hot gas
dust

black hole

NUSTAR X-ray spectroscopy of obscured AGN: newconstraints on the circum-nuclear gas and dust,and Compton-scattering model uncertainties
featuring: "The Markarian 3 case"
Matteo Guainazzi
ASTRO-H Science Operation Team (SOT) - ISAS/JAXA
ASTRO-H ESA Science Operation Center (SOC) - ESA/ESAC

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

OutlineBasic question of this talk: which quantitative constraints
can we put on the circum-nuclear gas and dust in AGN!

1. Constraints from IR/optical
2. Constraints from X-ray spectroscopy and spectral variability
3. A showcase: a recent monitoring campaign on Markarian 3
4. What do we need to make a step forward: modelling andASTRO-H

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

AGN Spectral Energy Distribution
Ho et al., 1995, ApJElvis et al., 2012, ApJ, 759. 6; Detmers 2011, A&A, 534, A37

Radio-quiet AGN (Elvis et el. 1994)
Radio-loud AGN (Elvis et al. 1994)
COSMOS AGN
Galaxy/startburst remplatesMatteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

AGN Spectral Energy Distribution
Elvis et al., 2012, ApJ, 759. 6; Detmers 2011, A&A, 534, A37

Ho et al., 1995, ApJ

Radio-quiet AGN (Elvis et el. 1994)
Radio-loud AGN (Elvis et al. 1994)
COSMOS AGN
Galaxy/startburst remplatesMatteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

AGN Spectral Energy Distribution
Ho et al., 1995, ApJ

Elvis et al., 2012, ApJ, 759. 6; Detmers 2011, A&A, 534, A37

Radio-quiet AGN (Elvis et el. 1994)
Radio-loud AGN (Elvis et al. 1994)
COSMOS AGN
Galaxy/startburst remplatesMatteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

IR constraints on the dust locationBurtscher et al., 2015, A&A, 558, A8149

Tristram et al., 2015, A&A, 563, A82

NIR+MIR interferometry + dust reverberation (→Ichikawa-san talk)[here compared with the location of the gas
producing broad optical spectral lines (BLR)]

Circinus Galaxy

maser disk

13.0 μm10.5 μm
8.0 μmMatteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Why is this important? And why X-rays?
Tremaine et al., 2002, ApJ, 574, 740, Sazonov et al., 2007, A&A, 462, 57

However, most of the gas in the AGN environment in within
the dust sublimation radius.

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Why is this important? And why X-rays?
Tremaine et al., 2002, ApJ, 574, 740, Sazonov et al., 2007, A&A, 462, 57

However, most of the gas in the AGN environment in within
the dust sublimation radius.
We need X-rays to study:•AGN innermost parsec structure

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Why is this important? And why X-rays?
Tremaine et al., 2002, ApJ, 574, 740, Sazonov et al., 2007, A&A, 462, 57

However, most of the gas in the AGN environment in within
the dust sublimation radius.
We need X-rays to study:•AGN innermost parsec structure•

AGN feeding from the host galaxy

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Why is this important? And why X-rays?
Tremaine et al., 2002, ApJ, 574, 740, Sazonov et al., 2007, A&A, 462, 57

However, most of the gas in the AGN environment in within
the dust sublimation radius.
We need X-rays to study:•AGN innermost parsec structure•

AGN feeding from the host galaxy•

AGN feed-back to the host galaxy

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Why is this important? And why X-rays?
Tremaine et al., 2002, ApJ, 574, 740, Sazonov et al., 2007, A&A, 462, 57

However, most of the gas in the AGN environment in within
the dust sublimation radius.
We need X-rays to study:

CXB as seen by INTEGRAL•AGN innermost parsec structure•

AGN feeding from the host galaxy•

AGN feed-back to the host galaxy•

Synthesis models of the Cosmic X-ray BackgroundMatteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

X-ray spectroscopy of obscured AGN: a primer
Yaqoob et al., 2015, arXiv:1508.07685

