Euclid preparation. XXXII. Evaluating the weak lensing cluster mass biases using the Three Hundred Project hydrodynamical simulations
Abstract
The photometric catalogue of galaxy clusters extracted from ESA Euclid data is expected to be very competitive for cosmological studies. Using state-of-the-art hydrodynamical simulations, we present systematic analyses simulating the expected weak lensing profiles from clusters in a variety of dynamic states and at wide range of redshifts. In order to derive cluster masses, we use a model consistent with the implementation within the Euclid Consortium of the dedicated processing function and find that, when jointly modelling mass and the concentration parameter of the Navarro-Frenk-White halo profile, the weak lensing masses tend to be, on average, biased low by 5-10% with respect to the true mass, up to z=0.5. Using a fixed value for the concentration , the mass bias is diminished below 5%, up to z=0.7, along with its relative uncertainty. Simulating the weak lensing signal by projecting along the directions of the axes of the moment of inertia tensor ellipsoid, we find that orientation matters: when clusters are oriented along the major axis, the lensing signal is boosted, and the recovered weak lensing mass is correspondingly overestimated. Typically, the weak lensing mass bias of individual clusters is modulated by the weak lensing signal-to-noise ratio, related to the redshift evolution of the number of galaxies used for weak lensing measurements: the negative mass bias tends to be larger toward higher redshifts. However, when we use a fixed value of the concentration parameter, the redshift evolution trend is reduced. These results provide a solid basis for the weak-lensing mass calibration required by the cosmological application of future cluster surveys from Euclid and Rubin.
Keywords
Cite
@article{arxiv.2302.00687,
title = {Euclid preparation. XXXII. Evaluating the weak lensing cluster mass biases using the Three Hundred Project hydrodynamical simulations},
author = {Euclid Collaboration and C. Giocoli and M. Meneghetti and E. Rasia and S. Borgani and G. Despali and G. F. Lesci and F. Marulli and L. Moscardini and M. Sereno and W. Cui and A. Knebe and G. Yepes and T. Castro and P. -S. Corasaniti and S. Pires and G. Castignani and L. Ingoglia and T. Schrabback and G. W. Pratt and A. M. C. Le Brun and N. Aghanim and L. Amendola and N. Auricchio and M. Baldi and C. Bodendorf and D. Bonino and E. Branchini and M. Brescia and J. Brinchmann and S. Camera and V. Capobianco and C. Carbone and J. Carretero and F. J. Castander and M. Castellano and S. Cavuoti and R. Cledassou and G. Congedo and C. J. Conselice and L. Conversi and Y. Copin and L. Corcione and F. Courbin and M. Cropper and A. Da Silva and H. Degaudenzi and J. Dinis and F. Dubath and X. Dupac and S. Dusini and S. Farrens and S. Ferriol and P. Fosalba and M. Frailis and E. Franceschi and M. Fumana and S. Galeotta and B. Garilli and B. Gillis and A. Grazian and F. Grupp and S. V. H. Haugan and W. Holmes and A. Hornstrup and K. Jahnke and M. Kümmel and S. Kermiche and M. Kilbinger and M. Kunz and H. Kurki-Suonio and S. Ligori and P. B. Lilje and I. Lloro and E. Maiorano and O. Mansutti and O. Marggraf and K. Markovic and R. Massey and S. Maurogordato and S. Mei and E. Merlin and G. Meylan and M. Moresco and E. Munari and S. -M. Niemi and J. Nightingale and T. Nutma and C. Padilla and S. Paltani and F. Pasian and K. Pedersen and V. Pettorino and G. Polenta and M. Poncet and L. A. Popa and F. Raison and A. Renzi and J. Rhodes and G. Riccio and E. Romelli and M. Roncarelli and E. Rossetti and R. Saglia and D. Sapone and B. Sartoris and P. Schneider and A. Secroun and S. Serrano and C. Sirignano and G. Sirri and L. Stanco and J. -L. Starck and P. Tallada-Crespí and A. N. Taylor and I. Tereno and R. Toledo-Moreo and F. Torradeflot and I. Tutusaus and E. A. Valentijn and L. Valenziano and T. Vassallo and Y. Wang and J. Weller and G. Zamorani and J. Zoubian and S. Andreon and S. Bardelli and A. Boucaud and E. Bozzo and C. Colodro-Conde and D. Di Ferdinando and G. Fabbian and M. Farina and H. Israel and E. Keihänen and V. Lindholm and N. Mauri and C. Neissner and M. Schirmer and V. Scottez and M. Tenti and E. Zucca and Y. Akrami and C. Baccigalupi and M. Ballardini and F. Bernardeau and A. Biviano and A. S. Borlaff and C. Burigana and R. Cabanac and A. Cappi and C. S. Carvalho and S. Casas and K. C. Chambers and A. R. Cooray and H. M. Courtois and S. Davini and S. de la Torre and G. De Lucia and G. Desprez and H. Dole and J. A. Escartin and S. Escoffier and I. Ferrero and F. Finelli and L. Gabarra and K. Ganga and J. Garcia-Bellido and K. George and F. Giacomini and G. Gozaliasl and H. Hildebrandt and I. Hook and A. JIMENEZ MU\{N}OZ and B. Joachimi and J. J. E. Kajava and V. Kansal and C. C. Kirkpatrick and L. Legrand and A. Loureiro and J. Macias-Perez and M. Magliocchetti and G. Mainetti and R. Maoli and S. Marcin and M. Martinelli and N. Martinet and C. J. A. P. Martins and S. Matthew and L. Maurin and R. B. Metcalf and P. Monaco and G. Morgante and S. Nadathur and A. A. Nucita and L. Patrizii and A. Peel and J. Pollack and V. Popa and C. Porciani and D. Potter and M. Pöntinen and P. Reimberg and A. G. Sánchez and Z. Sakr and A. Schneider and E. Sefusatti and A. Shulevski and A. Spurio Mancini and J. Stadel and J. Steinwagner and J. Valiviita and A. Veropalumbo and M. Viel and I. A. Zinchenko},
journal= {arXiv preprint arXiv:2302.00687},
year = {2024}
}
Comments
Accepted for publication in Astronomy & Astrophysics