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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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