Table 2: Spectral lines that display similar behaviour to Fe I 6141.7 Å and Si I 6155.1 Å in the temperature range from 3750 K to 5250 K and that have previously been used for Doppler imaging.
Ti I 5866.4 Å Fe I 6180.2 Å Li I 6707.9 Å

Ca I 6102.8 Å V I 6199.2 Å Ca I 6717.7 Å

Ni I 6108.1 Å Fe I 6430.9 Å Ti I 6743.1 Å

Ca I 6122.2 Å Ca I 6439.1 Å Ca I 7148.2 Å

Fe I 6151.6 Å Fe I 6546.2 Å K I 7699.0 Å

Ca I 6166.4 Å Ni I 6643.6 Å Ti I 8412.4 Å

Fe I 6173.3 Å

**Table 2:** Spectral lines that display similar behaviour to Fe I 6141.7 Å and Si I 6155.1 Å in the temperature range from 3750 K to 5250 K and that have previously been used for Doppler imaging.
Ti I 5866.4 Å	Fe I 6180.2 Å	Li I 6707.9 Å
Ca I 6102.8 Å	V I 6199.2 Å	Ca I 6717.7 Å
Ni I 6108.1 Å	Fe I 6430.9 Å	Ti I 6743.1 Å
Ca I 6122.2 Å	Ca I 6439.1 Å	Ca I 7148.2 Å
Fe I 6151.6 Å	Fe I 6546.2 Å	K I 7699.0 Å
Ca I 6166.4 Å	Ni I 6643.6 Å	Ti I 8412.4 Å
Fe I 6173.3 Å

Source LaTeX | All tables | In the text

	1 Introduction
	2 Simulations of starspots and faculae
	3 Results and discussion
	4 Summary and conclusions
	References