Notes. In Col. 1 the upper radius of the dark dust agglomerates is specified, in Col. 2 the goodness χ² of the best-fit model, and below the number N of models that are consistent with the observational constraints and fit the reddening and Serkowski curve at χ² < 1. Corresponding parameters of the specific mass in percent per gram dust (Cols. 3–8) of dark dust as lower limit m_Dark, and for large silicates m_Si, nano-sized silicates m_vSi, large amorphous carbon m_aC, very small graphite m_VSG, and PAHs m_PAH. Below, in the second row of Cols. 4–8, exemplified dust abundances [X]/[H] (ppm) are given by adopting [Si]/[H] = 15 ppm in large silicates. Column 9 gives the exponent of the dust size distribution q. The upper radius of large silicates (Col. 10) and amorphous carbon (Col. 11), their lower alignment radii and (Cols. 12 and 13), respectively, and the alignment efficiency (Col. 14) of large silicates δ₀(Si) is given. Derived quantities of the dust models are given for the dust abundance ratio [C]/[Si] (Col. 15), the gas-to-dust mass ratio M_gas/M_dust (Col. 16), the total-to-selective extinction R_V (Eq. (5), Col. 17), and the optical depth (Col. 18) that matches the optical-to-submm polarisation ratio of p_850µm/(p_V/τ_V) = 4.31 (Eq. (8)) by Planck Collaboration XII (2020). (†) The model violates the abundance constraint (Eq. (1)). (‡) Models without dark dust do not fit the Planck Collaboration XXI (2015); Planck Collaboration XII (2020) data at ≳0.8 mm.