A Primer on Far‐Infrared Polarimetry

By R. Hildebrand, J. Davidson, J. Dotson, C. Dowell, G. Novak, J. Vaillancourt. 2000

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Dust Dynamics in Compressible Magnetohydrodynamic Turbulence (2004, background): “Italso enablesm olecularhydrogen form ation and tracesthem agnetic eld via em ission and extinction polarization (see reviews by Hildebrand et al. 2000,Lazarian 2000,2002).”
Detection of polarization in the cosmic microwave background using DASI (2002, background): “Diffuse thermal dust emission may be polarized by several per cent (see for example ref”
Radiative torque alignment: essential physical processes (2007, background): “Polarization from absorption and emission by aligned grains is widely believed to trace magnetic field topology (see Hildebrand et al. 2000, Hildebrand 2002; Aitken et al. 2002; Hough et al. 1989).”
Studies of Regular and Random Magnetic Fields in the ISM: Statistics of Polarization Vectors and the Chandrasekhar-Fermi Technique (2008, methodology): “One of the most readily available methods of studying the perpendicular component of the magnetic field is based on the polarization of dust thermal emissions at infrared and submillimeter wavelengths (Hildebrand et al. 2000).”
Statistical Properties of Galactic Starlight Polarization (2001, methodology): “(Hildebrand et al. 1999 ; Novak et al. 2000 ; see also Hildebrand et al. 2000 ; Heitsch et al. 2001 for recent reviews) but they reÑect only rather local distortions of the large-scale magnetic Ðeld.”