Star Formation Activity in the Galactic HII Complex S255-S257

TL;DR

This study investigates star formation in the obscured S255-S257 complex using multi-wavelength data, revealing a diverse, young stellar population and evidence of induced star formation at the interface of evolved HII regions.

Contribution

It provides a detailed analysis of YSO populations, ages, and physical properties in the S255-S257 complex, highlighting non-coeval and induced star formation processes.

Findings

Identification of 109 YSO candidates, including 69 new ones.

Younger age (~1.2 Myr) of YSOs within the gas ridge compared to outside (~2.5 Myr).

Evidence of induced star formation at the interface of HII regions.

Abstract

We present results on the star-formation activity of an optically obscured region containing an embedded cluster (S255-IR) and molecular gas between two evolved HII regions S255 and S257. We have studied the complex using optical, near-infrared (NIR) imaging, optical spectroscopy and radio continnum mapping at 15 GHz, along with Spitzer-IRAC results. It is found that the main exciting sources of the evolved HII regions S255 and S257 and the compact HII regions associated with S255-IR are of O9.5 - B3 V nature, consistent with previous observations. Our NIR observations reveal 109 likely young stellar object (YSO) candidates in an area of ~ 4'.9 x 4'.9 centered on S255-IR, which include 69 new YSO candidates. Our observations increased the number of previously identified YSOs in this region by 32%. To see the global star formation, we constructed the V-I/V diagram for 51 optically identified IRAC YSOs in an area of ~ 13' x 13' centered on S255-IR. We suggest that these YSOs have an approximate age between 0.1 - 4 Myr, indicating a non-coeval star formation. Using spectral energy distribution models, we constrained physical properties and evolutionary status of 31 and 16 YSO candidates outside and inside the gas ridge, respectively. The models suggest that the sources associated within the gas ridge are of younger population (mean age ~ 1.2 Myr) than the sources outside the gas ridge (mean age ~ 2.5 Myr). The positions of the young sources inside the gas ridge at the interface of the HII regions S255 and S257, favor a site of induced star formation.