Abstract:
Using multi-wavelength data sets, we studied the star-formation activity in Hii region Sh 2-61
(hereafter S61). We identified a clustering in the region and estimated the membership using the Gaia proper
motion data. The physical environment of S61 is inspected using infrared to radio wavelength images. We also
determined the Lyman continuum flux associated with the Hii region and found that the Hii region is formed
by at least two massive stars (S1 and S2). We also analyzed the 12CO (J = 3–2) JCMT data of S61, and a shell
structure accompanying three molecular clumps are observed towards S61. We found that the ionized gas in
S61 is surrounded by dust and a molecular shell. Many young stellar objects and three molecular clumps are
observed at the interface of the ionized gas and surrounding gas. The pressure at the interface is higher than in
a typical cool molecular cloud.
