We present the first maps of NGC 3044 and NGC 4157 at \lambda 450 ~ { } \mu m and \lambda 850 ~ { } \mu m from the JCMT as well as the first maps at 617 MHz from the GMRT .
High latitude emission has been detected in both the radio continuum and sub-mm for NGC 3044 and in the radio continuum for NGC 4157 , including several new features .
For NGC 3044 , in addition , we find 617 MHz emission extending to the north of the major axis , beginning at the far ends of the major axis .
One of these low intensity features , more than 10 kpc from the major axis , has apparently associated emission at \lambda 20 cm and may be a result of in-disk activity related to star formation .

The dust spectrum at long wavelengths required fitting with a two-temperature model for both galaxies , implying the presence of cold dust ( T _ { c } = 9.5 K for NGC 3044 and T _ { c } = 15.3 K for NGC 4157 ) .
Dust masses are M _ { d } = 1.6 \times 10 ^ { 8 } ~ { } M _ { \odot } and M _ { d } = 2.1 \times 10 ^ { 7 } ~ { } M _ { \odot } for NGC 3044 and NGC 4157 , respectively , and are dominated by the cold component .

There is a clear correlation between the 617 MHz and \lambda 850 ~ { } \mu m emission in the two galaxies .
In the case of NGC 3044 for which the \lambda 850 ~ { } \mu m data are strongly dominated by cold dust , this implies a relation between the non-thermal synchrotron emission and cold dust .
The 617 MHz component represents an integration of massive star formation over the past 10 ^ { 7 - 8 } yr and the \lambda 850 ~ { } \mu m emission represents heating from the diffuse interstellar radiation field ( ISRF ) .

The 617 MHz – \lambda 850 ~ { } \mu m correlation improves when a smoothing kernel is applied to the \lambda 850 ~ { } \mu m data to account for differences between the CR electron diffusion scale and the mean free path of an ISRF photon to dust .
The best-fit relation is L _ { 617 _ { MHz } } \propto { L _ { 850 ~ { } \mu { m } } } ^ { 2.1 \pm 0.2 } for NGC 3044 .
If variations in the cold dust emissivity are dominated by variations in dust density , and the synchrotron emission depends on magnetic field strength ( a function of gas density ) as well as CR electron generation ( a function of massive star formation rate and therefore density via the Schmidt law ) then the expected correlation for NGC 3044 is L _ { 617 _ { MHz } } \propto { L _ { 850 ~ { } \mu { m } } } ^ { 2.2 } , in agreement with the observed correlation .