We present a BVRI CCD (Charge Coupled Device) surface photometry analysis of the galaxy group NGC 4410, which contains four galaxies in interaction. Along with our photometric study, we show residual images (after subtracting isophotal models) and unsharp masked images to uncover any hidden structures in this system of galaxies; we have also performed a two-dimensional bulge-disk decomposition for NGC 4410C and D, and a major axis sector profile for NGC 4410A. We have calculated BVRI surface brightnesses and colors within regions such as galaxy centers, bridges, tails and optical knots in the NGC 4410 system, generating B− V color maps and color profiles. The information obtained was used to discover the predominant stellar populations. The colors of the galaxies imply ages of ∼2 × 10 9 to ∼2 × 10 10 years for models using a range of metallicities. The bluer knots and H II regions have colors implying ages of a minimum of 5× 10 8 years, but possibly as high as 3× 10 9 years for stellar populations formed in the interaction. These results lead us to conclude that there is a moderate star formation rate and a tranquil evolving state of the system with a long timescale for interaction, much longer than the typical dynamical timescales of 10 8 years. Although we note that NGC 4410D has a blue nucleus (possible nuclear starburst?), bulge, bar, and short spiral arms, and may be interacting with a H I gas cloud. Some observed structures in NGC 4410A are coincident with previously studied H II regions, a tidal arm and optical/radio knots found in this galaxy. An optical knot E coincident with a radio knot may be an optical synchrotron emission or an H II region. The galaxy NGC 4410B appears to be a boxy giant elliptical with a possible dusty disk embedded (similar to Cen A?) and NGC 4410C is confirmed as a lenticular galaxy.

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We have carried out deep BV R surface photometry of 6 cD and cD-like galaxies using the 2.1-m telescope at San Pedro Mártir, cD galaxies are supergiant galaxies (M > 10 13 M ) with enormous halos (> 100 kpc in radius) surrounding a giant elliptical galaxy, found generally at the centre of rich clusters (Oemler 1976, Schombert 1988. The surface brightness profiles of their halos (envelopes) break from the r 1/4 law, containing more light at large radii (Schombert (1988)), although a detailed 1 and 2 dimensional analysis of their morphology has yet to be carried out. There have been four main theories as to the origin of cD envelopes (Schombert (1988) and references within), a) stripping of stars from other cluster member galaxies, b) formation of galaxy and envelope at the same time during the formation of the cluster, c) mergers of cluster members, which do not easily explain the high velocity dispersions in the envelopes (∼ 1000 km s −1 ), d) cooling flows: accumulation of cooling X-ray-emitting ICM gas around the central galaxy. Very red envelopes have been found around some cD's, and star formation biased towards lowmass stars in cooling flows were invoked to explain these red halos, but the expected very bright near-IR halos were not detected (Joy et al. 1995 and references within). Previous detailed studies of cD galaxies (e.g. Mackie 1992) found a range of colour gradients.Our sample included the cDs in the clusters A193, A426 (NGC 1275), A496, A754, A2634 and A2670. The typical colours of their envelopes are (B − V ) = 1.1 − 1.3 and (V − R) = 0.5 − 0.7. In most cases there is no obvious gradient over the entire radial range studied. In the two cD-like galaxies (A426, A754), a gradient of 0.5 to the red in (B − R) was detected, although no extended envelope was detected (neighbour galaxies make it difficult to follow the profile). For NGC 1275, the central regions are bluer due to many regions of active star formation. In the case of 2 objects with multiple nuclei (A193 and A2634), no colour gradients, nor zones of star formation, were found. In many cases the colours of nearby cluster members are very similar to the cD galaxy.These results favour a primordial origin for the cD envelope. Thus the envelope retains characteristics of the cluster, and its stellar population has evolved similarly to that of the central galaxy. Any changes caused by mergers, interactions, and cooling flows, are temporary. The envelope is dominated by an old stellar population ('red-and-dead'). The largest galaxies in the universe may well be the first to be fully formed, and this seems to be in agreement with recent ideas of 'downsizing' in which E/cD galaxies are the first to complete their star formation.

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