The determination of the mass of galaxy clusters from observations is subject to systematic uncertainties. Beyond the errors due to instrumental and observational systematic effects, in this work we investigate the bias introduced by modelling assumptions. In particular, we consider the reconstruction of the mass of galaxy clusters from convergence maps employing spherical mass density models. We made use of The Three Hundred simulations, selecting clusters in the same redshift and mass range as the NIKA2 Sunyaev-Zel’dovich Large Programme sample: 3 ≤ M500/1014 M ≤ 10 and 0.5 ≤ z ≤ 0.9. We studied different modelling and intrinsic uncertainties that should be accounted for when using the single cluster mass estimates for scaling relations. We confirm that the orientation of clusters and the radial ranges considered for the fit have an important impact on the mass bias. The effect of the projection adds uncertainties to the order of 10–16% to the mass estimates. We also find that the scatter from cluster to cluster in the mass bias when using spherical mass models is less than 9% of the true mass of the clusters

This work has been made possible by T HE T HREE H UNDRED collaboration ( https://the300-project.org ). M.D.P., A.F., and A.P. acknowledge support from Sapienza Università di Roma thanks to Progetti di Ricerca Medi 2021, RM12117A51D5269B. W.C. is supported by the STFC AGP Grant ST/V000594/1 and the Atracción de Talento Contract no. 2020-T1/TIC-19882 granted by the Comunidad de Madrid in Spain. W.C. and G.Y. thank the Ministerio de Ciencia e Innovación (Spain) for financial support under Project grant PID2021-122603NB-C21. This project was carried out using the Python libraries matplotlib (Hunter 2007), numpy (Harris et al. 2020), astropy (Astropy Collaboration 2013, 2018), and emcee (Foreman-Mackey et al. 2019; Goodman & Weare 2010).

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