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High-definition imaging of a filamentary connection between a close quasar pair at z=3
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Filaments connecting halos are a long-standing prediction of cold dark matter theories. We present a detection of the cosmic web emission connecting two quasar-host galaxies at redshift z ~3.22 in the MUSE Ultra Deep Field (MUDF). The very deep observations unlock a high-definition view of the filament morphology, a measure of the transition radius between the intergalactic and circumgalactic medium, and the characterization of the surface brightness profiles along the filament and in the transverse direction. Through systematic comparisons with simulations, we validate the filaments' typical density predicted in the current cold dark-matter model. Our analysis of the MUDF field, an excellent laboratory for quantitatively studying filaments in emission, opens a new avenue to constrain the physical properties of the cosmic web and to trace the distribution of dark matter on large scales.
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Cited by 3 Pith papers
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A MUltiwavelength Study of ELAN Environments (AMUSE$^2$): The Impact of Dense Environment on Massive Dusty Star-Forming Galaxies at Cosmic Noon
SMGs around z~2-3 quasars outside virial radii resemble field SMGs, while combined literature data show lower gas fractions inside quasar halos, suggesting environmental effects act only on halo scales.
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Modeling Mg II resonance doublet spectra from galaxy haloes at z $\sim$ 1
A radiative-transfer analysis of Mg II spectra from 624 z~1 galaxies finds more massive galaxies have higher column density and slower-moving cold gas.
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MUSEQuBES: Unveiling Cosmic Web Filaments at $z\approx3.6$ through Dual Absorption and Emission Line Analysis
Detection of an extremely metal-poor, low-density gas absorber, an aligned overdensity of seven Lyman-alpha galaxies, and a 260 pkpc Lyman-alpha nebula, interpreted as a cosmic filament at z≈3.6.
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