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Arecibo as a redshift machine

Perseus-Pisces Supercluster. ~11,000 galaxy redshifts:. Arecibo as a redshift machine. [Giovanelli, Haynes et al. 1980s]. Perseus-Pisces Supercluster. Two Sloan Digital Sky Survey (SDSS) Wedges near The equator. 67676 galaxies Within 5deg og Equator [Tegmark et al 2003].

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Arecibo as a redshift machine

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  1. Perseus-Pisces Supercluster ~11,000 galaxy redshifts: Arecibo as a redshift machine [Giovanelli, Haynes et al. 1980s]

  2. Perseus-Pisces Supercluster

  3. Two Sloan Digital Sky Survey (SDSS) Wedges near The equator. 67676 galaxies Within 5deg og Equator [Tegmark et al 2003]

  4. Power Spectrum Derived from SDSS redshift survey [Tegmark et al 2003]

  5. Composite Power Spectrum Of Density fluctuations

  6. Disk Formation: a primer • Protogalaxies acquire angular momentum through tidal torques with nearest neighbors during the linear regime [Stromberg 1934; Hoyle 1949] • As self-gravity decouples the protogalaxy from the Hubble flow, [l/(d l/d t)] becomes v.large and the growth of l ceases • N-body simulations show that at turnaround time values of l range between 0.01 and 0.1, for halos of all masses • The average for halos isl = 0.05 • Only 10% of halos havel < 0.025 or l > 0.10 • halos achieve very • modest rotational support The spin parameter l quantifies the degree of rotational support of a system : For E galaxies, l ~ 0.05 For S galaxies, l ~ 0.5 • Baryons collapse dissipatively within the potential well of their halo. They lose energy through radiative losses, largely conserving mass and angular momentum • Thus l of disks increases, as they shrink to the inner part of the halo. • [Fall & Efstathiou 1980] Angular momentum Mass Total Energy • If the galaxy retains all baryons  m_d~1/10 , and l_disk grows to ~ 0.5, • R_disk ~ 1/10 R_h (mass of disk) /(total mass)

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