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E  L

E  L. Comma galaxies. The Cosmic Runner (Park et al. 2005; Choi et al. 2010). Morphology – Luminosity – Local Density relation (Park et al. 2007). Morphology ( ). M r. (~5h -1 Mpc). Early-type fraction vs clustercentric radius / luminosity. -20.5~-22.5. -19~-20.5.

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E  L

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  1. E  L Comma galaxies

  2. The Cosmic Runner (Park et al. 2005; Choi et al. 2010)

  3. Morphology – Luminosity – Local Density relation (Park et al. 2007) Morphology ( ) Mr (~5h-1Mpc)

  4. Early-type fraction vs clustercentric radius / luminosity -20.5~-22.5 -19~-20.5 -17~-19 clustercentric radius

  5. Inflation The Observed Universe on a past light cone surface Deceleration (Matter Dominated) Reionization Epoch Decoupling Epoch Dark Ages Acceleration (Dark Energy Dominated) Here Now Structure Formation & Evolution The First Objects HI + g + He p + e- + g + He T H E H O R I Z O N R U N Kim, Park, Gott & Dubinski (2009) http://astro.kias.re.kr/Horizon_Run

  6. KASI 2012. 2. 18 Simulation of the SDSS Survey Region of the Universe A progress report KASI-YITP Joint-Workshop Feb. 18, 2012 Changbom Park (Korea Institute for Advanced Study) and Juhan Kim (KIAS), Yun-Young Choi (Kyunghee), Hyunbae Park(Austin), Inh Jee(Austin)

  7. Simulation of the SDSS Survey region Purposes To study the past history of environmental effects on the objects in the SDSS survey region. Possible because the evolution of the matter field on small scales is affected by the large-scale structures through the transfer of power from large to small scales.

  8. Method Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρr,g Map ρr,g to the matter density field ρr,m(z=0) @ Estimate vpec using the 2nd-order perturbation theory of the continuity equation, and correct galaxy positions for redshift effects goto @ if a convergence for correction is not reached, and iterate Calculate the smooth fg (z=0) from ρr,m(z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρr,m(initial) Gaussianize the field. Add small-scale power to match the LCDM P(k) Forward evolve the initial conditions

  9. Reconstruction Method Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρr,g Map ρr,g to the matter density field ρr,m @ Estimate vpec using the 2nd-order perturbation theory of the continuity equation, and correct galaxy positions for redshift effects goto @ if a convergence is not reached, and iterate Calculate the smooth fg (z=0) from ρr,m(z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρr,m(initial) Gaussianize the field.

  10. We need the galaxy – halo – matter relation (biasing). Popular halo bias model δhalo = Σbiδmatteri does not work. (Even worse for the halo number density field.) * Subhalos from an N-body simulation (20483m20483p10243v & WMAP3y LCDM ) halo # density halo mass density

  11. z=0 z=0.5 z=1 ln(1+δm) ln(1+δh)

  12. Reconstruction Method Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρr,g Map ρr,g to the matter density field ρr,m @ Estimate vpec using the 2nd-order perturbation theory of the continuity equation, and correct galaxy positions for redshift effects goto @ if a convergence is not reached, and iterate Calculate the smooth fg (z=0) from ρr,m(z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρr,m(initial) Gaussianize the field.

  13. (Jenkins 2010; Gramann 1993) where ∇2ф(2)=δ(2)=m2v

  14. where ∇2ф(2)=δ(2)=m2v

  15. Estimation of the peculiar velocities (2nd-order Lagrangian perturbation theory) and ∇fg=r

  16. Reconstruction Method Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρr,g Map ρr,g to the matter density field ρr,m @ Estimate vpec using the 2nd-order perturbation theory of the continuity equation, and correct galaxy positions for redshift effects goto @ if a convergence is not reached, and iterate Calculate the smooth fg (z=0) from ρr,m(z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρr,m(initial) Gaussianize the field.

