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The Space Density of Compton Thick AGN

The Space Density of Compton Thick AGN. Erin Bonning (Yale) On behalf of Ezequiel Treister (ESO). Meg Urry (Yale) Shanil Virani (Yale) and others. Compton Thick AGN. Defined as obscured sources with N H >10 24 cm -2 . Very hard to find (even in X-rays).

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The Space Density of Compton Thick AGN

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  1. The Space Density of Compton Thick AGN Erin Bonning (Yale) On behalf of Ezequiel Treister (ESO) Meg Urry (Yale) Shanil Virani (Yale) and others

  2. Compton Thick AGN • Defined as obscured sources with NH>1024 cm-2. • Very hard to find (even in X-rays). • Observed locally and needed to explain the X-ray background. • Number density highly uncertain. • High energy (E>10 keV) observations are required to find them.

  3. INTEGRAL Survey • PIs: MegUrry, ShanilVirani, Ezequiel Treister • Exp. Time (Msec): 0.7 (archive)+1.5 (2005)+ 1 (2008). Deepestextragalactic INTEGRAL survey • Field: XMM-LSS (largestXMM field) • Flux limit: ~4x10-12ergs cm-2 s-1(20-40 keV) • Area: ~1,000 deg2 • Sources: ~20 • Obscured AGN: ~15 (~5 Compton-thick)

  4. INTEGRAL Mosaic (2.2 Ms) Significance Image, 20-50 keV

  5. Exposure Map Maximum depth: 2.2 Ms (inner contour)

  6. INTEGRAL Flux Limit vs. Exposure Time Flim t–1/2

  7. MCG-02-08-014 INTEGRAL Mosaic (2.2 Ms) Significance Image, 20-50 keV

  8. MCG-02-08-014 • z=0.0168 • Optical class: Galaxy • IR source (IRAS) • Radio source (NVSS) • Narrow line AGN • (based on OIII emission) • No soft X-rays (ROSAT) • Good CT AGN candidate

  9. INTEGRAL AGN logN-logS Beckmann et al. 2006 Treister et al, submitted

  10. Space Density of CT AGN X-ray background does not constrain density of CT AGN Treister et al, submitted

  11. Treister & Urry, 2005 CT AGN and the XRB XRB Intensity HEAO-1 +40% Treister et al, submitted

  12. Treister & Urry, 2005 Gilli et al. 2007 CT AGN and the XRB XRB Intensity HEAO-1 Original HEAO-1 +10% HEAO-1 +40% Treister et al, submitted

  13. Treister & Urry, 2005 Gilli et al. 2007 Most likely solution CT AGN Space Density CT AGN and the XRB XRB Intensity HEAO-1 Original HEAO-1 +10% HEAO-1 +40% Treister et al, submitted

  14. X-ray Background Synthesis

  15. Summary • INTEGRAL (& Swift) give important constraints on Compton Thick AGN (at z=0) • X-ray “background” synthesis OK • (but XRBG spectrum somewhat uncertain) • Reflection component normalization ~ 1 • (agrees with spectra) • Deeper surveys probe evolution to z~1

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