The effect of massive neutrinos on the Sunyaev-Zel'dovich and X-ray observables of galaxy clusters

• Published in: Monthly Notices of the Royal Astronomical Society
• Main Authors: M. Roncarelli, C. Carbone, L. Moscardini
• Format: Article in Journal/Newspaper
• Language: English
• Published: Oxford University Press 2015
• Subjects: cluster; galaxie; general; cosmology; neutrinos; method; numerical; theory; large; scale structure of universe; x-ray; astronomy and astrophysic; space and planetary science; Settore FIS/05 - Astronomia e Astrofisica; South Pole; The ''Y''; South pole
• Online Access: http://hdl.handle.net/2434/565617; https://doi.org/10.1093/mnras/stu2546

Massive neutrinos are expected to influence the formation of the large-scale structure of the Universe, depending on the value of their total mass, Sigma m(nu). In particular Planck data indicate that a non-zero Sigma m(nu). may help to reconcile cosmic microwave background data with Sunyaev-Zel'dovich (SZ) cluster surveys. In order to study the impact of neutrinos on the SZ and X-ray cluster properties we run a set of six very large cosmological simulations (8 h(-3) Gpc(3) comoving volume) that include a massive neutrino particle component: we consider the values of Sigma m(nu) = (0, 0.17, 0.34) eV in two cosmological scenarios to test possible degeneracies. Using the halo catalogues extracted from their outputs we produce 50 mock light cones and, assuming suitable scaling relations, we determine how massive neutrinos affect SZ and X-ray cluster counts, the y-parameter and its power spectrum. We provide forecasts for the South Pole Telescope (SPT) and extended Roentgen Survey with an Imaging Telescope Array cluster surveys, showing that the number of expected detections is reduced by 40 per cent when assuming Sigma m(nu) = 0.34 eV with respect to a model with massless neutrinos. However the degeneracy with sigma(8) and Omega(m) is strong, in particular for X-ray data, requiring the use of additional probes to break it. The y-parameter properties are also highly influenced by the neutrino mass fraction, f(nu) with < y > proportional to (1-f(nu))(20), considering the cluster component only, and the normalization of the SZ power spectrum is proportional to (1-f(nu))(25-30). Comparing our findings with SPT and Atacama Cosmology Telescope measurements at l = 3000 indicates that, when Planck cosmological parameters are assumed, a value of Sigma m(nu) similar or equal to 0.34 eV is required to fit with the data.