SIMBAD references

2010MNRAS.405.1976V - Mon. Not. R. Astron. Soc., 405, 1976-1986 (2010/July-1)

Ionized gas, molecules and dust in Sh2-132.

VASQUEZ J., CAPPA C.E., PINEAULT S. and DURONEA N.U.

Abstract (from CDS):

We analyse the various interstellar components of the Hii region Sh2-132. The main stellar source is the double binary system that includes the Wolf-Rayet star WR153ab. We use radio continuum images at 408 and 1420 MHz, and Hi 21-cm line data taken from the Canadian Galactic Plane Survey, molecular observations of the 12CO(1-0) line at 115GHz 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/cm3 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, similar to the velocity of the ionized gas.

The emission at 8.3µm reveals a ring-like feature of about 15arcmin 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.


Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): stars: individual: WR153ab - stars: Wolf-Rayet - ISM: molecules - ISM: individual objects: Sh2-132 - ISM: bubbles - Hii regions

Nomenclature: Fig. 5, Table 4: [VCP2010] fN (Nos f1-f3), [VCP2010] psN (Nos ps1-ps3). Fig. 7, Table 5: [VCP2010] A (Nos A-F).

Simbad objects: 21

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2020.06.02-16:39:50

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