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We present the analysis of the magnetic field ($B$-field) structure ofgalaxies measured with far-infrared (FIR) and radio (3 and 6 cm) polarimetricobservations. We use the first data release of the Survey on extragALacticmagnetiSm with SOFIA (SALSA) of 14 nearby ($<20$ Mpc) galaxies with resolved (5arcsec-18 arcsec; $90$ pc--$1$ kpc) imaging polarimetric observations usingHAWC+/SOFIA from $53$ to $214$ \um. We compute the magnetic pitch angle($\Psi_{B}$) profiles as a function of the galactrocentric radius. We introducea new magnetic alignment parameter ($\zeta$) to estimate thedisordered-to-ordered $B$-field ratio in spiral $B$-fields. We find FIR andradio wavelengths to not generally trace the same $B$-field morphology ingalaxies. The $\Psi_{B}$ profiles tend to be more ordered with galactocentricradius in radio ($\zeta_{\rm{6cm}} = 0.93\pm0.03$) than in FIR($\zeta_{\rm{154\mu m}} = 0.84\pm0.14$). For spiral galaxies, FIR $B$-fieldsare $2-75$\% more turbulent than the radio $B$-fields. For starburst galaxies,we find that FIR polarization is a better tracer of the $B$-fields along thegalactic outflows than radio polarization. Our results suggest that the$B$-fields associated with dense, dusty, turbulent star-forming regions, thosetraced at FIR, are less ordered than warmer, less-dense regions, those tracedat radio, of the interstellar medium. The FIR $B$-fields seem to be moresensitive to the activity of the star-forming regions and the morphology of themolecular clouds within a vertical height of few hundred pc in the disk ofspiral galaxies than the radio $B$-fields.

Extragalactic magnetism with SOFIA (SALSA Legacy Program) -- V: First results on the magnetic field orientation of galaxies