clustering and evolution of radio, x-ray, and ir-selected...

Clustering and evolution of radio, X-ray, and IR-selected AGN

Ryan C. Hickox

Harvard-SmithsonianCenter for Astrophysics

SDSS SymposiumChicago, IL

15 August 2008

Collaborators on9 deg2 Boötes survey

Chandra (CfA)C. JonesW. FormanS. MurrayA. KenterR. Narayan

Optical photometry (NOAO/etc.)B. JanuzziA. DeyK. BrandM. Brownand the NDWFS Team

Spitzer IRAC (JPL/Caltech/CfA)P. EisenhardtM. BrodwinV. GorjianD. SternM. Pahreand the IRAC Shallow Survey Team

Optical spectroscopy (OSU/Arizona/CfA)K. KochanekD. EisensteinR. CoolN. Caldwelland the AGES Team

The AGN and Galaxy Evolution Survey

Hectospec on MMT used to obtain ~20,000 galaxy

redshifts over 7.3 deg2 to z ~ 0.8

~2,000 AGN redshifts

Complementary to

very wide/shallow

(e.g., SDSS) and

narrow/deep (e.g.,

DEEP2) redshift

surveys

The AGN and Galaxy Evolution Survey

Hectospec on MMT used to obtain ~20,000 galaxy

redshifts over 7.3 deg2 to z ~ 0.8

~2,000 AGN redshifts

Complementary to

very wide/shallow

(e.g., SDSS) and

narrow/deep (e.g.,

DEEP2) redshift

surveys

0.25 < z < 0.8

AGN feedback may needed to quench star formation and form the red sequence(e.g., Hopkins et al. 2006, Croton et al. 2006, Rafferty et al. 2008)

Black hole and bulge properties are tightly related(e.g., Magorrian et al. 1998, Ferrarese & Merritt 2000, Gebhart et al. 2000, Tremaine et al. 2002)

Links between AGN & galaxy evolution

Growing evidence for multiple AGN accretion modes“quasar” vs. “radio”(e.g., Churazov et al. 2005, Merloni & Heinz 2008, Somerville et al. 2008)

Questions we ask

What modes of AGN

accretion are found at “low”

redshift (z ~ 0.5), and how do

they depend on host galaxy

properties and environment?

Questions we ask

What modes of AGN

accretion are found at “low”

redshift (z ~ 0.5), and how do

they depend on host galaxy

properties and environment?

How does what we see at

z ~ 0.5 relate to our general

picture of galaxy and AGN

evolution?

How we answer them

How we answer them

Select AGNs at multiple

wavelengths for a (more)

complete AGN sample

1) Host galaxy propertieshost masses, stellar populations

2) Eddington ratiosfueling, accretion modes

3) Spatial correlationsenvironments, DM halo mass

How we answer them

Select AGNs at multiple

wavelengths for a (more)

complete AGN sample

1) Host galaxy propertieshost masses, stellar populations

2) Eddington ratiosfueling, accretion modes

3) Spatial correlationsenvironments, DM halo mass

How we answer them

Select AGNs at multiple

wavelengths for a (more)

complete AGN sample

Compare to theoretical

evolutionary picture

Boötes AGN selection

~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8

Boötes AGN selection

~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8

P1.4 GHz > 5 x 1023 W Hz-1

Boötes AGN selection

All X-ray sourcesLX > 1042 ergs s-1

~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8

P1.4 GHz > 5 x 1023 W Hz-1

Boötes AGN selection

All X-ray sourcesLX > 1042 ergs s-1

Color-color selection (Stern et al. 2005)

~6000 galaxies and 600 AGN with AGES redshifts at 0.25 < z < 0.8

P1.4 GHz > 5 x 1023 W Hz-1

(1) AGN host galaxies

Focus on AGN with extended optical counterparts (AGN is either intrinsically faint or obscured)

(1) AGN host galaxies

• Radio AGN live in luminous red galaxies

(1) AGN host galaxies

• Radio AGN live in luminous red galaxies• X-ray AGN are found preferentially in the “green valley” (see also Nandra et al. 2007, Silverman et al. 2007, Alonso-Hererro et al. 2008, Georgakakis et al. 2008)

(1) AGN host galaxies

• Radio AGN live in luminous red galaxies• X-ray AGN are found preferentially in the “green valley” (see also Nandra et al. 2007, Silverman et al. 2007, Alonso-Hererro et al. 2008, Georgakakis et al. 2008)

• Infrared AGN are primarily found in blue cloud galaxies

(2) Eddington ratios

(2) Eddington ratios

(2) Eddington ratios

Radio:Lbol/LEdd < 10-3

X-ray:10-3 < Lbol/LEdd < 1

IRAC:Lbol/LEdd > 10-2

courtesy S. Murray

(3) AGN clustering

courtesy S. Murray

(3) AGN clustering

courtesy S. Murray

(3) AGN clustering

DARK MATTER HALO?

courtesy S. Murray

Clustering measurements give us estimates of dark matter halo mass

Interesting fact: broad-line quasars reside in

DM halos of constant mass, (~3 x 1012 M☉ ) to z ~ 4 (e.g., Croom et al. 2005, Coil et al. 2007, Myers et al. 2007, Shen et al. 2007)

(3) AGN clustering

Correlation results

Correlation results

Galaxies show dependence on clustering with host galaxy color (as in SDSS, DEEP2, 2dFGRS, etc.)

