Large scale structure of the universe at high redshifts
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Large Scale Structure of the Universe at high redshifts. M. Demianski , A. Doroshkevich and S.Gottloeber. LSS at small redshifts – luminous matter. Ly- forest-LSS in DM & barions. Three characteristics of absorber Redshift – z Width - b km/s Depth - N HI cm -2

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Large scale structure of the universe at high redshifts

Large Scale Structureof the Universeat high redshifts

M.Demianski,A.Doroshkevich

and S.Gottloeber


Lss at small redshifts luminous matter
LSS at small redshifts – luminous matter


Ly forest lss in dm barions
Ly- forest-LSS in DM & barions

  • Three characteristics

    of absorber

    Redshift – z

    Width - b km/s

    Depth - NHIcm-2

    and

    UV background



Properties of 6000 absorbers 10 15 cm 2 n hi 10 12 cm 2
Properties of ~6000 absorbers 1015cm-2 >NHI > 1012cm-2




Puzzles
PUZZLES

  • 1. Weak redshift dependence of the PDFs,

    P(b/<b>), P(NHI/<NHI>), P(dsep/<dsep>)

  • 2. <b>=const.(z), b < bbg

  • 3. Slow regular redshift variations of

    <NHI> ~(1+z)2 and <dsep>~(1+z)-2


Dm simulation
DM simulation

  • Lbox =150h-1Mpc, Np= 2563 , Lcell=0.6h-1Mpc

  • Mass resolution: 2 107Mo,

  • Force resolution: 20h-1kpc,

  • Selected clusters: 10 < Np < 5000, =1.76


Simulated clusters

For colder

clusters

Np~<Np>/3

For hotter

clusters

Np~3<Np>

Relaxation:

frel~0.6-0.8

Simulated clusters


Core sampling approach l core 0 5h 1 mpc
Core-sampling approachLcore=0.5h-1Mpc



Probable causes of self similarity
Probable causes of self similarity

  • Deterministic character of simulations:

    all structure properties are determined by

    the initial power spectrum.

  • Zeldovich’ approximation

  • ri=(1+z)-1[qi-B(z) Si(q)]

  • Power spectrum

  • P(k)~k-3, k/k0> 1, k0~0.15Mpc-1




Possible interpretation
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)


Comparison with simulations
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)



Pdfs for cloud velocities w u mass function w m and surface density w q
PDFs for cloud velocities, W(U), mass function, W(M), and surface density, W(q)



Pdfs for the velocity dispersions along three principle axes of clouds
PDFs for the velocity dispersionsalong three principle axes of clouds


Mean characteristics
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



Problems and prospects
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


Dm simulation1
DM simulation

  • Lbox =150h-1Mpc, Np= 2563

  • Mass resolution 2 107Mo, Force resolution 20kpc/h

  • Selected clusters: 10 < Np < 5000, > 1.7

  • Mean comoving principal sizes:

  • L~0.5h-1Mpc, W~0.2h-1Mpc, S~0.1h-1Mpc

  • Velocity dispersions along principal directions:


Z 2 3
Z~2 - 3

  • Lgal ~1026 erg/s/Hz/Mpc3

    Giavalisco et al. 2004, GOODS,

  • LQSO~1023 – 1024 erg/s/Hz/Mpc3,


Next steps
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….





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