1. Anisotropic Cosmology :progress and problems A. Doroshkevich, M.Demianski Astro Space Centre of Lebedev Physical Institute University of Warsaw

2. Progress in cosmology • Measurements of H0 - SN, Hubble • CMB - COBE & WMAP, …. • Surveys of galaxies - SDSS & 2dF, • High precision observations of the Ly- α forest, metal systems, QSRs and galaxies at z=5 – 7 -- 10, • Simulations – LSS, halos …

3. Main result – standard cosmological model • Hubble h = 0.7  0.04 • Eucledian space tot = 1.  0.05 • Dark energy  = 0.7  0.1 • Dark matter m = 0.24  0.02 • Baryonic matter b = 0.044  0.004 • Galaxies Ωgal ~ (0.06-0.3)Ωb • Relict CMB Trad =2.726 K

4. Main problems • 1. Nature of the Dark Energy at small redshifts and in the inflation period. • 2. Nature and composition of the Dark Matter. • 3. Reliability of the ‘standard’ model. • 4. General anisotropy, rotation and magnetic field in the Universe. • 5. Evolution of the Universe at 6< z< 1000 : first galaxies and reionisation of the Universe.

5. SN Ia H2=H20( ) 75 low and 47 high redshifts SN Ia – Ωm=0.29±0.05 58 low and 48 high redshifts SN Ia – Ωm=0.18±0.05 Different methods of calibration Ω

6. Decomposition of temperature here Φlm and alm are the phase and amplitude of fluctuations Spectrum of fluctuations is

8. Expected Measured Axis of evil, direction to dipole, Virgo, ecliptic pole, Maxwell, etc. More than 100 references – magnetic field, strong anisotropy withΩ ~ 0.3 Quadrupole

9. Separation of CMB and foregrounds It is incorrect problem which can be solved only approximately. Example: S1=c+b1, S2 =c+b2, c=ω S1 +(1-ω) S2 ∂c/∂ω=0→ b1=κb2

10. Anisotropic cosmology • Possible anisotropy of the large scale power spectrum • and non Gaussianity of fluctuations • f(r)={sh r, r, sin r} • At the period of inflation

11. At small redshifts • Measured quadrupole • Required regular quadrupole • Regular quadrupole

12. Homogeneous magnetic fieldand matter rotation • Observational limit: B< G, • Faraday rotation: • Intermixture of ‘E’ and ‘B’ modes • Rotation: from galaxies from CMB

13. Why it is important • 1. Test for the models of inflation • 2. Test for PDFs of fluctuations and the power spectrum • 3. Test for “hidden parameters” B(0) and ω(0)

14. The end The end

15. The angular power spectra