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 12 CO(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 n e 20 cm −3 and M H II 1500 M . 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.

Aims. We analyze the distribution of the interstellar matter in the environs of the Hll region Gum31, excited by the open cluster NGC 3324, located in the complex Carina region, with the aim of investigating the action of the massive stars on the surrounding neutral material. Methods. We use neutral hydrogen 21-cm line data, radio continuum images at 0.843, 2.4 and 4.9 GHz, 12CO(1-0) observations, and IRAS and MSX infrared data.Results. Adopting a distance of 3 kpc for the H II region and the ionizing cluster, we derived an electron density of 33 ± 3 cnr3 and an ionized mass of (3.3 ± 1.1) x 103 MQ based on the radio continuum data at 4.9 GHz. The Hi 21-cm line images revealed an Hi shell surrounding the H II region. The Hi structure is 10.0 ± 1.7 pc in radius, has a neutral mass of 1500 ± 500 M^, and is expanding at 11 kms-1 . The associated molecular gas amounts to (1.1 ± 0.

We investigate the distribution of gas (ionized, neutral atomic and molecular) and interstellar dust in the complex star‐forming region NGC 6357 with the goal of studying the interplay between the massive stars in the open cluster Pis 24 and the surrounding interstellar matter. Our study of the distribution of the ionized gas is based on narrow‐band Hα, [S ii]and [O iii] images obtained with the Curtis–Schmidt Camera at CTIO, Chile, and on radio continuum observations at 1465 MHz taken with the VLA with a synthesized beam of 40 arcsec. The distribution of the molecular gas is analysed using 12CO(1−0) data obtained with the NANTEN radiotelescope, Chile (angular resolution = 2.7 arcmin). The interstellar dust distribution was studied using mid‐infrared data from the GLIMPSE survey and far‐infrared observations from IRAS. NGC 6357 consists of a large ionized shell and a number of smaller optical nebulosities. The optical, radio continuum, and near‐ and mid‐IR images delineate the distributions of the ionized gas and interstellar dust in the H ii regions and in previously unknown wind‐blown bubbles linked to the massive stars in Pis 24 revealing surrounding photodissociation regions. The CO line observations allowed us to identify the molecular counterparts of the ionized structures in the complex and to confirm the presence of photodissociation regions. The action of the WR star HD 157504 on the surrounding gas was also investigated. The molecular mass in the complex is estimated to be (4 ± 2) × 105 M⊙. The mean electron densities derived from the radio data suggest electron densities >200 cm−3, indicating that NGC 6357 is a complex formed in a region of high ambient density. The known massive stars in Pis 24 and a number of newly inferred massive stars are mainly responsible for the excitation and photodissociation of the parental molecular cloud.