The radiative transfer code POLARIS R. Brauer, S. Reissl, E. Pantin, and E. Habart October 30, 2018 Cosmic Dust and Magnetism 2018
Motivation Study magnetic fjelds in astrophysical environments • Observe polarized dust continuum emission • Observe Zeeman split spectral lines • Observe synchrotron radiation and Faraday rotation Polarized emission of the Bok globule B335 ( 1 29 mm ; Maury et al. 2018) 1
Motivation Study magnetic fjelds in astrophysical environments • Observe polarized dust continuum emission • Observe Zeeman split spectral lines • Observe synchrotron radiation and Faraday rotation Polarized emission of the Bok globule B335 1 ( λ = 1 . 29 mm ; Maury et al. 2018)
Motivation Study magnetic fjelds in astrophysical environments • Observe polarized dust continuum emission • Observe Zeeman split spectral lines • Observe synchrotron radiation and Faraday rotation Polarized emission of the disk around HD142527 1 ( λ = 0 . 87 mm ; Ohashi et al. 2018)
Motivation Study magnetic fjelds in astrophysical environments • Observe polarized dust continuum emission • Observe Zeeman split spectral lines • Observe synchrotron radiation and Faraday rotation CN Zeeman Stokes I and V profjles toward DR21 ( left , Crutcher et al. 1999) CARMA map of velocity-integrated CN ( right , Crutcher et al. 2012) 1
Motivation Study magnetic fjelds in astrophysical environments • Observe polarized dust continuum emission • Observe Zeeman split spectral lines • Observe synchrotron radiation and Faraday rotation Reconstruction of the Galactic Faraday depth (Oppermann et al. 2012) 1
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations The radiative transfer code POLARIS 2
Motivation Radiative transfer simulations • Provide predictions for observations • Required sensitivity and resolution (spectral, spatial) • Observability of particular regions and features • Derive constraints from existing observations Investigate magnetic fjelds • Observable quantities that are infmuenced by magnetic fjelds • Consider the outcome from MHD simulations 2 ⇒ The radiative transfer code POLARIS
Concept of POLARIS Combine radiative transfer with magnetic fjelds MHD simulation of a Bok globule by Bastian Körtgen Magnetic fjeld strength 3 • Polarized dust emission (Reissl et al. 2016) • Zeeman split spectral lines (Brauer et al. 2017) • Synchrotron radiation / Faraday rotation (Reissl et al. in prep.) 10 1 2000 1000 ∆ y [ AU ] B [ mG ] 10 0 0 − 1000 − 2000 10 − 1 − 2000 0 2000 ∆ x [ AU ]
Concept of POLARIS Combine radiative transfer with magnetic fjelds MHD simulation of a Bok globule by Bastian Körtgen Synthetic polarized emission map 3 • Polarized dust emission (Reissl et al. 2016) • Zeeman split spectral lines (Brauer et al. 2017) • Synchrotron radiation / Faraday rotation (Reissl et al. in prep.) 2000 35 30 1000 25 ∆ y [ AU ] P l [ % ] 20 0 15 − 1000 10 25 % 5 − 2000 − 2000 0 2000 ∆ x [ AU ]
Concept of POLARIS Combine radiative transfer with magnetic fjelds MHD simulation of a Bok globule by Bastian Körtgen Synthetic LOS magnetic fjeld strength map 3 • Polarized dust emission (Reissl et al. 2016) • Zeeman split spectral lines (Brauer et al. 2017) • Synchrotron radiation / Faraday rotation (Reissl et al. in prep.) 6 2000 4 1000 2 B LOS [ mG ] ∆ y [ AU ] 0 0 − 2 − 1000 − 4 − 2000 − 6 − 2000 0 2000 ∆ x [ AU ]
Concept of POLARIS Combine radiative transfer with magnetic fjelds • Polarized dust emission (Reissl et al. 2016) • Zeeman split spectral lines (Brauer et al. 2017) • Synchrotron radiation / Faraday rotation (Reissl et al. in prep.) Synthetic all sky Faraday RM map 3
Grid types – All-sky-maps (full Stokes) – Thermal emission of dust grains (including dust grain alignment, ray-tracing customization) – Spectral line emission (including Zeeman splitting and N-LTE level populations) – Synchrotron radiation Visualizations – Emission maps (full Stokes) – Line profjles, SEDs (full Stokes) – Magnetic fjeld maps (Zeeman) – Dust temperature distribution (including stochastic heating) – Optical depth and column density maps – 2D cuts through the grid PolarisTools (optional) – Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) Calculation modes – Cartesian (OcTree) – Dust temperatures – Spherical – Cylindrical – Voronoi Grid quantities – Hydrogen densities – Dust densities – Gas temperatures – Velocity fjeld – Zeeman properties – Magnetic fjeld strength – Dust and gas properties Additional data – Emission sources (stars, ISRF, …) – Detector parameter (direction, , …) – Dust properties (silicate, carbon, Themis, …) – Gas properties (LAMBDA, JPL, CDMS) – Plot POLARIS results
Grid types – All-sky-maps (full Stokes) – Thermal emission of dust grains (including dust grain alignment, ray-tracing customization) – Spectral line emission (including Zeeman splitting and N-LTE level populations) – Synchrotron radiation Visualizations – Emission maps (full Stokes) – Line profjles, SEDs (full Stokes) – Magnetic fjeld maps (Zeeman) – Dust temperature distribution (including stochastic heating) – Optical depth and column density maps – 2D cuts through the grid PolarisTools (optional) – Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) Calculation modes – Cartesian (OcTree) – Dust temperatures – Spherical – Cylindrical – Voronoi Grid quantities – Hydrogen densities – Dust densities – Gas temperatures – Velocity fjeld – Zeeman properties – Magnetic fjeld strength – Dust and gas properties Additional data – Emission sources (stars, ISRF, …) – Detector parameter (direction, , …) – Dust properties (silicate, carbon, Themis, …) – Gas properties (LAMBDA, JPL, CDMS) – Plot POLARIS results
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