Bibcode
Grandis, S.; Ghirardini, V.; Bocquet, S.; Garrel, C.; Mohr, J. J.; Liu, A.; Kluge, M.; Kimmig, L.; Reiprich, T. H.; Alarcon, A.; Amon, A.; Artis, E.; Bahar, Y. E.; Balzer, F.; Bechtol, K.; Becker, M. R.; Bernstein, G.; Bulbul, E.; Campos, A.; Carnero Rosell, A.; Carrasco Kind, M.; Cawthon, R.; Chang, C.; Chen, R.; Chiu, I.; Choi, A.; Clerc, N.; Comparat, J.; Cordero, J.; Davis, C.; Derose, J.; Diehl, H. T.; Dodelson, S.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Elvin-Poole, J.; Everett, S.; Ferte, A.; Gatti, M.; Giannini, G.; Giles, P.; Gruen, D.; Gruendl, R. A.; Harrison, I.; Hartley, W. G.; Herner, K.; Huff, E. M.; Kleinebreil, F.; Kuropatkin, N.; Leget, P. F.; Maccrann, N.; Mccullough, J.; Merloni, A.; Myles, J.; Nandra, K.; Navarro-Alsina, A.; Okabe, N.; Pacaud, F.; Pandey, S.; Prat, J.; Predehl, P.; Ramos, M.; Raveri, M.; Rollins, R. P.; Roodman, A.; Ross, A. J.; Rykoff, E. S.; Sanchez, C.; Sanders, J.; Schrabback, T.; Secco, L. F.; Seppi, R.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Troxel, M.; Tutusaus, I.; Varga, T. N.; Wu, H.; Yanny, B.; Yin, B.; Zhang, X.; Zhang, Y.; Alves, O.; Bhargava, S.; Brooks, D.; Burke, D. L.; Carretero, J.; Costanzi, M.; da Costa, L. N.; Pereira, M. E. S.; De Vicente, J.; Desai, S.; Doel, P.; Ferrero, I.; Flaugher, B.; Friedel, D.; Frieman, J.; García-Bellido, J. et al.
Bibliographical reference
Astronomy and Astrophysics
Advertised on:
7
2024
Journal
Citations
6
Refereed citations
2
Description
Context. Number counts of galaxy clusters across redshift are a powerful cosmological probe if a precise and accurate reconstruction of the underlying mass distribution is performed - a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing (WL) by clusters has become the method of choice for this measurement.
Aims: We measured and validated the WL signature in the shape of galaxies observed in the first three years of the Dark Energy Survey (DES Y3) caused by galaxy clusters and groups selected in the first all-sky survey performed by SRG (Spectrum Roentgen Gamma)/eROSITA (eRASS1). These data were then used to determine the scaling between the X-ray photon count rate of the clusters and their halo mass and redshift.
Methods: We empirically determined the degree of cluster member contamination in our background source sample. The individual cluster shear profiles were then analyzed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we performed mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allowed us to establish that hydrodynamical modeling uncertainties at low lens redshifts (z < 0.6) are the dominant systematic limitation. At high lens redshift, the uncertainties of the sources' photometric redshift calibration dominate.
Results: With regard to the X-ray count rate to halo mass relation, we determined its amplitude, its mass trend, the redshift evolution of the mass trend, the deviation from self-similar redshift evolution, and the intrinsic scatter around this relation.
Conclusions: The mass calibration analysis performed here sets the stage for a joint analysis with the number counts of eRASS1 clusters to constrain a host of cosmological parameters. We demonstrate that WL mass calibration of galaxy clusters can be performed successfully with source galaxies whose calibration was performed primarily for cosmic shear experiments, opening the way for the cluster cosmological exploitation of future optical and NIR surveys like Euclid and LSST.
Aims: We measured and validated the WL signature in the shape of galaxies observed in the first three years of the Dark Energy Survey (DES Y3) caused by galaxy clusters and groups selected in the first all-sky survey performed by SRG (Spectrum Roentgen Gamma)/eROSITA (eRASS1). These data were then used to determine the scaling between the X-ray photon count rate of the clusters and their halo mass and redshift.
Methods: We empirically determined the degree of cluster member contamination in our background source sample. The individual cluster shear profiles were then analyzed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we performed mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allowed us to establish that hydrodynamical modeling uncertainties at low lens redshifts (z < 0.6) are the dominant systematic limitation. At high lens redshift, the uncertainties of the sources' photometric redshift calibration dominate.
Results: With regard to the X-ray count rate to halo mass relation, we determined its amplitude, its mass trend, the redshift evolution of the mass trend, the deviation from self-similar redshift evolution, and the intrinsic scatter around this relation.
Conclusions: The mass calibration analysis performed here sets the stage for a joint analysis with the number counts of eRASS1 clusters to constrain a host of cosmological parameters. We demonstrate that WL mass calibration of galaxy clusters can be performed successfully with source galaxies whose calibration was performed primarily for cosmic shear experiments, opening the way for the cluster cosmological exploitation of future optical and NIR surveys like Euclid and LSST.