We present far-infrared and submillimeter images of five bright visual reflection nebulae, IC 446, NGC 2247, NGC 2245, NGC 7023, and CED 201 at wavelengths of 100, 160, and 200 or 370-mu-m obtained with cameras designed for NASA's Kuiper Airborne Observatory and the Infrared Telescope Facility. We supplement our results at wavelengths of 12, 25, 60, and 100-mu-m with data from the Infrared Astronomical Satellite. We use our images and composite infrared spectra to derive parameters such as the fraction of nebular emission attributed to molecule-sized grains, the range of nebular grain albedos, gas densities, and gas cloud geometries consistent with near-infrared-to-submillimeter observations, and the relative extinction efficiency Q(ext)(UV)/Q(em)(FIR) and the resultant mass-extinction coefficient chi-ext(FIR) consistent with observed equilibrium grain temperatures and inferred ambient radiative energy densities. We compare our observations with models of nebular far-infrared emission assuming large grains heated by photospheres characteristic of the central exciting stars. Our results show that 30%-45% of the nebular emission lies at wavelengths of lambda < 30-mu-m (emission attributed to an abundance of molecule-sized grains). Among our nebulae, the variation in infrared luminosity may be related to variations in nebular gas density and less than optimal gas cloud geometries rather than to anomalous grain albedos. For stellar photospheres with effective wavelengths of lambda-mean almost-equal-to 0.25-0.5-mu-m, we infer from our observations relative extinction efficiencies of Q(ext)(UV)/Q(em)(250-mu-m) almost-equal-to 1000-5000. Accounting for the extinction of molecule-sized grains, the resultant mass-extinction coefficient is chi-ext(250-mu-m) almost-equal-to 10-50 cm2 g-1. In comparison, models of nebular grain emission require Q(ext)(UV)/Q(em)(250-mu-m) almost-equal-to 8000(0.5-mu-m/lambda-mean) and chi-ext(250-mu-m) almost-equal-to 5-6 cm2 g-1. Radiative transfer models illustrate the variation in far-infrared surface brightness with nebular gas density and the apparent reduction in far-infrared optical depth associated with line-of-sight gradients in nebular radiative energy density.
