1. Prospects for Infrared AGN Surveys Scott Croom (AAO)

2. OutlineOutline What are the key scientific questions?What are the key scientific questions? The current “state of the art” regarding AGN surveys (mostly 2QZ).The current “state of the art” regarding AGN surveys (mostly 2QZ). IR selection of AGN.IR selection of AGN. Prospects for FMOS.Prospects for FMOS.

3. Fundamental questions: QSO (SMBH) formation & evolution:QSO (SMBH) formation & evolution: –How? –When? Cosmology:Cosmology: –Ω, Λ, H 0 - DONE? –W(z), “dark energy”, equation of state… –Evolution of the IGM and the formation of galaxies.

4. AGN Physics Basic questions:Basic questions: –How do AGN form? –What drives their evolution? –Unification - the obscured population? Issues:Issues: –Gal mass vs. BH mass vs. BH Luminosity –Fuelling: variable efficiency, time-scales... –Triggering: mergers, starbursts… –Our view: orientation, dust, BLR, NLR...

5. CosmologyCosmology Cosmological parameters:Cosmological parameters: –WMAP, 2dFGRS, SN Ia… Done? –New parameters - w(z), the equation of state etc. Galaxy formation & the IGM:Galaxy formation & the IGM: –Chemical history of the Universe –When was the gas used up? –When were most of the metals produced?

6. The “state of the art” Large homogeneous optically selected samples: 2dF, SDSSLarge homogeneous optically selected samples: 2dF, SDSS Smaller deep X-ray surveys: Chandra, XMMSmaller deep X-ray surveys: Chandra, XMM

7. The 2dF QSO Redshift Survey

8. Data release Data fully publicData fully public Available via:Available via: –www.2dfquasar.org –2QZ CD-ROM Includes:Includes: –Catalogue –Spectra –Completeness masks + software Croom et al. 2003, in press AdvertisementAdvertisement

9. QSO Optical LF Croom et al. 2003

10. X-ray LF Inconsistent with PLE.Inconsistent with PLE. LDDE is a better fit.LDDE is a better fit. How do we get consistency with optical?How do we get consistency with optical? From Ueda et al. 2003

11. Clustering evolution ?

12. 2QZ vs. 2dFGRS

13. The QSO power spectrum  CDM Outram et al. 2003 Fitting possible to ~500 h -1 Mpc.Fitting possible to ~500 h -1 Mpc.  =0.13  0.02  =0.13  0.02

14. The QSO power spectrum  b /  m =0.18  0.1  b /  m =0.18  0.1  m h=0.19  0.05  m h=0.19  0.05 + 2QZ best fit+ 2QZ best fit x 2dFGRS best fitx 2dFGRS best fit Marginal detection of baryon wiggles (non-zero  b ).Marginal detection of baryon wiggles (non-zero  b ).

15. Spectral properties

16. 2QZ Key results Over 23000 QSO redshifts measured.Over 23000 QSO redshifts measured. Geometric test   m =0.29,   =0.71Geometric test   m =0.29,   =0.71 P(k) on scales up to ~500 h -1 Mpc:P(k) on scales up to ~500 h -1 Mpc: –  b /  m =0.18  0.1 –  m h=0.19  0.05 Clustering evolution  lifetimes ~ 10 6 -10 7 yearsClustering evolution  lifetimes ~ 10 6 -10 7 years Optical LF consistent with PLE (still…!)Optical LF consistent with PLE (still…!) Host galaxies: L gal ~L QSO 0.4Host galaxies: L gal ~L QSO 0.4 No evolution in velocity width for a given L.No evolution in velocity width for a given L. And…And… –a lasting resource for the community.

