We present V and I CCD photometry of suspected low-surface brightness dwarf galaxies detected in a survey covering \sim 2.4 deg ^ { 2 } around the central region of the Dorado group of galaxies .
The low-surface brightness galaxies were chosen based on their sizes and magnitudes at the limiting isophote of 26.0V \mu .
The selected galaxies have magnitudes brighter than V \approx 20 ( M _ { V } \approx - 11 for an assumed distance to the group of 17.2 Mpc ) , with central surface brightnesses \mu _ { 0 } > 22.5 V mag/arcsec ^ { 2 } , scale lengths h > 2 ″ , and diameters \geq 14 ″at the limiting isophote .
Using these criteria , we identified 69 dwarf galaxy candidates .
Four of them are large very low-surface brightness galaxies that were detected on a smoothed image , after masking high surface brightness objects .
Monte Carlo simulations performed to estimate completeness , photometric uncertainties and to evaluate our ability to detect extended low-surface brightness galaxies show that the completeness fraction is , on average , > 80 % for dwarf galaxies with -17 < M _ { V } < -10.5 and 22.5 < \mu _ { 0 } < 25.5 V mag/arcsec ^ { 2 } , for the range of sizes considered by us ( D \geq 14″ ) .
The V - I colors of the dwarf candidates vary from -0.3 to 2.3 with a peak on V - I = 0.98 , suggesting a range of different stellar populations in these galaxies .
The projected surface density of the dwarf galaxies shows a concentration towards the group center similar in extent to that found around five X-ray groups and the elliptical galaxy NGC1132 studied by Mulchaey & Zabludoff ( 1999 ) , suggesting that the dwarf galaxies in Dorado are probably physically associated with the overall potential well of the group .