KELT-9 b atmos. model transmission spectra

Of these, we identified the elements that are expected to have spectral lines in the visible wavelength range and used those as cross-correlation templates. We detect (>5{sigma}) absorption by NaI, CrII, ScII and YII, and confirm previous detections of MgI, FeI, FeII, and TiII. In addition, we find evidence of CaI, CrI, CoI, and SrII that will require further observations to verify.

The detected absorption lines are significantly deeper than predicted by our model, suggesting that the material is transported to higher altitudes where the density is enhanced compared to a hydrostatic profile, and that the material is part of an extended or outflowing envelope. There appears to be no significant blue-shift of the absorption spectrum due to a net day-to-night side wind. In particular, the strong Fe ii feature is shifted by 0.18+/-0.27km/s, consistent with zero.

Using the orbital velocity of the planet we derive revised masses and radii of the star and the planet: M*= 1.978+/-0.023M_{sun}_, R*=2.178+/-0.011R_{sun}_, m_p_=2.44+/-0.70M_J_ and Rp=1.783+/-0.009R_J_.