The results of a UBV CCD photometric study of the cluster IC 4996 are presented. We obtain new values for the cluster parameters: E(B-V) = 0.71 ± 0.08, V0 - MV = 11.9 ± 0.1, and age = (7.5 ± 3) × 106 yr. The combined evidence from the photometric diagrams suggests the presence of a number of pre–main-sequence (PMS) cluster members with spectral types ~A0 to F5. The interpretation of these objects as PMS candidates is further supported by independent results from CCD uvby Hβ observations. If confirmed, these stars would bridge the existing gap in the sample of PMS stars, between the coolest Herbig AeBe stars (HAeBe), and the hottest T Tauri stars. These PMS candidates are located some 0.5 and 1 mag above the main sequence in the V-(B-V) diagram, around the location of spectral types AF. This feature, together with their locations in the (U-B)-(B-V) diagram and the interpretation that they are PMS members, suggest an additional reddening law with a slope α = E(U-B)/E(B-V) 0.55, probably caused by circumstellar material.
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