1. Clustering of QSOs and X-ray AGN at z=1 Alison Coil Hubble Fellow University of Arizona October 2007 Collaborators: Jeff Newman, Joe Hennawi, Marc Davis, Paul Nandra, Antonis Georgakakis

2. Main Points 1.Different QSO/AGN formation theories predict different clustering properties - amplitude as f(z,L). Clustering constrains models (even w/ current error bars). 2.Clustering constrains the mass of the host DM halo and host galaxy type and timescale between evolutionary stages. 3.Cross-correlating with large samples of galaxies rather than using QSO/AGN samples alone gives small errors - both Poisson and cosmic variance - and allows measures on small scales. Only need selection function of galaxies, not AGN. 4.Results: QSOs cluster like blue/star-forming galaxies, not red galaxies, at z~1. 5.Results: X ray-selected AGN cluster like red galaxies at z~1 (more clustered than QSOs).

3. Clustering Information What you can learn from clustering: close pairs / interactions / mergers radial profiles of galaxies/AGN w/in halos host dark matter halo mass halo occupation distribution function what kinds of galaxies host AGN trace evolving populations through different z’s connect different samples and z’s constrain timescales between different evolutionary stages compare with AGN formation and evolution models Very helpful to know clustering of galaxies at the same redshift, in the same volume, as a function of color/luminosity.

4. Galaxy Clustering: Luminosity, Color Brighter r 0 > Fainter r 0 + Redder r 0 > Bluer r 0 At z=0 and z=1 z=0.9: (for ~L* galaxies:) red red: r 0 =5.2 Mpc/h  =2.0 b=1.6 M min =2 10 12 M o /h blue: r 0 =3.8 Mpc/h  =1.7 b=1.3 M min =5 10 11 M o /h Coil et al 2006 Coil et al 2008 clustering amplitude separation - r p luminosity color

5. QSO+AGN clustering - z~1 DEEP2 is a completed redshift survey using the Keck II telescope, covering multiple fields on the sky (for cosmic variance) to study galaxy evolution and LSS at z=0.7-1.5. Sample is selected to R=24.1. DEEP2 has a high sampling rate (60%) and precise redshifts ( 40,000 galaxies in V~3x10 6 Mpc 3 /h 3. One field is the Extended Groth Strip (EGS), which has 8 Chandra pointings of 200 ks each over a 2 x 0.25 degree field. (Chandra team: K. Nandra, A. Georgakakis, E. Laird)

6. SDSS QSOs in DEEP2 fields 36 SDSS + 16 DEEP2 spectroscopic broad-line QSOs in the DEEP2 fields between z=0.7-1.4: SDSS DEEP2 (near M*) MBMB redshift

7. Clustering of Galaxies around QSOs Clustering of DEEP2 galaxies around SDSS QSOs at z=0.7-1.4. Errors include Poisson errors + cosmic variance (from mocks). Similar errors as surveys with 1000s of QSOs (eg. 2dF) through use of cross-correlation with 10,000s of galaxies. Divide by the clustering of DEEP2 galaxies around DEEP2 galaxies to get the relative bias of QSO hosts… Coil et al. 2007 ApJ separation 0.1 Mpc/h10 Mpc/h

8. Relative bias of QSOs to DEEP2 galaxies QSO relative bias = 0.9 (0.2) QSO absolute bias = 1.2 (0.3) Cluster like blue galaxies not red! Constrains host type for QSOs (blue) and QSO host halo masses: Min. halo mass = 5x10 11 M 0 /h Mean halo mass = 3x10 12 M 0 /h No dependence is seen on magnitude (M B =-22.8 vs -24.1) or redshift (z=0.7-1.0 vs 1.0-1.4) Coil et al. 2007 ApJ group clustering: M min = 6 x 10 12 M 0 /h r 0 =6.2 (0.4) Mpc/h  =1.5 (0.2)

9. Comparison w/ 2dF+SDSS: Our QSO clustering amplitude is ~1  lower than other results (with 20% errors). Done for free by having galaxy redshifts in SDSS QSO fields.

