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Hauptverfasser:	Lindholm, V., Sihvola, E., Valiviita, J., Fumagalli, A., Altieri, B., Andreon, S., Auricchio, N., Baccigalupi, C., Baldi, M., Bardelli, S., Battaglia, P., Biviano, A., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carbone, C., Cardone, V. F., Carretero, J., Casas, S., Castellano, M., Castignani, G., Cavuoti, S., Chambers, K. C., Cimatti, A., Colodro-Conde, C., Congedo, G., Conversi, L., Copin, Y., Courbin, F., Courtois, H. M., Da Silva, A., Degaudenzi, H., De Lucia, G., Dole, H., Dubath, F., Dupac, X., Dusini, S., Escoffier, S., Farina, M., Farinelli, R., Ferriol, S., Finelli, F., Fosalba, P., Fotopoulou, S., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., George, K., Gillis, B., Giocoli, C., Gracia-Carpio, J., Grazian, A., Grupp, F., Haugan, S. V. H., Holmes, W., Hormuth, F., Hornstrup, A., Jahnke, K., Jhabvala, M., Kermiche, S., Kiessling, A., Kubik, B., Kunz, M., Kurki-Suonio, H., Brun, A. M. C. Le, Ligori, S., Lilje, P. B., Lloro, I., Mainetti, G., Maiorano, E., Mansutti, O., Marcin, S., Marggraf, O., Martinelli, M., Martinet, N., Marulli, F., Massey, R. J., Medinaceli, E., Mei, S., Melchior, M., Meneghetti, M., Merlin, E., Meylan, G., Mora, A., Moresco, M., Moscardini, L., Nakajima, R., Neissner, C., Niemi, S. -M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L. A., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Roncarelli, M., Rosset, C., Saglia, R., Sakr, Z., Sánchez, A. G., Sapone, D., Schneider, P., Schrabback, T., Secroun, A., Seidel, G., Simon, P., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toft, S., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Vassallo, T., Kleijn, G. Verdoes, Wang, Y., Weller, J., Zamorani, G., Zucca, E., Castro, T., Martín-Fleitas, J., Monaco, P., Pezzotta, A., Scottez, V., Sereno, M., Viel, M., Sciotti, D.
Format:	Preprint
Veröffentlicht:	2026
Schlagworte:	Cosmology and Nongalactic Astrophysics
Online-Zugang:	https://arxiv.org/abs/2603.10735
Tags:	Tag hinzufügen Keine Tags, Fügen Sie den ersten Tag hinzu!

_version_	1866911506064474112
author	Lindholm, V. Sihvola, E. Valiviita, J. Fumagalli, A. Altieri, B. Andreon, S. Auricchio, N. Baccigalupi, C. Baldi, M. Bardelli, S. Battaglia, P. Biviano, A. Branchini, E. Brescia, M. Camera, S. Capobianco, V. Carbone, C. Cardone, V. F. Carretero, J. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Chambers, K. C. Cimatti, A. Colodro-Conde, C. Congedo, G. Conversi, L. Copin, Y. Courbin, F. Courtois, H. M. Da Silva, A. Degaudenzi, H. De Lucia, G. Dole, H. Dubath, F. Dupac, X. Dusini, S. Escoffier, S. Farina, M. Farinelli, R. Ferriol, S. Finelli, F. Fosalba, P. Fotopoulou, S. Frailis, M. Franceschi, E. Fumana, M. Galeotta, S. George, K. Gillis, B. Giocoli, C. Gracia-Carpio, J. Grazian, A. Grupp, F. Haugan, S. V. H. Holmes, W. Hormuth, F. Hornstrup, A. Jahnke, K. Jhabvala, M. Kermiche, S. Kiessling, A. Kubik, B. Kunz, M. Kurki-Suonio, H. Brun, A. M. C. Le Ligori, S. Lilje, P. B. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marcin, S. Marggraf, O. Martinelli, M. Martinet, N. Marulli, F. Massey, R. J. Medinaceli, E. Mei, S. Melchior, M. Meneghetti, M. Merlin, E. Meylan, G. Mora, A. Moresco, M. Moscardini, L. Nakajima, R. Neissner, C. Niemi, S. -M. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L. A. Raison, F. Renzi, A. Rhodes, J. Riccio, G. Romelli, E. Roncarelli, M. Rosset, C. Saglia, R. Sakr, Z. Sánchez, A. G. Sapone, D. Schneider, P. Schrabback, T. Secroun, A. Seidel, G. Simon, P. Sirignano, C. Sirri, G. Stanco, L. Tallada-Crespí, P. Taylor, A. N. Tereno, I. Toft, S. Toledo-Moreo, R. Torradeflot, F. Tutusaus, I. Vassallo, T. Kleijn, G. Verdoes Wang, Y. Weller, J. Zamorani, G. Zucca, E. Castro, T. Martín-Fleitas, J. Monaco, P. Pezzotta, A. Scottez, V. Sereno, M. Viel, M. Sciotti, D.
