IRAS 23385+6053 JWST observations

While the general spectrum is typical for an embedded protostar, we see many atomic and molecular gas lines boosted by the higher spectral resolution and sensitivity compared to previous space missions. Furthermore, ice and dust absorption features are also present. Here, we focus on the continuum emission, outflow tracers like the H2(0-0)S(7), [FeII](^4^F_9/2_-^6^D_9/2_) and [NeII](^2^P_1/2_-^2^P_3/2_) lines as well as the potential accretion tracer Humphreys {alpha} HI(7-6).

The short-wavelength MIRI data resolve two continuum sources A and B, where mid-infrared source A is associated with the main mm continuum peak. The combination of mid-infrared and mm data reveals a young cluster in its making. Combining the mid-infrared outflow tracer H_2_, [FeII] and [NeII] with mm SiO data shows a complex interplay of at least three molecular outflows driven by protostars in the forming cluster.

Furthermore, the Humphreys line is detected at a 3-4{sigma} level towards the mid-infrared sources A and B. Following Rigliaco et al. (2015), one can roughly estimate both accretion luminosities and corresponding accretion rates between ~2.6x10^-6^ and ~0.9x10^-4^M_{sun}_/yr. This is discussed in the context of the observed outflow rates. The analysis of the MIRI MRS observations for this young high-mass star-forming region reveals connected outflow and accretion signatures.

Furthermore, they outline the enormous potential of JWST to boost our understanding of the physical and chemical processes during star formation.