MULTICOLOR CCD SURFACE PHOTOMETRY FOR E-GALAXIES AND S0-GALAXIES IN 10 CLUSTERS

CCD surface photometry for 232 E and S0 galaxies is presented. The gal axies are observed in Gunn r and Johnson B, or Gunn r and g. For 48 of the galaxies surface photometry in Johnson U is also presented. Apert ure magnitudes in Gunn v are derived for half of the galaxies. Galaxie s in the following clusters have been observed: Abell 194, Abell 539, Abell 3381, Abell 3574, Abell S639, Abell S753, HydraI (Abell 1060), D C2345 - 28, Doradus and Grm15. The data are part of our ongoing study of the large-scale motions in the Universe and the physical background for the fundamental plane. We use a full model fitting technique for analysing the CCD images. This gives radial profiles of local surface brightness, colour, ellipticity and position angle. The residuals rela tive to the elliptical isophotes are described quantitatively by Fouri er expansions. Effective radius, mean surface brightness and total mag nitude are derived by fitting a de Vaucouleurs r(1/4) growth curve. We have derived a characteristic radius r(n) similar to the diameter D-n introduced by Dressier et al. The derivation of the effective paramet ers and of r(n) takes the seeing into account. We confirm the results by Saglia et al. that the effects of the seeing can be substantial. Se eing-corrected Values of the effective parameters and r(n) are also pr esented for 147 E and S0 galaxies in the Coma cluster. Colours, colour gradients and geometrical parameters are derived. The photometry is i nternally consistent within 0.016 mag. Comparison with the photoelectr ic aperture photometry from Burstein et al. shows a mean offset of 0.0 10 mag with an rms scatter of 0.034 mag. The global photometric parame ters are compared with data from Faber et al., Lucey et al. and Lucey and Carter. These comparisons imply that the typical rms errors are as follows - log r(n): +/- 0.015; log r(e): +/-0.045; m(T): +/-0.09 mag; [mu](e): +/-0.16 mag. The rms error on the combination log r(e)- 0.35 [mu](e) which enters the fundamental plane is +/-0.020. Also, compari sons with data from Saglia et al. are presented. The accuracy of the a bsolute photometry, as well as the derived parameters, makes the data suitable for our investigations of the fundamental plane and of the la rge-scale motions in the Universe.