On the thermodynamic self-similarity of the nearest, most relaxed, giant ellipticals

TL;DR

This study reveals that the thermodynamic properties of hot gas in the inner regions of the nearest relaxed giant ellipticals follow similar power-law distributions beyond 1 kpc, indicating a common heating-cooling equilibrium maintained by AGN jets.

Contribution

It provides detailed spatially resolved measurements showing self-similar thermodynamic profiles in giant ellipticals, highlighting the role of AGN jet heating in maintaining a steady-state.

Findings

Thermodynamic profiles follow power-law distributions beyond 1 kpc.

Entropy profiles are well described by a power-law with index 0.92-1.07.

Inner regions show significant deviations, indicating variable AGN activity.

Abstract

We present detailed spatially resolved measurements of the thermodynamic properties of the X-ray emitting gas in the inner regions of the five nearest, X-ray and optically brightest, and most X-ray morphologically relaxed giant elliptical galaxies known. Beyond the innermost region at r > 1 kpc, and out to r ~ 6 kpc, the density, pressure, entropy, and cooling time distributions for the X-ray emitting gas follow remarkably similar, simple, power-law like distributions. Notably, the entropy profiles follow a power-law form, with an index 0.92-1.07. The cumulative hot X-ray emitting gas mass profiles and the gas-mass to stellar-light ratios of all five galaxies are also similar. Overall the observed similarity of the thermodynamic profiles in this radial range argues that, in these systems, relativistic jets heat the gas at a similar rate averaged over time scales longer than the cooling time of 10^8 yr. These jets are powered by accretion from the hot gas, or material entrained within it, onto the central super-massive black hole. This jet heating creates an energy balance where heating and cooling are in equilibrium, keeping the hot galactic atmospheres in a `steady-state'. Within r < 1 kpc, this similarity breaks down: the observed entropy profiles show well resolved flattening and the values differ from system to system substantially. The accretion rate onto the black hole and the AGN activity, heating the interstellar medium, must therefore vary significantly on time scales shorter than the cooling time of 10^7 - 10^8 yr.