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SIMPLIFI—Study of Interstellar Magnetic Polarization: A Legacy Investigation of Filaments. I. Magnetically Guided Accretion onto the DR21 Ridge

  • Authors: Thushara G. S. Pillai, Jens Kauffmann, Juan D. Soler, Mark Heyer, Philip C. Myers, Laura M. Fissel, Dan Clemens, Koji Sugitani, Enrique Lopez-Rodriguez, Fumitaka Nakamura, Andrea Giannetti, Daniel Seifried, Paul F. Goldsmith, Helmut Wiesemeyer, Evangelia Ntormousi, Gabriel Franco, Stefan Reissl, Karl M. Menten

Thushara G. S. Pillai et al 2026 The Astrophysical Journal 1004 .

  • Provider: AAS Journals

Caption: Figure 5.

Projected Rayleigh statistic Z (top row; Equation (7)) and per-pixel alignment components zi (bottom row; Equation (13)) as a function of column density. Blue shading/empty circles indicate subfilaments, while green shading/gray crosses indicate the DR21 Main Ridge. Columns show the relative orientation between magnetic field and intensity gradient (left; Section 4.1), self-gravity and intensity gradient (middle; Section 4.2), and magnetic field and self-gravity (right; Section 4.3). For Z, error bars give σobs(Z) (Equation (12)), reflecting individual measurement uncertainties, while shading gives σgen(Z) (Equation (11)), our preferred uncertainty measure that also captures internal structural diversity (Section 3.4). An inset legend in the upper right panel illustrates both uncertainty types. For zi, dashed lines connect bin-averaged 〈zi〉 values and shading indicates σgen(〈zi〉).

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