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Interstellar filaments  Circumbinary disk  Galaxy formation  Molecular outflows  Star-forming region  OPIATE interface 

Interstellar filaments

(MHD simulation provided by Robi Banerjee and modified for demonstrative purposes)

Left panel: The image shows the logarithmically scaled flux map of a filamentary density structure resulting from a MHD simulation. The dust temperature was post-processed to account for five stars embedded in the filament. Right panel: Image of a linear polarization map for the filamentary structure. The degree of polarization is calculated with the radiative torque alignment mechanism considering the radiation of the embedded stars. An additional background polarization of a distant star field was considered. top

Circumbinary disk

(MHD simulation provided by Mario Flock)

Thermal emission at 850 μm of aligned non-spherical dust grains (left panel) of a circumbinary disk and the corresponding linearly polarized intensity (right panel) projected as a healpix all-sky map. (download video)

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Galaxy formation

(MHD galaxy evolution simulation provided by Philip Mocz and modified for demonstrative purposes)

Multi-color (red = 370μm, green = 500μm, blue = 870μm) dust emission image (top outer left) of a newly formed galaxy. Corresponding linear (top center left) and circular polarization (top center right) taking RAT dust grain alignment into account. Velocity maps derived from CO emission for an outside observer (top outer right) and a co-rotating observer within the disk (bottom center). (download video)

Extragalactic (squared images) and all-sky observation (elliptic maps) of synchrotron emission (top left) at a wavelength of 6.2 cm, linear polarization (top right), circular polarization (bottom right), and Faraday rotation measure (bottom left). (download video)

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Star-forming region

(MHD simulation provided by Daniel Seifried)

Multi-color (red = 7.2μm, green = 15.2μm, blue = 29.9μm) intensity image (outer left) of a star-forming region with 66 newly born stars. Corresponding linear (middle left) and circular polarization (middle right) taking RATs as dust grain alignment into account. Projected line of sight magnetic field considering SO emission and Zeeman effect. (download video)

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Molecular outflows

(MHD simulation by Daniel Seifried)

Intensity maps (at λ = 1.3 mm) overlaid with vectors of linear polarization considering RAT alignment for different inclination angles i and maximum dust grain sizes amax (see Reissl et al. 2016 for details). top

OPIATE interface

(MHD simulation by Thomas Peters, OPIATE database and image by Eric Pellegrini)

Multi-color (red = O I, green = O II, blue = OIII) intensity image of oxygen line emission.

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