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Detection of sodium in the atmosphere of WASP-69b

机译：在WASP-69b大气中检测钠

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Context. Transit spectroscopy is one of the most commonly used methods to characterize exoplanets’ atmospheres. From the ground, these observations are very challenging due to the terrestrial atmosphere and its intrinsic variations, but high-spectral-resolution observations overcome this difficulty by resolving the spectral lines and taking advantage of the different Doppler velocities of the Earth, the host star, and the exoplanet. Aims. We analyze the transmission spectrum around the Na I doublet at 589 nm of the extrasolar planet WASP-69b, a hot Jupiter orbiting a K-type star with a period of 3.868 days, and compare the analysis to that of the well-known hot Jupiter HD 189733b. We also present the analysis of the Rossiter-McLaughlin (RM) effect for WASP-69b. Methods. We observed two transits of WASP-69b with the High Accuracy Radial velocity Planet Searcher (HARPS-North) spectrograph ( R = 115 000 ) at the Telescopio Nazionale Galileo (TNG). We perform a telluric contamination subtraction based on the comparison between the observed spectra and a telluric water model. Then, the common steps of the differential spectroscopy are followed to extract the transmission spectrum. The method is tested with archival transit data of the extensively studied exoplanet HD 189733b, obtained with the HARPS-South spectrograph at ESO 3.6 m telescope, and then applied to WASP-69b data. Results. For HD 189733b, we spectrally resolve the Na I doublet and measure line contrasts of 0.72 ± 0.05% (D2) and 0.51 ± 0.05% (D1), and full width half maximum (FWHM) values of 0.64 ± 0.04 ? (D2) and 0.60 ± 0.06 ? (D1), in agreement with previously published results. For WASP-69b only the contrast of the D2 line can be measured ( 5.8 ± 0.3% ). This corresponds to a detection at the 5 σ -level of excess absorption of 0.5 ± 0.1% in a passband of 1.5 ? . A net blueshift of ~ 0.04 ? is measured for HD 189733b and no shift is obtained for WASP-69b. By measuring the RM effect, we get an angular rotation of 0.24_(-0.01)~(+0.02)rad/day and a sky-projected angle between the stellar rotation axis and the normal of orbit plane ( λ ) of 0.4_(-1.9)~(+2.0) ° for WASP-69b. Similar results to those previously presented in the literature are obtained for the RM analysis of HD 189733b. Conclusions. Even if sodium features are clearly detected in the WASP-69b transmission spectrum, more transits are needed to fully characterize the line profiles and retrieve accurate atmospheric properties.
机译：上下文。过境光谱学是表征系外行星大气的最常用方法之一。从地面上看，由于地面大气及其内在变化，这些观测非常具有挑战性，但是高光谱分辨率的观测通过解决光谱线并利用地球，主恒星的不同多普勒速度，克服了这一难题。和系外行星。目的我们分析了太阳系外行星WASP-69b（一颗热木星绕K型恒星以3.868天的周期）在589 nm处Na I双峰周围的透射光谱，并将分析结果与著名的热木星进行了比较HD 189733b。我们还介绍了针对WASP-69b的Rossiter-McLaughlin（RM）效应的分析。方法。我们用Telescopio Nazionale Galileo（TNG）的高精度径向速度行星搜索器（HARPS-North）光谱仪（R = 115 000）观测到WASP-69b的两次过渡。我们基于观察到的光谱和碲水模型之间的比较执行碲污染减法。然后，遵循差分光谱的通用步骤来提取透射光谱。使用广泛研究的系外行星HD 189733b的档案传输数据测试该方法，该数据是使用EPS 3.6 m望远镜的HARPS-South光谱仪获得的，然后应用于WASP-69b数据。结果。对于HD 189733b，我们通过光谱解析Na I双峰，并测量了0.72±0.05％（D2）和0.51±0.05％（D1）的线对比度，以及半峰宽（FWHM）值为0.64±0.04？ （D2）和0.60±0.06？ （D1），与先前发布的结果一致。对于WASP-69b，只能测量D2线的对比度（5.8±0.3％）。这对应于在1.5？通带中在5σ级别检测到0.5±0.1％的过量吸收。 。净蓝移约为0.04？ HD 189733b的测量值没有测量，而WASP-69b的测量值没有变化。通过测量RM效应，我们获得了0.24 _（-0.01）〜（+0.02）rad / day的角旋转，恒星旋转轴与轨道平面法线（λ）之间的天空投影角为0.4_（ WASP-69b为-1.9）〜（+2.0）°。 HD 189733b的RM分析获得了与文献中先前介绍的结果相似的结果。结论。即使在WASP-69b透射光谱中清楚地检测到钠特征，也需要进行更多的转换才能完全表征管线轮廓并获取准确的大气性质。

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