Heavily obscured AGN with INTEGRAL/SWIFT/XMM/CHANDRA

:prospect for SIMBOL-X

R. Della Ceca INAF-Osservatorio Astronomico di

Brera

In collaboration with:

P. Severgnini (INAF-OABrera, Italy)P. Severgnini (INAF-OABrera, Italy)A.A. Caccianiga (INAF-OABrera, Italy)Caccianiga (INAF-OABrera, Italy)V. Braito (John Hopkins Univ. V. Braito (John Hopkins Univ.

NASA/GSFC,USA)NASA/GSFC,USA)L. Ballo (ESAC/ESA, Spain)L. Ballo (ESAC/ESA, Spain)F. Fiore (INAF-OARoma,Italy)F. Fiore (INAF-OARoma,Italy)• Comastri (INAF-OABologna,Italy)Comastri (INAF-OABologna,Italy)G. Malaguti (INAF-IASFBo,Italy)G. Malaguti (INAF-IASFBo,Italy)R. Gilli (INAF-OABologna,Italy)R. Gilli (INAF-OABologna,Italy)C. Vignali (Bologna University,Italy)C. Vignali (Bologna University,Italy)

Plan of this talk

• Why heavily obscured (NH>1024 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?

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

Why heavily obscured (NH>1024 cm-2) AGN are so important?

SMBH are found in the center of most nearby bulge dominated galaxies

The CXB synthesis model + AGN Unification Models~50% of the accretion power produced in the Universe

could be produced in heavily obscured sources.

Log NH 21 22 23 24 25

Gilli et al., 2006

Why heavily obscured (NH>1024 cm-2) AGN are so important?

Many of these sources could be optically elusive

Hunting for Optically Elusive AGNs: the case of the merging system Arp 299

IC 694IC 694 NGC 3690NGC 3690

~22'‘ = 4.6 kpc~22'‘ = 4.6 kpc

(Alonso-Herrero et al. 2000)(Alonso-Herrero et al. 2000)

LLFIRFIR = 2.86 · 10 = 2.86 · 101111 L LSUNSUN

Optical and mid-/far-IR:Optical and mid-/far-IR:

LINER and/or starburstingLINER and/or starbursting

BeppoSAX observations:

NNHH = 2.5 · 10 = 2.5 · 102424 cm cm-2-2

LL(0.5-100 keV)(0.5-100 keV)= 1.9 · 10= 1.9 · 104343 erg s erg s-1-1

6.4 keV Fe-K6.4 keV Fe-Kaa: : EEem.lineem.line = 6.35 = 6.35 eVeV

EW = 636 eV but EWEW = 636 eV but EWtransmittedtransmitted ~ 7 keV ~ 7 keV

(Della Ceca et al. 2002, ApJL, 581, 9)

Fe-KaFe-Ka6.4 keV6.4 keV

thermal bumpthermal bump

big bump E>10 keVbig bump E>10 keVD = 44 Mpc

Hard (>10 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 ?

INTEGRAL/SWIFT AGN surveys

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

4 Compton Thick AGN

resolved ~few% of the hard (~10-50 keV) CXB

• INTEGRAL IBIS Survey (Bassani et al., 2006)(Bassani et al., 2006) sensitivity limit (20-100 keV): ~1.5x10sensitivity limit (20-100 keV): ~1.5x10-11 -11 cgs cgs

At the flux limit: - 49 E.L.AGN (41 with At the flux limit: - 49 E.L.AGN (41 with NH) - 5 - 5 Unidentified

5 Compton Thick AGN

• INTEGRAL IBIS Survey (Sazonov et al., 2006)(Sazonov et al., 2006) sensitivity limit (17-60 keV): ~7x10sensitivity limit (17-60 keV): ~7x10-11 -11 cgs cgs (75% of Sky at |b|>5)(75% of Sky at |b|>5) : ~4x10: ~4x10-11 -11 cgs cgs (50% of Sky at |b|>5)(50% of Sky at |b|>5)

Complete sample (SNR>5, |b|>5): - 66 E.L.AGN (60 with Complete sample (SNR>5, |b|>5): - 66 E.L.AGN (60 with NH) - 7 - 7 Unidentified

4 Compton Thick AGN

INTEGRAL/SWIFT AGN surveys

• INTEGRAL IBIS AGN Survey (Beckmann et al., 2006)(Beckmann et al., 2006) sensitivity limit (20-40 keV): ~3x10sensitivity limit (20-40 keV): ~3x10-11 -11 cgs cgs (76% of Sky)(76% of Sky) : ~1x10: ~1x10-11 -11 cgs cgs (17% of Sky)(17% of Sky)

Complete sample (SNR>5): - 38 E.L. AGN (32 with Complete sample (SNR>5): - 38 E.L. AGN (32 with NH) - 8 - 8 Unidentified (but at low |b|)