author_facet	Lindholm, V. Sihvola, E. Valiviita, J. Fumagalli, A. Altieri, B. Andreon, S. Auricchio, N. Baccigalupi, C. Baldi, M. Bardelli, S. Battaglia, P. Biviano, A. Branchini, E. Brescia, M. Camera, S. Capobianco, V. Carbone, C. Cardone, V. F. Carretero, J. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Chambers, K. C. Cimatti, A. Colodro-Conde, C. Congedo, G. Conversi, L. Copin, Y. Courbin, F. Courtois, H. M. Da Silva, A. Degaudenzi, H. De Lucia, G. Dole, H. Dubath, F. Dupac, X. Dusini, S. Escoffier, S. Farina, M. Farinelli, R. Ferriol, S. Finelli, F. Fosalba, P. Fotopoulou, S. Frailis, M. Franceschi, E. Fumana, M. Galeotta, S. George, K. Gillis, B. Giocoli, C. Gracia-Carpio, J. Grazian, A. Grupp, F. Haugan, S. V. H. Holmes, W. Hormuth, F. Hornstrup, A. Jahnke, K. Jhabvala, M. Kermiche, S. Kiessling, A. Kubik, B. Kunz, M. Kurki-Suonio, H. Brun, A. M. C. Le Ligori, S. Lilje, P. B. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marcin, S. Marggraf, O. Martinelli, M. Martinet, N. Marulli, F. Massey, R. J. Medinaceli, E. Mei, S. Melchior, M. Meneghetti, M. Merlin, E. Meylan, G. Mora, A. Moresco, M. Moscardini, L. Nakajima, R. Neissner, C. Niemi, S. -M. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L. A. Raison, F. Renzi, A. Rhodes, J. Riccio, G. Romelli, E. Roncarelli, M. Rosset, C. Saglia, R. Sakr, Z. Sánchez, A. G. Sapone, D. Schneider, P. Schrabback, T. Secroun, A. Seidel, G. Simon, P. Sirignano, C. Sirri, G. Stanco, L. Tallada-Crespí, P. Taylor, A. N. Tereno, I. Toft, S. Toledo-Moreo, R. Torradeflot, F. Tutusaus, I. Vassallo, T. Kleijn, G. Verdoes Wang, Y. Weller, J. Zamorani, G. Zucca, E. Castro, T. Martín-Fleitas, J. Monaco, P. Pezzotta, A. Scottez, V. Sereno, M. Viel, M. Sciotti, D.
contents	We study the properties of galaxy cluster 2-point correlation function covariance matrices estimated using the linear-construction (LC) method, which is computationally up to 20 times faster than the standard sample-covariance method. Our goal is to assess how well the LC method performs in cosmological parameter estimation compared to the sample covariance. We use a set of 1000 mock dark matter halo catalogues to compute both the LC-covariance and the sample-covariance estimates in four redshift shells. These numerical matrices are used to fit a theoretical four-parameter model for the covariance. We then use the two fitted covariance models in a likelihood function to estimate two cosmological parameters - the matter density parameter $Ω_{\rm m}$ and the amplitude of the matter density fluctuations $σ_8$ - from the simulated mock catalogues. The purpose of this is to validate the LC-covariance-based model against the sample-covariance model. The catalogues were simulated assuming the spatially flat $Λ$CDM cosmology, with $Ω_{\rm m} = 0.30711$ and $σ_8=0.8288$. We find that the parameter posteriors obtained using the sample- and LC-covariance models agree well with each other and with the simulation cosmology. The two pairs of marginalized constraints are $Ω_{\rm m} = 0.307 \pm 0.003$ and $σ_8 = 0.826\pm 0.009$ (sample covariance), and $Ω_{\rm m} = 0.308 \pm 0.003$ and $σ_8 = 0.825 \pm 0.009$ (LC covariance). The posterior widths are the same, and the difference in the median values is less than $0.16\,σ$ for both parameters.
