A holistic perspective on the dynamics of G035.39-00.33: the interplay between gas and magnetic fields
Creators: name: Liu, Tie
name: Li, Pak Shing
name: Juvela, Mika
name: Kim, Kee-Tae
name: Evans, Neal J.
name: Di Francesco, James
name: Liu, Sheng-Yuan
name: Yuan, Jinghua
name: Tatematsu, Ken'ichi
name: Zhang, Qizhou
name: Ward-Thompson, Derek
name: Fuller, Gary
name: Goldsmith, Paul F.
name: Koch, P. M.
name: Sanhueza, Patricio
name: Ristorcelli, I.
name: Kang, Sung-ju
name: Chen, Huei-Ru
name: Hirano, N.
name: Wu, Yuefang
name: Sokolov, Vlas
name: Lee, Chang Won
name: White, Glenn J.
name: Wang, Ke
name: Eden, David
name: Li, Di
name: Thompson, Mark
name: Pattle, Kate M
name: Soam, Archana
name: Nasedkin, Evert
name: Kim, Jongsoo
name: Kim, Gwanjeong
name: Lai, Shih-Ping
name: Park, Geumsook
name: Qiu, Keping
name: Zhang, Chuan-Peng
name: Alina, Dana
name: Eswaraiah, Chakali
name: Falgarone, Edith
name: Fich, Michel
name: Greaves, Jane
name: Gu, Q. -L.
name: Kwon, Woojin
name: Li, Hua-bai
name: Malinen, Johanna
name: Montier, Ludovic
name: Parsons, Harriet
name: Qin, Sheng-Li
name: Rawlings, Mark G.
name: Ren, Zhi-Yuan
name: Tang, Mengyao
name: Tang, Y. -W.
name: Toth, L. V.
name: Wang, Jiawei
name: Wouterloot, Jan
name: Yi, H. -W.
name: Zhang, H. -W.
Publisher: name: arXiv
Year: 2018
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: Magnetic field is one of the key agents that play a crucial role in shaping molecular clouds and regulating star formation, yet the complete information on the magnetic field is not well constrained due to the limitations in observations. We study the magnetic field in the massive infrared dark cloud G035.39-00.33 from dust continuum polarization observations at 850 $\micron$ with SCUBA-2/POL-2 at JCMT. The magnetic field tends to be perpendicular to the densest part of the main filament (F$_{M}$), whereas it has a less defined relative orientation in the rest of the structure, where it tends to be parallel to some diffuse regions. A mean plane-of-the-sky magnetic field strength of $\sim$50 $μ$G for F$_{M}$ is obtained using Davis-Chandrasekhar-Fermi method. Based on $^{13}$CO (1-0) line observations, we suggest a formation scenario of F$_{M}$ due to large-scale ($\sim$10 pc) cloud-cloud collision. Using additional NH$_3$ line data, we estimate that F$_{M}$ will be gravitationally unstable if it is only supported by thermal pressure and turbulence. The northern part of F$_{M}$, however, can be stabilized by a modest additional support from the local magnetic field. The middle and southern parts of F$_{M}$ are likely unstable even if the magnetic field support is taken into account. We claim that the clumps in F$_{M}$ may be supported by turbulence and magnetic fields against gravitational collapse. Finally, we identified for the first time a massive ($\sim$200 M$_{\sun}$), collapsing starless clump candidate, "c8", in G035.39-00.33. The magnetic field surrounding "c8" is likely pinched, hinting at an accretion flow along the filament.
description: Published on ApJ, 27 pages