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2005. 2. 16 - 19 Changbom Park (Korea Institute for Advanced Study)

Workshop for Underground Experiments and Astroparticle Physics. Dark Matter and Clustering Motivation and Findings on Dark Matter from the Study of Structure Formation. Dark Matter. 2005. 2. 16 - 19 Changbom Park (Korea Institute for Advanced Study). DM.

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2005. 2. 16 - 19 Changbom Park (Korea Institute for Advanced Study)

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  1. Workshop for Underground Experiments and Astroparticle Physics Dark Matterand ClusteringMotivation and Findings on Dark Matter from the Study of Structure Formation Dark Matter 2005. 2. 16 - 19 Changbom Park (Korea Institute for Advanced Study)

  2. DM Theme:Constraints on DM from Clustering of Matter Intimate relation between DM & structure formation because DM has been the gravitationally dominant component of the material universe after teq, and have been controlling the structure formation.

  3. What did we learn about DM from δρ & CMB ΔT? • Matter composition‘What’ and how much are there in our universe? • Properties of each matter componentSpatial distribution (uniform, clustered) Equ. of state

  4. Evolution of Modern Cosmology LSS CMBR 1917Einstein’s static model 1922External galaxies 22-24Friedmann’s models 29Expansion of space 50s Gravitational Instability(GI) Theory 29Big Bang model 65 Discovery of CMBR 70s BB+(γ,ν; baryon)+GI

  5. LSS CMBR 70s BB+(γ,ν; baryon)+GI Dark matter 82Inflation 80s CMBR dT/T < 10-4 Late70s Discovery of LSS mid80 SCDM Model BB+Inflation+(γ,ν; baryon, CDM)+GI 92 COBE dT/T~10-5 92 LSS P(k) Standard Model ruled out 00-03 WMAP Cℓ 98 Accelerating expansion 2005 Concordance LCDM Model BB+Inflation+(γ,ν; baryon, CDM; Dark E)+GI SDSS JWST Planck ?

  6. Energy Contents of the Universe Dark Energy(~73%; CC or dynamical?) + Non-baryonic Dark Matter(~23%; cold) + Baryon invisible(~4%; MACHOs, ionized gas-IG-intracluster) + visible(~0.3%; *s) Radiation + Neutrino Dark Energy Dark Matter If primordial gaussian adiabatic, scale-invariant density fluctuations

  7. Motivation for Dark MatterExistence through gravitational effects only Dark Matter Missing mass(baryon)  non-baryonic  DE 1. DM associated with galaxies & clusters [Ostriker..74; Einasto..74; Zwicky33] [Dark halos] stability of galaxies, clusters of galaxies 2. Baryonic DM [brown dwarfs] *s with m<0.08Mo? [Why mass & L should be correlated?] *s with m>Mo 95% light but m<Mo >75% mass [Ly-a clouds at high z] not seen now [Nucleosynthesis] Omega_B=0.02~0.1 vs Omega_Bobs=~0.006 (solar neighborhood) 3. Non-baryonic DM [Dynamical estimate of Omega] Omega_m=0.2~0.3 [Inflationary scenarios and flat universe] Omega_tot=1 4. Growth of matter fluctuations & epoch of structure formation

  8. δnow ~ 1 and δ(t) ~ a(t) in Einstein-de Sitter U  δdec(theory) ~ 10-3 but δdec(obs) ~10-5

  9. Consider DM which is NL at aeq !  Structure formation starts at aeq earlier than adec Baryon falls into the potential wells developed by DM adec a0 aeq

  10. Evolution of large scale density fluctuations in RDE & MDE During RDE : δm frozen (total grow=2.5) – Meszaros effect (for k ~ 0)

  11. Weighing Dark Matter Dark Matter CMBR Power Spectrum (z ~ 103) – Amplitude of Sachs-Wolfe effects: Ωtot ~1 – Amplitude of PS at subhorizon scales : Ωm – First 3 Doppler peaks : shape  ΩB = 0.04 (agreement btw z=103 & 109!) location  Ωtot ~1  Ωm Ly-a forest clouds (z ~ 3) – abundance vs ionizing photons  ΩB = 0.04 Galaxy clusters (z ~ 0) – X-ray emission of hot gas  ΩB = 0.04

  12. Initial conditions  Gravitational forcing, baryon loading Initial phase of osc. the same for all modes  peaks & troughs as a function of wavenumber (Doppler peaks) Cosmic Microwave Background Anisotropy

  13. Shape of ΔT/T Power Spectrum 1∼0.1rH fluc. with initially coherent phases Oscillation & Doppler effect Radial averaging & radiation diffusion Super-horizon scale fluc. SW effect Enhances the compressional phase !

  14. WMAP CMBR PS - baryon oscillation

  15. Hotlike babies?Coldlike old men? Horizon of human knowledge is expanding SDSS V ~ 102 CfA V ~ 10-4 Horizon V SKorea ~ 102 Seoul MPA ~ 10-4 Earth Surface 2004 SDSS 1986 CfA

  16. HDM?CDM? Clustering differences * observed LSS * fingers-of-god Epoch of formation of massive structures * 1st NL structures CDM : NR much before aeq

  17. HDM Real Space Matter CDM Real Space Galaxies HDM Z Space Matter CDM Z Space Galaxies

  18. HDM? CDM? Clusters of galaxies mass function High-z quasars Galaxy formation scenario top-down (pancake) vs bottom-up (hierarchical)

  19. Dark Energy Dynamics at horizon scale Affected by matter composition Riess..04

  20. PRECISION COMPARISON between cosmological models with the real universe • Validity of CDM • Initial conditions • Growth by gravitational instability • weakly interacting & cold matter ΛCDM Simulation(Kim & Park 2004) PMTree code(Dubinski, Kim, Park 2003) 20483 mesh (initial condition) 20483 (8.6G) CDM particles 1024 & 5632 h-1Mpc size boxes 50 & 275 h-1kpc force resolutions (Park et al. 1994) (Tegmark et al. 2004)

  21. LCDM1024

  22. Sloan Digital Sky Survey 1. Imaging of North Galactic Cap 2.5m APO telescope with a mosaic CCD camera u, g, r, i, z photometric bandpasses  selected for spectroscopy 2. Spectroscopy ~ 106 galaxies & 105 quasars with rms z-error ~ 30 km/s 3. Samples Main Galaxies: rPet < 17.77 ; Quasars Luminous Red Galaxies (LRG): z<0.4 & >0.4 samples

  23. 3D View of SDSS

  24. 3D View of a mock SDSS HOD galaxy formation prescription

  25. Way to the Future Measure Ωm , ΩB & ΩΛ ( Ωtot ) more accurately Measure eq. of state of DE component Find the clustering of DM at small scales through CMB anisotropy, LSS clustering, LS peculiar velocity field, high-z distance indicator, gravitational lensing New generation telescopes dedicated 8m, 30~100m optical, multi-λ New generation simulations matching the entire history of the universe

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