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Galaxy Luminosity Function of the Coma Cluster from Deep ﹩{u}^{{\prime} }﹩ − ﹩{g}^{{\prime} }﹩ − ﹩{r}^{{\prime} }﹩ Wendelstein Imaging Data

  • Authors: Raphael Zöller, Matthias Kluge, Ralf Bender, Jan-Niklas Pippert, Benjamin Seidel, Claus Gössl, Ulrich Hopp, Hanna Kellermann, Christoph Ries, Arno Riffeser, Michael Schmidt, Luis Thomas

Raphael Zöller et al 2026 The Astrophysical Journal 1011 .

  • Provider: AAS Journals

Caption: Figure 7.

Selected outputs of the fitting routine for LEDA 44562 in the ﹩{g}^{{\prime} }﹩ band with a cutout size of ﹩2\mathop{.}\limits^{^{\prime} }1\times 2\mathop{.}\limits^{^{\prime} }1﹩. The ellipticity, position angle, and central coordinates are automatically fixed beyond their respective fixed radii; the orange marked isophote indicates the radius beyond which the ellipticity is fixed. In this case, the P.A. is fixed at a lower isophote than the ellipticity. The background is determined at the red-marked position. In the surface brightness profile plot, the blue dots are the data points used for the fit, the orange dots are excluded from the fit, the solid green line corresponds to the best-fit Sérsic profile (with n = 4.4 ± 1.2), and the dashed green line indicates the threshold from which the Sérsic profile is used as the model. The Sérsic model assumes perfect ellipses, i.e., a4/a = 0.

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