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Table C.1

Best-fitting structural parameters for a two-component fit in which n for the inner (in situ) component is fixed.

Object μ e1 r e1 n 1 μ e2 r e2 n 2 m T,1 m T,2 f h
[mag/arcsec2] [arcsec] [mag/arcsec2] [arcsec] [mag] [mag]
NGC 1399 19.76 ± 0.06 19.48 ± 0.89 2 24.60 ± 0.06 382 ± 11 1.45 ± 0.08 9.92 8.30 82%
NGC 3923 20.41 ± 0.14 17.34 ± 1.90 2 24.11 ± 0.15 215 ± 16 3.36 ± 0.45 10.83 9.06 84%
NGC 4365 20.06 ± 0.24 10.72 ± 1.60 2 23.56 ± 0.15 159 ± 11 3.96 ± 0.36 11.52 9.17 90%
NGC 4472 21.08 ± 0.33 39.95 ± 7.50 2 25.32 ± 0.49 547 ± 118 6.10 ± 0.69 9.68 8.24 79%
NGC 5044 22.16 ± 0.05 39.3 ± 1.8 2.5 27.03 ± 0.17 678 ± 55 1.54 ± 0.27 10.80 9.49 77%
NGC 5846 21.11 ± 0.16 18.9 ± 1.1 2 26.87 ± 0.28 757 ± 101 5.47 ± 0.68 11.34 9.09 89%

Notes. Columns 2–4 report effective magnitude, effective radius, and Sérsic index for the inner component of each fit. The Sérsic index for the in situ component has been fixed to n ~ 2 using the models as a prior (Cooper et al. 2013). We allowed small variations of ±0.5 around the mean value of n = 2. This would bracket the range of n in the simulations and allows us to obtain a better fit. Columns 5–7 list the same parameters for the outer Sérsic component. Columns 8 and 9 report the total magnitude of the inner (mT,1) and outer Sérsic component (mT,2). Column 12 gives the relative fraction of the outer component with respect to the total luminosity of the galaxy.

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