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Observations
Observations
We use existing and new observational (polarization) data from world-class observatories, such as SOFIA/HAWC+, JCMT, ALMA, NOEMA, and incoming SKA, covering multi-wavelengths (UV/optical to FIR/submm/cm) and multi-scales from the diffuse Galactic scales, to Molecular Clouds, Filaments to Protostellar Cores and Disks, and the Galactic Center around Supermassive Black Hole Sgr A*.
Atacama Large Millimeter/submillimeter Array (ALMA)
James Clerk Maxwell Telescope (JCMT)
Stratospheric Observatory for Infrared Astronomy (SOFIA)
Square Kilometer Array (SKA)
numerical Modeling and Synthetic Observations
numerical Modeling and Synthetic Observations
DustPOL-py is a simple code used to model the polarization of starlight and thermal dust emission induced by aligned dust grains based on the Radiative Torque Paradigm. The DustPOL-py code predicts the polarization degree for the optimal situation where the magnetic fields lie in the plane of the sky. A stable version of Dustpol-py is available here.
POLArized RadIation Simulator (POLARIS) is the Monte-Carlo radiative transfer code used to model polarized thermal dust emission from aligned dust grains by radiative torques (RAT) for an analytical model or an MHD simulation model of astrophysical objects. The code is developed by Stefan Reissl from Heidelberg University.
Our group has been updating the original POLARIS by including new dust physical effects developed recently, including Magnetically enhanced radiative torque (MRAT) and Radiative Torque Disruption (RATD) effects. The updated POLARIS is especially important for physical modeling of dust polarization from dense star-forming regions or intense radiation fields, such as protostellar environments, massive star-forming regions, and dusty tori around active galactic nuclei. A stable version of updated POLARIS is available here.
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