A multi-wavelength analysis of the diffuse H ii region G25.8700+0.1350

• Published in: Monthly notices of the Royal Astronomical Society Vol. 474; no. 1; pp. 647 - 661
• Main Authors: Cichowolski, S., Duronea, N. U., Suad, L. A., Reynoso, E. M., Dorda, R.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 01-02-2018
• Subjects: Clumps; Emission analysis; Galaxies; H II regions; Molecular clouds; Molecular structure; O stars; Photodissociation; Red giant stars; Star & galaxy formation; Star formation; Supergiant stars; Wavelengths; H; stars: formation; stars: massive; infrared: ISM; regions; ISM: bubbles
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stx2676

Abstract
We present a multi-wavelength investigation of the H ii region G25.8700+0.1350, located in the inner part of the Galaxy. In radio continuum emission, the region is seen as a bright arc-shaped structure. An analysis of the H i line suggests that G25.8700+0.1350 lies at a distance of 6.5 kpc. The ionized gas is bordered by a photodissociation region, which is encircled by a molecular structure where four molecular clumps are detected. At infrared wavelengths, the region is also very conspicuous. Given the high level of visual absorption in the region, the exciting stars should be searched for in the infrared band. In this context, we found in the literature one Wolf–Rayet and one red supergiant, which, together with 37 2MASS sources that are candidate O-type stars, could be related to the origin of G25.8700+0.1350. Finally, as expanding H ii regions are hypothesized to trigger star formation, we used different infrared point source catalogues to search for young stellar object candidates (cYSOs). A total of 45 cYSOs were identified projected on to the molecular clouds.