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.