MMT Science Symposium1 “false-color” keV X-ray image of the Bootes field Thousands of AGNs in the 9.3 square degree Bootes field * X-ray and infrared properties of AGN * Using AGN to Map Cosmic Structure MMT Science Symposium June 2006

MMT Science Symposium2 Collaborators Chandra (CfA) S. Murray W. Forman A. Kenter R. Narayan R. Hickox C. Jones Spitzer (JPL/Caltech/CfA) P. Eisenhardt M. Brodwin V. Gorjian M. Pahre and the IRAC Shallow Survey Team Optical spectroscopy (OSU/Arizona) K. Kochanek D. Eisenstein and the AGES Team Optical photometry (NOAO) B. Januzzi A. Dey K. Brand and the NDWFS Team and more…

MMT Science Symposium3 Outline of Talk into into AGN AGN What is the Xbootes Survey? What is the Xbootes Survey? Using Hectospec, Chandra, Spitzer to characterize AGN Using Hectospec, Chandra, Spitzer to characterize AGN X-ray and IR properties of BLAGN X-ray and IR properties of BLAGN Mapping the cosmic web with AGN Mapping the cosmic web with AGN The local environment of AGN The local environment of AGN Future Plans Future Plans into into AGN AGN What is the Xbootes Survey? What is the Xbootes Survey? Using Hectospec, Chandra, Spitzer to characterize AGN Using Hectospec, Chandra, Spitzer to characterize AGN X-ray and IR properties of BLAGN X-ray and IR properties of BLAGN Mapping the cosmic web with AGN Mapping the cosmic web with AGN The local environment of AGN The local environment of AGN Future Plans Future Plans

MMT Science Symposium4 Bootes survey imaging data Optical photometry: NOAO DWFS photometry B,R,I,J,K (Januzzi & Dey 1999) Infrared: Spitzer IRAC Shallow Survey (Eisenhardt et al. 2004) The Bootes field was observed with the IRAC camera on Spitzer in four bands: 3.6, 4.5, 5.8, 8.0 microns. ~30,000 sources are detected in all four IRAC bands. X-ray: Chandra XBootes survey (Murray et al. 2004, Kenter et al. 2005), > 3000 X-ray sources

MMT Science Symposium5 MMT Bootes survey Optical spectroscopy: AGES survey w/ MMT/Hectospec The first sample contains ~1000 broad line AGNs, 80 narrow-line AGNs, and 27,000 “normal” galaxies.

MMT Science Symposium6 The XBootes Survey Xbootes: 126 Chandra ACIS pointings 126 Chandra ACIS pointings 5 ksec each field (630 ksec) 5 ksec each field (630 ksec) Joint GTO and GO program Joint GTO and GO program 14 h 32 m +34  06’ 14 h 32 m +34  06’ 4642 sources detected (>=2 cts) 4642 sources detected (>=2 cts) 625 spurious 625 spurious 3293 sources detected (>=4 cts) 3293 sources detected (>=4 cts) 22 spurious 22 spurious 42 extended sources (>=10 cts) 42 extended sources (>=10 cts) f min = 4(8)x erg cm -2 s -1 (0.5-7 keV) f min = 4(8)x erg cm -2 s -1 (0.5-7 keV) 98% sources >=4 cts matched to NDWFS candidates (R =4 cts matched to NDWFS candidates (R<=26)Xbootes: 126 Chandra ACIS pointings 126 Chandra ACIS pointings 5 ksec each field (630 ksec) 5 ksec each field (630 ksec) Joint GTO and GO program Joint GTO and GO program 14 h 32 m +34  06’ 14 h 32 m +34  06’ 4642 sources detected (>=2 cts) 4642 sources detected (>=2 cts) 625 spurious 625 spurious 3293 sources detected (>=4 cts) 3293 sources detected (>=4 cts) 22 spurious 22 spurious 42 extended sources (>=10 cts) 42 extended sources (>=10 cts) f min = 4(8)x erg cm -2 s -1 (0.5-7 keV) f min = 4(8)x erg cm -2 s -1 (0.5-7 keV) 98% sources >=4 cts matched to NDWFS candidates (R =4 cts matched to NDWFS candidates (R<=26) Murray et al. ApJ S 161, 1 (2005) Kenter et al. ApJ S 161, 9 (2005) Brand et al. ApJ, 641, 140 (2006)

