Dispersion of the luminosity distance as a cosmological probe
Dispersion of the luminosity distance as a cosmological probe
Dispersion of the luminosity distance as a cosmological probe
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Planck Me<strong>as</strong>urements <br />
! Even with PLANCK, Ly-‐alpha, etc. only <strong>probe</strong> ~8.5 e-folds<br />
out <strong>of</strong> 60. <br />
! Few observables, huge degeneracy between <br />
models. <br />
P prim. (k) =A s<br />
✓ k<br />
k 0<br />
◆ ns (k 0 ) 1+1/2↵(k 0 )ln(k/k 0 )+1/6 (k 0 )(ln(k/k 0 )) 2<br />
The power spectrum is <strong>the</strong> actual obsevrable and we <br />
need to me<strong>as</strong>ure it for <strong>as</strong> many e-‐folds possible!
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