Probing the Hot Gaseous Halos of Milky Way-like Galaxies in the TNG50 simulation

TL;DR

This study uses the TNG50 simulation to compare the properties of hot gaseous halos around Milky Way-like galaxies with observations, revealing that simulated halos are too compact and lack hotter gas phases.

Contribution

It provides a detailed comparison between simulated and observed hot gaseous halos, identifying key discrepancies and implications for galaxy formation models.

Findings

Simulated halos match observed X-ray luminosity and O VII absorption but decline too steeply at large radii.

Halos underproduce O VIII absorption, indicating a deficit of hotter gas.

Simulations suggest feedback models deposit energy too centrally, affecting halo extent and temperature.

Abstract

The origin and structure of the hot ($T\gtrsim10^6$K) gaseous halo around Milky Way (MW)-mass galaxies provide a critical test for galaxy formation models. We perform a comprehensive comparison for a sample of MW analogues from the TNG50 cosmological simulation by generating synthetic soft X-ray emission and O VII/O VIII absorption lines, viewed from both internal (Solar) and external perspectives. The simulated halos successfully reproduce the observed global soft X-ray luminosity, inner-halo X-ray surface brightness, emission measure, and O VII absorption strength. However, two interconnected discrepancies are identified. First, the azimuthally averaged X-ray surface brightness profile from external viewpoints declines too steeply with radius compared to the extended emission detected in eROSITA stacking of SDSS galaxies, falling below the observations by up to $\sim 1$ dex at $R \gtrsim 100$ kpc. Second, the halos systematically underproduce O VIII absorption, with a median equivalent width $\sim 65\%$ lower than that observed in the Galactic halo, pointing to a deficit of hotter-phase gas at $T\sim(1.6-3.2)\times10^6$ K. These findings indicate that the simulated hot halos are too spatially compact and lack a hotter gas phase, suggesting that the TNG50 feedback model, while generating hot gas, deposits energy too centrally and too vigorously to sustain a gently extended, multi-phase corona.