English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The entropy distribution of the intracluster gas reflects both accretion history of the gas and the processes of feedback which provide a further non‐gravitational energy besides the potential one. In this work, we study the profiles and the scaling properties of the gas entropy in 24 hot  ( kT  gas  &gt; 6 keV)  galaxy clusters observed with  Chandra  in the redshift range 0.14–0.82 and showing different states of relaxation. We recover the gas density, temperature and entropy profiles in a non‐parametric way, just relying on the assumption of a spherically symmetric emission in the deprojection of the best‐fitting results of the spatially resolved X‐ray spectral analysis. Adding the hydrostatic equilibrium hypothesis, radial profiles are also obtained from the deprojection of the surface brightness, allowing to verify whether the hydrostatic equilibrium is a tenable hypothesis by comparison with the spectral measurements. We confirm that this is the case on scales larger than 100 kpc and discuss the deviations observed in a few non‐cooling core clusters in the inner regions. We show that the entropy profiles are remarkably similar outside the core and can be described by simple power laws with slope of 1.0–1.2. We measure an entropy level at  0.1  R  200   of  100−500 keV cm 2   and a central plateau which spans a wide range of value (approximately a few  −200 keV cm 2  ) depending on the state of relaxation of the source. The entropy values resolved at a given fraction of the virial radius are proportional to the gas temperature in these hot systems and appear larger at higher redshift once they are compared to the local estimates. To characterize the energetic of the central regions, we compare the radial behaviour of the temperature of the gas with the temperature of the dark matter (DM)  T  DM  by estimating the excess of energy  Δ E = 3/2  k ( T  gas − T  DM ) . We point out that Δ E  ranges from ≈0 in typical cooling‐core clusters to a few keV within 100 kpc in non‐cooling‐core systems. We also measure a significant correlation between the total iron mass and the entropy outside the cooling region, whereas in the inner regions they anticorrelate strongly. We find that none of the current models in literature on the extra‐gravitational energy is able to justify alone the evidences we obtained on the entropy, metallicity and gas plus DM temperature profiles.

Entropy profiles in X‐ray luminous galaxy clusters at z > 0.1