17. SDSS & high z QSOs The SDSS will provide:The SDSS will provide: –~100000 QSOs –Including 7 (currently) at z>5.7… –High quality photometry and spectra Fan et al. 2003

18. SDSS/2dF Faint QSOs ~10000 faint QSOs, g’~22 mag (+LRGs!)~10000 faint QSOs, g’~22 mag (+LRGs!) Science (testing QSO formation models):Science (testing QSO formation models): –breaking the L-z degeneracy in clustering. –The faint end of the QSO LF. –QSO environments at z~0.7. –BH mass function via QSO line widths. plus improved measurements of LSS, z- space distortions etc.plus improved measurements of LSS, z- space distortions etc.

19. 2MASS & red AGN 2MASS has used J-K colours to select QSOs (e.g. Cutri et al)2MASS has used J-K colours to select QSOs (e.g. Cutri et al) At low redshift there is a significant population of “red AGN”At low redshift there is a significant population of “red AGN” 2MASS not deep enough to reach high z:2MASS not deep enough to reach high z: –K~15.5 flux limit. Much of the red colour will come from the host galaxy at low z.Much of the red colour will come from the host galaxy at low z. Barkhouse & Hall 2001

20. IR selection of QSOs Near IR colours:Near IR colours: –E.g. from red J-K colour –Drop out techniques Mid-IR from Spitzer surveys (e.g. SWIRE – see Seb’s talk).Mid-IR from Spitzer surveys (e.g. SWIRE – see Seb’s talk).

21. K-excessK-excess QSOs are bluer than stars at UV/optical wavelengths.QSOs are bluer than stars at UV/optical wavelengths. But they are also REDDER that stars at near IR wavelengths.But they are also REDDER that stars at near IR wavelengths. This suggests a K-excess (or KX) selection analogous to UVX in the UV/optical (Warren et al. 2000)This suggests a K-excess (or KX) selection analogous to UVX in the UV/optical (Warren et al. 2000)

22. K-excessK-excess Warren et al. 2000

23. KX & the NDWFS Preliminary results from a KX survey with the NOAO Deep Wide-field Survey.Preliminary results from a KX survey with the NOAO Deep Wide-field Survey. Deep BRIJHK imaging data.Deep BRIJHK imaging data. Spectroscopy from HYDRA & WYFFOS.Spectroscopy from HYDRA & WYFFOS. Reddening

24. The time domain… Largely unexplored regime.Largely unexplored regime. Potential science areas:Potential science areas: –BH masses via reverberation mapping to high redshift (how long will it take?). –Constraints on winds & outflow models via variations in intrinsic absorption lines. –Stratification of the broad line region via reverberation mapping of multiple lines. Simultaneous observations in optical/IR?Simultaneous observations in optical/IR?

25. FMOS surveys Based on UKIDSS (DXS) & Others.Based on UKIDSS (DXS) & Others. Combine with optical spectroscopic of brighter/bluer sources. E.g. AAOmega.Combine with optical spectroscopic of brighter/bluer sources. E.g. AAOmega. Also relatively low AGN surface density means that AGN surveys could be merged with other surveys (c.f. 2dFGRS/2QZ):Also relatively low AGN surface density means that AGN surveys could be merged with other surveys (c.f. 2dFGRS/2QZ): –extra science too.

26. FMOS advantages Efficient for red/reddened objects:Efficient for red/reddened objects: –The un-obscured population. Probes the same spectral window as optical at low z:Probes the same spectral window as optical at low z: –Spectral analysis -> BH mass estimates, AGN physics -> cause of evolution? Large FOV on an 8m:Large FOV on an 8m: –1 hr (J~22 mag) -> ~50 QSOs per FMOS field. –LSS/cosmology, QSO environments & triggering.

27. SummarySummary The near-IR is an ideal place to select and observe QSOs.The near-IR is an ideal place to select and observe QSOs. Only ultra deep surveys (X-rays?) would use 400 fibres in FMOS.Only ultra deep surveys (X-rays?) would use 400 fibres in FMOS. Large area QSO surveys should be a component of an integrated survey.Large area QSO surveys should be a component of an integrated survey. The time domain is still largely unexplored…The time domain is still largely unexplored…