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Observations
Observations
We use existing and new observational (polarization) data from world-class observatories, such as SOFIA/HAWC+, JCMT, ALMA, and NOEMA, covering multi-wavelengths (UV/optical to FIR/submm) and multi-scales from the diffuse ISM to Molecular Clouds, Filaments, Dense Cores 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
Square Kilometer Array
Modeling and Synthetic Observations
Modeling and Synthetic Observations
Dustpol-py code
Dustpol-py code
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.
POLARIS code
POLARIS code
POLArized RadIation Simulator (POLARIS) is the Monte-Carlor radiative transfer code used to model polarized thermal dust emission from aligned dust grains by radiative torques (RAT) for an analytical model or a 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. The updated POLARIS is especially important for physical modeling of dust polarization from dense star-forming regions or intense radiatio 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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