# Detection of the Missing Baryons toward the Sightline of H1821+643

## TL;DR

This study employs a novel stacking method on X-ray data to definitively detect the WHIM's OVII absorption line, addressing the missing baryon problem by revealing hot intergalactic medium components.

## Contribution

It introduces a stacking approach combining X-ray and UV data to detect WHIM absorption lines with unprecedented sensitivity, providing new insights into baryon distribution.

## Key findings

- Detected OVII absorption line at 3.3 sigma significance.
- Estimated OVII column density of (1.4±0.4)×10^{15} cm^{-2}.
- Constrained the baryonic mass density associated with OVII.

## Abstract

Based on constraints from Big Bang nucleosynthesis and the cosmic microwave background, the baryon content of the high-redshift Universe can be precisely determined. However, at low redshift, about one-third of the baryons remain unaccounted for, which poses the long-standing missing baryon problem. The missing baryons are believed to reside in large-scale filaments in the form of warm-hot intergalactic medium (WHIM). In this work, we employ a novel stacking approach to explore the hot phases of the WHIM. Specifically, we utilize the 470 ks Chandra LETG data of the luminous quasar, H1821+643, along with previous measurements of UV absorption line systems and spectroscopic redshift measurements of galaxies toward the quasar's sightline. We repeatedly blueshift and stack the X-ray spectrum of the quasar corresponding to the redshifts of the 17 absorption line systems. Thus, we obtain a stacked spectrum with $8.0$ Ms total exposure, which allows us to probe X-ray absorption lines with unparalleled sensitivity. Based on the stacked data, we detect an OVII absorption line that exhibits a Gaussian line profile and is statistically significant at the $3.3 \sigma$ level. Since the redshifts of the UV absorption line systems were known a priori, this is the first definitive detection of an X-ray absorption line originating from the WHIM. The equivalent width of the OVII line is $(4.1\pm1.3) \ \mathrm{m\AA}$, which corresponds to an OVII column density of $(1.4\pm0.4)\times10^{15} \ \mathrm{cm^{-2}}$. We constrain the absorbing gas to have a density of $n_{\rm H} = (1-2)\times10^{-6} \ \rm{cm^{-3}}$ for a single WHIM filament. We derive $\Omega_{\rm b} \rm(O\,VII) = (0.0023 \pm 0.0007) \, \left[ f_{O\,VII} \, {Z/Z_{\odot}} \right]^{-1}$ for the cosmological mass density of OVII, assuming that all 17 systems contribute equally.