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Heavily obscured AGN with INTEGRAL/SWIFT/XMM/CHAND
RAprospect for SIMBOL-X
R. Della Ceca INAF-Osservatorio Astronomico di
Brera
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• In collaboration with
• P. Severgnini (INAF-OABrera, Italy)
• Caccianiga (INAF-OABrera, Italy)
• V. Braito (John Hopkins Univ.
  NASA/GSFC,USA)
• L. Ballo (ESAC/ESA, Spain)
• F. Fiore (INAF-OARoma,Italy)
• Comastri (INAF-OABologna,Italy)
• G. Malaguti (INAF-IASFBo,Italy)
• R. Gilli (INAF-OABologna,Italy)
• C. Vignali (Bologna University,Italy)

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Plan of this talk

• Why heavily obscured (NHgt1024 cm-2) AGN
• are so important?
• What do we really know about the Compton
• Thick AGN Universe?
• From BeppoSAX, INTEGRAL, SWIFT, XMM, Chandra,
  SUZAKU
• Which is the expected improvement in this
• field with SIMBOL-X?

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Why heavily obscured (NHgt1024 cm-2) AGN are so
important?
SMBH are found in the center of most nearby bulge
dominated galaxies
Their masses are proportional to bulge properties
(e.g. luminosity, velocity dispersion)
Strong feedback mechanism between the formation
and evolution of SMBH and their host galaxy
Active Galactic Nuclei are leading actors in the
galaxy formation and evolution of structure in
the Universe
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Why heavily obscured (NHgt1024 cm-2) AGN are so
important?
The CXB synthesis model AGN Unification
Models 50 of the accretion power produced in
the Universe could be produced in heavily
obscured sources.

Many of these sources could be optically elusive
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Hunting for Optically Elusive AGNs the case of
the merging system Arp 299

• BeppoSAX observations
• NH 2.5 1024 cm-2
• L(0.5-100 keV) 1.9 1043 erg s-1
• 6.4 keV Fe-Ka Eem.line 6.35 eV
• EW 636 eV but EWtransmitted 7 keV

D 44 Mpc

• LFIR 2.86 1011 LSUN
• Optical and mid-/far-IR
• LINER and/or starbursting

(Della Ceca et al. 2002, ApJL, 581, 9)
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Hard (gt10 keV) X-ray data are fundamental to
unveil and to study this component and to have
the real
Census of Super-Massive Black Hole in the
Unviverse
What do we really know about the Compton Thick
AGN Universe ?
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INTEGRAL/SWIFT AGN surveys
resolved few of the hard (10-50 keV) CXB

• Swift/BAT Survey (Markwardt et al., 2005)
• sensitivity 10-11 erg cm-2 s-1 (14-195
  keV)
• 66 high Galactic latitude sources - 44
  E.L.AGN (39 with NH)
• 
  - 10 Unidentified
• 4 Compton Thick AGN

• INTEGRAL IBIS Survey (Bassani et al., 2006)
• sensitivity limit (20-100 keV) 1.5x10-11
  cgs
• At the flux limit - 49 E.L.AGN (41 with NH)
• - 5
  Unidentified
• 5 Compton Thick AGN

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INTEGRAL/SWIFT AGN surveys

• INTEGRAL IBIS Survey (Sazonov et al., 2006)
• sensitivity limit (17-60 keV) 7x10-11 cgs
  (75 of Sky at bgt5)
• 
  4x10-11 cgs (50 of Sky at bgt5)
• Complete sample (SNRgt5, bgt5) - 66 E.L.AGN
  (60 with NH)
• 
  - 7 Unidentified
• 4 Compton Thick AGN

• INTEGRAL IBIS AGN Survey (Beckmann et al., 2006)
• sensitivity limit (20-40 keV) 3x10-11 cgs
  (76 of Sky)
• 1x10-11 cgs
  (17 of Sky)
• Complete sample (SNRgt5) - 38 E.L. AGN (32
  with NH)
• -
  8 Unidentified (but at low b)
• 3 Compton Thick AGN

