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Molecular gas in cooling flows Interplay with AGN and starbursts

Molecular gas in cooling flows Interplay with AGN and starbursts. Ph. Salomé & F. Combes APEX workshop 3- February 2006. Cooling flows in galaxy clusters. Cooling time < Hubble time at the center of clusters  Gas Flow, 100 to 1000 Mo/yr Problem: cold gas or stars formed are not detected?

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Molecular gas in cooling flows Interplay with AGN and starbursts

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  1. Molecular gas in cooling flows Interplay with AGN and starbursts Ph. Salomé & F. Combes APEX workshop 3- February 2006

  2. Cooling flows in galaxy clusters Cooling time < Hubble time at the center of clusters  Gas Flow, 100 to 1000 Mo/yr Problem:cold gas or stars formed are not detected? Today, the amplitude of the flow has been reduced by 10 and the cold gas is detected Edge (2001) Salomé & Combes (2003) 23 detected galaxies in CO Results from Chandra & XMM: cooling flow self-regulated Re-heating process, feedback due to the active nucleus or black Hole: schocks, jets, acoustic waves, bubbles...

  3. Sound wavesin Perseuswith Chandra Fabian et al 2003 NGC 1275=Abell 426 Mechanical energy much larger than Lbol (Binney & Tabor 1995, Churazov et al 2002)

  4. Detection of CO with IRAM-30m CO survey Selected on dM/dt and Ha 6-10 detections among 32 galaxies Masses between 3 108 - 4 1010Mo Mgas versus z, Stars * are detections, Squares hints of detections Dash line: 3s sensitivity limit of IRAM 30m in 2h

  5. Correlation with Halpha Both Edge (2001) and Salome & Combes (2003) data Same excitation mechanisms, Ha shocked gas from cooling flows or ionised by young stars formed

  6. Comparison between MH2 and dM/dt dM/dt from Einstein (White et al 1997). Lines are 1%, 10%, and 100% dM/dt x 1 Gyr In blue, dM/dt (<r) ~raa ~1 taken into account

  7. MH2 versus Mdust  to be done with APEX Mdust from IRAS (assumed 35K). Straight lines represent gas-to-dust ratio of 200, 500 and 1500. Sputtering destroys dust in cluster hot gas Higher gas-to-dust ratio expected

  8. Abell 1795 cooling flow Cooling time 300 Myr (Fabian et al 01) 200 Mo/yr in R < 200kpc (Ettori et al 02) No gas below 2kev (Tamura et al 01, XMM) 60kpc Ha filament (Cowie et al 85) at V(cluster) Cooling wake The cD has V=374km/s w/o cluster

  9. Abell 1795: 2 new PdB fields (mosaic) 20% of the 30m flux retrieved, 4.8 109 Mo CO(1-0) 3.8 ’’ IRAM PdB CO(2-1) 1.8’’ Cold gas coincident with cooling flow, not with any galaxy (Salomé & Combes 2003) z=0.06326 Cont-3mm = 7mJy

  10. CO(2-1) integrated map Close correspondance between the CO(2-1) emission and the Ha +[NII] line emission (gray scale) 6cm contours van Breugel et al 1984 Cold gas may have deflected the expanding radio lobes? The jet creates a hole (bubble) in the hot gas, which is compressed at the boundaries, and cools

  11. CO(1-0) and (2-1) kinematics CO velocity not associated with the central galaxy, but with the cluster (-350km/s) Same kinematics along the filament than Ha Position-Velocity at PA=27 deg from North-South centred on the cD, 5" width

  12. Perseus Ha (WIYN) and optical (HST)

  13. NGC 1275 Ha (WIYN) and CO (IRAM) Ha, Conselice 01 Salome, Combes, Edge et al 05

  14. Perseus Cluster Fabian et al 2003

  15. Perseus cooling flow: M(H2) vs L (Ha)

  16. Perseus cooling flow: CO velocities HaCO

  17. CO (1-0) interferometric map Not centered on the cD galaxy RXJ0821+07 CO (2-1)

  18. PdB maps of RXJ0821+07 z=0.11 dM/dt ~ 30 Mo/yr Gas shifted from the center Could trace the cooling wake, since the central Galaxy is not at rest (Bayer-Kim et al 2002)

  19. Conclusions Now about 23 detections, MH2 up to 1010Mo, typically 20kpc central regions Abell 1795: CO clearly associated to the cooling wake, and not in rotation in the central galaxy  Perseus: CO associated to the cooling filaments (not the merger) The CO(2-1) closely associated to the Ha Confirms the global CO-Ha correlation H2 masses found corresponds to what is expected from the cooling rate Cold dust to be detected, and gas-to-dust ratio checked The AGN creates cavities in the hot gas. Cooling more efficient along the edges of cavities, where the CO and Ha are observed

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