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Fig. 4.


The detection of the cosmic web between neighbouring luminous red galaxies as detected through the weak lensing of background galaxies from different lensing surveys. Left: x-axis is the distance measured perpendicular to the filament axis scaled such that 1 is equivalent to the projected separation between the pair of LRGs. The y-axis is the nulled shear signal where ℱγ1 (blue data points) measures the average surface mass density of the filament, and ℱγ2 is expected to be consistent with zero and hence serves as a null test. Lower right small panel: measurements from the three-surveys combined using inverse variance weighting. We note that this additional panel is purely for illustration, however, as our joint survey-constraints on the filament model are derived from a combination of the surveys on the likelihood-level. Right: estimated parameters in the filament density model Eq. (5) from the stacked signal for all surveys individually and their combination. Upper: results from 3 ∼ 5 h−1 Mpc Physical Pairs, our filament candidates; Lower: results from 3 ∼ 5 h−1 Mpc non-physical Pairs, our control sample.

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