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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 8.

(Left) The centroid velocities of H13CO+ for the velocity-coherent gas components described in Section 3.4 as a function of the distance from the B2 core of the central binary system in the G35 filament are shown in Figure 1. The negative and positive distances mean the eastern and western sides of the core. The dashed lines indicate other core positions. The colors are shown red- and blueshifted velocities compared to the LSR velocity of 35 km s−1. (Right) The mean centroid velocities as a function of distance. The standard deviation is shown as an error bar.

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