Cross-correlation results in K_p − V_sys space for Ti I (left) and V I (right). Top panels: two-dimensional cross-correlation map. The dashed lines indicate the expected location of the signal compared to a purely Keplerian orbit. Bottom panels: one-dimensional cross-correlation function at the orbital velocity of the strongest absorption from the upper panel. The Ti I panel is multiplied by two to ensure visibility. The horizontal lines indicate the expected absorption depth at the indicated model temperature. The increase between lines is 100 K. V I requires a temperature of ∼3900 K, while for Ti I, the thermometer suggests ∼2900 K. Together with Fig. 9, this suggests that Ti I is significantly depleted compared to V I.