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The AGN Population and Its Contribution to the X-ray and IR Backgrounds

The AGN Population and Its Contribution to the X-ray and IR Backgrounds. Ezequiel Treister Advisors: Meg Urry (Yale) Jos é Maza (U. de Chile). Outline. Introduction - Active Galactic Nuclei - Cosmic X-ray Background - The IR Background

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The AGN Population and Its Contribution to the X-ray and IR Backgrounds

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  1. The AGN Population and Its Contribution to the X-ray and IR Backgrounds Ezequiel Treister Advisors: Meg Urry (Yale) José Maza (U. de Chile)

  2. Outline • Introduction - Active Galactic Nuclei - Cosmic X-ray Background - The IR Background • The Thesis - Goals - Data • Schedule

  3. Active Galactic Nucleus

  4. AGN Zoology

  5. AGN Unified Model Urry & Padovani 1995

  6. Unified Model Type 1 AGNs: - Broad Emission Lines - Blue optical continuum - Radio Loud if viewing angle is small Type 2 AGNs: - Obscuration in the optical/UV and soft X-rays - Narrow Emission Lines - Radio Quiet - Obscured by the Equatorial Dust Torus Fundamental Parameters: - Black Hole Mass (host galaxy mass) - Mass Accretion Rate (AGN Luminosity) - Black Hole Spin (Merger history?)

  7. Type 1 AGN SED X-rays mm far-IR near-IR Optical-UV Manners, 2002

  8. Type 2 AGN SED X-rays Radio far-IR optical-UV Norman et al, 2002

  9. X-ray Background

  10. AGN SED in X-rays Type 1 AGN Mainieri et al, 2002

  11. Absorption in X-rays Manners, 2002

  12. Type 2 AGN X-ray Spectrum NH=3x1023 cm-2 Mainieri et al, 2002

  13. XRB Models Gilli et al, 2001

  14. XRB Redshift Distribution Hasinger, 2002

  15. Cosmic IR Background Near IR (1.5-3.5 microns) Far IR (50-250 microns)

  16. CIRB Spectrum Franceschini et al, 2001

  17. Type 2 AGN SED Norman et al, 2002

  18. AGN Contribution Fadda et al, 2002

  19. The Thesis GOALS • Understand how AGN primary radiation in the UV and X-ray • wavelength range and re-radiation (in the far IR) combine to • produce the observed “backgrounds” or integrated light, that • have defied explanation for more than 30 years. • Improve Luminosity Functions, Redshift distributions and • evolution of Type 2 AGN, increasing the number of sources at • high redshift (z~2), population often missed by large area/shallow • surveys.

  20. Thesis Data • Chile-Yale Wide-Deep Survey: - 1 square degree in 4 30’x30’ fields evenly distributed in RA. - leveraging existing data. - 2 equatorial fields for northern hemisphere access. • Great Observatories Origin Deep Survey (GOODS): - 0.1 square degrees in 2 10’x16’ fields. - Fields are HDF-N and CDF-S. - SIRTF Legacy Program (PI: Dickinson). - HST Treasury Program (PI: Giavalisco).

  21. Chile-Yale Wide-Deep Survey • Ground Based Optical Coverage: CTIO 4m MOSAIC, ESO WFI. • Ground Based Near-IR imaging: CTIO 4m ISPI. • X-ray Data: XMM, Chandra. • Infrared Data: SIRTF IRAC+MIPS. • Follow-up Spectroscopy: VLT: VIMOS, FORS2 Magellan: IMACS FIELDS

  22. Expected Data Optical Near-IR

  23. Existing Data

  24. GOODS Optical Data

  25. GOODS Data Summary Dickinson et al 2002

  26. GOODS Chile-Yale Number Counts

  27. Comparison With Other Surveys

  28. Comparison With Other Surveys

  29. Data Analysis GOODS: - Candidate selection + slit design for spectroscopy runs (VIMOS). - Spectroscopic data reduction. Chile-Yale Wide-Deep Survey: - Optical Data Acquisition. - Optical Data Reduction. - Candidate selection + slit design for spectroscopy runs. - Spectroscopic data reduction. Data Modeling • Synthetic model to produce observed integral backgrounds, XRB and • CIRB.

  30. Schedule

  31. Summary My Thesis will: • Enlarge the sample of obscured AGN at high redshift. • Provide better constrains on the contribution of obscured AGN to the X-ray and Infrared Backgrounds. • Generate Luminosity Functions up to z~2 for Type II AGN. • Tell us more about the physics of AGN and the unified model by combining observations with model.

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