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Context: A complete study of the molecular and ionized gas in the environs ofthe nebula RCW 78 around WR 55 is presented. Aims: The aim of this work is toinvestigate the spatial distribution, physical characteristics, and kinematicalproperties of the molecular gas linked to the galactic nebula RCW 78 to achievea better understanding of its interaction with the star and with the ionizedgas. Methods: This study was based on 12CO(1-0) fully sampled observations of aregion of ~0.45{\deg} in size around the star WR 55 and the nebula RCW 78obtained with the 4-m NANTEN telescope, radio continuum archival data at 1.4and 4.85 GHz, obtained from SGPS and PMNRAO Southern Radio Survey,respectively, and available infrared MIPSGAL images at 24 microns. Results: Amolecular gas component in the velocity range from ~ -58 to -45 km s-1,compatible with the velocity of the ionized gas, was found to be associatedwith the optical nebula. Adopting a distance of ~ 5 kpc, the mass of thismolecular component is about 3.4 x 10^4 Msun. The analysis of the moleculardata revealed the presence of a velocity gradient, in agreement with the Halphaline. New radiocontinuum flux density determinations confirm the thermal natureof RCW 78. This indicates that the ionized gas in RCW 78 arises fromphotoionization of the molecular gas component in the velocity range from -58km s-1 to -45 km s-1. A molecular concentration at a velocity of -56.1 km s-1(identified as C1) is very likely associated with the star HD 117797 and with acollection of candidate YSOs, lying at a distance of 3.9 kpc, while the rest ofthe molecular gas at velocities between -56 and -46 km s-1 constitute anincomplete ring-like structure which expands around WR 55 at a velocity ofabout ~ 5 km s-1. Mechanical energy and time requirements indicate that WR 55is very capable of sustaining the expansion of the nebula.

NANTEN 12CO (J=1-0) observations around the star WR 55