Polarisation in Filaments with SPICA



Understanding of the star-formation process in the ISM is vital to the study of evolution of galaxies. Yet a number of issues remain to be answered, among which the onset trigger is crucial for our understanding of subsequent star-formation processes. Magnetic fields and turbulence have energy densities similar to those of thermal processes and radiation in the ISM (Draine 2010) and they must be important agents in the formation of structure in the ISM (Lesaffre et al. 2013).

Herschel and Planck findings lead to a “filamentary paradigm” for star-formation, in which both magnetic field and turbulence dissipation play critical roles in the onset of star-formation, as materials accrete to form filaments along magnetic force lines and dissipate their energy via radiative shocks to form first hydrostatic cores, followed by the class 0 stage of the proto-stellar phase. SPICA will obtain the necessary high spatial resolution polarimetry observations and refresh our view of star-formation, raising our understanding to a new level, by virtue of its efficient polarimetry in the FIR and its highly sensitive spectroscopy from MIR to FIR

Polarisation within Filaments

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