Presentation #102.30 in the session Poster Session.
Relatively large radii of some hot Jupiters observed in the ultraviolet and blue-optical are generally interpreted to be due to Rayleigh scattering by high-altitude haze particles. However, the haze composition and its production mechanisms are not fully understood, and observational information is still limited. Here, I will present our study of different haze extinction levels in the atmospheres of HD 209458 b and HD 189733 b with high resolution spectra. We have analysed water vapour cross-correlation signals in the red optical and in the near-infrared. To do so, a total of seven transits of the two planets were observed with the CARMENES spectrograph at the 3.5m Calar Alto telescope. Their Doppler-shifted signals were disentangled from the telluric and stellar contributions using the detrending algorithm SYSREM, and the residual spectra were cross-correlated with water vapour templates to measure the strength of the absorption bands. We detected the H2O bands in HD 209458 b in one transit, whereas no evidence of them was found in four transits of HD 189733 b. Therefore, the relative strength of the optical water bands compared to those in the near-infrared were found to be larger in HD 209458 b than in HD 189733 b. We interpret the non-detection of optical water bands in the transmission spectra of HD 189733 b, compared to the detection in HD 209458 b, to be due to the presence of high-altitude hazes in the former planet, which are largely absent in the latter. This is consistent with previous measurements with the Hubble Space Telescope. We show that currently available CARMENES observations of hot Jupiters can be used to investigate the presence of haze extinction in their atmospheres.