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OGLE-2018-BLG-1185b: A Low-mass Microlensing Planet Orbiting a Low-mass Dwarf
The Astronomical Journal ( IF 5.1 ) Pub Date : 2021-07-29 , DOI: 10.3847/1538-3881/ac00ba
Iona Kondo 1 , Jennifer C. Yee 2 , David P. Bennett 3, 4 , Takahiro Sumi 1 , Naoki Koshimoto 5 , Ian A. Bond 6 , Andrew Gould 7, 8 , Andrzej Udalski 9 , Yossi Shvartzvald 10 , Youn Kil Jung 11, 12 , Weicheng Zang 13 , Valerio Bozza 14, 15 , Etienne Bachelet 16 , Markus P. G. Hundertmark 17 , Nicholas J. Rattenbury 18 , F. Abe 19 , R. Barry 3 , A. Bhattacharya 3, 4 , M. Donachie 18 , A. Fukui 20, 21 , H. Fujii 19 , Y. Hirao 1 , S. Ishitani Silva 3, 22 , Y. Itow 19 , R. Kirikawa 1 , M. C. A. Li 18 , Y. Matsubara 19 , S. Miyazaki 1 , Y. Muraki 19 , G. Olmschenk 3 , C. Ranc 23 , Y. Satoh 1 , H. Shoji 1 , D. Suzuki 1 , Y. Tanaka 1 , P. J. Tristram 24 , T. Yamawaki 1 , A. Yonehara 25 , P. Mrz 26 , R. Poleski 9 , J. Skowron 9 , M. K. Szymański 9 , I. Soszyński 9 , S. Kozłowski 9 , P. Pietrukowicz 9 , K. Ulaczyk 9, 27 , K. A. Rybicki 9 , P. Iwanek 9 , M. Wrona 9 , M. D. Albrow 28 , S.-J. Chung 11, 12 , C. Han 29 , K.-H. Hwang 11 , H.-W. Kim 11 , I.-G. Shin 11 , S.-M. Cha 11, 30 , D.-J. Kim 11 , S.-L. Kim 11, 12 , C.-U. Lee 11 , D.-J. Lee 11 , Y. Lee 11, 30 , B.-G. Park 11, 12 , R. W. Pogge 8 , Y.-H. Ryu 11 , C. A. Beichman 31 , G. Bryden 32 , S. Calchi Novati 31 , S. Carey 31 , B. S. Gaudi 8 , C. B. Henderson 31 , W. Zhu 33 , D. Maoz 34 , M. T. Penny 35 , M. Dominik 36 , U. G. Jrgensen 37 , P. Longa-Pea 38 , N. Peixinho 39 , S. Sajadian 40 , J. Skottfelt 41 , C. Snodgrass 42 , J. Tregloan-Reed 43 , M. J. Burgdorf 44 , J. Campbell-White 45 , S. Dib 7, 37 , Y. I. Fujii 37, 46, 47, 48, 49 , T. C. Hinse 50, 51 , E. Khalouei 52 , S. Rahvar 52 , M. Rabus 53, 54 , J. Southworth 55 , Y. Tsapras 56 , R. A. Street 56 , D. M. Bramich 57, 58, 59 , A. Cassan 60 , K. Horne 61 , J. Wambsganss 56 , S. Mao 62 , A. Saha 63
Affiliation  

We report an analysis of the planetary microlensing event OGLE-2018-BLG-1185, which was observed by a large number of ground-based telescopes and by the Spitzer Space Telescope. The ground-based light curve indicates a low planet–host star mass ratio of q = (6.9 0.2) 10−5, which is near the peak of the wide-orbit exoplanet mass-ratio distribution. We estimate the host star and planet masses with a Bayesian analysis using the measured angular Einstein radius under the assumption that stars of all masses have an equal probability of hosting the planet. The flux variation observed by Spitzer is marginal, but still places a constraint on the microlens parallax. Imposing a conservative constraint that this flux variation should be Δf Spz < 4 instrumental flux units yields a host mass of ${M}_{\mathrm{host}}={0.37}_{-0.21}^{+0.35}\ {M}_{\odot }$ and a planet mass of ${m}_{{\rm{p}}}={8.4}_{-4.7}^{+7.9}\ {M}_{\oplus }$. A Bayesian analysis including the full parallax constraint from Spitzer suggests smaller host star and planet masses of ${M}_{\mathrm{host}}={0.091}_{-0.018}^{+0.064}\ {M}_{\odot }$ and ${m}_{{\rm{p}}}={2.1}_{-0.4}^{+1.5}\ {M}_{\oplus }$, respectively. Future high-resolution imaging observations with the Hubble Space Telescope or Extremely Large Telescope could distinguish between these two scenarios and help reveal the planetary system properties in more detail.



中文翻译:

OGLE-2018-BLG-1185b:一颗围绕低质量矮星运行的低质量微透镜行星

我们报告了对由大量地面望远镜和斯皮策太空望远镜观测到的行星微透镜事件 OGLE-2018-BLG-1185 的分析。地基光变曲线表明行星-宿主恒星质量比较低,q = (6.9 0.2) 10 -5,接近宽轨道系外行星质量比分布的峰值。在假设所有质量的恒星拥有行星的概率相等的情况下,我们使用测量的爱因斯坦角半径通过贝叶斯分析来估计主恒星和行星的质量。Spitzer 观察到的通量变化很小,但仍然对微透镜视差施加了限制。强加一个保守的约束,这个通量变化应该是 Δ f Spz< 4 仪器通量单位产生主机质量${M}_{\mathrm{host}}={0.37}_{-0.21}^{+0.35}\ {M}_{\odot }$和行星质量${m}_{{\rm{p}}}={8.4}_{-4.7}^{+7.9}\ {M}_{\oplus }$。包括来自斯皮策的全视差约束的贝叶斯分析表明,主恒星和行星质量分别为${M}_{\mathrm{host}}={0.091}_{-0.018}^{+0.064}\ {M}_{\odot }$${m}_{{\rm{p}}}={2.1}_{-0.4}^{+1.5}\ {M}_{\oplus }$。未来使用哈勃太空望远镜或超大望远镜进行的高分辨率成像观测可以区分这两种情况,并有助于更详细地揭示行星系统的特性。

更新日期:2021-07-29
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