prospects for infrared agn surveys scott croom (aao)

Prospects for Infrared Prospects for Infrared AGN SurveysAGN Surveys

Prospects for Infrared Prospects for Infrared AGN SurveysAGN Surveys

Scott Croom (AAO)Scott Croom (AAO)

OutlineOutlineOutlineOutline

• What are the key scientific questions?What are the key scientific questions?

• The current “state of the art” The current “state of the art”

regarding AGN surveys (mostly 2QZ).regarding AGN surveys (mostly 2QZ).

• IR selection of AGN.IR selection of AGN.

• Prospects for FMOS.Prospects for FMOS.

Fundamental Fundamental questions:questions:Fundamental Fundamental questions:questions:• QSO (SMBH) formation & evolution:QSO (SMBH) formation & evolution:

– How?

– When?

• Cosmology:Cosmology:

– Ω, Λ, H0 - DONE?

– W(z), “dark energy”, equation of state…

– Evolution of the IGM and the formation of galaxies.

AGN PhysicsAGN PhysicsAGN PhysicsAGN 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...

CosmologyCosmologyCosmologyCosmology

• 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?

The “state of the art”The “state of the art”The “state of the art”The “state of the art”

• Large homogeneous optically selected Large homogeneous optically selected

samples: 2dF, SDSSsamples: 2dF, SDSS

• Smaller deep X-ray surveys: Chandra, Smaller deep X-ray surveys: Chandra,

XMMXMM

The 2dF QSO Redshift Survey

Data releaseData releaseData releaseData 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. 2003Croom et al. 2003, in , in presspress

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QSO QSO Optical Optical LFLFQSO QSO Optical Optical LFLF

Croom et al. Croom et al. 2003 2003

X-ray LF X-ray LF X-ray LF X-ray LF • Inconsistent Inconsistent

with PLE.with PLE.

• LDDE is a LDDE is a better fit.better fit.

• How do we get How do we get consistency consistency with optical?with optical?

From Ueda et al. 2003From Ueda et al. 2003

Clustering evolutionClustering evolutionClustering evolutionClustering evolution

??

2QZ vs. 2dFGRS2QZ vs. 2dFGRS2QZ vs. 2dFGRS2QZ vs. 2dFGRS

The QSO power The QSO power spectrumspectrumThe QSO power The QSO power spectrumspectrum

CDMCDM

Outram et al. 2003Outram et al. 2003

•Fitting possible Fitting possible to ~500 hto ~500 h-1-1Mpc.Mpc.

=0.13=0.130.020.02

The QSO power The QSO power spectrumspectrumThe QSO power The QSO power spectrumspectrum

bb//mm=0.18=0.180.10.1

mmh=0.19h=0.190.050.05

•+ 2QZ best fit+ 2QZ best fit

•x 2dFGRS best fitx 2dFGRS best fit

•Marginal detection Marginal detection of baryon wiggles of baryon wiggles (non-zero (non-zero bb).).

Spectral propertiesSpectral propertiesSpectral propertiesSpectral properties

2QZ 2QZ Key resultsKey results2QZ 2QZ Key resultsKey results

• Over 23000 QSO redshifts measured.Over 23000 QSO redshifts measured.

• Geometric test Geometric test mm=0.29=0.29,, =0.71 =0.71

• P(k) on scales up to P(k) on scales up to ~500 h~500 h-1-1MpcMpc: : bb//mm=0.18=0.180.10.1

mmh=0.19h=0.190.050.05

• Clustering Clustering evolution evolution lifetimes ~ 10 lifetimes ~ 1066-10-1077 years years• Optical LF consistent with PLE (still…!)Optical LF consistent with PLE (still…!)

• Host galaxies: LHost galaxies: Lgalgal~L~LQSOQSO0.40.4

• No evolution in velocity width for a given L. No evolution in velocity width for a given L. • AndAnd… …

– a lasting resource for the community.

SDSS & high z QSOsSDSS & high z QSOsSDSS & high z QSOsSDSS & 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. 2003Fan et al. 2003

SDSS/2dF Faint QSOsSDSS/2dF Faint QSOsSDSS/2dF Faint QSOsSDSS/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-plus improved measurements of LSS, z-

space distortions etc.space distortions etc.

2MASS & red AGN2MASS & red AGN2MASS & red AGN2MASS & red AGN

• 2MASS has used J-K colours to select 2MASS has used J-K colours to select

QSOs (e.g. Cutri et al)QSOs (e.g. Cutri et al)

• At low redshift there is a significant At low redshift there is a significant

population of “red AGN”population of “red AGN”

• 2MASS not deep enough to reach high 2MASS not deep enough to reach high

z:z:– K~15.5 flux limit.

• Much of the red colour will come from Much of the red colour will come from

the host galaxy at low z.the host galaxy at low z. Barkhouse & Hall 2001Barkhouse & Hall 2001

IR selection of QSOsIR selection of QSOsIR selection of QSOsIR 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. Mid-IR from Spitzer surveys (e.g.

SWIRE – see Seb’s talk).SWIRE – see Seb’s talk).

K-excessK-excessK-excessK-excess

• QSOs are bluer than stars at UV/optical QSOs are bluer than stars at UV/optical wavelengths.wavelengths.

• But they are also But they are also REDDER REDDER that stars that stars at near IR wavelengths.at near IR wavelengths.

• This suggests a K-excess (or KX) This suggests a K-excess (or KX) selection analogous to UVX in the selection analogous to UVX in the UV/optical (Warren et al. 2000)UV/optical (Warren et al. 2000)

K-excessK-excessK-excessK-excess

Warren et al. 2000Warren et al. 2000

KX KX & the NDWFS& the NDWFSKX KX & the NDWFS& the NDWFS

• Preliminary results from a KX survey Preliminary results from a KX survey

with the NOAO Deep Wide-field Survey.with the NOAO Deep Wide-field Survey.

• Deep BRIJHK imaging data.Deep BRIJHK imaging data.

• Spectroscopy from HYDRASpectroscopy from HYDRA & WYFFOS. & WYFFOS.Reddening

The time domain…The time domain…The time domain…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?

FMOS surveysFMOS surveysFMOS surveysFMOS surveys

• Based on UKIDSS (DXS) & Others.Based on UKIDSS (DXS) & Others.

• Combine with optical spectroscopic of Combine with optical spectroscopic of brighter/bluer sources. E.g. AAOmega.brighter/bluer sources. E.g. AAOmega.

• Also relatively low AGN surface density Also relatively low AGN surface density means that AGN surveys could be means that AGN surveys could be merged with other surveys (c.f. merged with other surveys (c.f. 2dFGRS/2QZ): 2dFGRS/2QZ): – extra science too.

FMOS advantagesFMOS advantagesFMOS advantagesFMOS advantages

• Efficient for red/reddened objects:Efficient for red/reddened objects:– The un-obscured population.

• Probes the same spectral window as Probes the same spectral window as optical at low z: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.

SummarySummarySummarySummary

• The near-IR is an ideal place to select The near-IR is an ideal place to select

and observe QSOs.and observe QSOs.

• Only ultra deep surveys (X-rays?) Only ultra deep surveys (X-rays?)

would use 400 fibres in FMOS.would use 400 fibres in FMOS.

• Large area QSO surveys should be a Large area QSO surveys should be a

component of an integrated survey.component of an integrated survey.

• The time domain is still largely The time domain is still largely

unexplored…unexplored…