1. Circulation Flows Fabrizio Brighenti (Bologna) David Buote (UC Irvine) Cooling flows with bubble return ! Bill Mathews (UC Santa Cruz)

2. O’Sullivan et al. 2001 X-ray Luminosity of Elliptical Galaxies Observed SNIa rate in E galaxies SNu = 0.16 per L B = 10 10 per 100 yrs Is almost certainly too high (Cappellaro et al. 1999) ROSAT

3. O’Sullivan et al. 2001 X-ray Luminosity of Elliptical Galaxies

4. Range of L x /L B determined by extent of circumgalactic gas Mathews & Brighenti 1998 L x /L B = (r ex /r e ) 0.6

5. O’Sullivan et al. 2001 Optically Dark Groups & Elliptical Galaxies Filled circles: Optically dark galaxies/groups aka “Overluminous Elliptical Galaxies” (OLEG) “Fossil Groups” Vikhlinin et al. 1999 Ponman et al. 1994 NGC 5044

6. Optically Dark Groups with M vir known from X-ray Observations L B ~ M vir may result from hierarchical assembly Several (all?) dark groups are baryonically “closed” like rich clusters: f b = M bary /M tot ~ 0.16 (WMAP) NGC 6482

7. Caon et al. 2001 Warm gas in NGC 5044 -- Stellar Ejecta? H  + [NII] very disturbed with crazy velocity field scale > SNIa remnants ejecta receives momentum 6 kpc stellar isophotes

8. Extended Dusty Core in NGC 5044 -- Stellar Ejecta? B-I image 12 x 12 kpc Goudfrooij 1991

9. Van Dokkum & Franx 1995 Verdoes Kleijn et al. 1999 ~50-60% of Normal Ellipticals and ~90% of Radio-Jet Ellipticals have Dusty Cores HST images

10. Mathews & Brighenti 2003 Accelerated Cooling in Dusty Stellar Ejecta Even dusty gas at 10 7 K cools very rapidly Cooled gas still contains dust Reliable minimum gas flow to black hole Cooling at 1 kpc in NGC 4472 no dust

11. Buote, Lewis, Brighenti, Mathews 2003 XMM & Chandra Observations of NGC 5044 150 kpc 20 kpc In pressure equilibrium |  /  |~|  T/T| Scale of hot bubbles >> size of SNIa remnants Filling factor f ~ 0.5 in r < 20kpc XMM image is smooth beyond ~30 kpc

12. Buote, Lewis, Brighenti, Mathews 2003 Gas Temperature Profile in NGC 5044 r (kpc) Multiphase temperature T c ~ T * ≤ T ≤ T h but no gas with T ≤ T c (dM/dt) cool < 0.4 M sun /yr expected: ~5 M sun /yr 2T -- a better fit to data:1T fit to data:

13. Sun et al. 2003 Gas Temperature Profiles in Groups & Clusters Groups Clusters Allen et al. 2001 dT/dr > 0 at small radii

14. Buote, Lewis, Brighenti, Mathews 2003 2T Multi-phas Emission in NGC 5044 r (kpc) Cool Cool phase dominates in r ≤ 30 kpc Filling factor of cool gas is f ~ 0.5 in r < 20 kpc

15. Global Properties of NGC 5044 E/group r (kpc) M gas (M sun ) M * (M sun ) M tot (M sun ) M Fe,gas (M sun ) r obs 32713x10 11 5.8x10 11 2.0x10 13 3.5x10 8 r vir 87045x10 11 7.4x10 11 3.9x10 13 9.0x10 8 M bary /M tot M Fe /L B 5044 group0.140.006 Rich clusters0.13 - 0.170.015 R eE = 10 kpc L B,E = 4.5x10 10 ∑L B,dwarfs = 10x10 10 Buote, Brighenti & Mathews 2004 160 missing iron~WMAP baryons

16. Global Energetics of NGC 5044 E/group Energy in cavities E cav = PfV = 1 x 10 58 erg Total SN energy E sn = 8 x 10 60 erg Gas binding energyE bind = E th = ∫  th  dV = 2 x 10 61 erg Black hole mass M bh = 7.6x10 -5 M * 1.12 = 6 x10 8 M sun Haring & Rix 2004 Black hole energyE bh =.1 M bh c 2 = 1 x 10 62 erg to retain gas: the efficiency of black hole heating is < 0.02 power to maintain low density phase: PfV/t buoy ~ 10 43 erg/sec ~ L x,bol = 6 x 10 42 erg/sec => dM bh /dt = 4 x 10 -3 M sun /yr

17. Circulation Flows Construct flows that simultaneously move in both radial directions with no net cooling or radial mass flow: cooling inflows balanced by bubble outflows This is not convection as in stellar interiors, the  S variations are more extreme Successful circulation flows: must look like cooling flows with dT/dr > 0 near center but with no cooling below ~T vir /3 must reproduce observed iron abundance profiles to achieve this must recirculate both mass and thermal energy out from the center of the flows

18. Mathews et al. 2003 Simple Steady State Circulation Flows Can low-density, heated bubbles carry enough gas upstream to balance the cooling inflow mass flux?

