All Tables

Table 1: Best-fit parameters derived from RT-modelling of NGC 4013, NGC 5907 and NGC 4565 in the V-band. $\tau _{V}^{f}$ is the visual optical depth when the galaxy is viewed face-on and $\theta$ is the inferred inclination of the object. $h_{\rm d}$ and $z_{\rm d}$ are, respectively, the exponential scalelength and exponential scaleheight of the dust assuming the distance listed in the second column. Distances to NGC 4013, NGC 4565 and NGC 5907 are taken, respectively, from Bottema (1995), Rupen (1991) and van der Kruit & Searle (1982).
Table 2: Global flux densities, as defined in Sect. 5 for NGC 4013, NGC 5907 and NGC 4565. For each galaxy, the flux density $F_{\lambda }$ is given in Jy at wavelength ${\lambda }$ (in microns). The uncertainty in the flux density is $\pm$ 15%.
Table 3: Dust components derived from SED fitting of NGC 4013, NGC 5907 and NGC 4565 in the FIR/submm/mm regime. We decompose the spectrum into 2 components; warm dust of temperature $T^{\rm W}$ and cold dust of temperature $T^{\rm C}$ . The ratio of cold dust mass to warm dust mass is given as $\frac{M^{\rm C}}{M^{\rm W}}$ . An index of 1.5 has been assumed for the wavelength dependency of the emissivity ( $Q\propto \lambda ^{-1.5}$ ).
Table 4: Values for submillimeter and millimeter emissivity, $Q(\lambda )$ , collated from the literature. Estimates are given as $\frac{Q(V)}{Q(\lambda)}$ where the extinction efficiency in the V-band [Q(V)] has been taken, where necessary, to be 1.5 (Whittet 1992). The absorption mass coefficient $\kappa (\lambda )$ is calculated from $Q(\lambda )$ assuming a classical grain radius of $0.1~{\mu}$ m and a material density of $\rho =3 \times 10^{3}~$ kg m^-3. For each measurement the column "Medium'' denotes the type of astrophysical environment where the corresponding grains are believed to be situated.