2006A&A...452..141G

We present a study of the old globular cluster (GC) population of the dwarf irregular galaxy NGC1427A using multi-wavelength VLT observations in U,B,V,I, H_α and J bands under excellent observing conditions. We applied color and size selection criteria to select old GC candidates and made use of archival ACS images taken with the Hubble Space Telescope to reject contaminating background sources and blended objects from the GC candidates' list. The H_α observations were used to check for contamination due to compact, highly reddened young star clusters whose colors and sizes could mimic those of old GCs. After accounting for contamination we obtain a total number of 38±8 GC candidates with colors consistent with an old (∼10Gyr) and metal-poor (Z<0.4xZ_☉) population as judged by simple stellar population models. Our contamination analysis indicates that the density distribution of GCs in the outskirts of the Fornax central cD galaxy NGC1399 may not be spherically symmetric. We derive a present-day specific frequency S_N of 1.6 for NGC1427A, a value significantly larger than what is observed in the Local Group dwarf irregular galaxies and comparable with the values found for the same galaxy types in the Virgo and Fornax clusters. Assuming a universal globular cluster luminosity function turnover magnitude, we derive a distance modulus to NGC1427A of 31.01±0.21mag which places it ∼3.2±2.5(statistic)±1.6(systematic)Mpc in front of the Fornax central cD galaxy NGC1399. The implications of this result for the relationship between NGC1427A and the cluster environment are briefly discussed.