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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d L -‐z relation <br />
• Gauge inv. Light-‐cone avg. procedure. 2 nd <br />
order pert. <strong>the</strong>ory, NO DIVERGENCES! <br />
• kUV=30h Mpc -‐1 , WMAP data. <br />
sm<br />
0.14<br />
0.12<br />
0.10<br />
0.08<br />
0.06<br />
0.04<br />
PLANCK DATA <br />
• Flux is minimally bi<strong>as</strong>ed. <br />
• The dispersion is large ~ 2-‐10% ΛCDM, <strong>of</strong> <strong>the</strong> <br />
critical density depending on <strong>the</strong> spectrum. <br />
Scatter is mostly from <strong>the</strong> LC average. It <br />
gives <strong>the</strong>oretical explanation to part <strong>of</strong> <strong>the</strong> <br />
scatter <strong>of</strong> SN me<strong>as</strong>urements. At z>0.3 <br />
dominated by lensing. <br />
IBD, M. G<strong>as</strong>perini, G. Marozzi, F. Nugier, G. <br />
Veneziano <br />
m-m M<br />
0.02<br />
0.00<br />
0.3<br />
0.2<br />
0.1<br />
0.0<br />
-0.1<br />
-0.2<br />
0.6 0.8 1.0 1.2 1.4 1.6<br />
PLANCK DATA <br />
z<br />
0.02 0.05 0.10 0.20 0.50 1.00 2.00<br />
z
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