2021PASJ...73S.338K

We have performed a multi-wavelength study of the mid-infrared bubble S44 to investigate the origin of isolated high-mass star(s) and the star-formation process around the bubble formed by the H II region. We report on the results of new CO observations (12CO, 13CO J = 1-0, and 12CO J = 3-2) toward the isolated bubble S44 using the NANTEN2, Mopra, and ASTE radio telescopes. We found two velocity components at -84 km s-1 and -79 km s-1 in the direction of the bubble. These two clouds are likely to be physically associated with the bubble, because of the enhanced 12CO J = 3-2/1-0 intensity ratio from a ring-like structure affected by ultraviolet radiation from embedded high-mass star(s) and of the morphological correspondence between the 8 μm emission and the CO distribution. Assuming a single object, we estimate a spectral type of the embedded star inside the bubble to be O8.5-9 (∼20M⊙) from the radio-continuum free-free emission. We hypothesize that the two clouds collided with each other 3 Myr ago, triggering the formation of the isolated high-mass star in S44, as also occurred in RCW 120 and RCW 79. We argue that this scenario can explain the origin of the isolated O-star inside the bubble.