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The IC5146 cloud is a nearby star-forming region in Cygnus, consisting ofmolecular gas filaments in a variety of evolutionary stages. We used opticaland near-infrared polarization data toward the IC5146 cloud, reported in thefirst paper of this series, to reveal the magnetic fields in this cloud. Usingthe newly released $Gaia$ data, we found that the IC5146 cloud may contain twoseparate clouds: a first cloud, including the densest main filament at adistance of $\sim$600 pc, and a second cloud, associated with the Cocoon Nebulaat a distance of $\sim$800 pc. The spatially averaged H-band polarization maprevealed a well-ordered magnetic field morphology, with the polarizationsegments perpendicular to the main filament but parallel to the nearbysub-filaments, consistent with models assuming that the magnetic field isregulating cloud evolution. We estimated the magnetic field strength using theDavis-Chandrasekhar-Fermi method, and found that the magnetic field strengthscales with volume density with a power-law index of $\sim0.5$ in the densityrange from $N_{H_2}\sim$ 10 to 3000 cm$^{-3}$, which indicates an anisotropiccloud contraction with a preferred direction along the magnetic field. Inaddition, the mass-to-flux ratio of the cloud gradually changes fromsubcritical to supercritical from the cloud envelope to the deep regions. Thesefeatures are consistent with strong magnetic field star-formation models andsuggest that the magnetic field is important in regulating the evolution of theIC5146 cloud.

Multiwavelength Polarimetry of the Filamentary Cloud IC5146: II. Magnetic Field Structures