The predominance of infrared emission from the polar region of accreting supermassive black holes

7/25/2019 The predominance of infrared emission from the polar region of accreting supermassive black holes

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The predominance of infrared emission from

the polar region of accreting supermassive

black holes

Daniel AsmusESO, Chile

with

Sebastian Hnig & Poshak Gandhi


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AGN are bright(est) in the mid-infrared.


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Type 2AGN

Type 1

AGN


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Type 2AGN

Type 1

AGN

???


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WISE (0.4m)


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WISE (0.4m)

4

VLT/VISIR (8.2m)


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Asmus et al. 2014


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Only few without strong star formation are resolved (~10-100pc)Is the resolved emission coming from the torus?


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Establishing a system axis from ionisation cones [OIII],radio jets, maser disks, and polarized emission.

NGC 2110;credit: D. Evans

Circinus;Greenhill et al. 2003

Circinus;

Wilson et. al. 2000


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The resolved emission is coming from the polar axis of theAGN systems!

Asmus et al. 2016 (see also Braatz et al. 1993; Cameron et al. 1993; Bock et al. 2000;

Radomski et al. 2002, 2003; Whysong & Antonucci 2004; Packham et al. 2005;

Reunanen, Prieto & Siebenmorgen 2010; Hnig et al. 2010)

Angular difference (System Axis - MIR extension)


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Is the mid-infrared emission of AGN dominated by dustin/along the ionisation cone instead of the obscuring torus?

Relative amount of resolved emission

Asmus et al. 2016


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The resolved emission strongly correlates with the [OIV]emission produced in the ionisation cone

Relativeamountofre

solvedemission

[OIV] emissionAsmus et al. 2016


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Circinus;

T

ristrame

tal.201

4

NGC1068;

Lp

ezGonzagaetal.2

014

N

GC3783;Hnige

tal.2013

N

GC424;Hnige

tal.2012

Polar elongation is dominant also on parsec scaleas found with MIDI interferometry (Lopez-Gonzaga et al. 2016)


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The small and large scale elongation are aligned and seem totrace the edge of the ionisation cone.

Circinus; Tristram+14


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A new paradigm for the AGN dust structure?

Hnig et al. 2012


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39 40 41 42 43 44 45 46log Lint(2-10keV) [erg/s]

39

40

41

42

43

44

45

46

logLnuc(12m

)[erg/s]

The mid-infraredX-ray correlation for all types of AGN is drivenby dust in the ionisation cones rather than the torus

Absorption-corr. X-ray luminosity

ObservedMIR

luminosity

Asmus et al. 2015

(see also:Glass et al. 1982;

Krabbe et al. 2001;Lutz et al. 2004;Horst et al. 2006;Ramos Almeida et al. 2007;Horst et al. 2008;Gandhi et al. 2009;Levenson et al. 2009;Fiore et al. 2009;Hardcastle et al. 2009;Hoenig et al. 2010;Asmus et al. 2011;Mullaney et al. 2011;Mason et al. 2012;

Matsuta et al. 2012;Ichikawa et al. 2012;Sazonov et al. 2012;

Mateos et al. 2015;Stern 2015)


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What have we learned?


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Back-up Slides


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The chop & nod technique makes the target observable.


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The resolved emission is not correlated to the host orientation.

Asmus et al. 2016

Angular difference (System Axis - MIR extension)


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The outliers

Seyfert 1.2

[OIII] pointlike

marginally

resolved

PA error 27

Seyfert 1.5/2

wide opening

ionisation cones

edge-on spiral

emission traces

host dust lane

Seyfert 1.2

wide opening

ionisation cones

weakest AGN in

the sample

low S/N


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The reasons for the low detection rates

Distance unresolved

low S/N intrinsic weakness

Inclination no elongation


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Difference between type I and II is smaller than expected

39 40 41 42 43 44 45 46log Lint(2-10keV) [erg/s]

39

40

41

42

43

44

45

46

logLnuc(12m

)[erg/s]

Sy 1-1.5 (>=3 epochs)

Sy 1.8-1.9 (>=3 epochs)

Sy 2 (>=3 epochs)

LINER (>=3 epochs)

Sy 1-1.5 (

The predominance of infrared emission from the polar region of accreting supermassive black holes

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