Ikeda, PASJ, 2009, 692, 608

torus, Brightman & Nandra
2011, MNRAS, 413, 1206

mytorus, Murphy & Yaqoob, 2009, MNRAS, 397, 1549

Fitting for:• line-of-sight column density (NH,abs)• global column density (NH,global)• inclination angle (θincl)• half-opening angle (θop)

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Bonus: the “true” column density distribution
Lansbury et al., 2015, ApJ, 809, 115

Sample of a z<0.5 SDSS-selected QSOs
[measured][predicted][measured]Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Luminosity-dependent covering fraction
Brightman et al., 2015, ApJ, 805, 41

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Luminosity-dependent covering fraction
Brightman et al., 2015, ApJ, 805, 41

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Luminosity-dependent covering fraction
Brightman et al., 2015, ApJ, 805, 41

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

X-ray spectroscopy of obscured AGN: a primer
Yaqoob et al., 2015, arXiv:1508.07685

Ikeda, PASJ, 2009, 692, 608

torus, Brightman & Nandra
2011, MNRAS, 413, 1206

mytorus, Murphy & Yaqoob, 2009, MNRAS, 397, 1549

Fitting for:• line-of-sight column density (NH,abs)• global column density (NH,global)• inclination angle (θincl)• half-opening angle (θop)

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Geometry matters
NH,los=NH,global ("coupled")= 8x1023 cm-2
θop=600, θincl=700
Γ=1.8

only reflection

mytorus: fixed angles
torus: only "coupled" scenario

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Occultation by "cold" clouds
Risaliti et al., 2007, ApJ, 659, L111

NGC1365/Chandra

14 April 2006
16 April 2006
18 April 2006

X-ray source
Obscuring cloud

Assuming a cloud in: a) Keplerianmotion; b) virial turbulent motion; c)ionization equilibrium with the AGN:!
• Source Linear size D~1013-14 cm• Distance from the AGN d~10-1 pc

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Occultation event statistics
Markowitz et al,. 2014, MNRAS, 439, 1403

8 AGN withoccultation
events in theRXTE archive(~270 years inthe AGN life)!

BLR clouds
IR continuum
Dust (0.4-1 xsublimationradius, Rd)
X-ray clouds

“The Markarian 3 monitoring campaign”, NuSTAR AGN Physics WG, 9/3/2015

Mkn3 2014-2015 NuSTAR campaign
Guainazzi et al., in preparation

9 observations: 5 in autumn 2014 (7, 14 Sep, 1, 9, 23 Oct), 4 in spring2015 (19, 22 Mar, 5, 8 Apr). NuSTAR + Suzaku or XMM-Newton

The spectra of Markarian 3 above ~3 keV show variability
on all time-scales down to ~2 days

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Absorber column density variability
Guainazzi et al., in preparation

1=7/9/14
2=14/9/14
3=1/10/14
4=9/10/14
5=23/10/14

2014:
NH (1024 cm-2)!

6=19/3/15
7=23/3/15
8=5/4/15
9=8/4/15

2015:

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Absorber column density variability
Guainazzi et al., in preparation

1=7/9/14
2=14/9/14
3=1/10/14
4=9/10/14
5=23/10/14

NH (1024 cm-2)

2014:
NH,cloud=(4.9±1.4)x1022 cm-2
Nclouds=13-27
dcloud=0.6-1.4x1017 cm[Rdust~1017 cm]!

6=19/3/15
7=23/3/15
8=5/4/15
9=8/4/15

2015:

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Absorber column density variability
Guainazzi et al., in preparation

1=7/9/14
2=14/9/14
3=1/10/14
4=9/10/14
5=23/10/14

NH (1024 cm-2)

2014:
NH,cloud=(4.9±1.4)x1022 cm-2
Nclouds=13-27
dcloud=0.6-1.4x1017 cm[Rdust~1017 cm]!