format	Preprint
id	arxiv_https___arxiv_org_abs_2603_10735
institution	arXiv
publishDate	2026
record_format	arxiv
spellingShingle	Euclid: The linear-construction covariance and cosmology Lindholm, V. Sihvola, E. Valiviita, J. Fumagalli, A. Altieri, B. Andreon, S. Auricchio, N. Baccigalupi, C. Baldi, M. Bardelli, S. Battaglia, P. Biviano, A. Branchini, E. Brescia, M. Camera, S. Capobianco, V. Carbone, C. Cardone, V. F. Carretero, J. Casas, S. Castellano, M. Castignani, G. Cavuoti, S. Chambers, K. C. Cimatti, A. Colodro-Conde, C. Congedo, G. Conversi, L. Copin, Y. Courbin, F. Courtois, H. M. Da Silva, A. Degaudenzi, H. De Lucia, G. Dole, H. Dubath, F. Dupac, X. Dusini, S. Escoffier, S. Farina, M. Farinelli, R. Ferriol, S. Finelli, F. Fosalba, P. Fotopoulou, S. Frailis, M. Franceschi, E. Fumana, M. Galeotta, S. George, K. Gillis, B. Giocoli, C. Gracia-Carpio, J. Grazian, A. Grupp, F. Haugan, S. V. H. Holmes, W. Hormuth, F. Hornstrup, A. Jahnke, K. Jhabvala, M. Kermiche, S. Kiessling, A. Kubik, B. Kunz, M. Kurki-Suonio, H. Brun, A. M. C. Le Ligori, S. Lilje, P. B. Lloro, I. Mainetti, G. Maiorano, E. Mansutti, O. Marcin, S. Marggraf, O. Martinelli, M. Martinet, N. Marulli, F. Massey, R. J. Medinaceli, E. Mei, S. Melchior, M. Meneghetti, M. Merlin, E. Meylan, G. Mora, A. Moresco, M. Moscardini, L. Nakajima, R. Neissner, C. Niemi, S. -M. Padilla, C. Paltani, S. Pasian, F. Pedersen, K. Pettorino, V. Pires, S. Polenta, G. Poncet, M. Popa, L. A. Raison, F. Renzi, A. Rhodes, J. Riccio, G. Romelli, E. Roncarelli, M. Rosset, C. Saglia, R. Sakr, Z. Sánchez, A. G. Sapone, D. Schneider, P. Schrabback, T. Secroun, A. Seidel, G. Simon, P. Sirignano, C. Sirri, G. Stanco, L. Tallada-Crespí, P. Taylor, A. N. Tereno, I. Toft, S. Toledo-Moreo, R. Torradeflot, F. Tutusaus, I. Vassallo, T. Kleijn, G. Verdoes Wang, Y. Weller, J. Zamorani, G. Zucca, E. Castro, T. Martín-Fleitas, J. Monaco, P. Pezzotta, A. Scottez, V. Sereno, M. Viel, M. Sciotti, D. Cosmology and Nongalactic Astrophysics We study the properties of galaxy cluster 2-point correlation function covariance matrices estimated using the linear-construction (LC) method, which is computationally up to 20 times faster than the standard sample-covariance method. Our goal is to assess how well the LC method performs in cosmological parameter estimation compared to the sample covariance. We use a set of 1000 mock dark matter halo catalogues to compute both the LC-covariance and the sample-covariance estimates in four redshift shells. These numerical matrices are used to fit a theoretical four-parameter model for the covariance. We then use the two fitted covariance models in a likelihood function to estimate two cosmological parameters - the matter density parameter $Ω_{\rm m}$ and the amplitude of the matter density fluctuations $σ_8$ - from the simulated mock catalogues. The purpose of this is to validate the LC-covariance-based model against the sample-covariance model. The catalogues were simulated assuming the spatially flat $Λ$CDM cosmology, with $Ω_{\rm m} = 0.30711$ and $σ_8=0.8288$. We find that the parameter posteriors obtained using the sample- and LC-covariance models agree well with each other and with the simulation cosmology. The two pairs of marginalized constraints are $Ω_{\rm m} = 0.307 \pm 0.003$ and $σ_8 = 0.826\pm 0.009$ (sample covariance), and $Ω_{\rm m} = 0.308 \pm 0.003$ and $σ_8 = 0.825 \pm 0.009$ (LC covariance). The posterior widths are the same, and the difference in the median values is less than $0.16\,σ$ for both parameters.
title	Euclid: The linear-construction covariance and cosmology
topic	Cosmology and Nongalactic Astrophysics
url	https://arxiv.org/abs/2603.10735

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