constraining the nature and impact of agn
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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