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“false-color” 0.5-7 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. “false-color” 0.5-7 keV X-ray image of the Bootes field. Collaborators. Chandra (CfA) S. Murray W. Forman A. Kenter

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“false-color” 0.5-7 keV X-ray image of the Bootes field

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  1. 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 “false-color” 0.5-7 keV X-ray image of the Bootes field MMT Science Symposium

  2. 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 Symposium

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

  4. Bootes survey imaging data Optical photometry: NOAO DWFS photometry B,R,I,J,K (Januzzi & Dey 1999) X-ray:Chandra XBootes survey (Murray et al. 2004, Kenter et al. 2005), > 3000 X-ray sources 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. MMT Science Symposium

  5. 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 Symposium

  6. The XBootes Survey Xbootes: • 126 Chandra ACIS pointings • 5 ksec each field (630 ksec) • Joint GTO and GO program • 14h 32m +34 06’ • 4642 sources detected (>=2 cts) • 625 spurious • 3293 sources detected (>=4 cts) • 22 spurious • 42 extended sources (>=10 cts) • fmin= 4(8)x10-15 erg cm-2 s-1 (0.5-7 keV) • 98% sources >=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 Symposium

  7. Multiwavelength studies of AGN (Urry & Padovani 1995) 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) MMT Science Symposium

  8. AGN and Galaxy Evolution Survey (AGES) • MMT/Hectospec fiber spectrograph • 300 fibers/field • Complete galaxies I<19.5 • Complete X-ray >4 cts and I<21.5 • ~27,000 galaxies • ~1,500 X-ray selected • E.g., z=3.53 AGN with 12 X-ray counts - - Lx=3x1045 erg s-1 (0.5- 7keV) CXOXB J142547.4+352719 MMT Science Symposium

  9. 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 Symposium

  10. Infraredselection of AGN Following Stern et al. (2005) MMT Science Symposium

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

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

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

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

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

  16. z=0 z=1 z=3 OCDM SCDM LCDM Large Scale Structure • Other Surveys • DEEP2 • 0.7 < z < 1.4 • 4 x 1 sq. deg • 40,000 redshifts • 2dF • z<0.2 • 1500 sq. deg • 200,000 redshifts • SDSS (~12 AGN /sq deg) • z<2.3 • 6600 sq. deg • 850,000 redshifts Jenkins et al., 1998 (ApJ, 499, 20-40) MMT Science Symposium

  17. Redshift Distributions MMT Science Symposium

  18. Survey Results (0 < z < 5) • Not X-ray Selected (18,820) • Most galaxies with z<0.7 • 531 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’ MMT Science Symposium

  19. Structure (0.25 < z < 0.50) MMT Science Symposium

  20. Structure (0.25 < z < 0.50) MMT Science Symposium

  21. X-ray Selected AGN • 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 • X-ray selected AGN are an efficient means to study large scale structure in the redshift range 1-3 MMT Science Symposium

  22. 2 Point 3-D Correlation for X-ray AGN X-ray AGN ( r ) =( r/r0)-1.71 r0 = 6.7h100 Possible Evolution MMT Science Symposium

  23. Mapping structure with 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 • 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 Symposium

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

  25. Future Plans • Chandra AO-8/Hectospec • Chandra proposal to re-survey Bootes to double number of AGN and measure variabilty • 1/3 with I<22.5 ?? -> 1300 additional Hectospec targets Questions -- How does environment affect the AGN (XBONGS vs BLAGN)? Why is X-ray emission less for IR brighter galaxies? Does cosmic structure change with redshift? Can we identify a large population of absorbed AGN? MMT Science Symposium

  26. 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 Symposium

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

  28. Infraredselection of AGN Colder dust/PAHs (Lagache et al. 2004) Dust heated by AGN (Glikman et al. 2005) MMT Science Symposium

  29. IR vs. UV luminosity IR AGNs Broad-line AGNs MMT Science Symposium

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