Presentation is loading. Please wait.

Presentation is loading. Please wait.

Deep Chandra and XMM-Newton Observations of NGC 4472 R. P. Kraft, S. W. Randall, W. R. Forman, P. E. J. Nulsen, C. Jones, A. Bogdan, M. J. Hardcastle,

Similar presentations


Presentation on theme: "Deep Chandra and XMM-Newton Observations of NGC 4472 R. P. Kraft, S. W. Randall, W. R. Forman, P. E. J. Nulsen, C. Jones, A. Bogdan, M. J. Hardcastle,"— Presentation transcript:

1 Deep Chandra and XMM-Newton Observations of NGC 4472 R. P. Kraft, S. W. Randall, W. R. Forman, P. E. J. Nulsen, C. Jones, A. Bogdan, M. J. Hardcastle, E. Hallman, T. Maccarone, T. Joseph, S. Raychaudhury, D. Evans, G. Sivakoff, C. Sarazin (+ M. Machacek, J. ZuHone, R. Johnson) SAO/University of Hertfordshire/Southampton University/Birmingham University/University of Alberta/University of Virginia 29JUN11 - Presentation at ‘The X-ray Universe 2011’ conference

2 Introduction – Cluster and Group Mergers – Potpourri of Gas Dynamics Merging is central to the hierarchical formation of structure paradigm Chandra and XMM-Newton have studied large number of cluster and group mergers – Shocks/supersonic infall (e.g. Bullet Cluster) – Cold fronts/ram pressure stripping (e.g. Fornax cluster, M86) – Sloshing (e.g. Abell 1795, NGC 7618/UGC 12941) Shocks Cold Fronts Sloshing

3 Introduction – Cluster and Group Mergers – Potpourri of Gas Dynamics Merging is central to the hierarchical formation of structure paradigm Chandra and XMM-Newton have studied large number of cluster and group mergers – Shocks/supersonic infall (e.g. Bullet Cluster) – Cold fronts/ram pressure stripping (e.g. Fornax cluster, M86) – Sloshing (e.g. Abell 1795, NGC 7618/UGC 12941) Shocks Cold Fronts Sloshing Entropy, temperature, and emission weighted projected temperature from cold front simulation (Heinz et al. 2003)

4 Introduction – What is NGC 4472 and why do we care NGC 4472 is most optically luminous galaxy in local Universe Member of Virgo cluster (d=17 Mpc, 1”=80 pc) Lies at virial radius (1.35 Mpc) of the Virgo cluster M SMBH =6x10 8 M  Best example of group/cluster merger in local Universe for detailed study – Proximity – Luminosity – Gas temperature (<1.5 keV) Chandra LP (380 ks total) approved in last AO Received data 3 months ago ROSAT mosaic of Virgo cluster (Bohringer et al. 1995)

5 Previous X-ray Observations (Biller et al and Kraft et al. 2011) 100 ks XMM-Newton (PI: T. Maccarone) – MOS1+2 in keV band Direction of infallM87

6 Broadband Overview 380 ks Chandra/ACIS-S Smoothed (  =1.5’’), exposure corrected keV band Point sources removed Features of Interest Multiple Surface Brightness Discontinuities Filamentary Arms Around Radio Bubbles + cavities Large scale X-ray filaments to the E and SW of the nucleus (seen by XMM)

7 Narrower Bands keV keV

8 Core Region keV image with radio contours overlaid Temperature map with radio contours overlaid Gas core is clearly sloshing Complex temperature structure aligned with radio lobes - Uplift 9.7 kpc

9 Radio Outburst Density jump implies M= P mech =1.3x10 57 ergs Significant energy in shocks+ uplift (e.g. filaments in Hyd A) Shock visible in harder band Similar to shocks in M keV band, smoothed exposure corrected

10 Temperature map (1000 counts per cell) On scales of tens of kpc, hot gas distributed asymmetrically around nucleus Cold filaments to the E and SW of the core – relic buoyant radio bubble? Origin? Related to merger process? Sloshing? Looks much different than Abell 3667 and the simulations of Heinz et al. (2003)

11 Temperature map (1000 counts per cell) On scales of tens of kpc, cold gas is distributed asymmetrically around nucleus Cold filaments to the E and SW of the core – relic buoyant radio bubble? Origin? Related to merger process? Looks much different than Abell 3667 and the simulations of Heinz et al. (2003) Abell 3667 (Vikhlinin et al. 2001)

12 Discontinuities in large scale gas k B T=0.96±0.02 keV Z fe =0.47±0.04 Z si =0.68±0.07 k B T=1.04±0.02 Z fe =0.36±0.04 Z si =0.56±0.07 Small temperature jump across discontinuity – significant abundance jump Evidence of flow separation (?) or just sloshing

13 Discontinuities in large scale gas k B T=0.96±0.02 keV Z fe =0.47±0.04 Z si =0.68±0.07 k B T=1.04±0.02 Z fe =0.36±0.04 Z si =0.56±0.07 Small temperature jump across discontinuity – significant abundance jump Evidence of flow separation (?) or just sloshing Re tail ≈1000 assuming Spitzer type viscosity

14 Infall into the Virgo Cluster M87 M49 What is NGC 4472 falling into? Infall velocity between 1200 and 2500 km s -1 Could this be the WHIM? Virgo cluster gas falling back into NGC 4472 group potential?

15 Infall into the Virgo Cluster M87 M49 What is NGC 4472 falling into? Infall velocity between 1000 and 2500 km s -1 Could this be the WHIM? NGC 4522 – small spiral RPS -> 4000 km s -1 !! (Kenney et al. 2004) NGC 4649 group created sloshing structures in M87 (Rodiger et al.2011)

16 Preliminary Conclusions and Future Work NGC 4472 clearly not a ‘classical’ cold front Disentangling everything will not be trivial! Detected a weak shock around radio lobe + evidence up significant uplift Multiple contact discontinuities in gas tail from merger – flow separation (?) Large-scale mosaic with XMM-Newton from NGC 4472 to NGC 4261 needed! Need better radio data!

17 Hydrodynamic Simulation of Group/Cluster Merger (from John ZuHone) and Cold Front (Heinz et al. 2003) Entropy, temperature, and emission weighted projected temperature from cold front simulation (Heinz et al. 2003) Temperature slice of supersonic merger

18 Nuclear Outburst and Feedback Feedback now a central theme in astrophysics – particularly relevant to clusters and galaxies Many Chandra studies of supersonic inflation of radio lobes – Cen A, M87, Per A, Her A, etc. Suppress cooling flows, control star formation, distribute metals Less dramatic outbursts more common and probably more important! Cen A (Kraft et al. 2008) M87 (Forman et al. 2005)

19 Active Nucleus keV image with radio contours overlaid Temperature map with radio contours overlaid n 0 =0.2 cm -3, k B T=700 eV P bondi =5x10 44 ergs s -1,P mech =5x10 42 ergs s -1, L x = 2x10 38 ergs s -1 Complex temperature structure of gas makes it difficult to study Bondi flow 9.7 kpc

20 Compact Binary Population Disk BB Temperature versus L x (curves from Gierlinski & Done 2004) Filled squares – NGC 4472 (Joseph et al. in preparation) Crosses – NGC 3379 (Brassington et al. 2009) Dozens/hundreds of points on this graph (Cen A, NGC 4649, M31, etc.)


Download ppt "Deep Chandra and XMM-Newton Observations of NGC 4472 R. P. Kraft, S. W. Randall, W. R. Forman, P. E. J. Nulsen, C. Jones, A. Bogdan, M. J. Hardcastle,"

Similar presentations


Ads by Google