Ionized gas, molecules and dust in Sh2-132

• Published in: Monthly notices of the Royal Astronomical Society Vol. 405; no. 3; pp. 1976 - 1986
• Main Authors: Vasquez, J., Cappa, C. E., Pineault, S., Duronea, N. U.
• Format: Journal Article
• Language: English
• Published: Oxford, UK Blackwell Publishing Ltd 01-07-2010; Wiley-Blackwell; Oxford University Press
• Subjects: Astronomy; Dust; Earth, ocean, space; Exact sciences and technology; Gases; H ii regions; Ions; ISM: bubbles; ISM: individual objects: Sh2-132; ISM: molecules; Molecules; stars: individual: WR 153ab; stars: Wolf–Rayet; stars: Wolf-Rayet; regions; ISM: molecules; ISM: bubbles; ISM: individual objects: Sh2-132; H; stars: individual: WR 153ab; Stellar winds; Ionized gases; Galactic planes; 21cm-Line; H regions; Infrared observation; Molecular gas; Photodissociation; Wolf-Rayet stars; HII regions; Massive stars; Continuum; Radio astronomy observatory; Radio map; Radio counterpart; Polycyclic aromatic hydrocarbons; Electron density
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2010.16590.x

We analyse the various interstellar components of the H ii region Sh2-132. The main stellar source is the double binary system that includes the Wolf–Rayet star WR 153ab. We use radio continuum images at 408 and 1420 MHz, and H i 21-cm line data taken from the Canadian Galactic Plane Survey, molecular observations of the 12CO(1–0) line at 115 GHz from the Five College Radio Astronomy Observatory, and available mid- and far-infrared observations obtained with the MSX and IRAS satellites, respectively. Sh2-132 is composed of two shells showing radio continuum counterparts at both frequencies. The emission is thermal in nature. The estimated rms electron density and ionized mass of the nebula are ne≃ 20 cm−3 and . The distribution of the CO emission shows molecular gas bordering the ionized nebula and interacting with it. The velocities of the molecular gas is in the range −38 to −53 km s−1, similar to the velocity of the ionized gas. The emission at 8.3 μm reveals a ring-like feature of about 15 arcmin that encircles the bright optical regions. This emission is due to the polycyclic aromatic hydrocarbons and marks the location of photodissociation regions. The gas distribution in the environs of Sh2-132 can be explained in a scenario where the massive stars in the region photodissociated, ionized and swept up the dense molecular material from the parental cloud through their strong stellar winds and intense ultraviolet (UV) photon flux.