$i(cm)z$, a semi-analytic model for the thermodynamic properties in galaxy clusters: calibrations with mass and redshift, and implication for the hydrostatic bias

S. Ettori; L. Lovisari; D. Eckert

doi:10.1051/0004-6361/202245002

paper

$i (c m) z$ , a semi-analytic model for the thermodynamic properties in galaxy clusters: calibrations with mass and redshift, and implication for the hydrostatic bias

arXiv:2211.03082 · doi:10.1051/0004-6361/202245002

Abstract

In the self-similar scenario for galaxy cluster formation and evolution, the thermodynamic properties of the X-ray emitting plasma can be predicted in their dependencies on the halo mass and redshift only. However, several departures from this simple self-similar scenario have been observed. We show how our semi-analytic model $i (c m) z$ , which modifies the self-similar predictions through two temperature-dependent quantities, the gas mass fraction $f_{g} = f_{0} T^{f_{1}} E_{z}^{f_{z}}$ and the temperature variation $f_{T} = t_{0} T^{t_{1}} E_{z}^{t_{z}}$ , can be calibrated to incorporate the mass and redshift dependencies. We used a published set of 17 scaling relations to constrain the parameters of the model. We were subsequently able to make predictions as to the slope of any observed scaling relation within a few percent of the central value and about one $σ$ of the nominal error. Contextually, the evolution of these scaling laws was also determined, with predictions within $1.5 σ$ and within 10 percent of the observational constraints. Relying on this calibration, we have also evaluated the consistency of the predictions on the radial profiles with some observational datasets. For a sample of high-quality data (X-COP), we were able to constrain a further parameter of the model, the hydrostatic bias $b$ . By calibrating the model, we have determined that (i) the slopes of the temperature dependence are $f_{1} = 0.403 (\pm 0.009)$ and $t_{1} = 0.144 (\pm 0.017)$ ; and that (ii) the dependence upon $E_{z}$ are constrained to be $f_{z} = - 0.004 (\pm 0.023)$ and $t_{z} = 0.349 (\pm 0.059)$ . These values permit one to estimate directly how the normalizations of a given quantity $Q_{Δ}$ changes as a function of the mass (or temperature) and redshift halo in the form $Q_{Δ} \sim M^{a_{M}} E_{z}^{a_{z}} \sim T^{a_{T}} E_{z}^{a_{T z}}$ , in very good agreement with the current observational constraints.

arXiv comment15 pages; A&A in press. Updated to match the published version; a few typos were corrected, and a reference added

$i (c m) z$ , a semi-analytic model for the thermodynamic properties in galaxy clusters: calibrations with mass and redshift, and implication for the hydrostatic bias

Abstract

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i(cm)z, a semi-analytic model for the thermodynamic properties in galaxy clusters: calibrations with mass and redshift, and implication for the hydrostatic bias

Abstract

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Cited by in corpus (5)

$i (c m) z$ , a semi-analytic model for the thermodynamic properties in galaxy clusters: calibrations with mass and redshift, and implication for the hydrostatic bias