Host galaxies, clustering, and evolution of radio, X-ray, and IR AGN at z < 1Ryan C. HickoxHarvard-SmithsonianCenter for AstrophysicsRadio Galaxies in the Chandra Era10 July 2008“three-color” Chandra 0.5-7 keV image from the XBoötes surveyCollaboratorsChandra (CfA)C. JonesW. FormanS. MurrayA. KenterR. NarayanOptical photometry (NOAO/etc.)B. JanuzziA. DeyK. BrandM. Brownand the NDWFS TeamSpitzer IRAC (JPL/Caltech/CfA)P. EisenhardtM. BrodwinV. GorjianD. SternM. Pahreand the IRAC Shallow Survey TeamOptical spectroscopy (OSU/Arizona/CfA)K. KochanekD. EisensteinR. CoolN. Caldwelland the AGES TeamData from 9 deg2 Boötes surveyOptical photometry: NOAO DWFS photometry Bw,R,I,J,K (Januzzi & Dey 1999)Infrared: Spitzer IRAC Shallow Survey (Eisenhardt et al. 2004)~30,000 sources are detected in all four IRAC bands. X-ray: Chandra XBoötes survey (Murray et al. 2004, Kenter et al. 2005), > 3000 X-ray sourcesOptical spectroscopy: AGES survey w/ MMT/Hectospec Radio from WSRT 1.4 GHz surveyMotivation:AGN are fascinating objects!AGN and their host galaxies are closely linked!Galaxies are divided into two color typesBlanton (2006)Zehavi et al. (2005)Red (bulge-dominated) galaxies show stronger clustering than blue (spiral, star-forming) galaxies Cosmological history of stars & SMBHSTAR FORMATION(Nagamine et al. 2006)QUASAR ACCRETION(Hasinger et al. 2005)Present-day relationship between stars and SMBHTremaine et al. (2002)AGN feedback and galaxy colorsFeedback from AGN may be required in the evolution from blue cloud to red sequence, both to initially quench star formation (e.g., Hopkins et al. 2006), and too suppress further star formation(e.g., Croton et al. 2006, Khalatyan et al. 2008)Croton et al. (2006)with feedbackno feedbackAGN 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)Cosmic histories of SF and accretion are similar(e.g., Nagamine et al. 2006, Hasinger et al. 2005)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)Our primary questions:What types of AGN accretion are found at “low” redshift (z < 1), and how do they depend on host galaxy and environment?How does what we see in the “local” universe relate to the general picture of galaxy and AGN evolution?What is the role of radio AGN in a cosmological context?AGN hosts and clusteringPrevious studies of AGN hosts and clustering:z < 0.6: --Seyferts prefer less dense environments and are found mainly in disk galaxies, while LINERS have no relative bias and are found mainly in early-types(e.g., SDSS, Miller et al. 2003, Kauffmann et al. 2004, Constantin & Vogeley 2006) --Radio AGN lie in massive early-type galaxies in the centers of clusters (e.g., Yee & Green 1987)z ~ 1:--X-ray AGN lie in overdense environments (DEEP2/EGS, Georgakakis et al. 2007)--broad-line quasars cluster like blue galaxies (DEEP2, Coil et al. 2007)NASA/CXC/Ohio State Univ./J.Eastman et alz ~2-3:--Broad-line quasar clustering increases with redshift -- they have typical DM halo masses of ~1012 Msun (e.g., Croom et al. 2005, Myers et al. 2006)courtesy S. MurrayHickox et al. 2008, in prep.AGN in the AGES redshift survey at 0.25 < z < 0.8AGES galaxies and AGN (0.25<z<0.8)Hickox et al. (2008), in prepAGN selection: RadioSelect sources with log P > 23.5 [W/Hz] at 1.4 GzMostly FR-I radio galaxiesAGN selection: X-raySelect all X-ray sources associated with AGES galaxies4 counts corresponds to LX ~ 1042 ergs/s at z~0.25! AGN selection: InfraredStern et al. (2005)AGN selection regionAGN selection All X-ray sourcesColor-color selection (Stern et al. 2005)~6000 galaxies and 600 AGN over 8 deg2Colors and magnitudes of AGN hostsRadio AGN live in luminous red galaxiesX-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 galaxiesFocus on AGN with extended optical counterparts (AGN is either intrinsically faint or obscured)courtesy S. MurrayFor broad-line quasars, clustering increases with redshift -- they have typical DM halo masses of ~3 x 1012 M☉ (e.g., Croom et al. 2005, Myers et al. 2006) AGN clustering in AGESCross-correlation resultsGalaxies show dependence on clustering with host galaxy color (as in SDSS, DEEP2, 2dFGRS, etc.)Cross-correlation resultsRadio AGN are strongly clustered (b=1.47 ± 0.16) X-ray AGN are clustered like a typical AGES galaxy (b=0.98 ± 0.11)Infrared AGN are weakly clustered (b=0.78 ± 0.12)X-ray stacking of radio AGNLX ~ 1041 ergs/sr90 ~ 30 h-1 kpcX-ray undetected radio AGN (0.5-2 keV image, scaled to PSF size)C0.5-2 keV = 27 ± 6 ctsC2-7 keV = 4.9 ± 3.3HR = -0.7 ± 0.2very soft spectrum!kT ~ 1.5 keVLimits on AGN contribution:LX ≲ 1042 ergs/sLbol/LEdd < 10-3Radio galaxies at z ~ 0.5 show very soft (thermal?) emission in the X-rays!BH masses and Eddington ratiosX-ray properties vs. galaxy colorFor, X-ray AGNs, clustering bias and X-ray hardness both increase for redder host galaxiesAre AGN in red host galaxies more absorbed?or,Is the intrinsic spectrum harder for ellipticals (with lower Lbol/LEdd)? A different AGN accretion state? (e.g., Churazov et al. 2005, Vasudevan et al. 2007)The AGN census at 0.25 < z < 0.8: Radio AGN: lie in luminous early-type, are strongly clustered, have very soft (thermal?) X-ray emission, and low Eddington ratios X-ray AGN are most common in the “green valley”, and have clustering typical of normal galaxies IRAC AGN avoid the red sequence, are weakly clustering, and have relatively high Eddington ratiosInitial halo mass (and clustering bias)HighMediumSMG/ULIRGOptical/IR quasarOptically-faintX-ray AGNEarly-type galaxyRadio galaxyEarly-type galaxyDisk galaxy(s)LowCosmic timez ~ 4z ~ 1z ~ 0(and halo mass)Optical/IR Seyfert galaxyObserved at0.25 < z < 0.8Optically-faintX-ray AGNMhalo ~ 3 x 1012 M☉ A cartoon model for AGN evolutionNuclear contamination color correctionNuclear contamination color correctionNuclear contamination color correction