The multiwavelength surveys of the ELAISS1 and GOODS fields

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The multiwavelength surveys of the ELAIS-S1 and
GOODS fields
Fabrizio Fiore M. Brusa, A. Comastri, C.
Feruglio, A. Fontana, A. Grazian, F. La Franca,
P. Santini, E. Piconcelli, S. Puccetti and many
others
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GOAL

• AGN Bolometric Luminosity function
• Complete SMBH census
• Strong constraints to models for the formation
  and evolution of structure in the Universe

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Co-evolution of galaxies and SMBH

• Two seminal results
• The discovery of SMBH in the most local bulges
  steep and tight correlation between MBH and bulge
  properties.
• The BH mass density obtained integrating the AGN
  L.-F. and the CXB that obtained from local
  bulges

? most BH mass accreted during luminous AGN
phases! Most bulges passed a phase of
activity Need to understand AGN physics and
evolution to fully understand galaxy evolution
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Why multiwavelength surveys

• X-ray surveys
• very efficient in selecting unobscured and
  moderately obscured AGN
• Miss most highly obscured AGN

La Franca et al. 2005
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2-10 keV AGN luminosity function models
Solid observed dashed best fit
LDDE with constant NH distribution
La Franca et al.
2005
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Highly obscured Mildly Compton
thick INTEGRAL survey 100
AGN Sazonov et al. 2006
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2-10 keV AGN luminosity function models
2-10keV 0.5-2keV
LDDE with variable absorbed AGN fraction La
Franca et al. 2005, see the poster by Fabio La
Franca
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A working scenario
small mass progenitors. Feedback is effective in
self-regulating accretion and SF, cold gas is
left available
Galactic cold gas available for accretion and
obscuration increases at high z
Menci hierarchical clustering model, Menci,
Puccetti Fiore 2006
large mass progenitors. Feedback is less
effective, most gas is quickly converted in stars
at high z.
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• 1) Paucity of Seyfert like sources _at_ zgt1 is real?
  Or, is it, at least partly, a selection effect?
• Are we missing in Chandra and XMM surveys highly
  obscured (NH?1024 cm-2) AGN? Which are common in
  the local Universe

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Why multiwavelength surveys

• IR surveys
• AGNs even highly obscured at optical and X-ray
  energies shine in the MIR
• Very difficult to isolate AGN from passive and
  starforming galaxies (Lacy 2004, Barnby 2005,
  Stern 2005, Polletta 2006 and many others)

Polletta et al. 2006
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Why multiwavelength surveys

• Use both X-ray and MIR surveys
• Select unobscured and moderately obscured AGN in
  X-rays
• Add highly obscured AGNs selected in the MIR
• Simple approach Differences are emphasized in a
  wide-band SED analysis

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X-ray-MIR surveys

• CDFS-Goods MUSIC catalog (Grazian et al. 2006).
  Area 0.04 deg2
• 173 X-ray sources, 104 2-10 keV down to 3?10-16
  cgs, 109 spectroscopic redshifts
• 4300 MIPS sources down to 6.8 ?Jy, 3.6?m
  detection down to 0.08 ?Jy
• Ultradeep Optical/NIR photometry, R27.5, K24
• ELAIS-S1 SWIRE/XMM/Chandra survey (Puccetti et
  al. 2006, Feruglio et al. 2006). Area 0.5 deg2
• 500 sources, 205 2-10 keV down to 3?10-15 cgs,
  half with spectroscopic redshifts.
• 2600 MIPS sources down to 100 ?Jy, 3.6?m
  detection down to 6 ?Jy
• Relatively deep Optical/NIR photometry, R25,
  K19
• In future we will add
• COSMOS XMM/Chandra/Spitzer. Area 2 deg2 see
  Marcella talk
• CDFN-Goods. Area 0.04 deg2
• Etc.

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MIR selection
CDFS obs. AGN ELAIS-S1 obs. AGN
GOODS 24?m galaxies ELAIS-S1 24?m
galaxies Open symbols unobscured AGN Filled
symbols optically obscured AGN
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MIR selection
CDFS obs. AGN ELAIS-S1 obs. AGN
GOODS 24?m galaxies
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MIR AGNs
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F24?m/FR gt1000 R-Kgt4.5
F(0.3-1.5keV)10-17 cgs
F(1.5-4keV)10-17 cgs
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F24?m/FR gt1000 R-Kgt4.5

• 119 sources (3 of the MIPS sample)
• 17 detected by Chandra (9 2-10 keV band) 4 more
  visible in the image ltLXgt43.45/-0.24,
  ltNHgt22.9/-0.8, ltzgt2.1
• logF(1.5-4keV) stacked sources-17
• _at_z2 logLobs(2-8keV) stacked sources 41.8
• logltLIRgt44.6 gt logL(2-8keV) unabs.43
• Difference implies logNH?24
• ltSFR-IRgt400!!
• Msun/yr
• ltSFR-UVgt5!!
• Msun/yr
• ltSFR-Xgt65
• Msun/yr

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F24?m/FR gt1000 R-Kgt4.5
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F24?m/FR lt100 R-Kgt4.5
F(0.3-1.5 keV)2?10-17 cgs
F(1.5-4 keV) lt 5?10-18 cgs
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F24?m/FR lt100 R-Kgt4.5

• 125 sources (3 of the MIPS sample)
• 29 detected by Chandra, 19 2-10 keV,
  ltLXgt43.4/-0.4 ltNHgt23.2/-0.6, ltzgt1.4
• ltSFR-IRgt 8 Msun/yr
• ltSFR-UVgt 2.6 Msun/yr
• ltSFR-Xgt20 Msun/yr

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Summary

• XMM Chandra surveys can probe unobscured and
  moderately obscured accretion up to z2-4
• INTEGRAL/Swift find highly obscured AGN up to
  z0.1
• Spitzer finds highly obscured AGN at z1-3
• Herschel will further increase the band, so
  helping in separating AGN from normal galaxies
  and pushing toward higher z.
• During the next decade highly obscured AGN will
  be confirmed and studied in detail using hard
  X-ray focusing telescopes.
• All this will allow a precise determination of
  the evolution of the accretion in the Universe
  and a precise census of accreting SMBH.

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MIR selected vs. X-ray selected AGNs