Notes. The rows in boldface show the results of this study, either using the spectroscopic or the seismic log g (given in square brackets). The abundances were rescaled to our adopted solar values when appropriate and whenever these were not quoted in the original paper. E: from excitation equilibrium of the Fe i lines; I: from ionisation equilibrium of Fe; P: from photometric data; LMT: from estimates of the luminosity, mass, and effective temperature; S: from spectral synthesis; F: from fitting of the spectral energy distribution; LDR: from line-depth ratios; B: from fitting the Balmer line wings; A: from asteroseismology.

Reference. (1) Hill 1997; (2) Gonzalez & Wallerstein 1998; (3) Tomkin & Lambert 1999; (4) Smith et al. 2000; (5) Mishenina & Kovtyukh 2001; (6) Reddy et al. 2002; (7) Zoccali et al. 2004; (8) Mortier et al. 2013 (using Kurucz models and the ’TS13’ line list); (9) Gratton & Sneden 1987; (10) Brown et al. 1989; (11) Fernández-Villacañas et al. 1990; (12) Brown & Wallerstein 1992; (13) Peterson et al. 1993; (14) McWilliam & Rich 1994; (15) Griffin & Lynas-Gray 1999; (16) Decin et al. 2003; (17) Meléndez et al. 2003; (18) Recio-Blanco et al. 2006; (19) Lecureur et al. 2007; (20) Ramírez & Allende Prieto 2011; (21) Ramírez et al. 2013; (22) Smith et al. 2013; (23) Fulbright et al. 2006; (24) Bruntt et al. 2010; (25) Takeda et al. 2008; (26) Hekker & Meléndez 2007; (27) Ghezzi et al. 2010; (28) McWilliam 1990; (29) Kovtyukh et al. 2006; (30) Valenti & Fischer 2005; (31) Fuhrmann & Chini 2012; (32) Matrozis et al. 2013; (33) Luck & Heiter 2007; (34) Liu et al. 2007; (35) Luck & Heiter 2006; (36) Allende Prieto et al. 2004; (37) Fuhrmann 2004.