Table 2
Definition of the four radial regions studied in this analysis.
| Regions | General | Selene | Oceanus | |||
| Lower limit | Upper limit | Lower limit | Upper limit | Lower limit | Upper limit | |
| [kpc] | [kpc] | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
|
|
||||||
| 1 | 0.0 | hin | 0.00 | 5.67 | 0.0 | 8.07 |
| 2 | R7/2 – hin/2 | R7/2 + hin/2 | 5.67 | 8.59 | 8.07 | 11.09 |
| 3 | R7 – hin/2 | R7 + hin/2 | 8.67 | 14.34 | 11.09 | 18.14 |
| 4 | R7 + 0.75 × hin | R7 + 3.5× hin | 15.75 | 31.35 | 20.15 | 42.35 |
Notes. The table includes (1) number of the region; (2) general definition of the lower limit in units of inner disc scale length (hin, 5.67 and 8.07 kpc for Selene and Oceanus) and the radius corresponding to a stellar mass surface density of 107 M⊙kpc-2 (R7, 11.5 and 14.1 kpc for Selene and Oceanus); (3) general definition of the upper limit in units of hin and R7; (4) lower limit for Selene (kpc); (5) upper limit for Selene (kpc); (6) lower limit for Oceanus (kpc); (7) upper limit for Oceanus (kpc). The value hin was obtained analysing the SDSS r-band mock images from SUNRISE (Jonsson 2006); those images can be seen in Few et al. (2012). The values of hin for all the simulated discs can be found in Table A.1 summarising the results from our surface brightness analysis. Several of the values in Cols. (4)−(7) coincide as a consequence of applying the general definition avoiding overlapping between regions.
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