A High-mass, Young Star-forming Core Escaping from Its Parental Filament

Abstract

We studied the unique kinematic properties in massive filament G352.63-1.07 at 10 ^3 au spatial scale with the dense molecular tracers observed with the Atacama Large Millimeter/submillimeter Array. We find the central massive core M1 (12 M _⊙ ) being separated from the surrounding filament with a velocity difference of $v-{\overline{v}}_{\mathrm{sys}}=-2\,\mathrm{km}\,{{\rm{s}}}^{-1}$ and a transverse separation within 3″. Meanwhile, as shown in multiple dense-gas tracers, M1 has a spatial extension closely aligned with the main filament and is connected to the filament toward both its ends. M1 thus represents a very beginning state for a massive, young star-forming core escaping from the parental filament, within a timescale of ∼4000 yr. Based on its kinetic energy (3.5 × 10 ^44 erg), the core escape is unlikely solely due to the original filament motion or magnetic field but requires more energetic events such as a rapid intense anisotropic collapse. The released energy also seems to noticeably increase the environmental turbulence. This may help the filament to become stabilized again.

Keywords

• Star formation
• Young stellar objects
• Dense interstellar clouds
• Interstellar filaments
• Gravitational collapse