Issue |
A&A
Volume 670, February 2023
|
|
---|---|---|
Article Number | A17 | |
Number of page(s) | 16 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/202244626 | |
Published online | 30 January 2023 |
Structural and dynamical modeling of WINGS clusters
III. The pseudo phase-space density profile
1
INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy
e-mail: andrea.biviano@inaf.it
2
IFPU-Institute for Fundamental Physics of the Universe, Via Beirut 2, 34014 Trieste, Italy
3
Institut d’Astrophysique de Paris, UMR 7095: CNRS & Sorbonne Université, 98 bis Bd Arago, 75014 Paris, France
Received:
29
July
2022
Accepted:
28
November
2022
Numerical simulations indicate that cosmological halos display power-law radial profiles of pseudo phase-space density (PPSD), Q ≡ ρ/σ3, where ρ is the mass density and σ is the velocity dispersion. We tested these predictions for Q(r) using the parameters derived from the Markov chain Monte Carlo (MCMC) analysis performed with the MAMPOSSt mass-orbit modeling code on the observed kinematics of a velocity dispersion based stack (σv) of 54 nearby regular clusters of galaxies from the WINGS data set. In the definition of PPSD, the density is either in total mass ρ (Qρ) or in galaxy number density ν (Qν) of three morphological classes of galaxies (ellipticals, lenticulars, and spirals), while the velocity dispersion (obtained by inversion of the Jeans equation using the MCMC parameters) is either the total (Qρ and Qν) or its radial component (Qr, ρ and Qr, ν). We find that the PPSD profiles are indeed power-law relations for nearly all MCMC parameters. The logarithmic slopes of our observed Qρ(r) and Qr, ρ(r) for ellipticals and spirals are in excellent agreement with the predictions for particles in simulations, but slightly shallower for S0s. For Qν(r) and Qr, ν(r), only the ellipticals have a PPSD slope matching that of particles in simulations, while the slope for spirals is much shallower, similar to that of subhalos. However, for cluster stacks based on the richness or gas temperature, the fraction of power-law PPSDs is lower (esp. Qν) and the Qρ slopes are shallower, except for S0s. The observed PPSD profiles, defined using ρ rather than ν, appear to be a fundamental property of galaxy clusters. They would be imprinted during an early phase of violent relaxation for dark matter and ellipticals, and later for spirals as they move toward dynamical equilibrium in the cluster gravitational potential, while S0s are either intermediate (richness and temperature-based stacks) or a mixed class (σv stack).
Key words: galaxies: clusters: general / galaxies: kinematics and dynamics / dark matter
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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