Large Scale Structure of the Universe at high redshifts

1. Large Scale Structureof the Universeat high redshifts M.Demianski &A.Doroshkevich

2. LSS at small redshifts

3. Three characteristics of absorber Redshift – z Depth - NHIcm-2 Width - b km/s blending of absorbers

4. QSO spectra used QSR Z_emZ_minZ_maxNo HI lines Ref. 1055+461 4.16 2.8 4.16 998 Rough & Sargent 0000-260 4.11 3.4 4.1 431 Lu et al. 0055-259 3.66 3.0 3.6 534 Kim 1422+230 3.6 2.7 3.6 811 Rough & Sargent 0014+813 3.41 2.7 3.2 262 Hu et al. 0956+122 3.30 2.6 3.1 256 Hu et al. 0302-003 3.29 2.6 3.1 356 Kim 0636+680 3.17 2.5 3.0 531 Rough & Sargent 0636+680 3.17 2.4 3.1 313 Hu et al. 1759+754 3.05 2.4 3.0307 Djorgovski et al. 1946+766 3.02 2.4 3.0 461 Kirkman & Tytler 1107+485 3.0 2.1 3.0 609 Rough & Sargent 1347-246 2.63 2.1 2.6 361 Kim 1122-441 2.42 1.9 2.4 353 Kim 2217-282 2.41 1.9 2.3 262 Kim 1626-???2.32 1.5 2.2 281 Rough & Sargent 2233-606 2.24 1.5 2.2 293 Cristiani & D'Odorico 1101-264 2.15 1.6 2.1 277 Kim 0515-4411.72 1.5 1.7 76 Kim

5. Cosmological model

6. Self similarity and weak regular redshift variations of measured characteristics.

7. 1. All PDFs are weakly dependent from redshift. 2. Rapidly expanded regions. 3. Gaussianity of perturbations

8. Metal systems (CIV)

9. PUZZLES • 1. Weak redshift dependence of the PDFs, P(b/<b>), P(NHI/<NHI>), P(dsep/<dsep> • 2. <b>=const.(z) • 3. Slow regular redshift variations of <NHI> ~(1+z)2 and <dsep>~(1+z)-2

10. Possible interpretation • <b>=const(z), W(xi)=const(z) • <dsep/(1+z)>~(1+z)-3~1/<nabsSabs> • Version 1 – relaxed clouds • nabs~(1+z)3, Sabs~const. • BUT <NHI>~(1+z)2 • Version 2 -- expanded clouds • Sabs~(1+z)-p, nabs~(1+z)3+p • BUT <b>=const., W(xi)=const(z)

11. Comparison with simulations. Lbox=100 h-1Mpc, Np=(256)3 , Lcell=0.4Mpc • Z=0, 1, 1.5, 2, 2.5, 3, 4, 5 • Two populations of clouds, and • Strongly deterministic approach • Previously – relaxed halos only • (galaxies, clusters of galaxies)

12. 60 Mpc/h

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

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

15. PDFs for the velocity dispersionsalong three principle axes of clouds

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

17. Real and simulated power spectrum

18. Probable causes of self similarity • Zeldovich’ approximation • ri=(1+z)-1[qi-B(z)Si(q)] • Power spectrum • P(k)~k-3, k/k0> 1, k0~0.15/Mpc

19. The end

20. Measured power spectrum

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

22. Z~2 - 3 • Lgal ~1026 erg/s/Hz/Mpc3 Giavalisco et al. 2004, GOODS, • LQSO~1023 – 1024 erg/s/Hz/Mpc3,

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

24. Period of reionization

28. Metal systems (CIV)