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We have carried out an extensive multi-wavelength study to investigate thestar formation process in the S235 complex. The S235 complex has a sphere-likeshell appearance at wavelengths longer than 2 $\mu$m and harbors an O9.5V typestar approximately at its center. Near-infrared extinction map traces eightsubregions (having A$_{V}$ $>$ 8 mag), and five of them appear to bedistributed in an almost regularly spaced manner along the sphere-like shellsurrounding the ionized emission. This picture is also supported by theintegrated $^{12}$CO and $^{13}$CO intensity maps and by Bolocam 1.1 mmcontinuum emission. The position-velocity analysis of CO reveals an almostsemi-ring like structure, suggesting an expanding H\,{\sc ii} region. We findthat the Bolocam clump masses increase as we move away from the location of theionizing star. This correlation is seen only for those clumps which aredistributed near the edges of the shell. Photometric analysis reveals 435 youngstellar objects (YSOs), 59\% of which are found in clusters. Six subregions(including five located near the edges of the shell) are very well correlatedwith the dust clumps, CO gas, and YSOs. The average values of Mach numbersderived using NH$_{3}$ data for three (East~1, East~2, and Central~E) out ofthese six subregions are 2.9, 2.3, and 2.9, indicating these subregions aresupersonic. The molecular outflows are detected in these three subregions,further confirming the on-going star formation activity. Together, all theseresults are interpreted as observational evidence of positive feedback of amassive star.

A multi-wavelength study of star formation activity in the S235 complex