Abstract We explore the physical environment of the Galactic mid-infrared (MIR) bubble HKS2019 E71 (hereafter E71) through a multiwavelength approach. E71 is located at the edge of a filamentary structure, as traced in Herschel images (250–500 μ m), Herschel column density map, and molecular maps in the velocity range −20, −14 km s −1 . It hosts a stellar cluster (radius ∼ 1.26 pc, distance ∼1.81 ± 0.15 kpc) associated with radio continuum emission, including a centrally positioned B1.5-type massive star (hereafter “m2”), along with an enhanced population of evolved low-mass stars and young stellar objects. MIR images and molecular line maps reveal a photodissociation region surrounding “m2,” exhibiting an arc-like structure along the edges of E71. Regularly spaced molecular and dust condensations are identified along this structure. The position–velocity map of 12 CO (1–0) emission suggests an expansion of molecular gas concentrated at the periphery of E71. Near-infrared spectroscopic observations with TANSPEC confirm the presence of the accretion process in a massive young stellar object (MYSO) located near the edge of the bubble. High-resolution uGMRT radio continuum maps uncover substructures in the ionized emission, both toward the MYSO and the center of E71. These findings support that “m2” has shaped an arc-like morphology through its feedback processes. The pressure exerted by “m2” and the velocity structure of the 12/13 CO (1–0) emission suggest that the stellar feedback has likely driven out molecular material, leading to the formation of the expanding E71 bubble. Our overall investigation infers that the “collect and collapse” process might be a possible mechanism that can describe the ongoing star formation activities around the E71 bubble.
Verma et al. (Thu,) studied this question.
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