Excitation source of Br α filaments in the left portion of the JWST field

Determine the excitation mechanism responsible for the Br α emission in the left portion of the JWST NIRCam field toward the Sagittarius C H II region, specifically resolving whether these filaments are excited by massive stars within Sagittarius C, by other Central Molecular Zone OB stars along the line of sight, or instead trace shocks from supernova remnants in the Central Molecular Zone.

Background

JWST NIRCam Br α imaging of the Sagittarius C H II region reveals extensive filamentary structure, including features outside the suspected boundary of the region. The left portion of the JWST field shows filaments whose excitation is not directly attributable from the presented data.

The authors note that these filaments could be excited by massive stars (either within Sgr C or elsewhere in the CMZ) or could instead be shock-related features tied to supernova remnants. Clarifying the excitation mechanism is important for interpreting the morphology, energetics, and environmental interactions of ionized gas in the CMZ.