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Polarized dust emission is a key tracer in the study of interstellar mediumand of star formation. The observed polarization, however, is a product ofmagnetic field structure, dust grain properties and grain alignment efficiency,as well as their variations in the line of sight, making it difficult tointerpret polarization unambiguously. The comparison of polarimetry at multiplewavelengths is a possible way of mitigating this problem. We use data fromHAWC+/SOFIA and from SCUBA-2/POL-2 (from the BISTRO survey) to analyse the NGC2071 molecular cloud at 154, 214 and 850 $\mu$m. The polarization angle changessignificantly with wavelength over part of NGC 2071, suggesting a change inmagnetic field morphology on the line of sight as each wavelength best tracesdifferent dust populations. Other possible explanations are the existence ofmore than one polarization mechanism in the cloud or scattering from very largegrains. The observed change of polarization fraction with wavelength, and the214-to-154 $\mu$m polarization ratio in particular, are difficult to reproducewith current dust models under the assumption of uniform alignment efficiency.We also show that the standard procedure of using monochromatic intensity as aproxy for column density may produce spurious results at HAWC+ wavelengths.Using both long-wavelength (POL-2, 850 $\mu$m) and short-wavelength (HAWC+,$\lesssim 200\, \mu$m) polarimetry is key in obtaining these results. Thisstudy clearly shows the importance of multi-wavelength polarimetry atsubmillimeter bands to understand the dust properties of molecular clouds andthe relationship between magnetic field and star formation.

The JCMT BISTRO Survey: Multi-wavelength polarimetry of bright regions in NGC 2071 in the far-infrared/submillimetre range, with POL-2 and HAWC+