large scale structure of the universe at high redshifts

Large Scale StructureLarge Scale Structureof the Universeof the Universeat high redshiftsat high redshifts

M.M.DemianskiDemianski,, A.A.Doroshkevich Doroshkevich

and S.Gottloeberand S.Gottloeber

LSS at small redshiftsLSS at small redshifts – – luminous matterluminous matter

Ly- forest-LSS in DM & barionsLy- forest-LSS in DM & barions

Three Three characteristicscharacteristics

of absorber of absorber

Redshift – Redshift – zz

Width - Width - b b km/skm/s

Depth - Depth - NNHIHIcmcm-2-2

andand

UV background UV background

Cosmological modelCosmological model

Properties of ~6000 absorbersProperties of ~6000 absorbers 10 101515cmcm-2-2 >N >NHI HI > 10> 101212cmcm-2-2

Metal systems (CIV)Metal systems (CIV)

Properties of observed LSSProperties of observed LSS

PUZZLESPUZZLES

1. Weak redshift dependence of the PDFs, 1. Weak redshift dependence of the PDFs,

P(b/<b>), P(NP(b/<b>), P(NHIHI/<N/<NHIHI>), P(d>), P(dsepsep/<d/<dsepsep>)>)

2. <b>=const.(z), b < b2. <b>=const.(z), b < bbgbg

3. Slow regular redshift variations of 3. Slow regular redshift variations of

<N<NHIHI> ~(1+z)> ~(1+z)22 and <d and <dsepsep>~(1+z)>~(1+z)-2-2

DM simulationDM simulation

LLboxbox =150h =150h-1-1Mpc, NMpc, Npp= 256= 2563 3 , L, Lcellcell=0.6h=0.6h-1-1MpcMpc

Mass resolution: 2 10Mass resolution: 2 1077MMoo, ,

Force resolution: 20hForce resolution: 20h-1-1kpc,kpc,

Selected clusters: 10 < NSelected clusters: 10 < Np p < 5000, =1.76< 5000, =1.76thr

Simulated clustersSimulated clusters

For colderFor colder

clustersclusters

NNpp~<N~<Npp>/3>/3 For hotter For hotter

clustersclusters

NNpp~3<N~3<Npp>> Relaxation:Relaxation:

ffrelrel~0.6-0.8~0.6-0.8

Core-sampling approachCore-sampling approachLLcorecore=0.5h=0.5h-1-1MpcMpc

ConclusionsConclusions

Probable causes of self similarityProbable 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 rrii=(1+z)=(1+z)-1-1[q[qii--B(z) B(z) SSii(q)](q)] Power spectrumPower spectrum P(k)~kP(k)~k-3-3,, k/k k/k00> 1, k> 1, k00~0.15Mpc~0.15Mpc-1-1

Real and simulated BBKS power spectrumReal and simulated BBKS power spectrum

The The endend

Possible interpretationPossible interpretation

<b>=const(z), W(x<b>=const(z), W(xii)=const(z))=const(z) <d<dsepsep/(1+z)>~(1+z)/(1+z)>~(1+z)-3-3~1/<n~1/<nabsabsSSabsabs>>

Version 1 – Version 1 – relaxed cloudsrelaxed clouds nnabsabs~(1+z)~(1+z)33, S, Sabsabs~const.~const.

BUT BUT <N<NHIHI>~(1+z)>~(1+z)22

Version 2 -- Version 2 -- expanded clouds expanded clouds SSabsabs~(1+z)~(1+z)-p-p, n, nabsabs~(1+z)~(1+z)3+p3+p

BUT BUT <b>=const., W(x<b>=const., W(xii)=const(z))=const(z)

1

Comparison with simulations.Comparison with simulations.

LLboxbox=100 h=100 h-1-1Mpc, NMpc, Npp=(256)=(256)3 3 , L, Lcellcell=0.4Mpc=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 approachStrongly deterministic approach

Previously – relaxed halos onlyPreviously – relaxed halos only (galaxies, clusters of galaxies)(galaxies, clusters of galaxies)

1 125.0

60 Mpc/h

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

PDFs for three principle sizes PDFs for three principle sizes of clouds, L, w, hof clouds, L, w, h

PDFs for the velocity dispersionsPDFs for the velocity dispersionsalong three principle axes of cloudsalong three principle axes of clouds

Mean Mean characteristicscharacteristics

High density clouds, High density clouds,

LL~ ~ (1+z)(1+z)1/41/4, , ww~ ~ (1+z)(1+z)1/21/2, , hh~~(1+z)(1+z)1/21/2

VVhh~ ~ (1+z)-1/2(1+z)-1/2..

Low density clouds, Low density clouds,

L~w~hL~w~h~ ~ const(z)const(z)

VVhh~ ~ const(z). const(z).

Cores and envelopesCores and envelopes

125.0

1

Measured power spectrumMeasured power spectrum

Problems and prospectsProblems and prospects 1. 1. Ly-Ly-άά emitters emitters and population and population

of of earlier galaxiesearlier galaxies (~20 000 LBG) (~20 000 LBG) 2. DM compact objects 2. DM compact objects 3. First luminous objects - 3. First luminous objects -

stars or galaxiesstars or galaxies 4. Spatial distribution of metal 4. Spatial distribution of metal

systems – systems – bubblesbubbles ~2Mpc ~2Mpc

DM simulationDM simulation

LLboxbox =150h =150h-1-1Mpc, NMpc, Npp= 256= 25633

Mass resolution 2 10Mass resolution 2 1077MMoo, Force resolution 20kpc/h, Force resolution 20kpc/h

Selected clusters: 10 < NSelected clusters: 10 < Np p < 5000, > 1.7< 5000, > 1.7 Mean comoving principal sizes:Mean comoving principal sizes: L~0.5hL~0.5h-1-1Mpc, W~0.2hMpc, W~0.2h-1-1Mpc, S~0.1hMpc, S~0.1h-1-1MpcMpc Velocity dispersions along principal directions: Velocity dispersions along principal directions:

skmzskm

zskm

/45,)1(/45

,)1(/55

34/124/11

Z~2 - 3Z~2 - 3

LLgalgal ~10 ~102626 erg/s/Hz/Mpc erg/s/Hz/Mpc3 3

Giavalisco et al. 2004, GOODS, Giavalisco et al. 2004, GOODS,

LLQSOQSO~10~102323 – 10 – 1024 24 erg/s/Hz/Mpcerg/s/Hz/Mpc33, , A900~

A1500

Next StepsNext Steps

Detailed analysis of evolution of the UniverseDetailed 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 Shape of the small scale initial power

spectrum at L<100 kpc.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….

Real and simulated power spectrumReal and simulated power spectrum

Period of reionizationPeriod of reionization

Metal systems (CIV)Metal systems (CIV)