asmus exgal short

7/31/2019 Asmus Exgal Short

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Absorption-corr. X-ray luminosity

Obser

ved

MIRlu

minos

ity

The MIR--X-ray

correlation

of AGN

Daniel Asmus

Poshak Gandhi

Sebastian F. HnigAlain Smette

Wolfgang J. Duschl


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Fine-structure

Outline

Summarylast talk

Understanding

the

MIRX-ray

correlation


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Types of nuclear activity

B. Keel

NASA

Type 1AGN

Type 2AGN


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AGN in the mid-infrared

VISIR manual


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My PhD thesis

Low-luminosity AGN BAT AGN

High-res.

Photometry

High-res.

Photometry

Non-AGNContamination

MIR SED

Asmus et al. 2011 Asmus et al. 2012A,B, in prep.


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12m 2-10keV correlation

(absorption-corrected)

Correlation fromGandhi et al. 09...

Objects: 42 Spearman Rank:

= 0.88(log p = -17)

Power-law fit:log L

MIR~

(1.00 0.08) log LX

Power-law fit to:all AGN from G09


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Adding theLLAGN...


= 0.94(log p = -30)

Power-law fit:log L

MIR~

(1.05 0.05) log LX



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all AGN


Adding the BATAGN...


= 0.90(log p = -42)

Power-law fit:log L

MIR~

(1.00 0.04) log LX

Fit depends somewhaton algorithm used

Correlation dominated

by X-ray uncertainties


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all AGN




= 0.90(log p = -42)

Power-law fit:log L

MIR~

(1.00 0.04) log LX




Correlation applicableto all AGN


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Fine-structure

Outline

Summarylast talk

Understanding

theMIRX-ray

correlation


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all AGN




= 0.90(log p = -42)

Power-law fit:log L

MIR~

(1.00 0.04) log LX






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all AGN




= 0.90(log p = -42)

Power-law fit:log L

MIR~

(1.00 0.04) log LX





Outliers?!


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Outliers

NGC 3125: Weak VISIR detection

seems extended LINER classification only from

compact X-ray core (Dudik et al.2005)

No broad optical emission lines(Kewley et al. 2001)

Optical and NIR show youngmassive Wolf-Rayet starcluster(Hadfield & Crowther 2006)

X-rays could also come fromULX

AGN nature unclear

NGC 4303: Weak VISIR detection Faintest object in sample in terms

of X-ray luminosity andmeasured MIR flux

X-ray data indicates an AGN(Tzanavaris & Georgantopoulos 2007)

Classified as HII in optical(Ho et al. 1995)

Nuclear young star cluster(Colinaet al. 2002) X-rays could also come from

ULX AGN nature unclear

smoothed


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Local typicalstarburst galaxies

(Ranalli+03)


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Where is thiscorrelation coming from?


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Origin of the observed MIR emission

Small MIR variability (< 30%)Large X-ray variability (>50%)

MIR emissionfrom larger andcomplex structure

Silicate feature in theaverage MIR SEDs of AGN

dusty origin ofMIR emission

Star formation origin in generalexcluded (no PAH emission)

dust isAGN heated

Clumpy torus modelsmatch most observations

dust in aclumpy

torus-likestructure


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X-ray emission of AGN

emission region


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The MIRX-ray correlation

UV

X-ray

UV

Mid-infrared


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What causes thedispersion

non-AGN emission?

A id t i ti 'W ll l d' & ' ' AGN


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Avoid contamination: 'Well-resolved' & 'pure' AGN

MIRX-rayrat io

intrinsic scale

maximum star formationcontribution


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Li

ttle

improv

emen

t


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Host galaxy distribution


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Host galaxy distribution

Influence of the host galaxy


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Influence of the host galaxy

MIR

t o

X-ra

y ra

tio

M

IR

t o

X-ra

y r a

t io

only V. type >= -2


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only V. type >= -2


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The AGN itself?

Clumpy torus models


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Clumpy torus models

CAT3D(Clumpy AGN Tori in a 3D geometry)- Hnig & Kishimoto (2010)- IR model SEDs

- Monte Carlo radiative transfer calculations andray-tracing techniques

- 3D dust cloud distributions- illumination: standard thin accretion disk

simulated 13m images

type 1 AGN (0)

type 2 AGN (90)

Clumpy torus models


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Clumpy torus models

CAT3D(Clumpy AGN Tori in a 3D geometry)- Hnig & Kishimoto (2010)- IR model SEDs

- Monte Carlo radiative transfer calculations andray-tracing techniques- 3D dust cloud distributions- illumination: standard thin accretion disk

simulated 13m images

type 1 AGN (0)

type 2 AGN (90)

90

0

0.3

Effect of the column density


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Torus models: MIR emission when torus inclination (max difference of ~0.3 dex) column density N

Hwhen torus inclination

MIRX-ray luminosity ratio RX

M when column density NH

...



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Torus models: MIR emission when torus inclination (max difference of ~0.3 dex) column density N

Hwhen torus inclination

MIRX-ray luminosity ratio RXM when column density NH ...

no dependency observed

Type 1 AGN

Type 2 AGN

LINER

lo

gL

(12m)/

L(2-10k

eV

)

Effect of the accretion rate


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Effect of the accretion rate

Predicted change in accretion structure at low rates change in MIR--X-ray ratio...

Type 1 AGN

Type 2 AGN

LINER

jet or ADAF? standard accretion

... some evidence of an additional component (to the torus) at lowestaccretion rates likely a strong jet.

log

L(12m)/L(2-10keV

)

Conclusions


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Co c us o s

MIR--X-ray luminosity correlation... Strongest 12m2-10keV correlation for all AGN combined (slope ~1)

MIR--X-ray correlation valid for all AGN down to LX~1040 erg/s!

fundamental physical connection uniform structure in all AGN

Origin of MIR emission in AGN: reprocessed accretion disk emission (UV)from a dusty AGN-heated structure

Origin of the X-ray emission in AGN: reprocessed accretion disk emission(UV) from a hot corona

Fine-structure independent of host galaxy. however obscuration in some cases caused by

host galaxy Independent of nuclear obscuration, contradicting torus models...

Fine-structure depends on the accretion rate! Low-rate objects presumably have additional non-thermal component, e.g.,

jet...

asmus exgal short

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