10. Clustering of X-ray AGN -24-16MBMB color red Nandra et al. 2006 ApJL Chandra survey in the EGS: 200 ks depth Have ~10,000 galaxies and ~250 (so far) X-ray sources w/ z=0.2-1.4 1/2 from DEEP2 (R=24.1) 1/2 from MMT (R=23) X-ray AGN hosts are bright and on red sequence or massive end of blue cloud. (even the faint ones: L x ~10 42-44 erg/s) Log Eddington ratio= -2.5 to -4.0 quasars z=0.7-1.4 blue

11. ACS Imaging of X-ray AGN ~60% of hosts have early- type morphologies (Pierce et al. 2007) Not dominated by major mergers but early-types do show more minor merger asymmetry than normal ellipticals (Georgakakis et al. 2007, submitted) (to my untrained eye, ~50% spheroids ~33% spirals ~10% mergers/Irr 9% blue point sources)

12. Clustering of X-ray AGN Split into 2 redshift bins: z=0.2-0.7 and z=0.7-1.4 X-ray AGN cluster like red galaxies, not blue galaxies, at both z~0.5 and z~0.9 Coil et al. in prep Relative bias of X-ray AGN to galaxies: z=0.7-1.4 red gals: 1.1 (0.1) blue gals: 1.7 (0.1) z=0.2-0.7 red gals: 1.1 (0.1) blue gals: 1.4 (0.1) Jacknife errors for now - will update w/ simulations

13. Clustering of X-ray AGN AGN on red sequence are more clustered than in blue cloud Coil et al. in prep Relative bias of red to blue AGN: z=0.7-1.4 red/blue AGN=1.5 z=0.2-0.7 red/blue AGN=1.3 Similar to galaxy red/blue relative bias=1.4 Relative bias of brighter to fainter AGN: z=0.7-1.4 M B = -21.3/-20.5 bias=1.2 z=0.2-0.7 M B = -20.7/-19.8 bias=1.2 Similar to galaxy bright/faint bias for same magnitude range - 1.2 ( errors may be too large to make this statistically significant )

14. Clustering of X-ray AGN Results: -split into 2 z bins - same results at z~0.5 and z~0.9 -X-ray AGN cluster like red galaxies, not blue galaxies -X-ray AGN are more clustered than QSOs! -red AGN are more clustered than blue AGN Consistent w/ galaxies undergoing a QSO phase before settling on the red sequence w/ an X-ray AGN Coil et al. in prep

15. QSO/AGN Evolution Models Competing QSO/AGN formation and evolution models predict different clustering properties. All assume major mergers trigger QSO formation. - Kauffmann and Haenelt 2001 predict a strong luminosity- dependence to QSO clustering: - assume an exponentially declining light curve, time=  - M_B ~ gas mass accreted /  - gas mass accreted ~ host halo mass - luminosity~halo mass brighter QSOs cluster much more ruled out by clustering observations

16. QSO/AGN Evolution Models Lidz, Hopkins predict less luminosity-dependence (still some) - bright and faint QSOs have similar clustering - bias predicted at z~1 is a bit too high (b~2) - would predict X-ray AGN cluster like quasars (?) Croton et al. 2006 include a ‘radio’ mode for low-L AGN - if halo M > M threshold then no cold gas accretion, shuts off SF - no QSO - but there is a low-L AGN fed by hot gas - predict blue galaxies have QSOs and red galaxies have low-L AGN - good qualitative agreement with our results Scannapieco + Thacker 2006 model predicts both auto- and cross- correlation of QSO and matches our z=1 cross-correlation very well! Have their QSOs in the right halos and galaxies at z=1.

17. Conclusions 1.QSOs are less clustered than X-ray selected AGN at z~1. 2.QSOs cluster like blue star-forming galaxies while AGN cluster like red quiescent galaxies (overdense regions). 3.Red galaxies w/ AGN are more clustered than blue galaxies w/ AGN. 4.These results favor galaxies undergoing a bright QSO phase before settling on the red sequence with a lower luminosity AGN. 5.Possibly QSO=early merger phase, X-ray AGN=later merger phase. Measuring QSO/AGN clustering in fields with galaxy redshifts allows cross-correlation (small scales with small errors) and environment measures. Compare with red and blue galaxies at the same z and in the same volume (cosmic variance ~cancels).