  17. Backward evolution of the potential  Fg at high z  initial r λ=5RG

  18. -2, -1, +1, +2σ contours Halos at z=0  estimate matter at z=0 Fg at high z  initial r Genuine initial r

  19. Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρr,g Map ρr,g to the matter density field ρr,m @ Estimate vpec using the 2nd-order perturbation theory of the continuity equation, and correct galaxy positions for redshift effects goto @ if a convergence is not reached, and iterate Calculate the smooth fg (z=0) from ρr,m(z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρr,m(initial) Gaussianize the field. Add small-scale power to match the LCDM P(k) Forward evolve the initial conditions

  20. 초기  현재 Final conditions from the true initial density field Final conditions from the reconstructed initial density field with random small-scale fluctuations

  21. Final conditions from the true or reconstructed initial conditions More works to do 1. Constrained small-scale field 2. Application to the SDSS with non-periodic boundaries

  22. Effects of non-periodic boundaries Gravitational shear tensor from full 1024h-1Mpc cube from a 512h-1Mpc subcube From a 256h-1Mpc subcube (Park, Kim & Park 2010)

  23. SDSS DR7: KIAS-VAGC Northern Galactic Cap (Choi, Han & Kim, JKAS, 2010; http://jkas.kas.org) A SDSS galaxy catalog with 597.1K(10<r<17.6) + 114.3K(17.6<r<17.77) redshifts

  24. SDSS DR7: KIAS-VAGC Northern Galactic Cap (Choi et al. 2010) A SDSS galaxy catalog with 597.1K(10<r<17.6) + 114.3K(17.6<r<17.77) redshifts (bright galaxies added, extinction & K-corrections, L-evolution corrected) 10° 0° 10h 9h 7698 sq. deg

  25. The Sloan Great Wall (Gott et al. 2005)

  26. BEST A volume-limited sample with the largest # of galaxieswith Mr < -20.09

  27. Boundary Effects: a case when the analyses remain 60 h-1Mpc away from all boundaries (Park, Park & Kim 2011)

  28. Effects of non-periodic ‘SDSS’ boundaries

  29. Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρr,g Map ρr,g to the matter density field ρr,m @ Estimate vpec using the 2nd-order perturbation theory of the continuity equation, and correct galaxy positions for redshift effects goto @ if a convergence is not reached, and iterate Calculate the smooth fg (z=0) from ρr,m(z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρr,m(initial) Gaussianize the field. Add small-scale power to match the LCDM P(k) Forward evolve the initial conditions

  30. Large-scale background density r20 E/S0 & S/Irr galaxies with Mr<-19 200 h-1Mpc

  31. SUMMARY   Reconstructing the initial density field within the SDSS survey region. Replaying the structure formation in this local volume of the universe. For this purpose we studied 1. halo-matter density connection 2. effects of non-periodic boundaries 3. 2nd-order perturbation theory of the continuity equation for peculiar velocity correction and initial density reconstruction. Properties of the objects formed in the simulation can be statistically compared with those of the observed SDSS galaxies. * Possible to know the past history of evolution of objects located in different environments, and also gives us information on the environmental parameters that cannot be directly obtained observationally. Better understanding of formation and evolution of galaxies in conjunction with large-scale structures in the universe.

  32. * Understanding cosmology & GF closely coupled. GF depends on environment.

  33. Cosmology at KASI ! Thanks & Best Wishes

  34. Title: Simulation of the SDSS Survey Region of the Universe Speaker:  Prof. Changbom Park (Korea Institute for Advanced Study) Date & Time:Place: Abstract: We plan to reconstruct the large-scale initial density field from the distribution of galaxies observed by the Sloan Digital Sky Survey (SDSS). After adding the small-scale fluctuations to match the power spectrum to that of the standard LCDM model, we make a cosmological N-body simulation of structure formation from the initial conditions. Properties of the objects formed in the simulation can be statistically compared with those of the observed SDSS galaxies. The simulation makes it possible to know the past history of evolution of objects located in different environments, and also gives us information on the environmental parameters that cannot be directly obtained observationally. It is hoped that this comparative study leads us to better understanding of formation and evolution of galaxies in conjunction with large-scale structures in the universe.

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