.contributor.author | Hirao, Yuki | |
dc.contributor.author | Itow, Yoshitaka | |
dc.contributor.author | Kirikawa, Rintaro | |
dc.contributor.author | Kondo, Iona | |
dc.contributor.author | Koshimoto, Naoki | |
dc.contributor.author | Li, Man Cheung Alex | |
dc.contributor.author | Matsubara, Yutaka | |
dc.contributor.author | Muraki, Yasushi | |
dc.contributor.author | Miyazaki, Shota | |
dc.contributor.author | Ranc, Clément | |
dc.contributor.author | Rattenbury, Nicholas J. | |
dc.contributor.author | Satoh, Yuki | |
dc.contributor.author | Shoji, Hikaru | |
dc.contributor.author | Suzuki, Daisuke | |
dc.contributor.author | Tanaka, Yuzuru | |
dc.contributor.author | Tristram, Paul J. | |
dc.contributor.author | Yamawaki, Tsubasa | |
dc.contributor.author | Yonehara, Atsunori | |
dc.contributor.author | Bachelet, Etienne | |
dc.contributor.author | Hundertmark, Markus P.G. | |
dc.contributor.author | Jaimes, R. Figuera | |
dc.contributor.author | Maoz, Dan | |
dc.contributor.author | Penny, Matthew T. | |
dc.contributor.author | Street, Rachel A. | |
dc.contributor.author | Tsapras, Yiannis | |
dc.date.accessioned | 2024-09-26T00:46:39Z | |
dc.date.available | 2024-09-26T00:46:39Z | |
dc.date.issued | 2022-08-01 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | https://repositorio.uss.cl/handle/uss/13490 | |
dc.description | Publisher Copyright: © 2022 The Author(s). | |
dc.description.abstract | We report the discovery and analysis of a planet in the microlensing event OGLE-2018-BLG-0799. The planetary signal was observed by several ground-based telescopes, and the planet-host mass ratio is q = (2.65 ± 0.16) × 10-3. The ground-based observations yield a constraint on the angular Einstein radius θE, and the microlensing parallax vector πE, is strongly constrained by the Spitzer data. However, the 2019 Spitzer baseline data reveal systematics in the Spitzer photometry, so there is ambiguity in the magnitude of the parallax. In our preferred interpretation, a full Bayesian analysis using a Galactic model indicates that the planetary system is composed of an Mplanet = 0 . 26 + 0 . 22-0 . 11 MJ planet orbiting an Mhost = 0 . 093 +0.082-0.038 M ⊙, at a distance of DL = 3 . 71 + 3 . 24-1 . 70 kpc. An alternate interpretation of the data shifts the localization of the minima along the arc-shaped microlens parallax constraints. This, in turn, yields a more massive host with median mass of 0.13 M⊙ at a distance of 6.3 kpc. This analysis demonstrates the robustness of the osculating circles formalism, but shows that further investigation is needed to assess how systematics affect the specific localization of the microlens parallax vector and, consequently, the inferred physical parameters. | en |
dc.language.iso | eng | |
dc.relation.ispartof | vol. 514 Issue: no. 4 Pages: 5952-5968 | |
dc.source | Monthly Notices of the Royal Astronomical Society | |
dc.title | OGLE-2018-BLG-0799Lb : a q ∼2.7 × 10-3planet with Spitzer parallax | en |
dc.type | Artículo | |
dc.identifier.doi | 10.1093/mnras/stac1631 |
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