Development of Monte Carlo Based X-RayClumpy Torus Model and Its Applications toNearby Obscured Active Galactic Nuclei

2020/03/02
Atsushi Tanimoto (Kyoto University)
Y. Ueda, H. Odaka, T. Kawaguchi, & Y. Fukazawa

Table of Contents
Chapter 1: Active Galactic Nucleus(Tanimoto+16, Tanimoto+18)

Chapter 2: X-Ray Observatories

Chapter 3: X-Ray Spectral Model from Clumpy Torus(XClumpy : Tanimoto+19)

Chapter 4: Application of XClumpy to 10 Obscured AGNs
(Tanimoto+20, submitted to the ApJ)

Active Galactic Nucleus (AGN)©NASAAGN: Mass accretion onto Supermassive Black Hole (SMBH)

AGN: SMBH growth

AGN Torus

Mass reservoir: Hydrogen column density?

AGN classification : Torus covering factor?

X-Ray Spectrum of AGN

1Fe KaTotal

0.1

Reflection

10ï30.01

EFE

Direct1

X-ray spectrum : Surrounding material
Reflection: Torus paramters

10Energy (keV)

100

MYTorus Model (Murphy & Yaqoob 09)
Murphy & Yaqoob 09

Free parameter : NH, i
Problem: Opening angle is fixed

Ikeda Torus Model (Ikeda+09)
Ikeda+09

Free parameter : NH, θinc, θopen
We can examine the torus opening angle.

Opening angle with Ikeda Model
Tanimoto+18

Tanimoto+16, 18: investigated the opening angle

Tight correlation between opening angle and inclination???

0.1

1

Problems of Smooth Torus

EFE

θincl = θopen
0.01

θincl = θopen + 10

10ï3

θincl = θopen + 20

Ikeda model : Smooth Torus
θincl = θopen: soft X-ray flux↗

1

10Energy (keV)100

Smooth Torus → Clumpy Torus

ClumpySmooth

Clumpy torus : larger soft X-ray flux than smooth one (Furui+16)
Clumpy torus : can explain the observed X-ray spectrum?

Smooth Torus → Clumpy Torus

ClumpySmoothClumpy torus : larger soft X-ray flux than smooth one (Furui+16)
Clumpy torus : can explain the observed X-ray spectrum?

Table of Contents
Chapter 1: Active Galactic Nucleus(Tanimoto+16, Tanimoto+18)

Chapter 2: X-Ray Observatories

Chapter 3: X-Ray Spectral Model from Clumpy Torus(XClumpy : Tanimoto+19)

Chapter 4: Application of XClumpy to 10 Obscured AGNs
(Tanimoto+20, submitted to the ApJ)Clump Distribution

Clump distribution : Nenkova+08 (CLUMPY)
Radial direction: Power law distribution

Elevation direction : Gaussian distribution

Free Parameters

NH : Hydrogen column density along the equatorial planeσ: Torus angular width (standard deviation)i: Inclination angle

Monte Carlo Simulation
Odaka+16

Complicated geometry: Monte Carlo simulation

Monte Carlo simulation code (MONACO: Odaka+16)

Method : X-ray Spectral Model

Method : X-ray Spectral Model

1Comparison among Models

10ï30.01

EFE

0.1

XCLUMPY
MYTorusIkeda Torus

110Energy (keV)

XCLUMPY : high soft X-ray flux

100Application to Circinus Galaxy
Ichikawa+15

One of the closest obscured AGNs
Ichikawa+15 investigated the torus parameters with CLUMPY.

Application to Circinus Galaxy

Emission lines
Suzaku/XIS
Suzaku/PIN
Suzaku/GSO

Total

XMM/EPN
XMM/MOSNuSTAR/FPM

Reflection
Thermal

Direct

XMM-Newton, Suzaku, & NuSTAR data
Our model well reproduced the observed X-ray spectra.

σX vs. σIRσ: Torus angular width

σX < σIR?

