CHARACTERIZATION OF THE ATMOSPHERE OF THE HOT JUPITER HAT-P-32Ab AND THE M-DWARF COMPANION HAT-P-32B
CHARACTERIZATION OF THE ATMOSPHERE OF THE HOT JUPITER HAT-P-32Ab AND THE M-DWARF COMPANION HAT-P-32B
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DOI：
10.1088/0004-637x/796/2/115
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发表时间：
2014-10
期刊：
影响因子：
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通讯作者：
Ming Zhao;J. O'Rourke;J. Wright;H. Knutson;A. Burrows;J. Fortney;H. Ngo;B. Fulton;C. Baranec;R. Riddle;N. Law;P. Muirhead;S. Hinkley;A. Showman;J. Curtis;R. B. P. S. University;Center for Exoplanets;Habitable Worlds;C. I. O. Technology.;Princeton University;U. California;Santa Cruz;University of Hawaii at Manoa;U. N. C. C. Hill-U.-N.-C.-C.-Hill-90504321;B. University;The University of Arizona;Jet propulsion Laboratory
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文献类型：
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作者：
Ming Zhao;J. O'Rourke;J. Wright;H. Knutson;A. Burrows;J. Fortney;H. Ngo;B. Fulton;C. Baranec;R. Riddle;N. Law;P. Muirhead;S. Hinkley;A. Showman;J. Curtis;R. B. P. S. University;Center for Exoplanets;Habitable Worlds;C. I. O. Technology.;Princeton University;U. California;Santa Cruz;University of Hawaii at Manoa;U. N. C. C. Hill-U.-N.-C.-C.-Hill-90504321;B. University;The University of Arizona;Jet propulsion Laboratory
本文报道了用黑尔/宽视场红外照相机（WIRC）在H和KS波段以及斯皮策/IRAC在3.6和4.5 μm波段对热木星HAT-P-32 Ab进行的二次食光度测量。对主星星星HAT-P-32 A及其伴星HAT-P-32 B进行了近红外和可见光自适应光学成像。我们清楚地分辨出这两颗恒星，发现它们之间的距离为2.“923 ± 0.”004，位置角为110.°64 ± 0.°12。我们测量了该双星在g′r′i′z′、H和KS波段的流量比，确定伴星星星的Teff= 3565 ± 82 K，相当于一颗M1.5矮星。我们使用PHOENIX恒星大气模型来校正由于M1.5伴星的存在而导致的热木星的二次日食深度的稀释。我们还改善了二次日食测光占非经典的，通量依赖的非线性的WIRC红外探测器在H波段。在H、KS、3.6和4.5 μm波段，我们测量到行星-星星的流量比分别为0.090% ± 0.033%、0.178% ± 0.057%、0.364% ± 0.016%和0.438% ± 0.020%。我们比较这些行星大气模型，并发现他们更喜欢一个逆温和低效的热量再分配的大气。然而，我们也发现，数据同样很好地描述了一个黑体模型的行星与Tp = 2042 ± 50 K。最后，我们测量了一个0.3 ± 1.3分钟的二次日食时间偏移，从预测的日食中期时间，这限制了e = 0.0072时，结合径向速度数据，更符合圆形轨道。
We report secondary eclipse photometry of the hot Jupiter HAT-P-32Ab, taken with Hale/Wide-field Infra-Red Camera (WIRC) in H and KS bands and with Spitzer/IRAC at 3.6 and 4.5 μm. We carried out adaptive optics imaging of the planet host star HAT-P-32A and its companion HAT-P-32B in the near-IR and the visible. We clearly resolve the two stars from each other and find a separation of 2.″923 ± 0.″004 and a position angle 110.°64 ± 0.°12. We measure the flux ratios of the binary in g′r′i′z′ and H and KS bands, and determine Teff= 3565 ± 82 K for the companion star, corresponding to an M1.5 dwarf. We use PHOENIX stellar atmosphere models to correct the dilution of the secondary eclipse depths of the hot Jupiter due to the presence of the M1.5 companion. We also improve the secondary eclipse photometry by accounting for the non-classical, flux-dependent nonlinearity of the WIRC IR detector in the H band. We measure planet-to-star flux ratios of 0.090% ± 0.033%, 0.178% ± 0.057%, 0.364% ± 0.016%, and 0.438% ± 0.020% in the H, KS, 3.6 and 4.5 μm bands, respectively. We compare these with planetary atmospheric models, and find they prefer an atmosphere with a temperature inversion and inefficient heat redistribution. However, we also find that the data are equally well described by a blackbody model for the planet with Tp = 2042 ± 50 K. Finally, we measure a secondary eclipse timing offset of 0.3 ± 1.3 minutes from the predicted mid-eclipse time, which constrains e = 0.0072 when combined with radial velocity data and is more consistent with a circular orbit.