Author:
Artis E.,Adam R.,Ade P.,Ajeddig H.,André P.,Arnaud M.,Aussel H.,Bartalucci I.,Beelen A.,Benoît A.,Berta S.,Bing L.,Bourrion O.,Calvo M.,Catalano A.,De Petris M.,Désert F.-X.,Doyle S.,Driessen E. F. C.,Ferragamo A.,Gomez A.,Goupy J.,Kéruzoré F.,Kramer C.,Ladjelate B.,Lagache G.,Leclercq S.,Lestrade J.-F.,Macías-Pérez J.-F.,Maury A.,Mauskopf P.,Mayet F.,Monfardini A.,Muñoz-Echeverría M.,Paliwal A.,Perotto L.,Pisano G.,Pointecouteau E.,Ponthieu N.,Pratt G. W.,Revéret V.,Rigby A. J.,Ritacco A.,Romero C.,Roussel H.,Ruppin F.,Schuster K.,Shu S.,Sievers A.,Tucker C.,Yepes G.
Abstract
PSZ2 G091.83+26.11 is a massive galaxy cluster withM500= 7:43 × 1014M⊙atz= 0:822. This object exhibits a complex morphology with a clear bimodality observed in X-rays. However, it was detected and analysed in thePlancksample as a single, spherical cluster following a universal profile [1]. This model can lead to miscalculations of thermodynamical quantities, like the pressure profile. As future multiwavelength cluster experiments will detect more and more objects at higher redshifts (where we expect the fraction of merging objects to be higher), it is crucial to quantify this systematic effect. In this work, we use high-resolution observations of PSZ2 G091.83+26.11 by the NIKA2 camera to integrate the morphological characteristics of the cluster in our modelling. This is achieved by fitting a two-halo model to the SZ image and then by reconstruction of the resulting projected pressure profile. We then compare these results with the spherical assumption.