G

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The X-ray background and the evolution of AGN

• Günther Hasinger, MPE Garching TUM

Active Galactic Nuclei From Atoms to Black
Holes, Hagai-Fest Tel Aviv, February 22, 2006
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Collaborators
CDFS J. Bergeron, S. Borgani, A. Finoguenov, R.
Giacconi, R. Gilli, R. Gilmozzi, K. Kellerman, L.
Kewley, A. Koekemoer, I. Lehmann, V. Mainieri, M.
Nonino, C. Norman, M. Romaniello, P. Rosati, E.
Schreier, A. Streblyanskaya, G. Szokoly, P.
Tozzi, J.X. Wang, W. Zheng, A. Zirm E-CDFS V.
Mainieri, D. Alexander, F. Bauer, E. Bell , J.
Bergeron, W. Brandt, E. Fomalont, R Gilli, K.
Kellermann, A. Koekomoer, B. Lehmer, T. Miyaji,
H.W. Rix, P. Rosati, D. Schneider, J. Silverman,
G. Szokoly, P. Tozzi, L. Wisotzki Lockman Hole
X. Barcons, H. Böhringer, H. Brunner, A. Fabian,
A. Finoguenov, Y. Hashimoto, P. Henry, I.
Lehmann, V. Mainieri, S. Mateos, I. Matute, M.
Schmidt, A. Streblyanskaya, G. Szokoly, M.
Worsley COSMOS H. Böhringer, H. Brunner, M.
Brusa, N. Cappelluti, A. Comastri, M. Elvis, A.
Finoguenov, F. Fiore, A. Franceschini, R. Gilli,
R. E. Griffiths, C. Impey, I. Lehmann, S. Lilly,
V. Mainieri, G. Matt, I. Matute, T. Miyaji, S.
Molendi, S. Paltani, D. B. Sanders, N. Scoville,
J. Silverman, L. Tresse, M. Urry, P. Vettolani,
G. Zamorani XLF XrB Model A. Comastri, R.
Gilli, T. Miyaji, M. Schmidt, Y. Ueda
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Contents

• The X-ray Background
• X-ray luminosity function
• Future Surveys

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X-ray Background Spectrum
Worsley et al., 2004
Courtesy Brusa, Comastri, Gilli
gt Elt2keV XRB resolved at Egt5keV still very much
work to do!
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XMM Slew
CLASXS
N. Brandt G.H. 2005, ARAA 43, 827
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Ultra Deep Field
2.28p AGN - opt. faint
1.216 AGN - Ty 1, unobs
0.665 AGN - XBONG
0.773 AGN - XBONG
1.82p AGN - opt. faint
1.65p AGN - opt. faint
CDF-S ACS UDF
1.69p AGN - opt. faint
0.456 Starburst
3.193 AGN - Ty 1, unobs
1.309 AGN - XBONG
4.29p AGN - opt. faint
0.438 Starburst
3.064 AGN - Ty 2
Courtesy S. Beckwith
0.414 Starburst
1.53p AGN - opt. faint
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Chandra Deep Field IDs
CDFN Triangles CDFS Squares dot
unidentified 0ltzlt0.5 0.5ltzlt1 1ltzlt2 2ltzlt6
Brandt G.H. 2005
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LX vs. redshift
CDFN Triangles CDFS Squares I15-20 I20-22 I2
2-23 Igt23
Brandt G.H. 2005
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CDFS Optical IDs
Szokoly et al., 2004 (FORS spectro-z) Wolf et
al., 2004 (2.2m Combo-17) Zheng et al.,
2004 Mainieri et al., 2004 (FORS/ISAAC photo-z)
Number of Sources
Redshift
gt 95 have spectro- or photo-z thanks to VLT,
GOODS, GEMS, ACF UDS etc. Photo-z at higher z,
but all peak at z0.7
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Lockman Hole
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Pink Sources
LH 901
COSMOS 2608
Compton-thick spectra!
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X-ray Background average rest-frame spectra
800 ksec XMM-Newton Observation of the Lockman
Hole
Large equivalent width can be explained by 3 x
solar metallicity. BH spin within reach.
Good news for Next Generation X-ray Observatory !
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Optically identified hard samples
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Type 2 fraction f(LX)
Local Seyferts
Fraction of type-2s decreses with
luminosity. Strong unified model does not hold!
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Type 2 fraction f(z)
No significant evolution in absorption fraction
detected
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Contents

