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Magnetic Fields in Massive Star-forming Regions (MagMaR). VI. Magnetic Field Dragging in the Filamentary High-mass Star-forming Region G35.20–0.74N Due to Gravity

  • Authors: Jihye Hwang, Patricio Sanhueza, Josep Miquel Girart, Ian W. Stephens, Maria T. Beltrán, Chi Yan Law, Qizhou Zhang, Junhao Liu, Paulo Cortés, Fernando A. Olguin, Patrick M. Koch, Fumitaka Nakamura, Piyali Saha, Jia-Wei Wang, Fengwei Xu, Henrik Beuther, Kaho Morii, Manuel Fernández López, Wenyu Jiao, Kee-Tae Kim, Shanghuo Li, Luis A. Zapata, Jongsoo Kim, Spandan Choudhury, Yu Cheng, Kate Pattle, Chakali Eswaraiah, Panigrahy Sandhyarani, L. K. Dewangan, O. R. Jadhav

Jihye Hwang et al 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 2.

(Left) The skeleton of the filament in G35. The background image is the same as in Figure 1. White contours show the flux density of G35 at 3, 10, 20, 30, and 40 ×δI levels. (Right) Angle difference between the main skeleton and magnetic field orientations.

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