We present new BV time series data of the Carina dwarf spheroidal ( dSph ) galaxy .
Current data cover an area of \approx 0.3 degree ^ { 2 } around the center of the galaxy and allowed us to identify 92 variables .
Among them 75 are RR Lyrae stars , 15 are ” bona fide ” Anomalous Cepheids , one might be a Galactic field RR Lyrae , and one is located along the Carina Red Giant Branch ( RGB ) .
Expanding upon the seminal photographic investigation by Saha , Monet , & Seitzer ( 1986 ) we supply for the first time accurate estimates of their pulsation parameters ( periods , amplitudes , mean magnitude and colors ) on the basis of CCD photometry .
Approximately 50 % of both RR Lyrae and Anomalous Cepheids are new identifications .
Among the RR Lyrae sample 6 objects are new candidate double-mode ( RRd ) variables .
On the basis of their pulsation properties we estimated that two variables ( V152 , V182 ) are about 50 % more massive than typical RR Lyrae stars , while the bulk of the Anomalous Cepheids are roughly a factor of two more massive than fundamental mode ( RRab ) RR Lyrae stars .
This finding supports the evidence that these objects are intermediate-mass stars during central He burning phases .

We adopted three different approaches to estimate the Carina distance modulus , namely the First Overtone Blue Edge ( FOBE ) method , the Period-Luminosity-Amplitude ( PLA ) relation , and the Period-Luminosity-Color ( PLC ) relation .
We found DM = 20.19 \pm 0.12 , a result that agrees quite well with similar estimates based on different distance indicators .

The data for Carina , together with data available in the literature , strongly support the conclusion that dSph galaxies can barely be classified into the classical Oosterhoff dichotomy .
The mean period of RRab in Carina resembles that found for Oosterhoff type II clusters , whereas the ratio between first overtones ( RRc ) and total number of RR Lyrae is quite similar to that found in Oosterhoff type I clusters .