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We propose a new approach to the missing baryons problem. Building on thecommon assumption that the missing baryons are in the form of the Warm HotIntergalactic Medium (WHIM), we further assumed here that the galaxy luminositydensity can be used as a tracer of the WHIM. The latter assumption is supportedby our finding of a significant correlation between the WHIM density and thegalaxy luminosity density in the hydrodynamical simulations of Cui et al.(2012). We further found that the fraction of the gas mass in the WHIM phase issubstantially (by a factor of $\sim$1.6) higher within the large scale galacticfilaments, i.e. $\sim$70\%, compared to the average in the full simulationvolume of $\sim$0.1\,Gpc$^3$. The relation between the WHIM overdensity and thegalaxy luminosity overdensity within the galactic filaments is consistent withlinear: $\delta_{\rm whim}\,=\,0.7\,\pm\,0.1\,\times\,\delta_\mathrm{LD}^{0.9\pm 0.2}$. We applied our procedure to the line of sight to the blazarH2356-309 and found evidence for the WHIM in correspondence of the SculptorWall (z $\sim$0.03 and $\log{N_H}$ = $19.9^{+0.1}_{-0.3}$) and Pisces-Cetussuperclusters (z $\sim$0.06 and $\log{N_H}$ = $19.7^{+0.2}_{-0.3}$), inagreement with the redshifts and column densities of the X-ray absorbersidentified and studied by Fang et al. (2010) and Zappacosta et al. (2010). Thisagreement indicates that the galaxy luminosity density and galactic filamentsare reliable signposts for the WHIM and that our method is robust in estimatingthe WHIM density. The signal that we detected cannot originate from the halosof the nearby galaxies since they cannot account for the large WHIM columndensities that our method and X-ray analysis consistently find in the SculptorWall and Pisces-Cetus superclusters.

Missing baryons traced by the galaxy luminosity density in the large-scale WHIM filaments