3 Compton Thick AGN

Compton Thick AGN selected above 10 keV

8 Compton Thick AGN in total from statistically complete sample !!!

CT Fraction = (5 – 20)%

10-40 keV

Fx=10

-11 c

gs

Compton Thick AGN detected above 10 keV

Complete samples + pointing

observations

16 Compton Thick AGN in total!!!

10-40 keV

Fx=10

-11 c

gs

Broad band spectra: NGC4945 and NGC1068

Guainazzi et al 2000

BeppoSAX

MECS+PDS

Normalized to the Crab spectrum (~2)

NGC 4945 NH~2x1024 cm-2

L10-40~3x1042 cgs

NGC 1068 NH>1025 cm-2

L10-40>5x1041 cgs

NH~2x1024 cm-2

L10-40~1x1043 cgs

Comastri et al., 2007

Broad band spectra: NGC 5728

Primary PL component

Reflected component

Scattered component

Fe lines

SUZAKU

XIS+HXD/pin

Candidate CT AGN detected below 10 keV

CT AGN candidate having a prominent (EW > 800 eV) Iron

Line

Redshift

L2

-10

keV(o

bserv

ed

)

21 objects ASCA,BeppoSAX,XMM

Fx=10

-13 c

gs

2-10 keV

Candidate CT AGN detected below 10 keV

CT AGN Candidate in the CDFS

Redshift

L2

-10

keV(o

bserv

ed

)

CT AGN candidate having a prominent (EW > ~800 eV) Iron

Line

21 objects

21 objects

2-10 keV

ASCA,BeppoSAX,XMM

Fx=10

-13 c

gs

Fx=10

-15 c

gs

We do not see the absorption cut-off only a lover limit on NH

We do not know Lxintrinsic for 90% of these sources!!!!

Compton Thick AGN detected above 10 keV

Complete samples + pointing

observations

16 Compton Thick AGN in total!!!

10-40 keV

Fx=10

-11 c

gs

Comparison with AGN Compton Thin (NH<1024 cm-2)

From La Franca et al., 2005

508 AGN

NH<1022

1022<NH<1024

307 201

Good coverage of the Lx-z plane up to z~2

What can we do with SIMBOL-X?

AccuracyNH 5% 0.5%NormPL 10%NormREFL

30%NormSCATT 5%

AccuracyE6.4,6.7 1%Norm 15%

Counts: ~ 11000 (MPD) ~ 8000 (CZT)

NH ~3x1024 cm-2; z=0.2

F10-40~10-11 cgs F2-10~5x10-13 cgs

Exp = 100Ksec

Iron K line

Iron K line

The Compton Thick AGN Universe

Fx=10

-11 c

gs

According to the CXB models

~40 CT AGN in the sky at |b|

>20

Possible SIMBOL-X targets:

a) Well known CT AGN from hard Xb) Infrared Bright Local Galaxies

0.007 0.1

What can we do with SIMBOLX?

NH ~3x1024 cm-2 ; z=0.5

Counts: ~ 1500 (MPD) ~ 800 (CZT)

AccuracyNH 10% 3%NormPL 20%NormREFL unc.NormSCATT 10-20%E6.4 1%Norm6.4 30-50%

F10-40~10-12 cgs F2-10~10-13 cgs

Exp = 100Ksec

The Compton Thick AGN Universe

Fx=10

-12 c

gs

~1500 CT AGN in the sky at |b|

>20

0.02 0.5

Possible SIMBOL-X targets:

a) Candidate CT from 2-10 keV data already known from bright 2XMM sources candidateb) Infrared Bright Local Galaxiesc) ULIRGs

What can we do with SIMBOLX?

NH ~3x1024 cm-2 ; z=1.5

Counts: ~ 350 (MPD) ~ 150 (CZT)

AccuracyNH 20-40% 10%NormPL within a factor 2

F10-40~10-13 cgs F2-10~3x10-14 cgs

Exp = 100Ksec

The Compton Thick AGN Universe

Fx=10

-13 c

gs

~2x106 CT AGN in the sky at |b|

>20

Possible SIMBOL-X targets:

a) Candidate CT AGN Spitzer/Hershel surveys b) ULIRGs

0.06 1.5

What about the CT AGN with NH> 1025 cm-2

Counts: ~ 11000 (MPD) ~ 8000 (CZT)L10-40~1045 cgs; z=0.2

Counts: ~ 1300 (MPD) ~ 500 (CZT)NH > 1025 cm-2; z=0.2

Counts: ~ 270 (MPD) ~ 150 (CZT)NH > 1025 cm-2; z=0.5

F10-40~10-11 cgs; NH ~3x1024cm-

2

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

(z~1.5-2.0)

Summary and conclusion

THANKS