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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200<br />
100<br />
50<br />
Power spectrum <br />
! HaloFit cannot be trusted for large running or <br />
running <strong>of</strong> running. <br />
! Treat F(k,z)=P NL /P L <strong>as</strong> a transfer function, at z=1. <br />
! 2 methods: 1) step function 2) interpolated function. <br />
Both extremely underestimating. <br />
! kUV=320h. kUV=30h degrades results but still cuts out <br />
parameter space allowed by PLANCK. <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 />
20<br />
10<br />
5<br />
2<br />
1<br />
0.01 0.1 1 10 100<br />
T 2 (P )=<br />
T 2 (P )=<br />
Z kUV<br />
H 0<br />
dkk 2 P L (1 + bH(k k NL ))<br />
Z kUV<br />
H 0<br />
dkk 2 P L (k)(1 b + bH(k k NL )F (k, z))
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