Comparative modelling of the spectra of cool giants

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Table 3

Results and references for previous spectroscopic works on α Tau.

T _eff	(a)	log g	^(b)	[Fe/H]	Reference

4140	sp	1.0	sp	−0.33	Lambert & Ries (1981)
3830	ph	1.2	sp	−0.14	Kovacs (1983)
3850	ph	1.5	ev	(c)	Smith & Lambert (1985)
3800	ph	1.8	ph	−0.17	Fernandez-Villacanas et al. (1990)
3910	ph	1.6	ev	−0.34	McWilliam (1990)
3875	ph	0.6	sp	−0.16	Luck & Challener (1995)
3850	ph	0.6	li	−0.10	Mallik (1998)
4100	sp	1.7	sp	−0.36	Hekker & Meléndez (2007)
3890	sp^d	1.2	sp^d	−0.15	Meléndez et al. (2008)

Notes.

^(a)

Method for T_eff determination: sp ... spectroscopic (excitation equilibrium of iron line abundances), ph ... photometric calibrations.

^(b)

Method for log g determination: sp ... spectroscopic (ionization equilibrium of iron line abundances), ph ... photometric calibrations, ev ... from absolute magnitudes and stellar evolution calculations, li ... from literature.

^(c)

α Tau was used as a reference object for the spectroscopic analysis of M giants.

^(d)

from infrared spectra.

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