19. Mathews et al. 2003 Simple Steady State Circulation Flow in NGC 4472 Red: cooling inflow Green: bubble outflow Steady circulation flows with no net mass flux are possible Bubbles do not heat inflowing gas very much the emission-weighted profile is that of the cooling inflow; but bubbles may contribute to the X-ray spectrum Bubbles with larger mass m b require more heating at r h, but if m b is too large, there is no volume left for cool phase, f --> 0 Small bubbles move too slowly and also consume all available volume near r h, f--> 0 h = 3 r h = 5 kpc

20. Buote, Lewis, Brighenti & Mathews 2003 Radial Abundances in NGC 5044 A measure of integrated historical stellar enrichment are central abundance dips real? ironsilicon large metal enhancements in r < 100 kpc much larger than stellar R e r (kpc)

21. Buote, Lewis, Brighenti & Mathews 2003 More XMM-Chandra Abundances in NGC 5044 em = 0.83 solar => 70-80% of iron from SNIa within 100 kpc silicon/ironmagnesium sulfur oxygen Why do O and Mg vary differently? r (kpc)

22. Buote, Lewis, Brighenti & Mathews 2003 XMM Iron Abundances in NGC 5044 Total iron mass within r = 100 kpc is ~ 10 8 M sun from all historic SNIae? Iron in r < 100 kpcIron in 100 < r < 300 kpc z Fe ~ 0.1 - 0.2 solar (where is the missing iron?) Buote, Brighenti & Mathews 2004

23. De Grandi et al. 2004 Central Iron Abundance Peaks are Common in group NGC 507in 12 CF and 10 non-CF clusters Kim & Fabbiano 2004

24. De Grandi et al. 2004 Central Iron Abundance Peaks are Common in group NGC 507in 12 CF and 10 non-CF clusters Kim & Fabbiano 2004 about 200 kpc “excess” iron mass in CF clusters correlates with L B of central E galaxy Excess iron mass ~ total iron from all SNIae in central E

25. Mathews, Brighenti & Buote 2004 Time-dependant Cooling flows for NGC 5044 with f( r) assume fixed filling factor profile f(r ) for inflow begin with standard cooling flows for NGC 5044 with three f(r) no heating -- only radiative cooling range of flow: r h = 5 < r < r e = 500 kpc calculate for 10 Gyrs result: (dM/dt) cool (r h ) ~ 6 M sun /yr cooling flow is very insensitive to filling factor profile so choose constant...profile with f(r h ) = 0.5 as observed

26. Mathews, Brighenti & Buote 2004 Time-dependant Circulation flows for NGC 5044 Now assume no gas flows in past r h = 5 kpc The incoming mass flux at r h and stellar mass loss are heated by AGN and instantaneously circulated outward according to dp/dV Only the inflowing cool phase is computed Circulated gas may be heated further if  h > 0 Ignore bubble drag momentum exchange

27. Mathews, Brighenti & Buote 2004 Time-dependant Circulation flows for NGC 5044 Normalized recirculation probability: parameters are (m, n, r p,kpc, )

28. Mathews, Brighenti & Buote 2004 Time-dependant Circulation flows for NGC 5044 Spatially concentrated recirculation of gas without additional heating (  h = 0): Flow begins at t = 2.7 Gyrs After only ~ 1 Gyr, gas near r p cools Dotted lines are NGC 5044 observations unacceptable

29. Mathews, Brighenti & Buote 2004 Time-dependant Circulation flows for NGC 5044 Spatially extended recirculation of gas without additional heating (  h = 0): Temperature too low Density too high z Fe peak too low and broad Flow began at t = 2.7 Gyrs Flow is shown at t = 8 Gyrs when catastrophic cooling occurred unacceptable

30. Mathews, Brighenti & Buote 2004 Time-dependant Circulation flows for NGC 5044 Flows with additional heating continue until t = 13.7 Gyrs without cooling Spatially extended recirculation of heated gas (  h = 1.6 and 1.9) Luminosity of AGN in NGC 5044 is ~  h L h = 4 10 42 erg/s Temperature peak is reproduced Density is acceptable No gas flows into origin No gas cools Iron abundance peak from SNIae contains ~10 8 M sun of iron! All major attributes of 5044 are reproduced

32. Does the SNIa iron cool or mix into hot gas? SNIa with 10 51 ergs and M Fe = 0.7 M sun explodes in elliptical ISM: n e = 0.01 T = 10 7 equilibrium temperature profile after 5 x 10 4 years: Star-ISM boundary at 20 pc Diffusion zone

33. Cooling of an Iron-rich Plasma

34. Cooling plus Diffusion To avoid cooling, Fe must mix with ~5 M sun in the ISM If magnetic fields reduce the diffusion rate, the SNIa iron may cool z Fe T t cool Four mixing times t m 10 5, 10 7, 2x10 7, 2x10 8 yrs

39. Van Dokkum & Franx 1995 ~60 % of Ellipticals have Dusty Cores HST images

40. Brighenti & Mathews 2002 Heated Bubbles have Adiabatically Cooled Rims Gas adjacent to expanding bubbles is cooled by adiabatic expansion

41. Brighenti & Mathews 2002 Heated Bubbles have Adiabatically Cooled Rims Self-similar flow around spherical piston expanding into isothermal gas of decreasing density Gas temperature just beyond piston is lowered M = Mach No. at shock