Milky Way linear filaments exhibit no strong B-field alignment and bimodal galactic-plane orientations (parallel near midplane, perpendicular far from it), supporting a super-Alfvénic bubbly disk model.
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Synthetic Herschel observations from simulations yield 8832 filaments hosting 94% of clumps, with power-law mass and length distributions and a density relation qualitatively matching the Hi-GAL survey.
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The Milky Way Atlas for Linear Filaments III: Giant filaments and magnetic fields as evidence of a bubbly Galactic disk
Milky Way linear filaments exhibit no strong B-field alignment and bimodal galactic-plane orientations (parallel near midplane, perpendicular far from it), supporting a super-Alfvénic bubbly disk model.
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From filaments to clumps: filament properties with synthetic Herschel observations
Synthetic Herschel observations from simulations yield 8832 filaments hosting 94% of clumps, with power-law mass and length distributions and a density relation qualitatively matching the Hi-GAL survey.