1. Large Scale Structure of the Universe at high redshifts Large Scale Structure of the Universe at high redshifts M.Demianski, A.Doroshkevich and S.Gottloeber

2. LSS at small redshifts – luminous matter LSS at small redshifts – luminous matter

3. Ly- forest-LSS in DM & barions Three characteristics Three characteristics of absorber of absorber Redshift – z Width - b km/s Depth - N HI cm -2 and and UV background

4. Cosmological model

5. Properties of ~6000 absorbers 10 15 cm -2 >N HI > 10 12 cm -2 Properties of ~6000 absorbers 10 15 cm -2 >N HI > 10 12 cm -2

6. Metal systems (CIV) Metal systems (CIV)

7. Properties of observed LSS

8. PUZZLES PUZZLES 1. Weak redshift dependence of the PDFs, 1. Weak redshift dependence of the PDFs, P(b/ ), P(N HI / ), P(d sep / ) P(b/ ), P(N HI / ), P(d sep / ) 2. =const.(z), b =const.(z), b < b bg 3. Slow regular redshift variations of 3. Slow regular redshift variations of ~(1+z) 2 and ~(1+z) -2 ~(1+z) 2 and ~(1+z) -2

9. DM simulation L box =150h -1 Mpc, N p = 256 3, L cell =0.6h -1 Mpc L box =150h -1 Mpc, N p = 256 3, L cell =0.6h -1 Mpc Mass resolution: 2 10 7 M o, Mass resolution: 2 10 7 M o, Force resolution: 20h -1 kpc, Force resolution: 20h -1 kpc, Selected clusters: 10 < N p < 5000, =1.76 Selected clusters: 10 < N p < 5000, =1.76

10. Simulated clusters For colder clusters clusters N p ~ /3 N p ~ /3 For hotter For hotter clusters clusters N p ~3 N p ~3 Relaxation: Relaxation: f rel ~0.6-0.8 f rel ~0.6-0.8

11. Core-sampling approach L core =0.5h -1 Mpc

12. Conclusions

13. Probable causes of self similarity Deterministic character of simulations: Deterministic character of simulations: all structure properties are determined by all structure properties are determined by the initial power spectrum. the initial power spectrum. Zeldovich’ approximation Zeldovich’ approximation r i =(1+z) -1 [q i -B(z) S i (q)] r i =(1+z) -1 [q i -B(z) S i (q)] Power spectrum Power spectrum P(k)~k -3, k/k 0 > 1, k 0 ~0.15Mpc -1 P(k)~k -3, k/k 0 > 1, k 0 ~0.15Mpc -1

14. Real and simulated BBKS power spectrum Real and simulated BBKS power spectrum

15. The end The end

16. Possible interpretation Possible interpretation =const(z), W(x i )=const(z) =const(z), W(x i )=const(z) ~(1+z) -3 ~1/ ~(1+z) -3 ~1/ Version 1 – relaxed clouds Version 1 – relaxed clouds n abs ~(1+z) 3, S abs ~const. n abs ~(1+z) 3, S abs ~const. BUT ~(1+z) 2 BUT ~(1+z) 2 Version 2 -- expanded clouds Version 2 -- expanded clouds S abs ~(1+z) -p, n abs ~(1+z) 3+p S abs ~(1+z) -p, n abs ~(1+z) 3+p BUT =const., W(x i )=const(z) BUT =const., W(x i )=const(z)

17. Comparison with simulations. L box =100 h -1 Mpc, N p =(256) 3, L cell =0.4Mpc L box =100 h -1 Mpc, N p =(256) 3, L cell =0.4Mpc Z=0, 1, 1.5, 2, 2.5, 3, 4, 5 Z=0, 1, 1.5, 2, 2.5, 3, 4, 5 Two populations of clouds, and Two populations of clouds, and Strongly deterministic approach Strongly deterministic approach Previously – relaxed halos only Previously – relaxed halos only (galaxies, clusters of galaxies) (galaxies, clusters of galaxies)

18. 60 Mpc/h

23. PDFs for cloud velocities, W(U), mass function, W(M), and surface density, W(q)

24. PDFs for three principle sizes of clouds, L, w, h

25. PDFs for the velocity dispersions along three principle axes of clouds PDFs for the velocity dispersions along three principle axes of clouds

26. Mean characteristics High density clouds, L~ (1+z) 1/4, w~ (1+z) 1/2, h~(1+z) 1/2 V h ~ (1+z)-1/2. Low density clouds, L~w~h~ const(z) V h ~ const(z). Cores and envelopes

27. Measured power spectrum Measured power spectrum

28. Problems and prospects 1. Ly-ά emitters and population 1. Ly-ά emitters and population of earlier galaxies (~20 000 LBG) of earlier galaxies (~20 000 LBG) 2. DM compact objects 2. DM compact objects 3. First luminous objects - 3. First luminous objects - stars or galaxies stars or galaxies 4. Spatial distribution of metal 4. Spatial distribution of metal systems – bubbles ~2Mpc systems – bubbles ~2Mpc

29. DM simulation L box =150h -1 Mpc, N p = 256 3 L box =150h -1 Mpc, N p = 256 3 Mass resolution 2 10 7 M o, Force resolution 20kpc/h Mass resolution 2 10 7 M o, Force resolution 20kpc/h Selected clusters: 10 1.7 Selected clusters: 10 1.7 Mean comoving principal sizes: Mean comoving principal sizes: L~0.5h -1 Mpc, W~0.2h -1 Mpc, S~0.1h -1 Mpc L~0.5h -1 Mpc, W~0.2h -1 Mpc, S~0.1h -1 Mpc Velocity dispersions along principal directions: Velocity dispersions along principal directions:

30. Z~2 - 3 L gal ~10 26 erg/s/Hz/Mpc 3 L gal ~10 26 erg/s/Hz/Mpc 3 Giavalisco et al. 2004, GOODS, L QSO ~10 23 – 10 24 erg/s/Hz/Mpc 3, L QSO ~10 23 – 10 24 erg/s/Hz/Mpc 3,

31. Next Steps Detailed analysis of evolution of the Universe. Detailed analysis of evolution of the Universe. Properties of DM particles Properties of DM particles (composition, masses, stability). (composition, masses, stability). Shape of the small scale initial power spectrum at L<100 kpc. Shape of the small scale initial power spectrum at L<100 kpc. Galaxy and quasar formation. Galaxy and quasar formation. Reheating and reionization of the Reheating and reionization of the Universe. Universe. Etc…. Etc….

32. Real and simulated power spectrum Real and simulated power spectrum

33. Period of reionization

37. Metal systems (CIV) Metal systems (CIV)