Table of Contents
Chapter 1: Active Galactic Nucleus(Tanimoto+16, Tanimoto+18)

Chapter 2: X-Ray Observatories

Chapter 3: X-Ray Spectral Model from Clumpy Torus(XClumpy : Tanimoto+19)

Chapter 4: Application of XClumpy to 10 Obscured AGNs
(Tanimoto+20, submitted to the ApJ)Sample Selection
Selection

SampleIchikawa+15

21

Obscured AGN

17Suzaku & NuSTAR data

10We applied XCLUMPY to X-ray spectra of 10 obscured AGNs.
This enables us to directly compare the X-ray and infrared.

1

Broadband X-Ray Spectrum

Suzaku/HXD

IC 5063

IC 506310ï45010ï3

NuSTAR/FPM

Emission lines

Total
Direct

ThermalReflection

10ï410ï3

Suzaku/XIS0.01

0.01

10ï5Scatteringï511010ï5(dataïmodel)/error

0.1

0.1

keV2 (Photons cmï2 sï1 keVï1)

keV2 (Photons cmï2 sï1 keVï1)

1Energy (keV)

1

10Energy (keV)

We analyzed the Suzaku & NuSTAR data.
Our model well reproduced the observed X-ray spectrum.

Broadband X-Ray Spectrum
NGC 21100.01
10ï310ï40.1

1NGC 3227

0.01
10ï310ï45

ï5
1

100
ï51

1

10ï4

50
ï510

keV2 (Photons cmï2 sï1 keVï1)

10ï30.1

NGC 5643

0.01
10ï310ï40.1

10ï310ï410ï5550ï51

100ï51

Energy (keV)

0.01
10ï310ï40.1

1
keV2 (Photons cmï2 sï1 keVï1)

keV2 (Photons cmï2 sï1 keVï1)

NGC 7172

NGC 7582

0.01
10ï310ï40.1

10ï310ï4555ï510
Energy (keV)ï5110
Energy (keV)(dataïmodel)/error10ï5(dataïmodel)/error

10ï50NGC 7674

0.01

10ï5010
Energy (keV)

11NGC 5728

0.01

10ï5

Energy (keV)
1

101(dataïmodel)/error

NGC 5506

0.01

0.1

ï5

Energy (keV)

1

10Energy (keV)

keV2 (Photons cmï2 sï1 keVï1)

0.1

10(dataïmodel)/error5(dataïmodel)/error

keV2 (Photons cmï2 sï1 keVï1)

10ï4510ï5(dataïmodel)/error

10ï310ï50NGC 3281

0.01

10ï51keV2 (Photons cmï2 sï1 keVï1)0.1

10ï5Energy (keV)(dataïmodel)/error

keV2 (Photons cmï2 sï1 keVï1)

keV2 (Photons cmï2 sï1 keVï1)

0.1

1(dataïmodel)/error(dataïmodel)/error

keV2 (Photons cmï2 sï1 keVï1)10ï51

10Energy (keV)σX vs. σIRσX < σIR
Dust distribution : vertically more extended?

σX vs. σIRσX < σIR
Dust distribution : vertically more extended?

iX vs. σIR - σXiX↗ : σIR - σX↗
Dusty polar outflows?

Evidences of Polar Dust
Tristram+14N100offset δ DEC [mas]50

E0−50−100Circinus Galaxy
100500−50offset δ RA [mas]1 pc−100Tristram+14 discovered polar dust with infrared interferometry.
Polar dust : 80% of the mid infrared emission

Evidences of Polar Dust
Wada+16

Wada+16 : RHD simulation
Edge on : Polar dust

AGN Unification Model (Classical)

AGN unification model was suggested (Antonucci 93)
Torus surrounds the SMBH and the accretion disk.

AGN Unification Model (Current)Hickox & Alexsander 18

Smooth torus → Clumpy torus
Polar dust component

Summary
Elucidating the torus parameters is essential for understanding
the SMBH growth and AGN classification.

We constructed the X-ray spectral model from realistic clumpy
torus (XClumpy) for the first time (Tanimoto+19).

We applied XClumpy to 10 obscured AGNs. Dust distribution isvertically more extended due to polar dust (Tanimoto+20).