Combining clustering and abundances of galaxy clusters to test cosmology and primordial non-Gaussianity

Дата и время публикации : 2013-03-01T21:00:01Z

Авторы публикации и институты :
Annalisa Mana (LMU Munich)
Tommaso Giannantonio (LMU Munich)
Jochen Weller (LMU Munich)
Ben Hoyle (LMU Munich)
Gert Huetsi (MPA Garching)
Barbara Sartoris (Trieste U.)

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 12 pages, 9 figures. To be submitted to MNRAS
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO

Краткий обзор статьи: We present the clustering of galaxy clusters as a useful addition to the common set of cosmological observables. The clustering of clusters probes the large-scale structure of the Universe, extending galaxy clustering analysis to the high-peak, high-bias regime. Clustering of galaxy clusters complements the traditional cluster number counts and observable-mass relation analyses, significantly improving their constraining power by breaking existing calibration degeneracies. We use the maxBCG galaxy clusters catalogue to constrain cosmological parameters and cross-calibrate the mass-observable relation, using cluster abundances in richness bins and weak-lensing mass estimates. We then add the redshift-space power spectrum of the sample, including an effective modelling of the weakly non-linear contribution and allowing for an arbitrary photometric redshift smoothing. The inclusion of the power spectrum data allows for an improved self-calibration of the scaling relation. We find that the inclusion of the power spectrum typically brings a ~50% improvement in the errors on the fluctuation amplitude sigma_8 and the matter density Omega_m. Finally, we apply this method to constrain models of the early universe through the amount of primordial non-Gaussianity of the local type, using both the variation in the halo mass function and in the cluster bias. We find a constraint on the amount of skewness f_NL = 12 +/- 157 (1 sigma) from the cluster data alone.

Category: Physics