The Kinetic Sunyaev-Zel'dovich effect of the Milky Way Halo

Virial shocks in galaxy and cluster halosYuval Birnboim Hebrew University of Jerusalem, Israel1What governs evolution of galaxies?

M100 and NGC1365 (AAO)

M87 (AAO)

SpiralsEllipticalColorBlueRedMassSmall-mediumSmall-hugeAgeYoungOldGasLotsLittle2Gas & Galaxies:Common wisdomHubble expansionGravitational instabilityShock heatingCoolingAngular momentumAccretion to galactic spiral diskStars, SN, feedback3Galaxy/Cluster segregation

Blumenthal, Faber, Primack & Rees 86 Rees & Ostriker (1977) Silk (1977) Binney(1977) White & Rees (1978):tcooltff hydrostatic halo + many objects (cluster)4

Evolution of radii of gas shells big haloT(k)diskshocked gascooling radiusBirnboim & Dekel 20035

T(k)Same stuff for a smaller halodiskno shock Cools like crazy!6When can gas be hydrostatic?(argument for the adiabatic case)

Ideal gas:

Gas in the haloIsentropic:

Power law profile:Homologeous collapse

7 Start with hydrostatic equilibrium:

The gravitational acceleration is:

Stable: small perturbation inwards increases the ratio of pressure to gravity

8

Birnboim & Dekel 2003Lets check the stability behind the shockfor non-adiabatic processes:

the ideal EOS:

Compression timeCooling time9Perturbation analysis of the force equation

(sub-sonic)(homology)10 and after some algebra:

So,

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Had there been a shock hereWouldve it been stable?Assume hypothetic shock there and find out.12Simulation confirms analytic model: shock when eff > crit=1.43

No free parameters, no fudge factors13Mvir [M] Cold Flows in Halosredshift z1013

1012

10110 1 2 3 4 51 (22%)2 (4.7%)M* of Press Schechterat z>1 most halos are M6x1011 clusterMhalo>DfilamentCosmological ContextMW: Halo is hot, filaments are hot.Dekel & Birnboim 2006Cold flowsAlways unstable(1D analysis)Groups, Clusters, satellites27Kere et al. 2005Kere et al. 2009

3D SPH hydro-simulations28

Ocvirk et al. 2008

2e12 halo, z=42e12 halo, z=2.53D Eulerian hydro-simulations

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Accretion at high-zWechsler et al 2002, Dekel et al. 2009

Agertz et al. 2009Dekel & Birnboim2006Keres et al. 05-0930Star forming galaxiesCold accretion vs. Merger induced star bursts

Dekel, Birnboim et al. 2009,NatureBX/BM/sBzK, 31z=2 disksSINS H survey

Frster Schreiber et al. 2009 Daddi et al. 2004

Bouch et al. 200732High accretion rate and galaxy structure: Clump clusters

Elmegreen et al. 2007Clumps in clump clusters: M=107-109M,D=~1kpc (Elmegreen et al. 07,09, SINS)Gas splashes into galaxies at ~200km/sec Turbulence in ISM is ~50km/sec Jeans mass goes up, disk becomes more Toomre stable 33

Ceverino, Dekel & Bournaud 2009

Genzel et al. 2010High accretion rate and galaxy structure: Clump clusters34ApplicationsThe galaxy bi-modalityHigh-z star forming galaxiesGroups and clustersTowards a solution of the overcooling problem of clusters(the high-riskhigh-gain part of the talk)35The cooling flow Problem in Cool Core ClustersNo cool (