1. 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)

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 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

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
Radio
far-IR
X-rays
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 ( microns)
Far IR ( 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
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
10:30:27.1
05:24:55
0.02
1.01
2.3E+20
12:55:40
01:07:00
0.81

22. 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

23. 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)

26. 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

27. GOODS Data Summary
Dickinson et al 2002

30. Number Counts
Chile-Yale
GOODS

31. Comparison With Other Surveys

32. Comparison With Other Surveys

33. 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.

34. Schedule

35. 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.