2017MNRAS.469.3564J

We derive detailed dynamical models for two galaxies, the massive spiral galaxy NGC 5055 and the dwarf irregular DDO 154. We used Navarro, Frenk & White (NFW) and isothermal halo models for the dark matter (DM) distribution, along with the most recent and reliable radio observations of H I to determine the rotation curves of these galaxies. Contributions from the neutral gas and the luminous matter were accounted for. For NGC 5055, the latest stellar population synthesis (SPS) models, combining metallicity and age as indicators of the stellar mass-to-light ratio (M/L) were used to better constrain both the DM model and the contribution to the total mass from all components. The isothermal dark halo model successfully fitted both observed rotation curves with realistic values for stellar M/L, while the NFW model needed further constraints for M/L to fit the rotation curve of DDO 154. In the case of NGC 5055, we found the best-fitting M/L in the 3.6 µm band (M/L_3.6) for stellar disc to be 0.57 ± 0.04 for isothermal, and 0.50 ± 0.05 for NFW DM model. The most probable value for M/L_3.6 from SPS models is 0.46, which is in agreement within uncertainties with our best-fitting NFW model. In the case of DDO 154, we obtained the stellar disc M/L_3.6 of 0.25 ± 0.20 for the isothermal DM model. The stellar disc M/L_3.6 for the NFW model was fixed to 0.26, as best reasonable value. For NGC 5055, we derived radial profiles of stellar M/L for our best estimate for a particular DM model.