تقرير
Ogle-2018-BLG-0799lb: A Q ∼ 2.7 × 10(−3) Planet With Spitzer Parallax
| العنوان: | Ogle-2018-BLG-0799lb: A Q ∼ 2.7 × 10(−3) Planet With Spitzer Parallax |
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| المؤلفون: | Weicheng Zang, Yossi Shvartzvald, Andrzej Udalski, Jennifer C. Yee, Chung-Uk Lee, Takahiro Sumi, Xiangyu Zhang, Hongjing Yang, Shude Mao, Sebastiano Calchi Novati, Andrew Gould, Wei Zhu, Charles A. Beichman, Geoffery Bryden, Sean Carey, B. Scott Gaudi, Calen B. Henderson, Przemek Mroz, Jan Skowron, Radoslaw Poleski, Michał K. Szymanski, Igor Soszynski, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Richard Barry, David P. Bennett |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 514(4) |
| بيانات النشر: | United States: NASA Center for Aerospace Information (CASI), 2022. |
| سنة النشر: | 2022 |
| مصطلحات موضوعية: | Astrophysics |
| الوصف: | 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 −0.11M(J) planet orbiting an Mhost = 0.093+0.082 −0.038 Mʘ , 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 Mʘ 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. |
| نوع الوثيقة: | Report |
| اللغة: | English |
| تدمد: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stac1631 |
| URL الوصول: | https://ntrs.nasa.gov/citations/20230002416 |
| ملاحظات: | 907524.02.01.14.06 80GSFC22CA003 12133005 1571564 2014/14/A/ST9/00121 JP17H02871 JP16H06287 JSPS15H00781 JSPS23340064 JSPS24253004 JSPS26247023 AST-1516842 1500811 321035 2019R1A2C2085965 2017R1A4A1015178 |
| رقم الأكسشن: | edsnas.20230002416 |
| قاعدة البيانات: | NASA Technical Reports |
Full Text Finder | تدمد: | 13652966 00358711 |
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| DOI: | 10.1093/mnras/stac1631 |