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|Title:||The effect of massive neutrinos on the Sunyaev-Zel'dovich and X-ray observables of galaxy clusters||Authors:||Roncarelli, M.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||447||Issue:||2||First Page:||1761||Abstract:||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 m<SUB>ν</SUB>. In particular Planck data indicate that a non-zero Σ m<SUB>ν</SUB> 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<SUP>-3</SUP> Gpc<SUP>3</SUP> comoving volume) that include a massive neutrino particle component: we consider the values of Σ m<SUB>ν</SUB> = (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 m<SUB>ν</SUB> = 0.34 eV with respect to a model with massless neutrinos. However the degeneracy with σ<SUB>8</SUB> and Ω<SUB>m</SUB> 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<SUB>ν</SUB>, with < y > ∝ (1 - f<SUB>ν</SUB>)<SUP>20</SUP>, considering the cluster component only, and the normalization of the SZ power spectrum is proportional to (1 - f<SUB>ν</SUB>)<SUP>25-30</SUP>. 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 m<SUB>ν</SUB> ≃ 0.34 eV is required to fit with the data.||Acknowledgments:||Most of the computations necessary for this work have been performed thanks to the Italian SuperComputing Resource Allocation (ISCRA) of the Consorzio Interuniversitario del Nord Est per il Calcolo Automatico (CINECA). MR and LM acknowledge financial contributions from contract ASI/INAF I/023/12/0, from PRIN MIUR 2010-2011 ‘The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid’ and from PRIN INAF 2012 ‘The Universe in the box: multiscale simulations of cosmic structure’. CC acknowledges financial support to the ‘INAF Fellowships Programme 2010’ and to the European Research Council through the Darklight Advanced Research Grant (#291521). We thank an anonymous referee that contributed to improve the precision of our results and the presentation of our work. We thank M. Brusa, S. Ettori, F. Marulli, F. Finelli, F. Petracca and M. Sereno for useful suggestions and discussions. We are particularly grateful to M. Viel for allowing us to access the non-public version of gadget-3 modified to account for massive neutrino particles. We warmly thank A. Saro and J. Liu for providing us the data on the SPT noise.||URI:||http://hdl.handle.net/20.500.12386/23962||URL:||https://academic.oup.com/mnras/article/447/2/1761/2593769||ISSN:||0035-8711||DOI:||10.1093/mnras/stu2546||Bibcode ADS:||2015MNRAS.447.1761R||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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