Notes. From left to right the columns give the target name; the variable type (from GCVS); the logarithmic period; the mean magnitudes in J, H, and K bands. Columns 7 and 8 give the iron abundance available in the literature rescaled to our solar abundance, and the current iron abundance. Column 9 gives the number of spectra used to estimate the mean iron abundance. Columns 10 and 11 list the true distance modulus and the Galactocentric distance. The last two columns give the notes on the NIR photometry and distances for individual objects and the references. a) Mean magnitudes provided by Monson & Pierce (2011) transformed into the 2MASS photometric system using the zero-points given in their Table 1. b) Mean magnitudes provided by Laney & Stobie (1992) and by Laney (priv. comm.) transformed into the 2MASS photometric system using the zero–points provided by Koen et al. (2007). The objects marked with a ^† (Laney, priv. comm.) do not have a complete coverage of the light-curve (the number of phase points ranges from 4 to 14). c) Mean magnitudes based on single-epoch measurements from the 2MASS catalog and the NIR template light curves provided by Soszyński et al. (2005). An asterisk indicates the use of single-epoch photometry in the distance determination (see Sect. 3 for details). For these stars the magnitudes listed in Cols. 4–6 are the single-epoch measurements retrieved from the 2MASS catalog. d) The weighted mean of the three true distance moduli. The errors account for uncertainties affecting the mean magnitudes and for the intrinsic dispersion of the adopted NIR PW relations. e) The weighted mean Galactocentric distances were estimated assuming R_G = 7.94 ± 0.37 ± 0.26 kpc (Groenewegen et al. 2008). The errors account for uncertainties affecting both the solar Galactocentric distance and the heliocentric distances. f) References for the iron estimate given in Col. 7. The priority was given, in the following order, to evalutions from our group (G13: Genovali et al. 2013; PED: Pedicelli et al. (2010); LEM: Lemasle et al. (2007, 2008); ROM: Romaniello et al. (2008)) and from the literature: LII: Luck et al. (2011); LIII: Luck & Lambert (2011).