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Lyman Alpha Radiative Transfer& Polarimetric Modeling
for LABd05
Seok-Jun ChangSejong University
Contents
1. Introduction
2.Lyα Radiative Transfer
3.LABd05 (Yang et al. 2014)
4.Polarimetric Modeling
5.Summary & Future Work
Lyman Alpha Blobs
Polarization of LAB
Polarization of LAB
You et al 2017 Kim et al in prep
Lyman Alpha Radiative Transfer
Lyman Alpha Radiative Transfer
H
,ො, , ,
= +Incident Photon
Lyman Alpha Radiative Transfer
H
,ො, , ,
= +Incident Photon
Grid-Based Radiative Transfer
=
= 1 + 2 + 3 + 4 + 5
=
==
=
Lyman Alpha Radiative Transfer
H
,ො, , ,
= +Incident Photon
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen Total Cross Section near Lya(Chang et al. 2017)
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen Total Cross Section near Lya(Chang et al. 2017)
Resonance Scattering(Core Scattering)
Rayleigh Scattering(Wing Scattering)
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen Total Cross Section near Lya
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen Resonance Line(Neufeld 1990)
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen
Resonance Scattering(Core Scattering)
Rayleigh Scattering(Wing Scattering)
Lyman Alpha Radiative Transfer
2s
1s
2p
Energy Level of Atomic Hydrogen
Resonance Scattering(Core Scattering)
Rayleigh Scattering(Wing Scattering)
2p1/2
2p3/2
Resonance Scattering(Core Scattering)
Rayleigh Scattering(Wing Scattering)
H H
ො, ො,
Resonance Scattering(Core Scattering)
Rayleigh Scattering(Wing Scattering)
HH
cos =3
8(1 + cos )
cos = ො ∙ ොcos ~
~
~
>>
~0Strongly Polarized
Weakly Polarized :1𝑠 2 3/2
Un-Polarized : 1𝑠 2 1/2
Polarization Direction
,ො , , ,
Polarization Direction
Polarization Direction
Code Check – Circular Pattern
Code Check – Circular Pattern
Code Check – Chandrasekhar 1960
Code Check – Chandrasekhar 1960
Code Check – Dijkstra & Leob 2008
1920
LABd05
1. Galaxies and AGN in this region show spatial offset from the Lya peak.
(Dey et al 2005, Yang et al 2014)
2. CO and dust are concentrated on Galaxy 36.
3. Galaxy 36 is obscured AGN.
~ .~
LABd05
~ .~
1. Galaxies and AGN in this region show spatial offset from the Lya peak.
(Dey et al 2005, Yang et al 2014)
2. CO and dust are concentrated on Galaxy 36.
3. Galaxy 36 is obscured AGN.
LABd05
~ .~
1. Galaxies and AGN in this region show spatial offset from the Lya peak.
(Dey et al 2005, Yang et al 2014)
2. CO and dust are concentrated on Galaxy 36.
3. Galaxy 36 is obscured AGN.
2D-Spectrum of LABd05
= 295 /
1. The profiles of Lya and CO is symmetric.
2. The peaks of Lya and UV show offset.
2D-Spectrum of LABd05
1. The peaks of Lya and He II show small offset.
2. The profile of Lya show red asymmetry.
Polarimetric Modeling
Polarimetric Modeling
Neutral Region
Fully-ionized
AGN
= 0
2𝑠
0 2
C overing F actor=1
4
= 0
0 = 100 km/s
Grid : (300,300,300)
= 1020cm 2
Polarimetric Modeling : Model 1
= .
= .
= .
Polarimetric Modeling : Model 1
= .
= .
= .Region 1
Region 2
Region 3
Polarimetric Modeling : Model 1
= 0.1 = 0.1 = 0.1
Polarimetric Modeling : Model 1
Polarimetric Modeling : Model 2
= .
= .
= .
Polarimetric Modeling : Model 2
= .
= .
= . Region 1
Region 2
Region 3
Polarimetric Modeling : Model 2
= 0.1 = 0.1 = 0.1
Polarimetric Modeling : Model 2
Comparison with Observation and Simulation
Model 1
Model 2
Comparison with Observation and Simulation
Model 1
Model 2
Summary & Future Work
1. Our Lyα RT code provide (I,Q,U)[x,y,λ] datacube.
2. The polarization by Rayleigh scattering is stronger than resonance scattering.
3. We consider more accurate and various model to analyze LABd05.
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