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: RONCARELLI, MAURO, CARBONE, CARMELITA, MOSCARDINI, LAURO
• Other Authors: Roncarelli, M., Carbone, C., Moscardini, L.
• Format: Article in Journal/Newspaper
• Language: English
• Published: 2015
• Subjects: Cluster; Galaxie; General - cosmology; Neutrinos - method; Numerical - galaxie; Theory - large-scale structure of universe -X-ray; Space and Planetary Science; Astronomy and Astrophysics; South Pole; The ''Y''; South pole
• Online Access: http://hdl.handle.net/11585/548004; https://doi.org/10.1093/mnras/stu2546; http://mnras.oxfordjournals.org/content/447/2/1761

Massive neutrinos are expected to influence the formation of the large-scale structure of the Universe, depending on the value of their total mass, Σ mν In particular Planck data indicate that a non-zero Σ mν 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 propertieswe run a set of six very large cosmological simulations (8 h-3 Gpc3 comoving volume) that include a massive neutrino particle component: we consider the values of Σ mν = (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 Σ mν = 0.34 eV with respect to a model with massless neutrinos. However the degeneracy with σ8 and Ωm 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, fν, with (y)∝(1 - fν)20, considering the cluster component only, and the normalization of the SZ power spectrum is proportional to (1 - fν)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 Σ mν ≃0.34 eV is required to fit with the data.