The Search for the Missing Baryons at Low Redshift

TL;DR

This paper reviews the current observational efforts and challenges in detecting the missing baryons at low redshift, highlighting that most are theorized to be in warm-hot intergalactic medium but remain largely undetected.

Contribution

It provides a comprehensive overview of observational evidence and limitations regarding the detection of missing baryons in different temperature regimes at low redshift.

Findings

Most missing baryons are in warm-hot intergalactic medium.

Current observations have not definitively detected the intergalactic hot gas.

Instrumental sensitivity improvements could enable detection of missing baryons.

Abstract

At low redshift, only about one-tenth of the known baryons lie in galaxies or the hot gas seen in galaxy clusters and groups. Models posit that these "missing baryons" are in gaseous form in overdense filaments that connect the much denser virialized groups and clusters. About 30% are cool (<1E5 K) and are detected in Ly alpha absorption studies, but about half is predicted to lie in the 1E5-1E7 K regime. Gas is detected in the 2-5E5 K range through OVI absorption studies (7% of the baryons) and possibly near 1E5 K from broad Ly absorption (20% of the baryons). Hotter gas (0.5-2E6 K) is detected at zero redshift by OVII and OVIII K X-ray absorption, and the OVII line strengths seem to correlate with the Galactic soft X-ray background, so it is probably produced by Galactic Halo gas, rather than a Local Group medium. There are no compelling detections of the intergalactic hot gas (0.5-10E6 K) either in absorption or emission and these upper limits are consistent with theoretical models. Claimed X-ray absorption lines are not confirmed, while most of the claims of soft emission are attributable to artifacts of background subtraction and field-flattening. The missing baryons should become detectable with moderate improvements in instrumental sensitivity.