1998AJ....115.2009Y

We have carried out ¹²CO, ¹³CO, and C¹⁸O (J = 1-0) observations toward IRAS 22103+5828 in the H II region S134 with the 4 m telescope at Nagoya University and the 45 m telescope at Nobeyama Radio Observatory. We find a molecular cloud and a dense core around the IRAS point source. The molecular cloud is elongated, consisting of a dense ``head'' and a diffuse extended ``tail,'' with the head pointing toward the star exciting the H II region, λ Cep. The cloud shows a velocity gradient of ∼0.2 km.s^–1.pc^–1 along the major axis. A molecular outflow has been discovered at the position of the IRAS point source. The combination of (1) the head-tail structure and the velocity gradient of the molecular cloud, (2) the presence of the dense core and the molecular outflow, and (3) the high ratio of the IRAS luminosity to the cloud mass strongly implies that IRAS 22103+5828 formed in the cloud associated with S134. The possibility is suggested that the rocket effect may be the major mechanism causing the observed velocity gradient of the quiescent molecular cloud.