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Warm-hot baryons comprise 5-10 per cent of filaments in the cosmic web.

Eckert, D. and Jauzac, M. and Shan, H. and Kneib, J.-P. and Erben, T. and Israel, H. and Jullo, E. and Klein, M. and Massey, R. and Richard, J. and Tchernin, C. (2015) 'Warm-hot baryons comprise 5-10 per cent of filaments in the cosmic web.', Nature., 528 . pp. 105-107.


Observations of the cosmic microwave background indicate that baryons account for 5 per cent of the Universe’s total energy content1. In the local Universe, the census of all observed baryons falls short of this estimate by a factor of two2, 3. Cosmological simulations indicate that the missing baryons have not condensed into virialized haloes, but reside throughout the filaments of the cosmic web (where matter density is larger than average) as a low-density plasma at temperatures of 105−107 kelvin, known as the warm–hot intergalactic medium3, 4, 5, 6. There have been previous claims of the detection of warm–hot baryons along the line of sight to distant blazars7, 8, 9, 10 and of hot gas between interacting clusters11, 12, 13, 14. These observations were, however, unable to trace the large-scale filamentary structure, or to estimate the total amount of warm–hot baryons in a representative volume of the Universe. Here we report X-ray observations of filamentary structures of gas at 107 kelvin associated with the galaxy cluster Abell 2744. Previous observations of this cluster15 were unable to resolve and remove coincidental X-ray point sources. After subtracting these, we find hot gas structures that are coherent over scales of 8 megaparsecs. The filaments coincide with over-densities of galaxies and dark matter, with 5–10 per cent of their mass in baryonic gas. This gas has been heated up by the cluster’s gravitational pull and is now feeding its core. Our findings strengthen evidence for a picture of the Universe in which a large fraction of the missing baryons reside in the filaments of the cosmic web.

Item Type:Article
Full text:(AM) Accepted Manuscript
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Date accepted:01 October 2015
Date deposited:11 April 2016
Date of first online publication:02 December 2015
Date first made open access:03 May 2016

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