MMT Science Symposium7 Multiwavelength studies of AGN X-rays: direct probe of central engine and accretion luminosity Optical/UV: probe of regions close to (BL) or farther from (NL) the black hole; most affected by extinction Infrared: due to reprocessed emission from dust, heated by the central engine ALL THREE can be used to select AGN (Manners 2002) (Urry & Padovani 1995)

MMT Science Symposium8 AGN and Galaxy Evolution Survey (AGES) MMT/Hectospec fiber spectrograph MMT/Hectospec fiber spectrograph 300 fibers/field 300 fibers/field Complete galaxies I<19.5 Complete galaxies I<19.5 Complete X-ray >4 cts and I 4 cts and I<21.5 ~27,000 galaxies ~27,000 galaxies ~1,500 X-ray selected ~1,500 X-ray selected E.g., z=3.53 AGN with 12 X-ray counts - - L x =3x10 45 erg s -1 (0.5- 7keV) E.g., z=3.53 AGN with 12 X-ray counts - - L x =3x10 45 erg s -1 (0.5- 7keV) MMT/Hectospec fiber spectrograph MMT/Hectospec fiber spectrograph 300 fibers/field 300 fibers/field Complete galaxies I<19.5 Complete galaxies I<19.5 Complete X-ray >4 cts and I 4 cts and I<21.5 ~27,000 galaxies ~27,000 galaxies ~1,500 X-ray selected ~1,500 X-ray selected E.g., z=3.53 AGN with 12 X-ray counts - - L x =3x10 45 erg s -1 (0.5- 7keV) E.g., z=3.53 AGN with 12 X-ray counts - - L x =3x10 45 erg s -1 (0.5- 7keV) CXOXB J

MMT Science Symposium9 Samples of AGN -> X-ray/optical Broad-line AGN -> X-ray/optical Narrow-line AGN -> X-ray/optical “normal” galaxies (XBONGS?) -> Mid-infrared selected AGN (color-color criteria, Stern et al. 2005, Lacy et al. 2004) photometric redshifts for those objects with no spectra (Brodwin et al. 2006)

MMT Science Symposium10 Infrared selection of AGN Following Stern et al. (2005)

MMT Science Symposium11 X-ray vs. IR luminosity Broad-line AGNs IR AGNs “Normal” galaxies Narrow-line AGNs

MMT Science Symposium12 X-ray vs. IR luminosity Broad-line AGNs IR AGNs “Normal” galaxies Narrow-line AGNs

MMT Science Symposium13 X-ray vs. IR luminosity Broad-line AGNs IR AGNs Average X-ray fluxes from stacking analysis

MMT Science Symposium14 IR vs. UV luminosity (Hickox et al. 2006) Broad-line AGNs IR AGNs

* Using AGN to Observe the Cosmic Web Xbootes 9.3 Square Degree Survey

MMT Science Symposium16 Large Scale Structure z=0z=1z=3 OCDM SCDM LCDM Jenkins et al., 1998 (ApJ, 499, 20-40) Other Surveys Other Surveys DEEP2 DEEP2 0.7 < z < < z < x 1 sq. deg 4 x 1 sq. deg 40,000 redshifts 40,000 redshifts 2dF 2dF z<0.2 z< sq. deg 1500 sq. deg 200,000 redshifts 200,000 redshifts SDSS (~12 AGN /sq deg) SDSS (~12 AGN /sq deg) z<2.3 z< sq. deg 6600 sq. deg 850,000 redshifts 850,000 redshifts Other Surveys Other Surveys DEEP2 DEEP2 0.7 < z < < z < x 1 sq. deg 4 x 1 sq. deg 40,000 redshifts 40,000 redshifts 2dF 2dF z<0.2 z< sq. deg 1500 sq. deg 200,000 redshifts 200,000 redshifts SDSS (~12 AGN /sq deg) SDSS (~12 AGN /sq deg) z<2.3 z< sq. deg 6600 sq. deg 850,000 redshifts 850,000 redshifts

MMT Science Symposium17 Redshift Distributions

MMT Science Symposium18 Not X-ray Selected (18,820) Most galaxies with z< z>1, must be AGN, but not detected in shallow x-ray survey X-ray Selected (1531) 306 “galaxies” 50 “narrow emission line” 1175 “AGN’ Survey Results (0 < z < 5)

MMT Science Symposium19 Structure (0.25 < z < 0.50)

MMT Science Symposium20 Structure (0.25 < z < 0.50)

