A powerful tool to uncover hidden monsters? Daniel Asmus ESO, Chile
Asmus et al. 2014
Only use those objects with: - reliable AGN classification, - no composites, - good S/N X-ray data - consistent intrinsic luminosity estimates Asmus et al. 2014 -> 151 AGN
The mid-infrared emission strongly correlates with the X-ray emission for all types of AGN Observed MIR luminosity log L nuc (12µm) [erg/s] 46 45 44 43 42 41 40 39 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) 39 40 41 42 43 44 45 46 log L int (2-10keV) [erg/s] Absorption-corr. X-ray luminosity
including Compton-thick obscured AGN Observed MIR luminosity log L nuc (12µm) [erg/s] 46 45 44 43 42 41 40 39 CT CT CT CT CT CT CT CT CT CT 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) 39 40 41 42 43 44 45 46 log L int (2-10keV) [erg/s] Absorption-corr. X-ray luminosity
Difference between type I and II is smaller than expected 46 1.0 0.8 45 44 fraction of total 0.6 0.4 0.2 log L nuc (12µm) [erg/s] 43 42 41 40 Sy 1-1.5 (>=3 epochs) Sy 1.8-1.9 (>=3 epochs) Sy 2 (>=3 epochs) LINER (>=3 epochs) Sy 1-1.5 (<3 epochs) Sy 1.8-1.9 (<3 epochs) Sy 2 (<3 epochs) LINER (<3 epochs) NLS1 Compton-thick 39 39 40 41 42 43 44 45 46 log L int (2-10keV) [erg/s] number of objects 20 15 10 5 0-0.6-0.3 0.0 0.3 0.6 0.9 1.2 1.5 1.8 log L nuc (12µm) - log L int (2-10keV) Asmus et al. 2015
The correlation can be used as absorption indicator (+/- 0.3 dex) Obscuring column For log NH > 23: Asmus et al. 2015 see also: Brightman & Nandra 2011 Severgnini et al. 2012 F(mid-infrared)/F(observed X-ray)
?
The mid-infrared emission is dominated by a polar dusty wind
The resolved mid-infrared emission is coming from the polar axis of the AGN systems Asmus et al. 2016 T T
The resolved mid-infrared emission is coming from the polar axis of the AGN systems Angular difference (System Axis - MIR extension) 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; Hönig et al. 2010)
The small and large scale elongation are aligned and seem to trace the edge of the ionisation cone. Tristram et al. 2014 López Gonzaga et al.2014 Circinus see also Hönig et al. 2012, Hönig et al. 2013, López Gonzaga et al. 2016 10 pc 12µm (VISIR)
The small and large scale elongation are aligned and seem to trace the edge of the ionisation cone. Tristram et al. 2014 López Gonzaga et al.2014 Circinus see also Hönig et al. 2012, Hönig et al. 2013, López Gonzaga et al. 2016 10 pc 12µm (VISIR)
The small and large scale elongation are aligned and seem to trace the edge of the ionisation cone. Tristram et al. 2014 López Gonzaga et al.2014 Circinus see also Hönig et al. 2012, Hönig et al. 2013, López Gonzaga et al. 2016 10 pc 12µm (VISIR)
Try modelling of Circinus with a hollow dusty cone and flared disk geometry Tristram et al. 2014 Circinus 10 pc 12µm (VISIR)
Try modelling of Circinus with a hollow dusty cone and flared disk geometry Tristram et al. 2014 Circinus 10 pc 12µm (VISIR)
Try modelling of Circinus with a hollow dusty cone and flared disk geometry Tristram et al. 2014 Circinus 10 pc 12µm (VISIR)
Try modelling of Circinus with a hollow dusty cone and flared disk geometry Tristram et al. 2014 Circinus 10 pc 12µm (VISIR)
Try modelling of Circinus with a hollow dusty cone and flared disk geometry Tristram et al. 2014 Circinus 10 pc 12µm (VISIR)
Apply Monte Carlo Radiative Transfer PRELIMINARY Stalevski, Asmus and Tristram, in prep.
Apply Monte Carlo Radiative Transfer PRELIMINARY Stalevski, Asmus and Tristram, in prep.
Apply Monte Carlo Radiative Transfer PRELIMINARY Stalevski, Asmus and Tristram, in prep.
Model SED doesn t seem to match F [W/m 2 ] 10-11 10-12 10-13 10-14 10-15 MIDI spectrum HR photometry disk+cone PRELIMINARY 0.1 1 10 100 [µm] Stalevski, Asmus and Tristram, in prep.
but significant foreground absorption present Roche et al. 2006
Extinction-corrected SED works well 10-11 F [W/m 2 ] 10-12 10-13 10-14 10-15 MIDI spectrum HR photometry disk+cone disk+cone+extinction PRELIMINARY 0.1 1 10 100 [µm] Stalevski, Asmus and Tristram, in prep.
What have we learned? Mid-infrared X-ray correlation is a powerful tool Mid-infrared emission of AGN dominated by polar dust emission (instead of torus) Radiative transfer modelling of dust structure proves that this scenario can work Circinus: MIR morphology explained but requires detailed modelling Stalevski, Asmus and Tristram, in prep.
SNEAK PEEK
Back-up Slides
The correlation also exist in flux flux space and thus is not distance effect -8-9 log F nuc (12µm) [erg/cm 2 /s] -10-11 -12-13 -14-14 -13-12 -11-10 -9-8 log F int (2-10keV) [erg/cm 2 /s]
No strong differences in MIR X-ray ratio with X-ray column density 2 1 R X M 0 0.5 L int (2-10keV) L obs (14-195keV) -1 M R HX 1 0-1 log L nuc (12µm) - log L X 0.0-2 1-0.5 0 X R HX -1 19 20 21 22 23 24 25 log N H [cm -2 ] -2 19 20 21 22 23 24 25 log N H [cm -2 ]
Difference with radio-loudness 46 45 radio-quiet radio-loud log L nuc (12µm) [erg/s] 44 43 42 MIR synchrotron dominated Jet contributes to X-rays? 41 40 39 39 40 41 42 43 44 45 46 log L int (2-10keV) [erg/s]
The chop & nod technique makes the target observable.
Asmus et al. 2014
Establishing a system axis from ionisation cones [OIII], radio jets, maser disks, and polarized emission. Circinus; Wilson et. al. 2000 T T NGC 2110; credit: D. Evans Circinus; Greenhill et al. 2003
The resolved emission is not correlated to the host orientation. Angular difference (System Axis - MIR extension) Asmus et al. 2016
The outliers Seyfert 1.2 [OIII] pointlike marginally resolved PA error 27º 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
The reasons for the low detection rates Distance low S/N unresolved intrinsic weakness Inclination no elongation
Is the mid-infrared emission of AGN dominated by dust in/along the ionisation cone instead of the obscuring torus? Relative amount of resolved emission Asmus et al. 2016
The resolved emission strongly correlates with the [OIV] emission produced in the ionisation cone Relative amount of resolved emission [OIV] emission Asmus et al. 2016
A new paradigm for the AGN dust structure? Hönig et al. 2012