Table 2: Spectroscopic and photometric metallicities and observed mean magnitudes of the SPS RRab sample.

Var.		 [Fe/H] $_{\rm spect}^{\rm a}$[Fe/H] $_{\rm phot}$ $\langle V\rangle_{\rm int}$Rem.$^{\rm b}$Ref. phot.$^{\rm c}$
  dex mag   
9 -0.87-1.53 15.630*2, 3
10 -1.55-1.48 15.615(Bl)2, 3, 4, 5
15 -1.24-1.47 15.597 2, 3, 5
18 -1.06-1.30 15.673 2, 3, 5
20 -1.51- 15.611Bl2, 3
36 -1.43-1.44 15.618 2, 3
39 -1.09- 15.674Bl2, 3
46 -1.35-1.11 15.668 1, 2, 3, 4
51 -1.34-1.33 15.621 2, 3, 5
52 -1.22- 15.705Bl2, 3, 5
59 -1.06-1.23 15.646(Bl)2, 3, 5
60 -1.28-1.28 15.520 2, 3
61 -1.33- 15.641Bl2, 3, 5
62 -1.28-1.14 15.620(Bl)2, 3, 5
63 -0.83- 15.661Bl2, 3, 5
66 -1.05- 15.607Bl1, 2, 3, 4, 5
77 -0.97-1.12 15.725**1, 2, 3, 4
78 -0.93- 15.554Bl1, 2, 3, 4
81 -1.41-1.43 15.656 2, 3
82 -1.59-1.57 15.601 3
84 -1.03-1.19 15.630 1, 2, 3, 4, 5
90 -1.05-1.36 15.639 2, 3, 5
93 -1.60-1.37 15.640 2, 3
94 -1.13-1.37 15.677 2, 3
113 -1.48- -** 
114 -0.92-1.27 15.686-3
115 -1.30- -**3
116 -1.42-1.26 15.685-2, 3
202 -1.19- 15.524***2, 3
$^{{\rm a}}$
[Fe/H] $_{\rm spect}$ = [Fe/H] $_{\rm FeII}$ from SPS.

$^{\rm b}$
Bl: no [Fe/H] $_{\rm phot}$ is calculated for Blazhko stars with large light curve modulation;

(Bl): Blazhko stars with slight light curve changes are included but photometric [Fe/H] is less certain;

* : spectroscopic [Fe/H] seems to be wrong, see the text for details;

** : photometric data have larger scatter;

*** : classification is uncertain;

- : no or poor quality light curve is available.

$^{\rm c}$
1) Bakos & Jurcsik (2000); 2) Benko et al. (2003); 3) Corwin & Carney (2001); 4) Carretta et al. (1998); 5) Kaluzny (1998).

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