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Astrometry and the expansion of the universe

Astrometry and the expansion of the universe. Michael Soffel & Sergei Klioner TU Dresden. Fundamental object for astrometry: metric tensor g. . IAU -2000 Resolutions: BCRS (t, x ) with metric tensor. BCRS-metric is asymptotically flat; ignores cosmological effects,

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Astrometry and the expansion of the universe

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  1. Astrometry and the expansion of the universe Michael Soffel & Sergei Klioner TU Dresden

  2. Fundamental object for astrometry: metric tensor g 

  3. IAU -2000 Resolutions: BCRS (t, x) with metric tensor

  4. BCRS-metric is asymptotically flat; ignores cosmological effects, fine for the solar-system dynamics and local geometrical optics

  5. The cosmological principle (CP): on very large scales the universe is homogeneous and isotropic The Robertson-Walker metric follows from the CP

  6. Consequences of the RW-metric for astrometry: - cosmic redshift - various distances that differ from each other: parallax distance luminosity distance angular diameter distance proper motion distance

  7. Is the CP valid? A simple fact: The universe is very clumpy on scales up to some 100 Mpc

  8. -10 solar-system: 2 x 10 Mpc : our galaxy: 0.03 Mpc the local group: 1 - 3 Mpc

  9. The local supercluster: 20 - 30 Mpc

  10. dimensions of great wall: 150 x 70 x 5 Mpc distance 100 Mpc

  11. Anisotropies in the CMBR WMAP-data

  12. First peak:  0.9 deg corresponds today to about 150 Mpc /h results from horizon scale at recombination

  13. -4 / < 10 for R > 1000 (Mpc/h) (O.Lahav, 2000)

  14. The WMAP-data leads to the present (cosmological) standard model: Age(universe) = 13.7 billion years Lum = 0.04 dark = 0.23  = 0.73 H0 = (71 +/- 4) km/s/Mpc

  15. The CP seems to be valid for scales R > R with R  400 h Mpc inhom -1 inhom

  16. One might continue with a hierarchy of systems • GCRS (geocentric celestial reference system) • BCRS (barycentric) • GaCRS (galactic) • LoGrCRS (local group) • LoSuCRS (local supercluster) • each systems contains tidal forces due to • system below; dynamical time scales grow if we go • down the list -> renormalization of constants (sec- aber) • expansion of the universe has to be taken into account

  17. The local expansion hypothesis: the cosmic expansion occurs on all length scales, i.e., also locally If true: how does the expansion influence local physics ? question has a very long history (McVittie 1933; Järnefelt 1940, 1942; Dicke et al., 1964; Gautreau 1984; Cooperstock et al., 1998)

  18. Validity of the local expansion hypothesis: unclear Hint: The Einstein-Straus solution matching surface S

  19. Matching of 1st and 2nd fundamental form on S • (R = R0 ) • plus Einstein eqs.: • r = R0 a(T) • t = t(R0,T) • dt/dT = ( 1 - 2 GM/(c^2 r)) • M = 4/3  r -1 3

  20. The swiss cheese model of the universe Global dynamics given by the RW- metric BUT: distance measurements depend upon clumpiness parameter  (grav. lensing inside bubbles) Dyer-Roeder distance () observations:   1 Dyer,C., Roeder,R., Ap.J. 174 (1972) L115 181 (1973) L31 Tomita, K., Prog.Th.Phys. 100 (1998) 79 133 (1999) 155

  21. Current issues of our work: - optimal matching the RW-metric to the BCRS assuming the local expansion hypothesis - improvements of the transition from the RW to the BCRS-metric - formulation of observables related with distance by means of a new metric tensor

  22. THE END

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