Table 2.
Priors used in the rotation curve decomposition.
| Component | Parameter | Prior type | Value range |
|---|---|---|---|
| Stars | log(M*/M⊙) | Uniform log | 9–12 |
| Reff, * (kpc) | Uniform | Reff, dust − Reff, [CII] | |
| n | Uniform | 0.2–10 | |
| Gas | Gas_norm | Uniform | 0–10 |
| Rgas (kpc) | Fixed | R[CII] | |
| DM | log(fbar) | Uniform log | −6 to −0.73 |
| c200 | Fixed | 3.4 |
Notes. The stellar component is assumed to be spherical, with a corresponding projected light distribution described by a Sérsic profile, defined by a stellar mass (M*), an effective radius (Reff, *) and a Sérsic index (n). The gas is described by an exponential disc defined by a disc scale length (Rgas) fixed to the scale length of the [CII] emission and a gas mass (Mgas) that is defined as as the CO luminosity times a gas normalisation (gas_norm). The CDM halo follows an NFW profile with a concentration fixed at 3.4. The CDM halo virial mass is calculated from the baryon fraction which varies between the cosmological baryon fraction and a baryon-dominated halo (see main text for further explanation).
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