The radiative transfer code POLARIS R. Brauer, S. Reissl, E. - - PowerPoint PPT Presentation

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The radiative transfer code POLARIS R. Brauer, S. Reissl, E. - - PowerPoint PPT Presentation

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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

slide-1
SLIDE 1

The radiative transfer code POLARIS

  • R. Brauer, S. Reissl,
  • E. Pantin, and E. Habart

October 30, 2018

Cosmic Dust and Magnetism 2018

slide-2
SLIDE 2

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

slide-3
SLIDE 3

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 (λ = 1.29 mm; Maury et al. 2018) 1

slide-4
SLIDE 4

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 (λ = 0.87 mm; Ohashi et al. 2018) 1

slide-5
SLIDE 5

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

slide-6
SLIDE 6

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

slide-7
SLIDE 7

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

slide-8
SLIDE 8

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

slide-9
SLIDE 9

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

slide-10
SLIDE 10

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

slide-11
SLIDE 11

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

slide-12
SLIDE 12

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

slide-13
SLIDE 13

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

slide-14
SLIDE 14

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

slide-15
SLIDE 15

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

slide-16
SLIDE 16

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.)

−2000 2000

∆x [AU]

−2000 −1000 1000 2000

∆y [AU]

10−1 100 101

B [mG]

Magnetic fjeld strength MHD simulation of a Bok globule by Bastian Körtgen 3

slide-17
SLIDE 17

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.)

−2000 2000

∆x [AU]

−2000 −1000 1000 2000

∆y [AU]

25 %

5 10 15 20 25 30 35

Pl [%]

Synthetic polarized emission map MHD simulation of a Bok globule by Bastian Körtgen 3

slide-18
SLIDE 18

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.)

−2000 2000

∆x [AU]

−2000 −1000 1000 2000

∆y [AU]

−6 −4 −2 2 4 6

BLOS [mG]

Synthetic LOS magnetic fjeld strength map MHD simulation of a Bok globule by Bastian Körtgen 3

slide-19
SLIDE 19

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

slide-20
SLIDE 20

Grid types

– Cartesian (OcTree) – Spherical – Cylindrical – Voronoi

Grid quantities

– Hydrogen densities – Dust densities – Gas temperatures – Dust temperatures – Velocity fjeld – 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) – Zeeman properties

Calculation modes

– Dust temperature distribution (including stochastic heating) – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) – 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) – All-sky-maps (full Stokes) – Magnetic fjeld maps (Zeeman) – Optical depth and column density maps – 2D cuts through the grid

PolarisTools (optional)

– Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Plot POLARIS results

slide-21
SLIDE 21

Grid types

– Cartesian (OcTree) – Spherical – Cylindrical – Voronoi

Grid quantities

– Hydrogen densities – Dust densities – Gas temperatures – Dust temperatures – Velocity fjeld – 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) – Zeeman properties

Calculation modes

– Dust temperature distribution (including stochastic heating) – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) – 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) – All-sky-maps (full Stokes) – Magnetic fjeld maps (Zeeman) – Optical depth and column density maps – 2D cuts through the grid

PolarisTools (optional)

– Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Plot POLARIS results

slide-22
SLIDE 22

Grid types

– Cartesian (OcTree) – Spherical – Cylindrical – Voronoi

Grid quantities

– Hydrogen densities – Dust densities – Gas temperatures – Dust temperatures – Velocity fjeld – Magnetic fjeld strength – Dust and gas properties

Additional data

– Emission sources (stars, ISRF, …) – Detector parameter (direction, λ, …) – Dust properties (silicate, carbon, Themis, …) – Gas properties (LAMBDA, JPL, CDMS) – Zeeman properties

Calculation modes

– Dust temperature distribution (including stochastic heating) – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) – 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) – All-sky-maps (full Stokes) – Magnetic fjeld maps (Zeeman) – Optical depth and column density maps – 2D cuts through the grid

PolarisTools (optional)

– Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Plot POLARIS results

slide-23
SLIDE 23

Grid types

– Cartesian (OcTree) – Spherical – Cylindrical – Voronoi

Grid quantities

– Hydrogen densities – Dust densities – Gas temperatures – Dust temperatures – Velocity fjeld – Magnetic fjeld strength – Dust and gas properties

Additional data

– Emission sources (stars, ISRF, …) – Detector parameter (direction, λ, …) – Dust properties (silicate, carbon, Themis, …) – Gas properties (LAMBDA, JPL, CDMS) – Zeeman properties

Calculation modes

– Dust temperature distribution (including stochastic heating) – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) – 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) – All-sky-maps (full Stokes) – Magnetic fjeld maps (Zeeman) – Optical depth and column density maps – 2D cuts through the grid

PolarisTools (optional)

– Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Plot POLARIS results

slide-24
SLIDE 24

Grid types

– Cartesian (OcTree) – Spherical – Cylindrical – Voronoi

Grid quantities

– Hydrogen densities – Dust densities – Gas temperatures – Dust temperatures – Velocity fjeld – Magnetic fjeld strength – Dust and gas properties

Additional data

– Emission sources (stars, ISRF, …) – Detector parameter (direction, λ, …) – Dust properties (silicate, carbon, Themis, …) – Gas properties (LAMBDA, JPL, CDMS) – Zeeman properties

Calculation modes

– Dust temperature distribution (including stochastic heating) – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) – 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) – All-sky-maps (full Stokes) – Magnetic fjeld maps (Zeeman) – Optical depth and column density maps – 2D cuts through the grid

PolarisTools (optional)

– Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Plot POLARIS results

slide-25
SLIDE 25

Grid types

– Cartesian (OcTree) – Spherical – Cylindrical – Voronoi

Grid quantities

– Hydrogen densities – Dust densities – Gas temperatures – Dust temperatures – Velocity fjeld – Magnetic fjeld strength – Dust and gas properties

Additional data

– Emission sources (stars, ISRF, …) – Detector parameter (direction, λ, …) – Dust properties (silicate, carbon, Themis, …) – Gas properties (LAMBDA, JPL, CDMS) – Zeeman properties

Calculation modes

– Dust temperature distribution (including stochastic heating) – Stellar or dust emission scattered at spherical dust grains (including ray-tracing approach) – 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) – All-sky-maps (full Stokes) – Magnetic fjeld maps (Zeeman) – Optical depth and column density maps – 2D cuts through the grid

PolarisTools (optional)

– Create dust/gas catalogs – Create POLARIS grids – Run POLARIS simulations – Plot POLARIS results

slide-26
SLIDE 26

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-27
SLIDE 27

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-28
SLIDE 28

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-29
SLIDE 29

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-30
SLIDE 30

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-31
SLIDE 31

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-32
SLIDE 32

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-33
SLIDE 33

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

Comprehensive analysis of the magnetic fjeld

5

slide-34
SLIDE 34

Conclusions

Investigate magnetic fjelds

  • Different observational techniques
  • Diverse objects from small to large scales
  • Many ambiguities and uncertainties

The radiative transfer code POLARIS

  • Simulates many observable quantities
  • Considers outcome of MHD simulations
  • Combines techniques of various fjelds

⇒ Comprehensive analysis of the magnetic fjeld

5

slide-35
SLIDE 35

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-36
SLIDE 36

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-37
SLIDE 37

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-38
SLIDE 38

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-39
SLIDE 39

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-40
SLIDE 40

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-41
SLIDE 41

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-42
SLIDE 42

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-43
SLIDE 43

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6

slide-44
SLIDE 44

Conclusions

First public release

  • Open source release (Linux and Mac)
  • New extensive manual and quickstart guides
  • Constant updates and bug fjxes

Homepage Upcoming features

  • Scattering at non-spherical dust grains
  • Emission from Spinning Dust Grains
  • Alignment to the radiation fjeld
  • Goldreich-Kylafjs effect

Thank you for your attention

6