Overview Results of JWST Observations of Star-Forming Clusters in the Extreme Outer Galaxy

TL;DR

This paper presents JWST infrared observations of star-forming clusters in the extreme outer Galaxy, revealing new details about low-mass stars and protostellar objects in a low-metallicity, low-density environment.

Contribution

It provides the first high-sensitivity, high-resolution infrared imaging of EOG clusters, detecting objects down to 0.01 solar masses and uncovering new star formation components.

Findings

Enhanced sensitivity allows detection of objects as low as 0.01 solar masses.

First resolution of individual YSOs in the EOG at MIR wavelengths.

Identification of new star formation features like class 0 candidates and jets.

Abstract

The extreme outer Galaxy (EOG), which we define as the region of the Milky Way with a galactocentric radius of more than 18 kpc, provides an excellent opportunity to study star formation in an environment significantly different from that in the solar neighborhood because of its lower metallicity and lower gas density. We carried out near- and mid-infrared (NIR and MIR) imaging observations toward two star-forming clusters located in the EOG using JWST NIRCam and MIRI with nine filters: F115W, F150W, F200W, F350W, F405N, F444W, F770W, F1280W, and F2100W. In this paper, we present an overview of the observations, data reduction, and initial results. The NIR sensitivity is approximately 10--80 times better than our previous observation with the Subaru 8.2 m telescope. Accordingly, the mass detection limit reaches to about 0.01--0.05 $M_\odot$, which is about 10 times better than the previous observations. At MIR wavelengths, the high sensitivity and resolution data enable us to resolve individual young stellar objects in such a distant region for the first time. The mass detection limit at MIR F770W filter reaches about 0.1--0.3 $M_\odot$. With these new observations, we have identified components of the clusters that previous surveys did not detect, including class 0 candidates, outflow/jet components, and distinctive nebular structures. These data will enable us to investigate the properties of star formation in the EOG at the same depth of detail as previous observations of star formation in the solar neighborhood.