Table 2
Bulge and disk photometric parameters of the original primary galaxies and of the final remnants in the merger experimentsa,b,c.
| Model | μ eff | r eff | n | μ 0,D | h D | B/D | MK(bulge) | MK(disk) | MK(total) |
| [mag/arcsec2] | [kpc] | [mag/arcsec2] | [kpc] | [mag] | [mag] | [mag] | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
|
|
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| Original S0b (B/D = 0.5) | 14.90 ± 0.08 | 0.90 ± 0.04 | 0.92 ± 0.11 | 17.10 ± 0.07 | 4.73 ± 0.10 | 0.51 ± 0.03 | –23.11 ± 0.24 | –23.86 ± 0.11 | –24.30 ± 0.12 |
| Original S0c (B/D = 0.08) | 15.97 ± 0.07 | 0.428 ± 0.007 | 0.52 ± 0.02 | 16.71 ± 0.07 | 2.66 ± 0.03 | 0.0760 ± 0.0024 | –20.92 ± 0.12 | –23.72 ± 0.09 | –23.80 ± 0.10 |
|
|
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| (a) M6 Ps Db | 14.52 ± 0.09 | 0.82 ± 0.06 | 1.7 ± 0.4 | 17.25 ± 0.07 | 5.00 ± 0.23 | 0.82 ± 0.10 | –23.6 ± 0.4 | –23.83 ± 0.17 | –24.47 ± 0.18 |
| (a2) M6 Ps Db TF3 | 14.65 ± 0.09 | 0.86 ± 0.06 | 1.6 ± 0.3 | 17.35 ± 0.07 | 5.22 ± 0.18 | 0.77 ± 0.08 | –23.5 ± 0.4 | –23.82 ± 0.14 | –24.45 ± 0.16 |
| (a3) M6 Ps Db TF4 | 14.62 ± 0.10 | 0.86 ± 0.10 | 1.8 ± 0.6 | 17.32 ± 0.07 | 5.09 ± 0.27 | 0.9 ± 0.3 | –23.6 ± 0.6 | –23.79 ± 0.19 | –24.46 ± 0.22 |
| (b) M6 Ps Rb | 14.65 ± 0.09 | 0.84 ± 0.06 | 1.7 ± 0.4 | 17.02 ± 0.07 | 4.64 ± 0.14 | 0.70 ± 0.11 | –23.5 ± 0.4 | –23.89 ± 0.13 | –24.47 ± 0.15 |
| (c) M6 Pl Db | 14.98 ± 0.08 | 0.985 ± 0.010 | 1.11 ± 0.04 | 16.90 ± 0.07 | 4.11 ± 0.04 | 0.676 ± 0.024 | –23.32 ± 0.12 | –23.75 ± 0.09 | –24.31 ± 0.09 |
| (d) M6 Pl Rb | 14.96 ± 0.08 | 0.97 ± 0.014 | 1.02 ± 0.06 | 16.40 ± 0.07 | 3.53 ± 0.03 | 0.55 ± 0.03 | –23.26 ± 0.14 | –23.92 ± 0.09 | –24.39 ± 0.10 |
| (e) M6 Ps Ds | 15.78 ± 0.08 | 0.44 ± 0.03 | 2.29 ± 0.16 | 16.78 ± 0.07 | 2.77 ± 0.07 | 0.179 ± 0.012 | –21.9 ± 0.3 | –23.74 ± 0.13 | –23.92 ± 0.14 |
| (f) M6 Ps Rs | 15.55 ± 0.08 | 0.35 ± 0.03 | 2.44 ± 0.22 | 16.51 ± 0.07 | 2.48 ± 0.06 | 0.140 ± 0.012 | –21.6 ± 0.4 | –23.77 ± 0.12 | –23.91 ± 0.14 |
|
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| (g) M9 Ps Db | 14.52 ± 0.09 | 0.82 ± 0.05 | 1.5 ± 0.3 | 17.30 ± 0.07 | 5.13 ± 0.18 | 0.77 ± 0.08 | –23.5 ± 0.4 | –23.83 ± 0.14 | –24.44 ± 0.16 |
| (g2) M9 Ps Db TF3 | 14.60 ± 0.09 | 0.83 ± 0.07 | 1.3 ± 0.3 | 17.22 ± 0.07 | 5.00 ± 0.14 | 0.65 ± 0.06 | –23.4 ± 0.4 | –23.85 ± 0.13 | –24.40 ± 0.14 |
| (g3) M9 Ps Db TF4 | 14.75 ± 0.08 | 0.90 ± 0.05 | 1.3 ± 0.3 | 17.35 ± 0.07 | 5.18 ± 0.18 | 0.75 ± 0.08 | –23.4 ± 0.4 | –23.80 ± 0.14 | –24.39 ± 0.16 |
| (h) M9 Ps Rb | 14.52 ± 0.11 | 0.78 ± 0.11 | 1.9 ± 0.8 | 17.07 ± 0.07 | 4.73 ± 0.23 | 0.72 ± 0.18 | –23.5 ± 0.7 | –23.88 ± 0.17 | –24.47 ± 0.21 |
|
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| (i) M18 Ps Db | 14.52 ± 0.11 | 0.81 ± 0.10 | 1.5 ± 0.3 | 17.32 ± 0.07 | 5.13 ± 0.23 | 0.60 ± 0.08 | –23.5 ± 0.5 | –23.81 ± 0.16 | –24.41 ± 0.18 |
| (j) M18 Ps Rb | 14.55 ± 0.09 | 0.79 ± 0.07 | 1.6 ± 0.3 | 17.20 ± 0.07 | 4.95 ± 0.14 | 0.68 ± 0.07 | –23.4 ± 0.4 | –23.86 ± 0.13 | –24.47 ± 0.14 |
| (k) M18 Pl Db | 14.96 ± 0.08 | 0.945 ± 0.015 | 1.05 ± 0.05 | 16.95 ± 0.07 | 4.28 ± 0.07 | 0.60 ± 0.03 | –23.22 ± 0.14 | –23.79 ± 0.10 | –24.30 ± 0.10 |
| (l) M18 Pl Rb | 14.92 ± 0.08 | 0.896 ± 0.014 | 1.06 ± 0.05 | 16.98 ± 0.07 | 4.54 ± 0.06 | 0.51 ± 0.03 | –23.15 ± 0.14 | –23.88 ± 0.10 | –24.33 ± 0.10 |
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Notes.Columns: (1) model code from Table 1; (2) effective surface brightness of the bulge in mag/arcsec2; (3) bulge effective radius in kpc; (4) bulge Sersic index; (5) central surface brightness of the disk in mag/arcsec2; (6) disk scale-length in kpc; (7) bulge-to-disk luminosity ratio in the K band; (8) K-band absolute magnitude of the bulge; (9) K-band absolute magnitude of the disk; (10) K-band total absolute magnitude.
The photometric parameters are provided for the K band. A mass-to-light ratio in the K band equal to M/LK = 1 is assumed to transform surface density profiles in the models to surface brightness profiles (see Sect. 4).
The values listed in this table assume the scaling discussed in Sect. 4, i.e., the original primary galaxy with B/D = 0.5 is scaled to the mass and size of the Milky Way, and the one with B/D = 0.08 is scaled to NGC 253. We have kept these scalings throughout the paper to facilitate the comparison with observational data, but they can be modified by assuming different mass and size units.
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