| Issue |
EPJ Web Conf.
Volume 257, 2022
mm Universe @ NIKA2 - Observing the mm Universe with the NIKA2 camera
|
|
|---|---|---|
| Article Number | 00018 | |
| Number of page(s) | 6 | |
| DOI | https://doi.org/10.1051/epjconf/202225700018 | |
| Published online | 17 January 2022 | |
https://doi.org/10.1051/epjconf/202225700018
Velocity dispersion vs cluster mass: A new scaling law with The Three Hundred clusters
1 Dipartimento di Fisica, Sapienza Universitá di Roma, Piazzale Aldo Moro 5, I-00185 Roma, Italy
2 Departamento de Física Téorica, Módulo 15, Facultad de Ciencias, Universidad Autónoma de Madrid, E-28049 Madrid, Spain
3 Centro de Investigación Avanzada en Física Fundamental (CIAFF), Facultad de Ciencias, Universidad Autónoma de Madrid, E-28049 Madrid, Spain
4 Univ. Grenoble Alpes, CNRS, LPSC-IN2P3, 53, avenue des Martyrs, 38000 Grenoble, France
5 Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, United Kingdom
* e-mail: ferragamoantonio@gmail.com
Published online: 17 January 2022
The Planck Collaboration has shown that the number of clusters as a function of their mass and redshift is an extremely powerful tool for cosmological analyses. However, the true cluster mass is not directly measurable. Among the possible approaches, clusters mass could be related to different observables via self similar scaling law. These observables are related to the baryonic components of which a cluster is composed. However, the theoretical relations that allow the use of these proxies often are affected by observational and physical biases, which impacts on the determination of the cluster mass. Fortunately, cosmological simulations are an extremely powerful tool to assess these problems. We present our calibration of the scaling relation between mass and velocity dispersion of galaxy members from the study of the simulated clusters of The Three Hundred project with mass above 1013M⊙. In order to investigate the presence of a redshift dependence, we analyzed 16 different redshifts between z = 0 and z = 2. Finally, we investigated the impact of different AGN feedback models.
© The Authors, published by EDP Sciences, 2022
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