论文标题
检测h $ _2 $ o与crires+：WASP-20B的情况
Detecting H$_2$O with CRIRES+: the case of WASP-20b
论文作者
论文摘要
事实证明，在广泛的光谱范围内和最高分辨能力（R> 70 000）的红外光谱法被证明是公开数十个大气组成的领先技术之一。 VLT（CRIRES+）最近升级的光谱CRIRES仪器在2021年9月进行了首次科学验证，其大气表征方面的新功能已准备好进行测试。 We analysed transmission spectra of the Hot Saturn WASP-20b in the K-band (1981-2394 nm) acquired with CRIRES+, aiming at detecting the signature of H2O and CO. We used Principal Component Analysis to remove the dominant time-dependent contaminating sources such as telluric bands and the stellar spectrum and we extracted the planet spectrum by cross-correlating observations with 1D and 3D合成光谱，不包括循环。我们分别仅使用H2O 1D和3D模型，在S/N处的分子吸收的暂定性检测等于4.2和4.7。 CCF的峰值发生在两种模型类型的相同的休息时速度（VREST = -1 $ \ pm $ 1 kmms $^{ - 1} $），在同一投影的行星轨道速度下，但具有不同的误差频段（1D模型：1D：KP = 131 $^{+18} $^{+18} $} $ {-29 $} $ {-29 $^ - {-29} $^; kp = 131 $^{+23} _ { - 39} $ kmms $^{ - 1} $）。我们的结果与文献中的预期（132.9 $ \ pm $ 2.7 kms $^{ - 1} $）一致。尽管在校准和减少原始数据集时，在校准和减少原始数据集时进行了最佳的观察条件和管道问题，但我们在WASP-20B大气中获得了第一次暂定水的暂定检测。我们建议进行更深入的分析和其他观察结果，以确认我们的结果并揭示CO的存在。
Infrared spectroscopy over a wide spectral range and at the highest resolving powers (R>70 000) has proved to be one of the leading technique to unveil the atmospheric composition of dozens of exoplanets. The recently upgraded spectrograph CRIRES instrument at the VLT (CRIRES+) was operative for a first Science Verification in September 2021 and its new capabilities in atmospheric characterisation were ready to be tested. We analysed transmission spectra of the Hot Saturn WASP-20b in the K-band (1981-2394 nm) acquired with CRIRES+, aiming at detecting the signature of H2O and CO. We used Principal Component Analysis to remove the dominant time-dependent contaminating sources such as telluric bands and the stellar spectrum and we extracted the planet spectrum by cross-correlating observations with 1D and 3D synthetic spectra, with no circulation included. We present the tentative detection of molecular absorption from water-vapour at S/N equal to 4.2 and 4.7 by using only-H2O 1D and 3D models, respectively. The peak of the CCF occurred at the same rest-frame velocity for both model types (Vrest=-1 $\pm$ 1 kms$^{-1}$), and at the same projected planet orbital velocity but with different error bands (1D model: KP=131$^{+18}_{-29}$ kms$^{-1}$; 3D: KP=131$^{+23}_{-39}$ kms$^{-1}$). Our results are in agreement with the one expected in literature (132.9 $\pm$ 2.7 kms$^{-1}$). Although sub-optimal observational conditions and issues with pipeline in calibrating and reducing our raw data set, we obtained the first tentative detection of water in the atmosphere of WASP-20b. We suggest a deeper analysis and additional observations to confirm our results and unveil the presence of CO.
