Table 1.
Parameters of the MGE decompositions of the surface brightness maps of NGC 1277 and NGC 1278.
| log I0 (log (L⊙ pc−2)) | σ⋆ (arcsec) |
 |
|---|---|---|
| NGC 1277 (F625W) | ||
| 5.119 | 0.019 | 0.700 |
| 4.618 | 0.114 | 0.700 |
| 4.282 | 0.297 | 0.700 |
| 3.771 | 0.724 | 0.700 |
| 3.693 | 0.732 | 0.435 |
| 3.517 | 1.227 | 0.700 |
| 2.913 | 2.085 | 0.700 |
| 2.987 | 2.836 | 0.413 |
| 2.700 | 5.043 | 0.400 |
| 2.345 | 6.887 | 0.502 |
| 1.767 | 9.974 | 0.400 |
| 1.219 | 14.197 | 0.400 |
| 1.631 | 14.197 | 0.700 |
| NGC 1278 (F850LP) | ||
| 4.658 | 0.025 | 1.000 |
| 4.184 | 0.173 | 1.000 |
| 3.681 | 0.479 | 1.000 |
| 3.748 | 0.797 | 0.834 |
| 3.378 | 1.659 | 0.786 |
| 3.053 | 2.757 | 0.857 |
| 2.740 | 3.391 | 0.750 |
| 2.673 | 5.727 | 0.750 |
| 2.403 | 8.461 | 0.952 |
| 2.456 | 9.875 | 0.750 |
| 1.331 | 22.483 | 0.750 |
| 2.034 | 22.483 | 1.000 |
Notes. I0 stands for the central surface brightnesses of the projected Gaussian components, σ⋆ denotes their dispersion, and 
their projected axial ratio. An approximate conversion between the F850LP and F625W surface brightnesses can be obtained by dividing the NGC 1278 I0 values by 1.7 (corresponding to r − z = 0.74, and accounting for the different brightness of the Sun in the two bands). The images were corrected for cosmological dimming before producing the MGE decomposition.
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