Constraining the Nature and Impact of

AGN

Constraining the Nature and Impact of

AGNEvan Scannapieco

School of Earth and Space Exploration

Arizona State University

Evan ScannapiecoSchool of Earth and Space

ExplorationArizona State University

Downsizing & PreheatingDownsizing & Preheating

Ueda etal 2004Ueda etal 2004

Cavaliere, Menci, &Tozzi (1999)

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

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

Locally adaptive Fourier-mesh scheme

140,000 cpu hours, down to 140,000 cpu hours, down to

z=1.2z=1.2Total disk output ~ 5 TB Total disk output ~ 5 TB

(1/5th size of (1/5th size of Millennium Run)Millennium Run)

Simulating QuasarsSimulating QuasarsThacker, ES & Couchman 2006, ApJ, 653, 86

Simulating QuasarsSimulating Quasars

Modification of work done on SN outflows

Modification of work done on SN outflows

(ES, Thacker, & Davis 2001, (ES, Thacker, & Davis 2001, Thacker, ES, & Davis 2002)Thacker, ES, & Davis 2002)

Outflows are modeled as thin spherical shells.Host galaxy remains intact.

Quasar are associated with 3:1 mergers, Quasar are associated with 3:1 mergers, ““LIGHTBULB”-- L-Edd as in Wyithe & Loeb LIGHTBULB”-- L-Edd as in Wyithe & Loeb BH mass calculated from baryonic velocity dispersionBH mass calculated from baryonic velocity dispersion5% of energy in light is put into outflow5% of energy in light is put into outflow

Thacker, ES & Couchman 2006, ApJ, 653, 86

Quasar trackingQuasar tracking

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

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

Time1 2 3 4 5 6 7 8

9 10

1112

13

14

15

QuickTime™ and aVideo decompressor

are needed to see this picture.

Galaxy Clusters

Temperature/ keV

LX

1040

1042

1044

1046

LXT3.2

This Works!

Thacker, ES, & Couchman (2006)

Quasar Luminosity FunctionQuasar Luminosity Function

Thacker, ES, & Couchman (2006)

Correlation function of Quasars

Correlation function of Quasars

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”

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)

2dF results (Croom et al 2001)Blue=sim

Quasar-Galaxy cross correlation Quasar-Galaxy cross correlation functionfunction

Quasar-Galaxy cross correlation Quasar-Galaxy cross correlation functionfunction

Blue=ggRed=qgHash=DEEP2 (from Coil etal 06)blue line = 2x1012 DM halos

Could this be 3-body

interactions?

Blue=ggRed=qgHash=DEEP2 (from Coil etal 06)blue line = 2x1012 DM halos

Could this be 3-body

interactions?

Thacker, ES, & Couchman (2006)

Dynamical Friction

Dynamical Friction

Three-body interactions

|V12|

V12 • r12 ^

| V12 r12 |^

Sunyaev Zel’dovich Effect

Comparison SimulationComparison 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!

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!

QuickTime™ and aMPEG-4 Video decompressor

are needed to see this picture.

6 arcmin

Cross-Correlations6 arcmin

Cross-Correlations - Ellipticals

Measuring AGN Feedback

Measuring AGN Feedback

Clustering: Enhanced clustering at small separations Enhanced clustering at small separations

appears to be a robust feature of appears to be a robust feature of mergers.mergers.

This appears to be driven by statistics This appears to be driven by statistics and not dynamics.and not dynamics. Needs to be quantified better…

Clustering: Enhanced clustering at small separations Enhanced clustering at small separations

appears to be a robust feature of appears to be a robust feature of mergers.mergers.

This appears to be driven by statistics This appears to be driven by statistics and not dynamics.and not dynamics. Needs to be quantified better…

Thanks!Thanks!

SZ Observations:SZ Observations: Provide a direct way of measuring Provide a direct way of measuring AGN feedbackAGN feedback Coadding Bulges - Radio Loud = Coadding Bulges - Radio Loud = EETotTot(M(MBulgeBulge))

South Pole TelescopeSensitivity: 10 KBeam: 1 arcminStatus: Initial Engineering Obs.

Atacama Cosmology TelescopeSensitivity: 2 KBeam: 2 arcminStatus: Initial Engineering Obs.

Cross-Correlations - QSOs