Combining clustering and abundances of galaxy clusters to test cosmology and primordial non-Gaussianity
| Autor: | Tommaso Giannantonio, Jochen Weller, Ben Hoyle, A. Mana, Barbara Sartoris, Gert Hütsi |
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| Přispěvatelé: | Mana, Annalisa, Giannantonio, Tommaso, Weller, Jochen, Hoyle, Ben, Hütsi, Gert, Sartoris, Barbara |
| Rok vydání: | 2013 |
| Předmět: |
Physics
Cosmology and Nongalactic Astrophysics (astro-ph.CO) media_common.quotation_subject Astronomy FOS: Physical sciences Astronomy and Astrophysics Astrophysics methods: statistical galaxies: clusters: general cosmological parameters Astrophysics::Cosmology and Extragalactic Astrophysics Cosmology Galaxy Universe Determining the number of clusters in a data set Space and Planetary Science Brightest cluster galaxy statistical galaxies: clusters: general cosmological parameters [methods] Cluster analysis Galaxy cluster Photometric redshift media_common Astrophysics - Cosmology and Nongalactic Astrophysics |
| DOI: | 10.48550/arxiv.1303.0287 |
| Popis: | 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 $\sim 50$ per cent improvement in the errors on the fluctuation amplitude $\sigma_8$ and the matter density $\Omega_{\mathrm{m}}$. 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 the variation in the cluster bias. We find a constraint on the amount of skewness $f_{\mathrm{NL}} = 12 \pm 157 $ ($1\sigma$) from the cluster data alone. Comment: 12 pages, 10 figures, 2 tables. Minor changes to match published version on MNRAS |
| Databáze: | OpenAIRE |
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