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Constraining the Nature and Impact of AGN

Constraining the Nature and Impact of AGN. Evan Scannapieco School of Earth and Space Exploration Arizona State University. Downsizing & Preheating. Cavaliere, Menci, &Tozzi (1999). Ueda etal 2004. Simulating Quasars. Thacker, ES & Couchman 2006, ApJ, 653, 86.

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Constraining the Nature and Impact of AGN

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  1. Constraining the Nature and Impact of AGN Evan Scannapieco School of Earth and Space Exploration Arizona State University

  2. Downsizing & Preheating Cavaliere, Menci, &Tozzi (1999) Ueda etal 2004

  3. Simulating Quasars Thacker, ES & Couchman 2006, ApJ, 653, 86 • OpenMP version of the ‘Hydra’ SPH code (Pearce & Couchman 1997, Thacker et al 2003, Thacker & Couchman, 2006) • 2x 6403 mass elements (half gas, half dark matter) • Largest cosmological SPH simulation ever carried out at that time • 147 h-1 Mpc box, mass resolution 2.2x108 baryons, 1.2x109 DM • 140,000 cpu hours, down to z=1.2 • Total disk output ~ 5 TB (1/5th size of Millennium Run) Locally adaptive Fourier-mesh scheme

  4. Simulating Quasars Thacker, ES & Couchman 2006, ApJ, 653, 86 Quasar are associated with 3:1 mergers, “LIGHTBULB”-- L-Edd as in Wyithe & Loeb BH mass calculated from baryonic velocity dispersion 5% of energy in light is put into outflow Modification of work done on SN outflows (ES, Thacker, & Davis 2001, Thacker, ES, & Davis 2002) Outflows are modeled as thin spherical shells. Host galaxy remains intact.

  5. Quasar tracking Time 1 2 3 6 7 4 5 8 • Merger model requires that we find groups and identify mergers while the simulation is running • Need fast group finder • Previous work used group finder to identify the mass of objects and determine star formation events • Simple to adapt this to include a group index 9 10 12 11 13 14 15

  6. Galaxy Clusters 1046 1044 This Works! LX 1042 LXT3.2 1040 Thacker, ES, & Couchman (2006) Temperature/ keV

  7. Quasar Luminosity Function Thacker, ES, & Couchman (2006)

  8. Correlation function of Quasars Blue=sim 2dF results (Croom et al 2001) • Our simulation agrees with the observed turn-up in the small scale clustering of quasars • CF is explained by the “halo model” of clustering • No need for “special physics” Sloan binary quasar data (Hennawi et al 2005)

  9. Quasar-Galaxy cross correlation function Blue=gg Red=qg Hash=DEEP2 (from Coil etal 06) blue line = 2x1012 DM halos Could this be 3-body interactions? Thacker, ES, & Couchman (2006)

  10. Dynamical Friction

  11. Dynamical Friction

  12. Three-body interactions

  13. |V12| ^ | V12  r12 | ^ V12 • r12

  14. Sunyaev Zel’dovich Effect

  15. Comparison Simulation • 2x 3203 mass elements (half gas, half dark matter) • 67.5 h-1 Mpc box, mass resolution 2.2x108 baryons, 1.2x109 DM • Mergers are exactly as the were in the feedback run, but no outflows are included. • Outputs every 50 Myrs!

  16. 6 arcmin Cross-Correlations 6 arcmin

  17. Cross-Correlations - Ellipticals

  18. Measuring AGN Feedback

  19. Measuring AGN Feedback

  20. Thanks! • Clustering: • Enhanced clustering at small separations appears to be a robust feature of mergers. • This appears to be driven by statistics and not dynamics. Needs to be quantified better… • SZ Observations: • Provide a direct way of measuring AGN feedback • Coadding Bulges - Radio Loud = ETot(MBulge)

  21. South Pole Telescope Sensitivity: 10 K Beam: 1 arcmin Status: Initial Engineering Obs. Atacama Cosmology Telescope Sensitivity: 2 K Beam: 2 arcmin Status: Initial Engineering Obs.

  22. Cross-Correlations - QSOs

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