AGN-galaxy cross-correlation

Radio AGN are strongly clustered (b = 2.4)

Mhalo ~ 5 x 1013 h-1 M☉

AGN-galaxy cross-correlation

Radio AGN are strongly clustered (b = 2.4)

X-ray AGN are clustered like a typical AGES galaxy (b = 1.5) Mhalo ~ 1013 h-1 M☉

AGN-galaxy cross-correlation

Radio AGN are strongly clustered (b = 2.4)

X-ray AGN are clustered like a typical AGES galaxy (b = 1.5)

Infrared AGN are weakly clustered (b = 1.1)

Mhalo ~ 2 x 1012 h-1 M☉

The AGN census 0.25 < z < 0.8

Optically-faintX-ray AGN

Optical/IRSeyfert galaxy

Radio AGN

The AGN census 0.25 < z < 0.8

Optically-faintX-ray AGN

Optical/IRSeyfert galaxy

Radio AGN

• Red host galaxies• Low Lbol/LEdd

• Large DM halos

(~ 5 x 1013 h-1 M☉)

The AGN census 0.25 < z < 0.8

Optically-faintX-ray AGN

Optical/IRSeyfert galaxy

Radio AGN

• Red host galaxies• Low Lbol/LEdd

• Large DM halos

(~ 5 x 1013 h-1 M☉)

• Green host galaxies• Moderate Lbol/LEdd

• Medium DM halos

(~ 1013 h-1 M☉)

The AGN census 0.25 < z < 0.8

Optically-faintX-ray AGN

Optical/IRSeyfert galaxy

Radio AGN

•Blue host galaxies•High Lbol/LEdd

•Small DM halos

(~ 2 x1012 h-1 M☉)

• Red host galaxies• Low Lbol/LEdd

• Large DM halos

(~ 5 x 1013 h-1 M☉)

• Green host galaxies• Moderate Lbol/LEdd

• Medium DM halos

(~ 1013 h-1 M☉)

Initial halo mass (and clustering bias)

High Medium

SMG/ULIRG

Optical/IR quasar

Optically-faintX-ray AGN

Early-type galaxy

Radio galaxy

Early-type galaxy

Disk galaxy(s)

Low

Co

smic

time

z ~ 4

z ~ 1

z ~ 0

(an

d h

alo

ma

ss)

Mh

alo

~ 1

012 -

1013

M☉

A cartoon model for AGN evolution

Initial halo mass (and clustering bias)

High Medium

SMG/ULIRG

Optical/IR quasar

Optically-faintX-ray AGN

Early-type galaxy

Radio galaxy

Early-type galaxy

Disk galaxy(s)

Low

Co

smic

time

z ~ 4

z ~ 1

z ~ 0

(an

d h

alo

ma

ss)

Optically-faintX-ray AGN

Mh

alo

~ 1

012 -

1013

M☉

A cartoon model for AGN evolution

Initial halo mass (and clustering bias)

High Medium

SMG/ULIRG

Optical/IR quasar

Optically-faintX-ray AGN

Early-type galaxy

Radio galaxy

Early-type galaxy

Disk galaxy(s)

Low

Co

smic

time

z ~ 4

z ~ 1

z ~ 0

(an

d h

alo

ma

ss)

Optical/IR Seyfert galaxyOptically-faint

X-ray AGN

Mh

alo

~ 1

012 -

1013

M☉

A cartoon model for AGN evolution

Initial halo mass (and clustering bias)

High Medium

SMG/ULIRG

Optical/IR quasar

Optically-faintX-ray AGN

Early-type galaxy

Radio galaxy

Early-type galaxy

Disk galaxy(s)

Low

Co

smic

time

z ~ 4

z ~ 1

z ~ 0

(an

d h

alo

ma

ss)

Optical/IR Seyfert galaxy

Observed at0.25 < z < 0.8

Optically-faintX-ray AGN

Mh

alo

~ 1

012 -

1013

M☉

A cartoon model for AGN evolution

The future

The future • Compare observables

to more detailed model

predictions

• Relate AGN accretion

modes to host galaxy

physical properties such

as mass & SF history (see forthcoming paper on AGN in

post-starburst galaxies by Brown et

al.)

• Direct evidence for

AGN /galaxy interaction?