CRIRES+ detection of CO emissions lines and temperature inversions on the dayside of WASP-18b and WASP-76b

TL;DR

This study used the CRIRES+ spectrograph to detect CO emission lines indicating temperature inversions on the daysides of two ultra-hot Jupiters, WASP-18b and WASP-76b, marking the first such detections for planets orbiting F-type stars.

Contribution

First detection of CO emission lines indicating temperature inversions on the dayside of UHJs orbiting F-type stars using high-resolution spectroscopy.

Findings

Detected strong CO emission lines in both planets.

Retrieved temperature-pressure profiles and CO mixing ratios.

Measured rotational velocities consistent with tidal locking.

Abstract

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.