6=19/3/15
7=23/3/15
8=5/4/15
9=8/4/15

2015:
NH,cloud=(3.2±0.4)x1022 cm-2
Nclouds=27-38

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Mkn3: X-ray vs. IR absorber/reprocessor
Guainazzi et al., in preparation; IR results from Sales et al., 2014. 441. 630

X-rays(gas+dust)

IR(dust)Still poorly known:•N(10N

2.2±0.913-38

0.5±0.39±3••θ

66.050X-ray cloud size/volume
filling factor(Rcloud ≲ 2000 RS/R2corona,10Rs)
X-ray cloud density[n ≳ 105 cm-3 (R2corona,10Rs)]
radial profile of gas and dust(no idea)
!

θ68.9

61

IR analysis suggests that thetorus extends up to ~7-8 pc

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Why is the IR opening angle than in X-rays?
Kawaguchi & Mori, 2011, ApJ, 737, 105

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Comparison of Compton-scattering results
Guainazzi et al., in preparation

Ikeda("decoupled")

N(10N
(10

mytorus! torus!
("decoupled")

2.2±0.9 0.12±0.01("coupled")

Comparison ofNH,los variability

N0.86-1.08 0.74-0.93 0.65-0.93θ66.0±0.4 60 (fixed) 58.3±1.8

θ

68.0±1.5

N/A>83

Good news: NH.los (i.e. Γ, LX)
does not strongly depend on thedetails of the torus modelBad news: comparison of torus
models is difficult due to theincongruent assumptions

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

1 month of the torus life in Markarian 3
dust-free
dustytlhgisf
ine-oMatteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

1 month of the torus life in Markarian 3
dust-free
dustytlhgisfine-oMatteo Guainazzi, “Obscured AGN: clues from NuSTAR”, MIT, 1 October 2015

A possible structure of the torus in Mkn3

Guainazzi et al., in preparation

thgisfne-oli

dust-freedusty

Matteo Guainazzi, “Obscured AGN: clues from NuSTAR”, MIT, 1 October 2015

Another possible structure of the torus in Mrk3
Guainazzi et al., in preparation

thgisfne-oli

dust-freedustyMatteo Guainazzi, “Obscured AGN: clues from NuSTAR”, MIT, 1 October 2015

A possible structure of the torus in Mkn3

Guainazzi et al., in preparation

thgisfne-oli

dust-freedusty

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

To make a step forward we need …
Liu & Li, 2014, ApJ, 787, 52

1. fully self-consistent models: homogeneous vs. clumpy(→Tanimoto-san talk)!
!
!
!

2. a direct estimate of the gas radial profile → ASTRO-H/SXSMatteo Guainazzi, “Obscured AGN: clues from NuSTAR”, MIT, 1 October 2015

Markarian 3 HETG spectrum (770 ks)
Guainazzi et al., in preparation

E=6.396±0.008 keV(i.e.: no outflow velocity)

Δv=600+200-90 km/s

New absorption
features
FeXXV/XXVI
NH~1021-22 cm-2

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

ASTRO-H/SXS vs. Chandra/HETG
Matt et al., 2002, MNRAS, 337, 147

Compton Shoulder relative intensity

100 ks SXSNH ↑Slab cos(θin)

Abs. lines

770 ks HETG

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Spectroscopy of optically thick nuclear gas
Reynolds et al., 2014, arXiv:1412.1177

To verify if this model is correct we need to know at which scale
Compton scattering and Fe Kα fluorescence line are produced
Measurements of the profile of the Kα iron line with the SXS!
1 pc

0.1 pcsimulation of 100 ks on NGC4388 (very similar AGN to Markarian 3)

0.01 pc

Matteo Guainazzi, “X-ray spectroscopy of obscured AGN”, "Prospects, challenges and evolution of AGN modeling in the Astro-H Era", Rikkyo University, 21 October 2015

Conclusions

Courtesy A.Merloni & S.Bonoli, MPE