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Compton Thick AGN selected above 10 keV
10-40 keV
8 Compton Thick AGN in total from statistically
complete sample !!!
CT Fraction (5 20)
Fx10-11 cgs
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Compton Thick AGN detected above 10 keV
10-40 keV
Complete samples pointing observations 16
Compton Thick AGN in total!!!
Fx10-11 cgs
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Broad band spectra NGC4945 and NGC1068
BeppoSAX MECSPDS
Normalized to the Crab spectrum (?2)
NGC 4945 NH2x1024 cm-2 L10-403x1042 cgs
NGC 1068 NHgt1025 cm-2 L10-40gt5x1041 cgs
Guainazzi et al 2000
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Broad band spectra NGC 5728
Primary PL component
SUZAKU XISHXD/pin
Fe lines
Reflected component
Scattered component
NH2x1024 cm-2 L10-401x1043 cgs
Comastri et al., 2007
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Candidate CT AGN detected below 10 keV
2-10 keV
CT AGN candidate having a prominent (EW gt 800
eV) Iron Line
21 objects
ASCA,BeppoSAX,XMM
L2-10keV(observed)
Fx10-13 cgs
Redshift
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Candidate CT AGN detected below 10 keV
2-10 keV
CT AGN candidate having a prominent (EW gt 800
eV) Iron Line
ASCA,BeppoSAX,XMM
21 objects
CT AGN Candidate in the CDFS
L2-10keV(observed)
21 objects
Fx10-13 cgs
Fx10-15 cgs
We do not see the absorption cut-off ? only a
lover limit on NH We do not know Lxintrinsic for
90 of these sources!!!!
Redshift
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Compton Thick AGN detected above 10 keV
10-40 keV
Complete samples pointing observations 16
Compton Thick AGN in total!!!
Fx10-11 cgs
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Comparison with AGN Compton Thin (NHlt1024 cm-2)
508 AGN NHlt1022 1022ltNHlt1024 307
201
Good coverage of the Lx-z plane up to z2
From La Franca et al., 2005
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What can we do with SIMBOL-X?
F10-4010-11 cgs
F2-105x10-13 cgs
NH 3x1024 cm-2 z0.2
Counts 11000 (MPD) 8000 (CZT)
Exp 100Ksec
Iron K? line
Iron K? line
Accuracy NH 5 ?
0.5 NormPL 10 NormREFL
30 NormSCATT 5
Accuracy E6.4,6.7 1 Norm
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The Compton Thick AGN Universe
According to the CXB models
40 CT AGN in the sky at bgt20
Fx10-11 cgs

• Possible SIMBOL-X targets
• Well known CT AGN from hard X
• Infrared Bright Local Galaxies

0.007
0.1
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What can we do with SIMBOLX?
F10-4010-12 cgs
F2-1010-13 cgs
NH 3x1024 cm-2 z0.5
Counts 1500 (MPD) 800 (CZT)
Accuracy NH 10 ?
3 NormPL 20 NormREFL
unc. NormSCATT 10-20 E6.4
1 Norm6.4 30-50
Exp 100Ksec
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The Compton Thick AGN Universe
1500 CT AGN in the sky at bgt20
Fx10-12 cgs

• Possible SIMBOL-X targets
• Candidate CT from 2-10 keV data
• already known
• from bright 2XMM sources candidate
• b) Infrared Bright Local Galaxies
• c) ULIRGs

0.02
0.5
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What can we do with SIMBOLX?
F10-4010-13 cgs
F2-103x10-14 cgs
NH 3x1024 cm-2 z1.5
Counts 350 (MPD) 150 (CZT)
Accuracy NH 20-40 ?
10 NormPL within a factor 2
Exp 100Ksec
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The Compton Thick AGN Universe
2x106 CT AGN in the sky at bgt20
Possible SIMBOL-X targets a) Candidate CT AGN
Spitzer/Hershel surveys b) ULIRGs
Fx10-13 cgs
0.06
1.5
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What about the CT AGN with NHgt 1025 cm-2
F10-4010-11 cgs NH 3x1024cm-2
Counts 11000 (MPD) 8000
(CZT) L10-401045 cgs z0.2
Counts 1300 (MPD) 500 (CZT) NH gt
1025 cm-2 z0.2
Counts 270 (MPD) 150 (CZT) NH gt
1025 cm-2 z0.5
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Summary and conclusion
The Compton thick AGN Universe is practically a
new field in high energy astrophysics since
very few Compton Thick (and local) AGN have been
studied so far.
The SIMBOL-X mission is expected to open this
field to detailed investigations up to
cosmological distance (z1.5-2.0)
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Summary and conclusion
THANKS