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Circulation Flows
Fabrizio Brighenti (Bologna)
David Buote (UC Irvine)
Cooling flows with bubble return!
Bill Mathews (UC Santa Cruz)
O’Sullivan et al. 2001
X-ray Luminosity of Elliptical Galaxies
Observed SNIa rate in E galaxies SNu = 0.16 per LB = 1010 per 100 yrs
Is almost certainly too high
(Cappellaro et al. 1999)
ROSAT
O’Sullivan et al. 2001
X-ray Luminosity of Elliptical Galaxies
Range of Lx/LB determined by extent of circumgalactic gas
Mathews & Brighenti 1998Lx/LB = (rex/re)0.6
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. 1999Ponman et al. 1994
NGC 5044
Optically Dark Groups with Mvir known from X-ray Observations
LB ~ Mvir may result from hierarchical assemblySeveral (all?) dark groups are baryonically “closed” like rich clusters:fb = Mbary/Mtot ~ 0.16 (WMAP)
NGC 6482
Caon et al. 2001
Warm gas in NGC 5044 -- Stellar Ejecta?
H + [NII] very disturbedwith crazy velocity fieldscale > SNIa remnantsejecta receives momentum
6 kpc
stellar isophotes
Extended Dusty Core in NGC 5044 -- Stellar Ejecta?
B-Iimage
12 x 12 kpcGoudfrooij 1991
Van Dokkum & Franx 1995Verdoes Kleijn et al. 1999
~50-60% of Normal Ellipticals and ~90% of Radio-Jet Ellipticals have Dusty Cores
HSTimages
Mathews & Brighenti 2003
Accelerated Cooling in Dusty Stellar Ejecta
Even dusty gas at 107 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
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 remnantsFilling factor f ~ 0.5 in r < 20kpc
XMM image is smooth beyond ~30 kpc
Buote, Lewis, Brighenti, Mathews 2003
Gas Temperature Profile in NGC 5044r (kpc) r (kpc)
Multiphase temperature Tc ~ T* ≤ T ≤ Th
but no gas with T ≤ Tc
(dM/dt)cool < 0.4 Msun /yr expected: ~5 Msun /yr
2T -- a better fit to data:1T fit to data:
Sun et al. 2003
Gas Temperature Profiles in Groups & ClustersGroups Clusters
Allen et al. 2001
dT/dr > 0 at small radii
Buote, Lewis, Brighenti, Mathews 2003
2T Multi-phas Emission in NGC 5044r (kpc) r (kpc)
Cool
Cool phase dominates inr ≤ 30 kpc
Filling factor of cool gas is f ~ 0.5 in r < 20 kpc
Global Properties of NGC 5044 E/group
r
(kpc)
Mgas
(Msun)
M*
(Msun)
Mtot
(Msun)
M Fe,gas
(Msun)
robs 327 13x1011 5.8x1011 2.0x1013 3.5x108
rvir 870 45x1011 7.4x1011 3.9x1013 9.0x108
Mbary/Mtot MFe/LB
5044 group 0.14 0.006
Rich clusters 0.13 - 0.17 0.015
ReE = 10 kpc LB,E = 4.5x1010 ∑LB,dwarfs = 10x1010
Buote, Brighenti & Mathews 2004
160
missing iron~WMAP baryons
Global Energetics of NGC 5044 E/groupEnergy in cavities Ecav = PfV = 1 x 1058 erg
Total SN energy Esn = 8 x 1060 erg
Gas binding energy Ebind = Eth = ∫thdV = 2 x 1061 erg
Black hole mass Mbh = 7.6x10-5 M*1.12 = 6 x108 Msun
Haring & Rix 2004
Black hole energy Ebh = .1 Mbh c2 = 1 x 1062 erg
to retain gas: the efficiency of black hole heating is < 0.02 power to maintain low density phase: PfV/tbuoy ~ 1043 erg/sec
~ Lx,bol = 6 x 1042 erg/sec
=> dMbh/dt = 4 x 10-3 Msun/yr
Circulation FlowsConstruct 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 ~Tvir/3 must reproduce observed iron abundance profiles to achieve this must recirculate both mass and thermal energy out from the center of the flows
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?
