Euclid preparation: TBD. The impact of line-of-sight projections on the covariance between galaxy cluster multi-wavelength observable properties -- insights from hydrodynamic simulations
Creators: name: Euclid Collaboration
name: Ragagnin, A.
name: Saro, A.
name: Andreon, S.
name: Biviano, A.
name: Dolag, K.
name: Ettori, S.
name: Giocoli, C.
name: Brun, A. M. C. Le
name: Mamon, G. A.
name: Maughan, B. J.
name: Meneghetti, M.
name: Moscardini, L.
name: Pacaud, F.
name: Pratt, G. W.
name: Sereno, M.
name: Borgani, S.
name: Calura, F.
name: Castignani, G.
name: De Petris, M.
name: Eckert, D.
name: Lesci, G. F.
name: Macias-Perez, J.
name: Maturi, M.
name: Amara, A.
name: Auricchio, N.
name: Baccigalupi, C.
name: Baldi, M.
name: Bardelli, S.
name: Bonino, D.
name: Branchini, E.
name: Brescia, M.
name: Brinchmann, J.
name: Camera, S.
name: Capobianco, V.
name: Carbone, C.
name: Carretero, J.
name: Casas, S.
name: Castellano, M.
name: Cavuoti, S.
name: Cimatti, A.
name: Colodro-Conde, C.
name: Congedo, G.
name: Conselice, C. J.
name: Conversi, L.
name: Copin, Y.
name: Courbin, F.
name: Courtois, H. M.
name: Da Silva, A.
name: Degaudenzi, H.
name: De Lucia, G.
name: Dinis, J.
name: Dubath, F.
name: Dupac, X.
name: Farina, M.
name: Farrens, S.
name: Ferriol, S.
name: Frailis, M.
name: Franceschi, E.
name: Fumana, M.
name: George, K.
name: Gillis, B.
name: Grazian, A.
name: Grupp, F.
name: Haugan, S. V. H.
name: Holmes, W.
name: Hook, I.
name: Hormuth, F.
name: Hornstrup, A.
name: Jahnke, K.
name: Keihänen, E.
name: Kermiche, S.
name: Kiessling, A.
name: Kilbinger, M.
name: Kubik, B.
name: Kümmel, M.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Ligori, S.
name: Lilje, P. B.
name: Lindholm, V.
name: Lloro, I.
name: Maino, D.
name: Maiorano, E.
name: Mansutti, O.
name: Marggraf, O.
name: Markovic, K.
name: Martinelli, M.
name: Martinet, N.
name: Marulli, F.
name: Massey, R.
name: Maurogordato, S.
name: Medinaceli, E.
name: Mei, S.
name: Mellier, Y.
name: Meylan, G.
name: Moresco, M.
name: Munari, E.
name: Neissner, C.
name: Niemi, S. -M.
name: Nightingale, J. W.
name: Padilla, C.
name: Paltani, S.
name: Pasian, F.
name: Pedersen, K.
name: Pettorino, V.
name: Polenta, G.
name: Poncet, M.
name: Popa, L. A.
name: Pozzetti, L.
name: Raison, F.
name: Renzi, A.
name: Rhodes, J.
name: Riccio, G.
name: Romelli, E.
name: Roncarelli, M.
name: Rossetti, E.
name: Saglia, R.
name: Sakr, Z.
name: Sánchez, A. G.
name: Sapone, D.
name: Sartoris, B.
name: Scaramella, R.
name: Schneider, P.
name: Schrabback, T.
name: Secroun, A.
name: Sefusatti, E.
name: Seidel, G.
name: Serrano, S.
name: Sirignano, C.
name: Sirri, G.
name: Stanco, L.
name: Steinwagner, J.
name: Tallada-Crespí, P.
name: Tereno, I.
name: Toledo-Moreo, R.
name: Torradeflot, F.
name: Tutusaus, I.
name: Valenziano, L.
name: Vassallo, T.
name: Kleijn, G. Verdoes
name: Veropalumbo, A.
name: Wang, Y.
name: Weller, J.
name: Zamorani, G.
name: Zucca, E.
name: Bolzonella, M.
name: Boucaud, A.
name: Bozzo, E.
name: Burigana, C.
