On the stellar content of the Carina dwarf spheroidal galaxy
  We present U,B,V,I photometry of the Carina dwarf spheroidal galaxy, based on
more than 4,000 CCD images. Special attention was given to the photometric
calibration, and the precision for the B,V,I bands is better than 0.01 mag. We
compared in the V,B-V and V,B-I color-magnitude diagrams (CMDs) Carina with
three Globular Clusters (GCs, M53, M55, M79). We find that only the more
metal-poor GCs (M55, [Fe/H]=-1.85; M53, [Fe/H]=-2.02 dex) provide a good match
with the Carina giant branch. We performed a similar comparison in the V,V-I
CMD with three SMC intermediate-age clusters (IACs, Kron3, NGC339, Lindsay38).
We find that the color extent of the SGB of the two more metal-rich IACs
(Kron3, [Fe/H]=-1.08; NGC339, [Fe/H]=-1.36 dex) is smaller than the range among
Carina's intermediate-age stars. However, the ridge line of the more metal-poor
IAC (Lindsay38, [Fe/H]=-1.59 dex) agrees quite well with the Carina
intermediate-age stars. These findings indicate that Carina's old stellar
population is metal-poor and seems to have a limited spread in metallicity
(Delta [Fe/H]=0.2--0.3 dex). Carina intermediate-age stars can hardly be more
metal-rich than Lindsay38 and its spread in metallicity appears modest. We also
find that the synthetic CMD constructed assuming a metallicity spread of 0.5
dex for intermediate-age stars predicts evolutionary features not supported by
observations. The above results are at odds with recent spectroscopic
investigations suggesting that Carina stars cover a broad range in metallicity
(Delta [Fe/H]~1--2 dex). We present a new method to estimate the metallicity of
complex stellar systems using the difference in color between the red clump and
the middle of the RR Lyrae instability strip. The observed colors of Carina's
evolved stars indicate a metallicity of [Fe/H]=-1.70+-0.19 dex, which agrees
quite well with spectroscopic measurements.
