Left panels: total cross-correlation values in the neighborhood of V _rest ~ 0. Right panels: theoretical models they correspond to. We use the best models containing methane only (in green, first panels), and water vapour only (in blue, second panels), and two models with temperature inversion with methane only, VMR ~ 10⁻⁵, (in green, third panels), and water vapor only, VMR ~ 10⁻³, (in blue, fourth panels). Since the emission lines in the models with temperature inversion correlated negatively with the absorption lines in the observed planetary spectrum, unlike the absorption lines in the noninverted models, we can infer a noninverted temperature profile for HD 102195b.