Dispersion of the luminosity distance as a cosmological probe

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200 100 50 Power spectrum ! HaloFit cannot be trusted for large running or running of running. ! Treat F(k,z)=P NL /P L as a transfer function, at z=1. ! 2 methods: 1) step function 2) interpolated function. Both extremely underestimating. ! kUV=320h. kUV=30h degrades results but still cuts out parameter space allowed by PLANCK. P prim. (k) =A s ✓ k k 0 ◆ ns (k 0 ) 1+1/2↵(k 0 )ln(k/k 0 )+1/6 (k 0 )(ln(k/k 0 )) 2 20 10 5 2 1 0.01 0.1 1 10 100 T 2 (P )= T 2 (P )= Z kUV H 0 dkk 2 P L (1 + bH(k k NL )) Z kUV H 0 dkk 2 P L (k)(1 b + bH(k k NL )F (k, z))
1-‐b+b F(k,z) 1309.xxxx Region of constraints Hs m > 0.12L
Page 1 and 2: Dispersion of the luminosity di
Page 3 and 4: Primordial Power Spectrum
Page 5 and 6: Example: “string vs. field th
Page 7 and 8: Current and Future
Page 9: Lensing Dispersion of SNIa ! Cu
Page 13 and 14: Summary ! Demonstrated the short
Page 15 and 16: From Step 0.08 Region of constrai
Page 17 and 18: LC Averaging ! Useful for inter
Page 19 and 20: Prescription Properties ! Dynamic
Page 21: Exact Result -‐ Flux LC a

Dispersion of the luminosity distance as a cosmological probe

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