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The [CII] 158 {\\mu}m far-infrared (FIR) fine-structure line is one of the most important cooling lines of the star-forming interstellar medium (ISM). High spectral resolution observations have shown complex structures in the line profiles of the [CII] emission. Aims. Our aim is to determine whether the complex profiles observed in [^{12}CII] are due to individual velocity components along the line-of-sight or to self-absorption based on a comparison of the [^{12}CII] and isotopic [^{13}CII] line profiles. Methods. Deep integrations with the SOFIA/upGREAT 7-pixel array receiver in M43,","authors_text":"C. Guevara, H. Beuther, J. P. P\\'erez-Beaupuits, J. Stutzki, R. G\\\"usten, R. Higgins, R. Simon, S. Bihr, U. Graf, V. 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