heavily obscured agn with integral/swift/xmm/chandra: prospect for simbol-x
DESCRIPTION
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) Caccianiga (INAF-OABrera, Italy) V. Braito (John Hopkins Univ. NASA/GSFC,USA) - PowerPoint PPT PresentationTRANSCRIPT
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