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) MrMr (~5h -1 Mpc) Morphology ( )

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

5. 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 Here Now The Observed Universe on a past light cone surface Decoupling Epoch Dark Ages The First ObjectsHI +  + He p + e - +  + He Reionization Epoch Structure Formation & Evolution Acceleration (Dark Energy Dominated) Deceleration (Matter Dominated) Inflation

6. Simulation of the SDSS Survey Region of the Universe 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 ) KASI 2012. 2. 18 A progress report

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 ρ r,g Map ρ r,g to the matter density field ρ r,m (z=0) Estimate v pec 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  g (z=0) from ρ r,m (z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρ r,m (initial) Gaussianize the field. @ Add small-scale power to match the  CDM 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 ρ r,g Map ρ r,g to the matter density field ρ r,m Estimate v pec 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  g (z=0) from ρ r,m (z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρ r,m (initial) Gaussianize the field. @

10. We need the galaxy – halo – matter relation (biasing). Popular halo bias model δ halo = Σb i δ matter i does not work. (Even worse for the halo number density field.) * Subhalos from an N-body simulation (2048 3 m2048 3 p1024 3 v & WMAP3y  CDM ) halo # density halo mass density

11. ln(1+δ h ) ln(1+δ m ) z=0z=0.5z=1

12. β1β1 β2β2 β0β0

13. Stochastic term Δ m =β 0 + β 1 Δ h + β 2 Δ h 2 + ε(?)

14. Reconstruction Method Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρ r,g Map ρ r,g to the matter density field ρ r,m Estimate v pec 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  g (z=0) from ρ r,m (z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρ r,m (initial) Gaussianize the field. @

15. (Jenkins 2010; Gramann 1993) where ∇ 2 ф (2) =δ (2) =m 2v

17. Estimation of the peculiar velocities (2 nd -order Lagrangian perturbation theory) and ∇  g 

18. Reconstruction Method Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρ r,g Map ρ r,g to the matter density field ρ r,m Estimate v pec 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  g (z=0) from ρ r,m (z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρ r,m (initial) Gaussianize the field. @

19. λ=5R G Backward evolution of the potential   g at high z  initial 

20. Halos at z=0  estimate matter at z=0   g at high z  initial  Genuine initial  -2, -1, +1, +2σ contours

21. Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρ r,g Map ρ r,g to the matter density field ρ r,m Estimate v pec 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  g (z=0) from ρ r,m (z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρ r,m (initial) Gaussianize the field. @ Add small-scale power to match the  CDM P(k) Forward evolve the initial conditions

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

23. 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

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

25. KIAS-VAGC (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 Base catalog: 583.9K redshifts in NYU-VAGC LSS sample (34.6K have borrowed redshifts) - some galaxies missing due to fiber collision & brightness Addition: 13.2K redshifts are added (1,608 galaxies with r<14.5) from other catalogs such as UZC, PSCZ, RC3, and 2dF. Angular selection function recalculated. The survey mask is the same as NYU-VAGC. 5.8% of the combined catalog still have borrowed redshifts. Corrections: wrong central position, mergers, part of large objects Parameters: Early(E/S0) and late(S/Irr) morphological parameter given to all galaxies. Seeing- and inclination-corrected Petrosian radius, concentration index, △ (g-i) color gradient measured from images. Higher spectroscopic completeness! Wider magnitude range!

26. 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

27. 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) 7698 sq. deg 0° 10° 9h9h 10 h

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

29. BEST A volume- limited sample with the largest # of galaxies with Mr < - 20.09

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

31. Effects of non-periodic ‘SDSS’ boundaries

34. Given a galaxy catalog in redshift space together with survey mask & SF Cluster identification and compression Calculate galaxy mass density field ρ r,g Map ρ r,g to the matter density field ρ r,m Estimate v pec 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  g (z=0) from ρ r,m (z=0) and evolve it backward in time using the 2nd-order perturbation theory Get the reconstructed initial density field ρ r,m (initial) Gaussianize the field. @ Add small-scale power to match the  CDM P(k) Forward evolve the initial conditions

35. Large-scale background density  20 200 h - 1 Mpc E/S0 & S/Irr galaxies with M r <-19

36. 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. 2 nd -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.

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

38. Cosmology at KASI ! Thanks & Best Wishes

39. 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.