It’s hard enough to figure out what dark energy and dark matter are, a task that will occupy physicists for a long time to come. But even if we confine ourselves to ‘normal’ or ‘baryonic’ matter (accounting only for some four or five percent of the universe), we’re still left with a problem. Baryons are heavy subatomic particles like protons and neutrons that experience the strong nuclear force, and the problem is that even these relatively familiar particles are only partially accounted for.

So where is the missing baryonic matter? The answer may lie in a thin haze of hot, low-density gas that connects galactic clusters. Call it WHIM, for warm-hot intergalactic medium. Dutch and German scientists now think they have uncovered a filament of such gas that connects the clusters Abell 222 and Abell 223. The properties of the gas, visible primarily in the far ultraviolet and X-ray bands, fit with simulations in terms of density and temperature. The scientists used the XMM-Newton X-ray observatory to identify the hitherto unobserved filament.

Filament between clusters

Image: Composite optical and X-ray image of galaxy clusters Abell 222 and Abell 223. The cluster pair is connected by a filament permeated by hot X-ray emitting gas. The optical image was obtained by SuprimeCam at the Subaru telescope, the X-ray image showing the distribution of the diffuse hot gas (yellow to red) was obtained by XMM-Newton. Credits: ESA/ XMM-Newton/ EPIC/ ESO (J. Dietrich)/ SRON (N. Werner)/ MPE (A. Finoguenov).

Norbert Werner (SRON Netherlands Institute for Space Research), who led this work, thinks the team is seeing at least some of the missing baryonic matter. Says Werner, “The hot gas that we see in this bridge or filament is probably the hottest and densest part of the diffuse gas in the cosmic web…”

That last phrase deserves explanation. I’m working through the paper, which likens the structure of the universe to such a web-like structure, with galactic clusters, the largest objects in the universe, congregating at the web’s densest nodes. Let me quote the scientists on this:

According to the standard theory of structure formation, the spatial distribution of matter in the Universe evolved from small perturbations in the primordial density field into a complex structure of sheets and filaments with clusters of galaxies at the intersections of this filamentary structure. The filaments have been identified in optical surveys of galaxies…, but the dominant fraction of their baryons is probably in the form of a low density warm-hot gas emitting predominantly soft X-rays.

Sheets and filaments, with the things we see clustering in the web’s threads and knots. Thirty to forty percent of the baryonic matter in the universe ought to reside in filaments connecting galactic clusters, according to a variety of simulations, but this seems to be the first unambiguous detection (although other candidates have been put forward). And while the observed filament closely tracks at least one previous simulation, we still haven’t seen the largest part of the missing matter:

…according to the simulations… the dominant fraction of the WHIM resides in a lower temperature and density phase, the existence of which still remains to be proven observationally. The detection of the dominant fraction of the WHIM will only be possible with dedicated future instrumentation…

In other words, we’re going to need a more advanced space-based observatory to extend such difficult work, this particular filament being detectable largely because it is along the line of sight from Earth, thus concentrating its emission in a small region of sky. Understanding how matter is distributed in these structures will help us better piece together this web-like structure and the place of baryons within it.

The paper is Werner, et al., “Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223,” Astronomy & Astrophysics Letters, Volume 482-3 (May, 2008), p. L29 (abstract).