Absorption signatures of warm-hot gas at low redshift: NeVIII

TL;DR

This paper presents an analytic model for NeVIII absorbers in low-redshift warm-hot gas, revealing their properties, distribution, and role as probes of shock-heated baryons, with implications for detecting the missing baryon problem.

Contribution

The paper introduces a new analytic model accounting for inhomogeneous metal distribution in NeVIII absorbers, aligning with simulation predictions and characterizing their physical conditions.

Findings

NeVIII absorbers mainly originate in low-density, collisionally ionized gas.

Strong NeVIII absorbers are associated with higher density, hotter gas.

NeVIII cloudlets contain only about 1% of the cosmic baryon budget.

Abstract

At z<1 a large fraction of the baryons is thought to reside in diffuse gas that has been shock-heated to high temperatures (log T=5-6). Absorption by the 770.41, 780.32 {\AA} doublet of NeVIII in quasar spectra represents a unique tool to study this elusive warm-hot phase. We have developed an analytic model for the properties of NeVIII absorbers that allows for an inhomogeneous metal distribution. Our model agrees with the predictions of a simulation from the OWLS project indicating that the average line-of-sight metal-filling fraction within the absorbing gas is low (c_L~0.1). Most of the NeVIII in our model is produced in low-density, collisionally ionized gas (log n=-6 to -4 cm^-3, log T=5-6). Strong NeVIII absorbers (log N(NeVIII)>14), like those recently detected by HST/COS, are found to arise in higher density gas (log n>-4, log T=5.75). NeVIII cloudlets harbour only 1 per cent of the cosmic baryon budget. The baryon content of the surrounding gas (which has similar densities and temperatures as the NeVIII cloudlets) is a factor 1/c_L higher. We conclude that NeVIII absorbers are robust probes of shock-heated diffuse gas, but that spectra with signal-to-noise ratios S/N>100 would be required to detect the bulk of the baryons in warm-hot gas.