CRIRES+ detection of CO emissions lines and temperature inversions on the dayside of WASP-18b and WASP-76b
F. Yan, L. Nortmann, A. Reiners, N. Piskunov, A. Hatzes, U. Seemann, D. Shulyak, A. Lavail, A. D. Rains, D. Cont, M. Rengel, F. Lesjak, E. Nagel, O. Kochukhov, … 展开作者
F. Yan, L. Nortmann, A. Reiners, N. Piskunov, A. Hatzes, U. Seemann, D. Shulyak, A. Lavail, A. D. Rains, D. Cont, M. Rengel, F. Lesjak, E. Nagel, O. Kochukhov, S. Czesla, L. Boldt-Christmas, U. Heiter, J. V. Smoker, F. Rodler, P. Bristow, R. J. Dorn, Y. Jung, T. Marquart, E. Stempels
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11 pages, 12 figures; accepted for publication in A&A
The dayside atmospheres of ultra-hot Jupiters (UHJs) are predicted to possess temperature inversion layers with extremely high temperatures at high altitudes. We observed the dayside thermal emission spectra of WASP-18b and WASP-76b with the new CRIRES+ high-resolution spectrograph at near-infrared wavelengths. Using the cross-correlation technique, we detected strong CO emission lines in both planets, which confirms the existence of temperature inversions on their dayside hemispheres. The two planets are the first UHJs orbiting F-type stars with CO emission lines detected; previous detections were mostly for UHJs orbiting A-type stars. Evidence of weak H2O emission signals is also found for both planets. We further applied forward-model retrievals on the detected CO lines and retrieved the temperature-pressure profiles along with the CO volume mixing ratios. The retrieved logarithmic CO mixing ratio of WASP-18b (-2.2) is slightly higher than the value predicted by the self-consistent model assuming solar abundance. For WASP-76b, the retrieved CO mixing ratio (-3.6) is broadly consistent with the value of solar abundance. In addition, we included the equatorial rotation velocity (Veq ) in the retrieval when analyzing the line profile broadening. The obtained Veq is 7.0 km/s for WASP-18b and 5.2 km/s for WASP-76b, which are consistent with the tidally locked rotational velocities.
Exploring the ultrahot Neptune LTT 9779 b with CRIRES+. Non-detection of helium transmission spectra and detection of H$_2$O on the dayside
University of Science and Technology of China（中国科学技术大学）；Georg-August-Universität Göttingen（哥廷根大学）；Ludwig-Maximilians-Universität München（慕尼黑大学）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿诺德·爱因斯坦天文研究所）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理学研究所）；Uppsala universitet（乌普萨拉大学）；Thüringer Landessternwarte Tautenburg（图林根州立陶滕堡天文台）
利用 CRIRES+ 对超热海王星 LTT 9779 b 进行凌星和白天侧光谱观测，未探测到氦吸收（上限 0.45%），但探测到 H2O 信号（4.8σ），联合反演表明低水丰度且无热反转，旋转速度与同步自转一致。
High-Resolution Dayside Spectroscopy of the Ultra-Hot Jupiter WASP-178b with GHOST/Gemini South
East Texas A&M University（东德克萨斯农工大学）；International Gemini Observatory/NSF NOIRLab（国际Gemini天文台/美国国家光学红外天文实验室研究组织）；University of Waterloo（滑铁卢大学）；Waterloo Centre for Astrophysics, University of Waterloo（滑铁卢大学滑铁卢天体物理中心）；Arizona State University（亚利桑那州立大学）；Queen’s University Belfast（贝尔法斯特女王大学）；California Institute of Technology（加州理工学院）；The Pennsylvania State University（宾夕法尼亚州立大学）
