For each of the 227 observations, we derived effective radius, , and mean surface brightness within this radius, , by fitting an r1/4 growth curve to the observed aperture magnitudes, . Only radii in the interval from to the radius where the uncertainty on exceeded were used for the fit. (FWHM is the seeing, cf. Sect. .) This applies to 215 of the observations. For 10 observations the minimum radius was decreased to , and for 2 observation also the maximum allowed uncertainty on was increased to . In this way, there was always at least 6 data points available for the fit.
It is important to take the seeing into account when deriving and (Saglia et al. 1993; see also JFK95a). We do this following JFK95a. First an initial guess on is obtained from a fit that does not take the seeing into account. From the resulting and the seeing of the data an intelligent guess on the real (i.e. seeing deconvolved) is calculated. An r1/4 growth curve corresponding to this is then convolved with a model PSF that is scaled to the seeing of the data. This growth curve is fitted to the data, giving a new estimate of . The process is iterated until is stable to within 0.005. Then is calculated. Since the seeing convolved growth curve depends on it is important to have a good guess on to start with, which is why we calculate the above `intelligent guess'. The model PSF is taken to be the Fourier transform of (cf. Wolf 1982; Saglia et al. 1993), which is the theoretical prediction for seeing caused by atmospheric turbulence. b is a scale factor that is proportional to the FWHM.
From the definition of and it follows that the total magnitude is given by .
At the effective radius in Gunn r the ellipticity and position angle were determined.
We determined effective colors
Properties of E and S0 Galaxies in the Clusters HydraI and Coma
Master's Thesis, University of Copenhagen, July 1997
Bo Milvang-Jensen (email@example.com)