Robust identification of distant Compton-thick AGNs

1. 1Ms simulated XEUS spectrum Optical AGN Robust identification of distant Compton-thick AGNs IR AGN Alexander et al. (2008) Need for deep optical-mid-IR spectroscopy: multiple lines of evidence for intrinsic AGN luminosity can make a case for distant Compton-thick absorption X-rays

2. Enhanced AGN Activity in a z=3.09 Protocluster David M Alexander, Bret Lehmer, Jim Geach (Durham) With Franz Bauer, Scott Chapman, Yuichi Matsuda, Ian Smail, Toru Yamada, amongst others

3. Broad Range of blank-field X-ray Surveys Murray et al. (2005) 5 ks NOAO DWFS now also 2Ms! Brandt & Hasinger (2005) 2 Ms CDF-N CDFN: LX~3x1040 erg/s at z~0.5; LX~1042 erg/s at z~2 (almost 100x deeper than Bootes but 100x larger) Alexander et al. (2003)

4. Evolution of AGNs from blank-field surveys Ueda et al. (2003) Hasinger et al. (2005) But what causes this “AGN downsizing”? What “drives” the growth of black holes? Fiore et al. (2003) Luminosity-dependent density evolution (LDDE): high-luminosity AGNs (i.e., quasars, such as those found by SDSS) peaked at higher redshifts than more typical AGNs

5. z=3.09 SSA22 protocluster A key laboratory of black-hole growth mechanisms: a distant protocluster? 400ks Chandra exposure of SSA22 Predicted to become a massive Coma-like cluster by the present day PI: D.M. Alexander The galaxy density is ~6x higher than the field already at z~3.09

6. First insight into AGN activity in a Distant Protocluster Bret Lehmer Many more obscured quasars in protocluster (400ks; blue) than found in field (2Ms; red) at z~3 Lehmer, Alexander, et al., in prep

7. Enhanced black-hole growth compared to the field LAEs LBGs Lehmer, Alexander, et al., in prep But is the shift in the x-axis or the y-axis? AGN fraction suggestively larger than found in the field (by a factor of ~3.4)

8. Shift may be in the x-axis: larger black holes? Steidel found that galaxies in a z=2.3 protocluster are more massive: if the same is found in SSA22 then this may imply that the black holes are larger Steidel et al. (2005) Implication: the characteristic X-ray luminosity and “active” black-hole mass may be a function of environment as well as redshift

9. Role of Environment? LAE density image Yamada et al., in prep Protocluster structure extends over 100+ Mpc region (1+ deg) and has variations in galaxy density: require more X-ray observations to explore the effect of galaxy density on enhanced AGN activity

10. Extended lyman-alpha outflows: AGN or star-formation powered? Jim Geach Geach, Alexander, et al., in prep 5/29 extended lyman-alpha objects are X-ray detected: considerably higher source density than radio galaxies Mbh/Msph~10-3 z=2.16 Lyman-alpha outflow: PKS1138-262 radio gal Do outflows forge this M-sigma relationship?

11. Lower luminosity (but much more typical) AGN outflows than found in radio galaxies? IFU constraints on outflow kinematics of PKS1138-262 High-z radio gals Nesvadba et al. (2006) Geach, Alexander, et al., in prep Require high-quality integral field unit observations (we have FLAMES observations in optical) to spatially resolve kinematics and test whether accretion-related outflows are a widespread phenomena

12. Summary • Compton-thick AGNs are very difficult to identify in the local Universe let alone at z~2: detailed observations are required to identify individual sources to strengthen the case for the “missing” distant Compton-thick AGN population • 400ks Chandra observation of z=3.09 SSA22 protocluster to explore AGN activity (black-hole growth) in an overdense environment: a laboratory on what drives black-hole growth • AGN fraction in galaxies higher than found in the field: large fraction are obscured quasars - longer AGN duty cycle OR higher characteristic AGN luminosity than found in field (Lehmer et al.)? • Some of the AGNs are associated with large-scale outflows (Ly-alpha): X-ray-Ly-alpha luminosity ratios similar to high-redshift radio galaxies but >1 order of magnitude less luminous: tentative evidence for accretion-related outflows in “typical” AGNs in the distant Universe (Geach et al.)? • Require more extensive observations of SSA22 to explore wider role of environment (galaxy density) on AGN activity - is this the primary driver for black-hole growth?

13. Role of Environment: Blank-field Surveys? Lehmer & Alexander AGNs from COSMOS compared to galaxies from GOODS Need: (1) large area (trace full range of environments), (2) large number of sources (explore the key parameters), and (3) good sensitivity (to trace dominant AGN at each epoch): e.g., 10 galaxy density bins, 5 redshift bins, 5 luminosity bins, 2 large-scale structure (clusters vs non clusters), and >10 objects/bin>10000 AGNs

14. Prospects for a Wide-Area XMM Proposal? Cosmological simulation of z~1 regions in 2 sq deg field

15. The Wide-Deep XMM-Newton Survey Proposal 3 Ms Proposal Failed Last Round: to give 10 sq deg at 50ks • Survey Parameters: • ~50 ks exp in 5 fields (9 pointings/sq deg) with IR-submm data (7.1 sq deg but total of 10 sq deg when combined with existing data) • Wide RA range eases stress on XMM scheduling and follow-up • f(0.5-2keV)~5x10-16 erg/s/cm2; f(2-10keV)~3x10-15 erg/s/cm2 • Sensitivity limits: 1.6x1043 erg/s (rest-frame 4-20 keV) at z~1; about order of magnitude higher at z~3 (trace AGN “downsizing”) • Source Statistics: • ~10000 X-ray AGNs; ~1000 with >100 counts (basic X-ray spectra) • ~500 z>3 quasars (obscured and unobscured) and ~10 at z>6 • ~100-150 Compton-thick AGNs (ID’d from SEDs) • ~80-160 X-ray starbursts • ~300-400 clusters (~30 with M>1014 solar masses; ~20-30 at z>1) Many possible science goals