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Dark Matter Halos

A.Klypin. Dark Matter Halos. GADET. Springel, SDM White. PKDGRAV - GASOLINE. Quinn, Steidel, Wadsley, Governato, Moore. ART. Kravtsov, Klypin, N.Gnedin, Gottlober. ENZO. Bryan, Norman. Major codes:. N-body Hydro Cooling/Heating/SF Metal enrichment Radiative transfer

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Dark Matter Halos

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  1. A.Klypin Dark Matter Halos

  2. GADET Springel, SDM White PKDGRAV - GASOLINE Quinn, Steidel, Wadsley, Governato, Moore ART Kravtsov, Klypin, N.Gnedin, Gottlober ENZO Bryan, Norman Major codes: • N-body • Hydro • Cooling/Heating/SF • Metal enrichment • Radiative transfer • Multistepping/Multiple masses

  3. Non-linear evolution: from Zeldovich approximation to DM halos

  4. Local Group:z=0 7

  5. Local Group:z=1 8

  6. Local Group:z=7 9

  7. Mass function of distinct halos Warren etal 2005: 13 sims each with 1G particles • It started long ago: 32 years to be precise • Now we live through 5th generation of this.

  8. Halo Mass Function depends on environment • Sheth&Tormen 2002 • GottlÖber etal 2003

  9. Clustering: DM halos and L • Conroy, Wechsler, Kravtsov (2005): N-body only • Get all halos from high-res simulation • Use maximum circular velocity (NOT mass) • For subhalos use Vmax before they became subhalos • Every halo (or subhalo) is a galaxy • Every halo has luminosity: LF is as in SDSS • No cooling or major mergers and such. Only DM halos • Reproduces most of the observed clustering of galaxies 12

  10. SDSS: z=0 DM galaxies DM SDSS

  11. DEEP: z=1

  12. Dark Matter and Galaxies • - Central DM closely correlates with L: Tully-Fisher, Faber-Jackson • - Morphology-density relation: morphology is mostly defined by halo mass. • - Environment (how many neighbors) is just an indicator of halo mass • Young etal(2003-5), Berrier etal(2005) : Halo occupation distribution→the same conclutions

  13. Cusps: simulations Diemand etal 2004

  14. Tasitsiomi etal 2004 Navarro etal 2004 Slope gets shallower with decreasing radius, but it does not go below -1 Consistent with what other groups found

  15. Profiles are NOT NFW NFW ρ(r)=ρo exp(-2nr1/n)+<ρ> n=6-8 3D Sersic NFW Navarro etal 2004 Merritt, Navarro 2004 Prada etal 2005

  16. Average profiles of Milky Way-size halos

  17. Infall velocities on halos of different massPrada et al 2005

  18. RMS velocity of isolated halos Full: simulations Dash: solution of Jeans equation

  19. SDSS and LCDM: surface number density of satellites around isolated galaxies LCDM

  20. Evolution of Halo structure • Most of the accreted mass stays in the outer region of halo. Diemand etal 2005

  21. Evolution of Halo structure Dwarf Halos at high z cusp evolves very little. Colin etal 2003

  22. Halo Concentrations Bullock etal 2003

  23. VoidsR>10Mpc Patiri et al 2006: SDSS

  24. Number-density Profiles of Voids: n(R)/<n> Patiri et al 2006 SDSS LCDM

  25. DM in central parts of galaxies • Adiabatic compression: old approximation • Adiabatic compression: Gnedin etal 2004

  26. How it works

  27. Structure of our Galaxy Prada etal 2004

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