We present a BVRI CCD surface photometry analysis of the interacting compact galaxy group NGC 4410. Along with our photometric study we show residual images (after subtracting isophotal models) and unsharp masked images in order to uncover any hidden structures in this system of galaxies. We have calculated BVRI surface brightnesses and colours within regions such as galaxy centers, bridges, tails and optical knots in this system, generating B-V color maps and color profiles. The information obtained was used to discover the predominant stellar populations. Most of the galaxies have the colours of K0-K5 giant stars, with ages at least 10 Gyr assuming solar metallicity. These results lead us to the conclusion of a moderate star formation rate and a tranquil evolving state of the system, apart from NGC 4410D which has a blue nucleus, bulge, bar and ring and may be interacting with a H I cold gas cloud. An optical knot E coincident with a radio knot may be optical synchrotron emission or an H II region. Some observed structures in NGC 4410A are coincident with previously studied H II regions, a tidal arm and an optical/radio knot found in this galaxy.