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Table B.2

Selection of Ti I and Fe I lines in the spectra of GX And (M1.0 V), Luyten’s star (M3.5 V), and Teegarden’s star (M7.0 V).

Range Atomic line (a) Magnetically Ref. (c) GX And Luyten’s Teegarden’s
λmin [Å] λmax [Å] λline [Å] Element χ [eV] loggf geff sensitive (b) star star
5636.61 5651.65 5644.134 Ti I 2.2674 +0.120 1.010 This work
5859.04 5874.01 5866.451 Ti I 1.0666 −0.790 1.170 This work
5914.95 5929.51 5922.110 Ti I 1.0460 −1.380 0.500 This work
5969.39 5985.75 5976.776 Fe I 3.9433 −1.236 1.100 This work
5978.541 Ti I 1.8732 −0.312 0.890 This work
6056.60 6072.73 6064.626 Ti I 1.0460 −1.670 1.990 This work
6065.481 Fe I 2.6085 −1.530 0.680 This work
6077.90 6092.38 6085.226 Ti I 1.0529 −1.331 1.750 This work
6119.00 6145.00 6126.216 Ti I 1.0666 −1.206 1.240 This work
6136.615 Fe I 2.4534 −1.400 0.840 This work

Notes. The corresponding wavelength ranges synthesised in this work are listed in the first two columns. χ, log gf, and geff are the excitation potential, the oscillator strength, and the effective Landé factors of the lines, respectively. (a) Atomic line data from the VALD3 database (Ryabchikova et al. 2015). (b)Lines particularly affected by the stellar magnetic field (López-Gallifa et al. in prep.). (c) Lines employed in Tabernero et al. (2018, Tab18), and Passegger et al. (2019, Pas19).

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