Exploring the ultra-hot Jupiter WASP-178b. Constraints on atmospheric chemistry and dynamics from a joint retrieval of VLT/CRIRES$^+$ and space photometric data
Enriched volatiles and refractories but deficient titanium on the dayside atmosphere of WASP-121b revealed by JWST/NIRISS
Observatoire astronomique de l’Université de Genève（日内瓦大学天文台）；Trottier Institute for Research on Exoplanets, Department of Physics, Université de Montréal（蒙特利尔大学物理系特罗蒂尔系外行星研究所）；Trottier Space Institute at McGill（麦吉尔大学特罗蒂尔太空研究所）；Department of Earth & Planetary Sciences, McGill University（麦吉尔大学地球与行星科学系）；Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles（加州大学洛杉矶分校地球、行星与空间科学系）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；School of Physics and Astronomy, University of St Andrews（圣安德鲁斯大学物理与天文学学院）
VLT/CRIRES+ observations of warm Neptune WASP-107 b: Challenges in detecting molecules with ground-based transmission spectroscopy of cooler and cloudy exoplanets
Uppsala University（乌普萨拉大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Georg-August-Universität（格奥尔格-奥古斯特大学）；Leibniz Institute for Astrophysics Potsdam (AIP)（波茨坦阿诺德·爱因斯坦天体物理研究所 (AIP)）；Ludwig-Maximilians-Universität München（慕尼黑路德维希-马克西米利安大学）；Namzitu Astro（Namzitu 天文台）
A JWST NIRSpec Phase Curve for WASP-121b: Dayside Emission Strongest Eastward of the Substellar Point and Nightside Conditions Conducive to Cloud Formation
Detection of Fe and evidence for TiO in the dayside emission spectrum of WASP-33b
理论研究预测在高辐射气体巨行星的大气中存在热反转。最近的观测已经确定了这些逆温层。然而，不同化学物质在其形成中的作用仍不清楚。我们在超热木星WASP-33 b的昼侧发射光谱中寻找热反转剂TiO和Fe的特征。用CARMENES和HARPS-N获得光谱，覆盖不同的波长范围。用SYSREM去除了大地和恒星的吸收线。我们交叉相关的剩余光谱与模型光谱检索信号从行星大气。我们发现TiO与CARMENES的显著性为4.9 $\mathrmσ$。TiO信号的强度在接近二次日食时下降。HARPS-N没有发现TiO信号。注入-恢复测试表明，TiO信号在HARPS-N覆盖的波长处低于检测水平。两种仪器分别在5.7 $\mathrmσ$和4.5 $\mathrmσ$的显著性水平下检测到Fe的发射特征。通过合并所有观察结果，我们获得Fe的显著性水平为7.3 $\mathrmσ$。我们发现TiO信号在$K_\mathrm{p}$ = $248.0_{-2.5}^{+2.0}$ km s $^{-1}$处，这与Fe检测在$K_\mathrm{p}$ = $225.0_{-3.5}^{+4.0}$ km s $^{-1}$处不一致。Fe的$K_\mathrm{p}$值与先前的研究一致。模型光谱需要不同的温度分布的TiO和Fe，以匹配的观察。我们观察到一个更广泛的线轮廓比TiO的Fe。我们的结果证实了在行星大气中存…
Thermal emission spectra of the ultra-hot Jupiter WASP-33 b
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；CAS Key Laboratory of Planetary Science, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台行星科学重点实验室）；Departamento de Astrofísica, Universidad de La Laguna（拉帕尔马大学天体物理学系）；Department of Astronomy, University of Science and Technology of China（中国科学技术大学天文系）；Deep Space Exploration Laboratory（深空探测实验室）
The panchromatic JWST dayside spectrum of WASP-121 b reveals a refractory-rich formation
Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Heidelberg University（海德堡大学）；University College Cork（科克大学学院）；Aarhus University（奥胡斯大学）；University of Bristol（布里斯托大学）；University of Newcastle（纽卡斯尔大学）；Lund University（隆德大学）；Observatoire astronomique de l’Université de Genève（日内瓦大学天文台）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Arizona State University（亚利桑那州立大学）；Espace pour la Vie（生命空间）；TU Graz（格拉茨工业大学）