• The X-ray Background
• X-ray luminosity function
• Future Surveys

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Multi-Cone Surveys

• Type-1 AGN in the 0.5-2 keV band
• Continuation of ROSAT work, most sensitive
  complete
• ROSAT Samples (Miyaji et al., 2000)
• ROSAT Bright Survey 203 (0) AGN (Schwope et
  al., 2000)
• RASS Selected North 134 (5) AGN (Appenzeller
  et al., 1996)
• RASS NEP Survey 101 (9) AGN (Gioia et
  al., 2003)
• RIXOS serendipitous 194 (14) AGN (Mason et
  al., 2000)
• ROSAT Deep Surveys 84 (7) AGN (e.g. Schmidt
  et al., 1998)
• XMM Deep Survey (Mainieri et al., 2002)
• Lockman Hole 48 (8) AGN
  (Lehmann et al., 2001 )
• Chandra Deep Surveys
• CDF North/HDF-N 67 (21) AGN (Barger et
  al., 2003)
• CDFS spec.phot. 113 (1) AGN
  (Szokoly, Zheng et al. 2003)
• Total 944 (65) AGN1

Yellow unidentified
G.H., Miyaji Schmidt, 2005, AA 441, 417
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XLF0.5-2 keVtype-1 AGN
Luminosity-dependent density evolution (LDDE)
confirmed
G.H., Miyaji Schmidt, 2005, AA 441, 417
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Comparison X-ray/SDSS
type-1 soft X-ray selected AGN (G.H., Miyaji,
Schmidt, 2005) Optically selected SDSS QSOs
(Richards et al., 2005)
LXLopt0.9
X-ray survey sample a much wider range of
luminosities !
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Direct comparison of hard vs. Soft XLF
m2
m1
Gilli, Comastri G. H., 2006
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Space/Luminosity density evolution
G.H., Miyaji Schmidt, 2005
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Densities in soft and hard band
Brandt G.H., 2005
G.H., Miyaji Schmidt, 2005 Ueda et al., 2003,
based on 1000 AGN-1 based on 250 AGN
Very similar behaviour in hard and soft band.
Soft samples go deeper and are more complete.
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Most recent Population Synthesis Model
total
type-1 C-thin
type-2 C-thick
type-2 C-thin
Gilli, Comastri G.H., 2006
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Local BH mass vs. accreted BH mass function

• Accreted Black Hole mass function derived from
  X-ray background can be compared with the mass
  function of dormant relic black holes in local
  galaxies (Soltan 1982).
• These two estimates can be reconciled, if an
  energy conversion efficiency of e0.1 is assumed.
  Such high efficiency requires a Kerr-BH!

l Eddington Ratio ?
Schwarzschild Kerr
e Conversion efficiency ?
Marconi et al., 2006, MNRAS
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Contents

• The X-ray Background
• X-ray luminosity function
• Future Surveys

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High-z QSO
Wall et al., 2005 Hiigh luminosity QSO

• Radio QSO (Wall et al., 2005)
• Soft X-ray ROSAT/Chandra/ XMM (G.H., Miyaji
  Schmidt 2005)
• Chandra/ROSAT(Silverman et al. 2004)
• Optical QSOs (Schmidt et al., 1995, Fan et al.
  (2001,2004)

Very large solid angle deep surveys required to
study zgt5 QSOs E-CDFS XMM/COSMOS eROSITA
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XMM-Newton Cosmos Survey
1.5 degrees
HST PI N. Scoville (Caltech) XMM-Newton 1.4
Msec, PI G. H.
Courtesy Cappelluti, Finoguenov
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X-ray color-color diagnostic
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COSMOS Redshift distribution
50 redshifts from the literature (mainly
SDSS) 40 redshifts from zCOSMOS (Lilly et al.,
2006) 150 redshifts from Magellan IMACS (Impey
et al., 2006) Compilation in Brusa et al., 2006
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eROSITA
Dark Universe Observatory
Study launch on Russian SRG platform from Kourou
into equatorial orbit
Lobster
ROSITA
XMM pn
ROSITA (on-axis)
ART
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1yr
2yr
eROSITA
½yr
100000 clusters 1 Mio AGN expected 20 with
zgt7
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Summary

• X-ray background practically resolved below 2 keV
• At 2-10 keV about 50 resolved still work to do
• Type-2 QSOs found, type-2 fraction decreases with
  LX
• Background AGN have strong relativistic Fe line
• Luminosity-dependent density evolution
• Seyferts peak much later than QSO
• Anti-hierarchical evolution not predicted even by
  most recent semi-analytic models
• Wider deep surveys for high-z QSO have started,
  good prospects for eROSITA
• gt Need (at least) 2 modes of BH accretion
• Role of re-triggering through stellar
  evolution?

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Thank you very much!
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X-ray vs. optical LF
0.40ltzlt0.68 0.68ltzlt0.97 0.97ltzlt1.25 1.25ltzlt1.53 1.
53ltzlt1.81 1.81ltzlt2.10
Miyaji, 2005, priv. comm
2dF QSO LF severely incomplete at low
luminosities! See also Richards et al., 2005
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SDSS Comparison
T. Miyaji, priv. comm. See also poster G.11