Astron. Astrophys. 351, 869-882 (1999) Appendix A: the optical growth curveLet be defined by where is such as . According to Prugniel & Héraudeau (1998), is defined by , where , if or - corresponding to a Sérsic (1968) luminosity profile -, and by if , i.e., interpolated between the de Vaucouleurs profile and the exponential profile valid respectively for giant ellipticals and pure-disk galaxies. Appendix B: computation of NIR magnitudes and uncertaintiesLet us first define , , where is the weight attributed to the point, , , , and . Two methods have been used, depending essentially on the number of observations and their accuracy. In the first one, the total NIR magnitude is computed assuming by minimizing with respect to . We obtain and the corresponding effective magnitude is We assume here that, for want of constraint on s, the uncertainty on s is equal to the intrinsic scatter for this type. In the second method, s is considered as a free parameter and is computed by minimizing with respect to and s. We then get and Note that we have made the questionable assumption that the errors in the aperture magnitudes of a given galaxy are independent. We are however not primarily interested in the best fitting growth curve, which would be determined assuming , but rather in the best estimate of the asymptotic magnitude. When there is only one point, the uncertainty on is , i.e., the uncertainty on decreases with the size of the aperture. It is therefore reasonable to adopt for all the points to give more weight to the large apertures. To deal with outliers, we apply an iterative procedure. We initially assume for the "slope" s and for all the points. At each step, we fit the growth curve to the data, compute from above equations, and estimate new values of the uncertainties by . This procedure is a compromise between our a priori uncertainty and the a posteriori estimate , where or 2 is the number of fitted parameters (and also the index of the method!). It has the advantage of reducing the weight of outliers and takes the scatter around the growth curve automatically into account. Practically, it improves the fit and gives a reasonable estimate of the uncertainties. The convergence is usually achieved in a few iterations. The second method provides a better fit than the first one but is less secure, because the "slope" s of the growth curve is free. It is used only when following conditions are fulfilled simultaneously:
© European Southern Observatory (ESO) 1999 Online publication: November 16, 1999 |