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

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

Active Galactic Nucleus

AGN Zoology Optical Emission Line Properties Radio Loudness Narrow Lines Broad Lines Unusual Radio Quiet Seyfert 2 Seyfert 1 QSO Radio Loud NLRG:-FR I -FR II BLRG SSRQ FSRQ Blazars

AGN Unified Model Urry & Padovani 1995

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?)

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

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

X-ray Background

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

Absorption in X-rays Manners, 2002

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

XRB Models Gilli et al, 2001

XRB Redshift Distribution Hasinger, 2002

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

CIRB Spectrum Franceschini et al, 2001

Type 2 AGN SED Norman et al, 2002

AGN Contribution Fadda et al, 2002

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.

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).

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 Field RA Dec E(B-V) 100 um NH HDF-S 22:32:35.6 -60:47:12 0.03 1.37 1.6E+20 CDF-S 03:32:29.0 -27:48:47 0.01 0.40 1030+05 10:30:27.1 05:24:55 0.02 1.01 2.3E+20 1256+01 12:55:40 01:07:00 0.81

Expected Data Optical Near-IR Band Area Vega AB U 36’x36’ 25.8 26.5 B 26.7 V R 26.3 I 25.1 25.5 z 24.5 25.0 NB4990 Band Area Vega AB J (wide) 30’x30’ 22.5 23.4 J (deep) 10’x10’ 23.2 24.1 H(wide) 21.5 22.9 H(deep) 23.9 Ks(wide) 20.5 22.3 Ks(deep) 23.3

Existing Data Band HDFS CDFS 1030+05 1256+01 U 100% 0% 70% B 85% V 28% R 71% I 57% 30% z 66% 33% J (deep) J (wide) 38% 25% 13% H (deep) H (wide) K (deep) K (wide)

GOODS Optical Data Band Area Depth F435W (B) 10’x16’ 27.9 F606W (V) 28.2 F775W( i ) 27.5 F850LP(z) 27.4 Band Area Depth U 36’x36’ 27.3 J 10’x15’ 25.2 H 24.7 Ks 24.4

GOODS Data Summary Dickinson et al 2002

Number Counts Chile-Yale GOODS

Comparison With Other Surveys

Comparison With Other Surveys

Data Analysis Data Modeling 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. Data Modeling Synthetic model to produce observed integral backgrounds, XRB and CIRB.

Schedule

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.