Table 2.
Overview of the different stellar populations and dust components in our model.
| Component | 2D geometry | Vertical dimension | SED template | Normalisation |
|---|---|---|---|---|
| Bulge | ||||
| Old SP (8 Gyr) | Sérsic profile geometry (a) | Bruzual & Charlot (2003) | 3.6 μm | |
| Disc | Exponential profile | |||
| Old SP (8 Gyr) | IRAC 3.6 μm (b) | (hdisc, z) (f) | Bruzual & Charlot (2003) | 3.6 μm |
| Young non-ionising SP (100 Myr) | GALEX FUV (c) | hyni, z = 1/2 × hdisc, z | Bruzual & Charlot (2003) | FUV |
| Young ionising SP (10 Myr) | Hα + 0.031 × MIPS 24 μm (d) | hyi, z = 1/4 × hdisc, z | MAPPINGS III (g) | FUV |
| Dust | FUV attenuation map (e) | hdust, z = 1/2 × hdisc, z | THEMIS dust mix (h) | Total dust mass |
Notes.
The parameters of the flattened Sérsic profile, like the effective radius Re, Sérsic index n, and intrinsic flattening factor q, were retrieved from the S4G database (Sheth et al. 2010; Salo et al. 2015).
Image corrected for old SP emission and dust attenuation (Cortese et al. 2008; Galametz et al. 2013), using images from IRAC 3.6 μm, SDSS r, MIPS 24 μm, and PACS 70-, 100-, 160 μm.
Image corrected for old SP emission. The map was constructed based on the prescription of Calzetti et al. (2007).
The dust map was constructed based on the prescriptions of Cortese et al. (2008) and Galametz et al. (2013). We used images from GALEX FUV, SDDS r, MIPS 24 μm, and PACS 70-, 100-, 160 μm.
We assumed an exponential distribution with a scale height hz in the vertical direction. The scale height for the old SP is, hdisc, z = 1/8.26 × hR (De Geyter et al. 2014), where hR is the scale length.
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