MMT Science Symposium21 X-ray Selected AGN At low z (<0.7), map the same structures as seen using galaxies At low z (<0.7), map the same structures as seen using galaxies At higher z, similar X-ray AGN structures continue to be seen At higher z, similar X-ray AGN structures continue to be seen X-ray selected AGN are an efficient means to study large scale structure in the redshift range 1-3 X-ray selected AGN are an efficient means to study large scale structure in the redshift range 1-3 At low z (<0.7), map the same structures as seen using galaxies At low z (<0.7), map the same structures as seen using galaxies At higher z, similar X-ray AGN structures continue to be seen At higher z, similar X-ray AGN structures continue to be seen X-ray selected AGN are an efficient means to study large scale structure in the redshift range 1-3 X-ray selected AGN are an efficient means to study large scale structure in the redshift range 1-3

MMT Science Symposium22 2 Point 3-D Correlation for X-ray AGN Redshift r 0 h Possible Evolution X-ray AGN  ( r ) =( r/r 0 ) r 0 = 6.7h 100

MMT Science Symposium23 Mapping structure with AGN Shallow survey covering 9.3 sq. deg yields 1200 X-ray selected AGN Shallow survey covering 9.3 sq. deg yields 1200 X-ray selected AGN AGN map the same structure at z<0.7 as do galaxies AGN map the same structure at z<0.7 as do galaxies X-ray selected AGN can map large scale structures out to z~3 and search for evolution of structure as predicted in numerical simulations X-ray selected AGN can map large scale structures out to z~3 and search for evolution of structure as predicted in numerical simulations Shallow survey covering 9.3 sq. deg yields 1200 X-ray selected AGN Shallow survey covering 9.3 sq. deg yields 1200 X-ray selected AGN AGN map the same structure at z<0.7 as do galaxies AGN map the same structure at z<0.7 as do galaxies X-ray selected AGN can map large scale structures out to z~3 and search for evolution of structure as predicted in numerical simulations X-ray selected AGN can map large scale structures out to z~3 and search for evolution of structure as predicted in numerical simulations

MMT Science Symposium24 AGN Environment Local Galaxy Density may impact: Activity Type Luminosity … Local Galaxy Density may impact: Activity Type Luminosity … Redshift Slice 0.41<z<0.43

MMT Science Symposium25 Future Plans Chandra AO-8/Hectospec Chandra AO-8/Hectospec Chandra proposal to re-survey Bootes to double number of AGN and measure variabilty Chandra proposal to re-survey Bootes to double number of AGN and measure variabilty 1/3 with I 1300 additional Hectospec targets 1/3 with I 1300 additional Hectospec targets Questions -- How does environment affect the AGN (XBONGS vs BLAGN)? How does environment affect the AGN (XBONGS vs BLAGN)? Why is X-ray emission less for IR brighter galaxies? Why is X-ray emission less for IR brighter galaxies? Does cosmic structure change with redshift? Does cosmic structure change with redshift? Can we identify a large population of absorbed AGN? Can we identify a large population of absorbed AGN? Chandra AO-8/Hectospec Chandra AO-8/Hectospec Chandra proposal to re-survey Bootes to double number of AGN and measure variabilty Chandra proposal to re-survey Bootes to double number of AGN and measure variabilty 1/3 with I 1300 additional Hectospec targets 1/3 with I 1300 additional Hectospec targets Questions -- How does environment affect the AGN (XBONGS vs BLAGN)? How does environment affect the AGN (XBONGS vs BLAGN)? Why is X-ray emission less for IR brighter galaxies? Why is X-ray emission less for IR brighter galaxies? Does cosmic structure change with redshift? Does cosmic structure change with redshift? Can we identify a large population of absorbed AGN? Can we identify a large population of absorbed AGN?

MMT Science Symposium26 Summary (by Ryan Hickox) Observations in a big wide field of nine whole square degrees Show us thousands upon thousands of new active galaxies We can pick them out with Chandra, but if we wish to look instead We can also use their colors in the Spitzer infrared As these AGNs get brighter in the UV and IR, Their X-rays also brighten, but more slow than linear And while the picture for the broad-line AGNs is somewhat sure a lot of IR objects may still be somewhat obscured It will be great to test a model and to see what it predicts! Thank you all for your attention, here at MMT 2006

MMT Science Symposium27 Infrared: AGN vs. starburst contribution? Broad-line AGNs IR AGNs

MMT Science Symposium28 Infrared selection of AGN Dust heated by AGN Colder dust/PAHs (Glikman et al. 2005) (Lagache et al. 2004)

MMT Science Symposium29 IR vs. UV luminosity Broad-line AGNs IR AGNs

MMT Science Symposium30 Galaxies in the Cosmic Web