A sample of low-luminosity M-type supergiants observed with AF2. All these objects are likely foreground to Ste 2, as they have lower v_LSR and lower E(J − K_S) colour excess. In these sources, Fe i 8621 Å is stronger than Fe i 8611 Å, indicating an important contamination by the 8620 Å DIB. The main luminosity indicators are the Ca ii lines and the 8648 Å blend, but note also the weakness of the 8514 Å feature compared to objects in Fig. 5. The growing strength of the TiO 8432 Å bandhead, blended with Ti i 8435 Å, can be seen to correlate very well with TiO 8660 Å (the Ti i 8427 Å line, immediately to its left, can be used as reference).