Clustering Discussion Session. Understanding LAE - Heidelberg 09/oct/08 Chair: Harold Francke, U. de Chile. Why do we care?. Clustering measurements allows the testing of DM hosting halos (of LAEs) Masses, number densities Can constrain evolution of LAE
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Understanding LAE - Heidelberg 09/oct/08
Chair: Harold Francke, U. de Chile
Talks by Ouchi san & Gawiser san
Talk by Blanc kun in the morning…
P=n2(1 + (12))d1d2 (angular)
P=2(1 + (r12))dV1dV2 (spatial)
Corresponds to excess probability of finding two points in areas (volumes) d1 and d2 (dV1 and dV2) separated by 12 (r12).
Dark matter halos are biased tracers of the matter field.
Autocorrelation function in a numerical simulation…
So measuring clustering tell us how massive and common are the DM halos hosting our galaxies…
SPATIAL correlation function
ANGULAR correlation function
Beware of narrow redshift distributions! (Simon 2006)
(C. Lacey’s & A. Orsi’s talks yesterday)
These models should also reproduce the clustering measurements that exist!!
at z~3: McLinden poster
at z~2: talks by Nilsson, Reddy)