Highly structured turbulence in high-mass star formation: an evolved infrared dark cloud G35.20-0.74 N

Abstract

Context. Massive stars are generally believed to form in supersonic turbulent environment. However, recent observations have challenged this traditional view. High spatial and spectral resolution observations of the Orion Molecular Cloud and an infrared dark cloud G35.39 show a resolution-dependent turbulence, and that high-mass stars are forming exclusively in subsonic to transonic cores in those clouds. These studies demand a re-evaluation of the role of the turbulence in massive star formation. Aims. We aim to study the turbulence in a typical massive star-forming region G35.20-0.74 N with a sufficient spatial resolution to resolve the thermal Jeans length, and a spectral resolution to resolve the thermal linewidth. Methods. We use the ALMA dust continuum emission to resolve fragmentation, JVLA 1.2 cm continuum to trace ionized gas, and JVLA NH3 (1,1) to (7,7) inversion transition lines to trace linewidth, temperature, and dynamics. We fit those lines and remove line broadening due to channel width, thermal pressure, and velocity gradient to obtain a clean map of intrinsic turbulence. Results. We find that (1) the turbulence in G35.20 is overall supersonic, with mean and median Mach numbers 3.7 and 2.8, respectively. (2) Mach number decreases from 6-7 at 0.1 pc scale to <3 towards the central cores at 0.01 pc scale. (3) The central ALMA cores appear to be decoupled form the host filament, evident by an opposite velocity gradient and significantly reduced turbulence. Because of intense star formation activities in G35.20 (as compared to the relatively young and quiescent IRDC G35.39), the supersonic turbulence is likely replenished by protostellar outflows. G35.20 is, thus, representative of an evolved form of IRDC G35.39. More observations of a sample of IRDCs are highly demanded to further investigate the role of turbulence in initial conditions for the massive star formation.

13 pages, 6 figures, 1 table

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