Revealing the Dark Threads of the Cosmic Web

Modern cosmology predicts that matter in our universe today has assembled into a vast network of filamentary structures colloquially termed the "cosmic web." Because this matter is either electromagnetically invisible (i.e., dark) or too diffuse to image in emission, tests of this cosmic w...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2020-03, Vol.891 (2), p.L35
Main Authors: Burchett, Joseph N., Elek, Oskar, Tejos, Nicolas, Prochaska, J. Xavier, Tripp, Todd M., Bordoloi, Rongmon, Forbes, Angus G.
Format: Article
Language:English
Subjects:
Absorption
Circumgalactic medium
Cosmic web
Cosmology
Density
Emission analysis
Filaments
Galaxies
Galaxy distribution
Galaxy evolution
Galaxy quenching
Intergalactic filaments
Intergalactic media
Intergalactic medium
Intergalactic voids
Ionization
Local group (astronomy)
Polls & surveys
Quasar absorption line spectroscopy
Quasars
Slime
Spectroscopy
Stars & galaxies
Universe
Voids
Webs
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Summary:Modern cosmology predicts that matter in our universe today has assembled into a vast network of filamentary structures colloquially termed the "cosmic web." Because this matter is either electromagnetically invisible (i.e., dark) or too diffuse to image in emission, tests of this cosmic web paradigm are limited. Wide-field surveys do reveal web-like structures in the galaxy distribution, but these luminous galaxies represent less than 10% of baryonic matter. Statistics of absorption by the intergalactic medium (IGM) via spectroscopy of distant quasars support the model yet have not conclusively tied the diffuse IGM to the web. Here, we report on a new method inspired by the Physarum polycephalum slime mold that is able to infer the density field of the cosmic web from galaxy surveys. Applying our technique to galaxy and absorption-line surveys of the local universe, we demonstrate that the bulk of the IGM indeed resides in the cosmic web. From the outskirts of cosmic web filaments, at approximately the cosmic mean matter density ( m) and ∼5 virial radii from nearby galaxies, we detect an increasing H i absorption signature toward higher densities and the circumgalactic medium, to ∼200 m. However, the absorption is suppressed within the densest environments, suggesting shock-heating and ionization deep within filaments and/or feedback processes within galaxies.
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/ab700c