TiO and VO broad band absorption features in the optical spectrum of the atmosphere of the hot-Jupiter HD209458b

TL;DR

This study investigates the presence of TiO and VO molecules in the atmosphere of the hot Jupiter HD209458b, suggesting their possible role in observed broad band absorption and thermal inversion, despite no unambiguous spectral signatures.

Contribution

It provides upper limits on TiO and VO abundances in HD209458b's atmosphere and links their potential opacities to observed spectral features and temperature inversion.

Findings

No unambiguous TiO/VO spectral signatures detected.

TiO and VO abundances are constrained to 10-1000 times below solar.

Broad band absorption may be explained by TiO/VO opacities.

Abstract

The presence of titanium oxide (TiO) and vanadium oxide (VO) gas phase species is searched for in the atmosphere of the hot Jupiter HD209458b. We compared a model for the planets transmitted spectrum to multi-wavelength eclipse-depth measurements (from 3000 to 10000 Angstrom), obtained by Sing et al. (2008a) using archived HST-STIS time series spectra. We make use of these observations to search for spectral signatures from extra absorbers in the planet atmosphere between 6000 and 8000 Angstrom. Along with sodium depletion and Rayleigh scattering recently published for this exoplanet atmosphere, an extra absorber of uncertain origin, redward of the sodium lines, resides in the atmosphere of the planet. Furthermore, this planet has a stratosphere experiencing a thermal inversion caused by the capture of optical stellar flux by absorbers that resides at altitude. Recent models have predicted that the presence of TiO and VO in the atmosphere of HD209458b may be responsible for this temperature inversion. Although no specific TiO and VO spectral band head signatures have been identified unambiguously in the observed spectrum, we suggest here that the opacities of those molecules are possible candidates to explain the remaining continuous broad band absorption observed between 6200 and 8000 Angstrom. To match reasonably well the data, the abundances of TiO and VO molecules are evaluated from ten to one thousand times below solar. This upper limit result is in agreement with expected variations with altitude due to depletion effects such as condensation.