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We present a statistical study on the orientation of outflows with respect tolarge-scale filaments and the magnetic fields. Although filaments are widelyobserved toward Galactic star-forming regions, the exact role of filaments instar formation is unclear. Studies toward low-mass star-forming regionsrevealed both preferred and random orientation of outflows respective to thefilament long-axes, while outflows in massive star-forming regions mostlyoriented perpendicular to the host filaments, and parallel to the magneticfields at similar physical scales. Here, we explore outflows in a sample of 11protoclusters in HII regions, a more evolved stage compared to IRDCs, usingALMA CO (3-2) line observations. We identify a total of 105 outflow lobes inthese protoclusters. Among the 11 targets, 7 are embedded within parsec-scalefilamentary structures detected in $^{13}$CO line and 870 $\mu m$ continuumemissions. The angles between outflow axes and corresponding filaments($\gamma_\mathrm{Fil}$) do not show any hint of preferred orientations (i.e.,orthogonal or parallel as inferred in numerical models) with respect to theposition angle of the filaments. Identified outflow lobes are also notcorrelated with the magnetic fields and Galactic plane position angles.Outflows associated with filaments aligned along the large-scale magneticfields are also randomly orientated. Our study presents the first statisticalresults of outflow orientation respective to large-scale filaments and magneticfields in evolved massive star-forming regions. The random distributionsuggests a lack of alignment of outflows with filaments, which may be a resultof the evolutionary stage of the clusters.

ALMA observations reveal no preferred outflow--filament and outflow--magnetic field orientations