name: Calabrese, M.
name: Di Ferdinando, D.
name: Vigo, J. A. Escartin
name: Farinelli, R.
name: Gracia-Carpio, J.
name: Mauri, N.
name: Scottez, V.
name: Tenti, M.
name: Viel, M.
name: Wiesmann, M.
name: Akrami, Y.
name: Allevato, V.
name: Anselmi, S.
name: Ballardini, M.
name: Bergamini, P.
name: Blanchard, A.
name: Blot, L.
name: Bruton, S.
name: Cabanac, R.
name: Calabro, A.
name: Canas-Herrera, G.
name: Cappi, A.
name: Carvalho, C. S.
name: Castro, T.
name: Chambers, K. C.
name: Contarini, S.
name: Cooray, A. R.
name: Costanzi, M.
name: De Caro, B.
name: de la Torre, S.
name: Desprez, G.
name: Díaz-Sánchez, A.
name: Di Domizio, S.
name: Dole, H.
name: Escoffier, S.
name: Ferrari, A. G.
name: Ferreira, P. G.
name: Ferrero, I.
name: Finelli, F.
name: Fornari, F.
name: Gabarra, L.
name: Ganga, K.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Giacomini, F.
name: Gozaliasl, G.
name: Hall, A.
name: Hildebrandt, H.
name: Hjorth, J.
name: Muñoz, A. Jimenez
name: Kajava, J. J. E.
name: Kansal, V.
name: Karagiannis, D.
name: Kirkpatrick, C. C.
name: Legrand, L.
name: Libet, G.
name: Loureiro, A.
name: Maggio, G.
name: Magliocchetti, M.
name: Mannucci, F.
name: Maoli, R.
name: Martins, C. J. A. P.
name: Matthew, S.
name: Maurin, L.
name: Metcalf, R. B.
name: Monaco, P.
name: Moretti, C.
name: Morgante, G.
name: Walton, Nicholas A.
name: Patrizii, L.
name: Pezzotta, A.
name: Pöntinen, M.
name: Popa, V.
name: Porciani, C.
name: Potter, D.
name: Risso, I.
name: Rocci, P. -F.
name: Sahlén, M.
name: Schneider, A.
name: Schultheis, M.
name: Simon, P.
name: Mancini, A. Spurio
name: Tao, C.
name: Testera, G.
name: Teyssier, R.
name: Toft, S.
name: Tosi, S.
name: Troja, A.
name: Tucci, M.
name: Valieri, C.
name: Valiviita, J.
name: Vergani, D.
name: Verza, G.
Publisher: name: arXiv
Year: 2024
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Cluster cosmology can benefit from combining multi-wavelength studies, which can benefit from characterising the correlation coefficients between different mass-observable relations. In this work, we aim to provide information on the scatter, the skewness, and the covariance of various mass-observable relations in galaxy clusters in cosmological hydrodynamic simulations. This information will help future analyses to better tackle accretion histories and projection effects and model mass observable relations for cosmology studies.We identify galaxy clusters in Magneticum Box2b simulations with mass $M_{\rm 200c}&gt;10^{14} {\rm M}_\odot$ at redshift $z=0.24$ and $z=0.90$. Our analysis includes \Euclid-derived properties such as richness, stellar mass, lensing mass, and concentration. Additionally, we investigate complementary multi-wavelength data, including X-ray luminosity, integrated Compton-$y$ parameter, gas mass, and temperature. The impact of projection effects on mass-observable residuals and correlations is then examined. At intermediate redshift ($z=0.24$), projection effects impact lensing concentration, richness, and gas mass the most in terms of scatter and skewness of log-residuals of scaling relations. The contribution of projection effects can be significant enough to boost a spurious hot- vs. cold-baryons correlation and consequently hide underlying correlations due to halo accretion histories.
 At high redshift ($z=0.9$), the richness has a much lower scatter (of log-residuals), and the quantity that is most impacted by projection effects is the lensing mass.
 Lensing concentration reconstruction, in particular, is affected by deviations of the reduced-shear profile shape from the one derived by an NFW profile rather than interlopers in the line of sight.
description: 26 pages, 22 figures, submitted to A&amp;A, replied to referee comments