Mathews et al. 2003
Simple Steady State Circulation Flow in NGC 4472
Red: cooling inflowGreen: bubble outflow
Steady circulation flows with no netmass flux are possible
Bubbles do not heat inflowing gas very much the emission-weighted <T> profile is that of the cooling inflow; but bubbles may contribute to the X-ray spectrum
Bubbles with larger mass mb require more heating at rh, but if mb 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 rh, f--> 0
h = 3rh = 5 kpc
Buote, Lewis, Brighenti & Mathews 2003
Radial Abundances in NGC 5044 A measure of integrated historical stellar enrichment
are central abundance dips real?
iron silicon
large metal enhancements in r < 100 kpc much larger than stellar Re
r (kpc) r (kpc)
Buote, Lewis, Brighenti & Mathews 2003
More XMM-Chandra Abundances in NGC 5044
<zSi/zFe>em = 0.83 solar => 70-80% of iron from SNIa within 100 kpc
silicon/iron magnesium sulfur oxygen
Why do O and Mg vary differently?
r (kpc) r (kpc)
Buote, Lewis, Brighenti & Mathews 2003
XMM Iron Abundances in NGC 5044
Total iron mass within r = 100 kpc is ~ 108 Msun from all historic SNIae?
Iron in r < 100 kpc Iron in 100 < r < 300 kpc
zFe ~ 0.1 - 0.2 solar (where is the missing iron?)
Buote, Brighenti & Mathews 2004
De Grandi et al. 2004
Central Iron Abundance Peaks are Commonin group NGC 507 in 12 CF and 10 non-CF clusters
Kim & Fabbiano 2004
De Grandi et al. 2004
Central Iron Abundance Peaks are Commonin group NGC 507 in 12 CF and 10 non-CF clusters
Kim & Fabbiano 2004
about 200 kpc
“excess” iron mass in CF clusters correlates with LB of central E galaxy
Excess iron mass ~ total iron from all SNIae in central E
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: rh = 5 < r < re = 500 kpc calculate for 10 Gyrs result: (dM/dt)cool(rh) ~ 6 Msun/yr
cooling flow is very insensitive to filling factor profile so choose constant ...profile with f(rh) = 0.5 as observed
Mathews, Brighenti & Buote 2004
Time-dependant Circulation flows for NGC 5044
Now assume no gas flows in past rh = 5 kpc
The incoming mass flux at rh and stellar mass loss are heated by AGN and instantaneously circulated outward according to dp/dVOnly the inflowing cool phase is computedCirculated gas may be heated further if h > 0
Ignore bubble drag momentum exchange
Mathews, Brighenti & Buote 2004
Time-dependant Circulation flows for NGC 5044
Normalized recirculation probability:
parameters are (m, n, rp,kpc, <h>)
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 GyrsAfter only ~ 1 Gyr, gas near rp cools
Dotted lines areNGC 5044 observations
unacceptable
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 highzFe peak too low and broad
Flow began at t = 2.7 GyrsFlow is shown at t = 8 Gyrs when catastrophic cooling occurred
unacceptable
Mathews, Brighenti & Buote 2004
Time-dependant Circulation flows for NGC 5044Flows 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 ~hLh = 4 1042 erg/sTemperature peak is reproduced Density is acceptableNo gas flows into originNo gas coolsIron abundance peak from SNIae contains ~108 Msun of iron!
All major attributes of 5044 are reproduced
Does the SNIa iron cool or mix into hot gas?SNIa with 1051 ergs and MFe = 0.7 Msun explodes in elliptical ISM: ne = 0.01 T = 107
equilibrium temperature profile after 5 x 104 years:
Star-ISM boundary at 20 pc
Diffusion zone
Cooling of an Iron-rich Plasma
Cooling plus Diffusion
To avoid cooling, Fe must mix with ~5 Msun in the ISM
If magnetic fields reduce the diffusion rate, the SNIa iron may cool
zFe
T
tcool
Four mixing times tm
105, 107, 2x107, 2x108 yrs
Van Dokkum & Franx 1995
~60 % of Ellipticals have Dusty Cores
HSTimages
Brighenti & Mathews 2002
Heated Bubbles have Adiabatically Cooled Rims
Gas adjacent to expanding bubbles is cooled by adiabatic expansion
Brighenti & Mathews 2002
Heated Bubbles have Adiabatically Cooled RimsSelf-similar flow around spherical piston expanding into isothermal gas of decreasing density
Gas temperature just beyond piston is lowered
M = Mach No. at shock