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

This thesis aims to unravel the mysteries surrounding Active Galactic Nuclei (AGN) and their impact on cosmic X-ray and Infrared backgrounds. Through detailed analyses and modeling, the study seeks to expand our understanding of the diverse AGN population and their contributions to the observed backgrounds. By leveraging data from surveys like Chile-Yale Wide-Deep Survey and Great Observatories Origin Deep Survey (GOODS), the research focuses on elucidating the behavior and characteristics of AGN, especially Type 1 and Type 2 AGNs, to enhance redshift distributions and luminosity functions. Through a combination of observational data and theoretical models, the thesis aims to shed light on the fundamental properties of AGNs and the Unified Model.

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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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