2016A&A...587A..74S

The probability distribution function of column density (N-PDF) serves as a powerful tool to characterise the various physical processes that influence the structure of molecular clouds. Studies that use extinction maps or H₂ column-density maps (N) that are derived from dust show that star-forming clouds can best be characterised by lognormal PDFs for the lower N range and a power-law tail for higher N, which is commonly attributed to turbulence and self-gravity and/or pressure, respectively. While PDFs from dust cover a large dynamic range (typically N∼10^20–24cm^–2 or A_v∼0.1-1000), PDFs obtained from molecular lines - converted into H₂ column density - potentially trace more selectively different regimes of (column) densities and temperatures. They also enable us to distinguish different clouds along the line of sight through using the velocity information. We report here on PDFs that were obtained from observations of ¹²CO, ¹³CO, C¹⁸O, CS, and N₂H⁺ in the Cygnus X North region, and make a comparison to a PDF that was derived from dust observations with the Herschel satellite. The PDF of ¹²CO is lognormal for A_v∼1-30, but is cut for higher A_v because of optical depth effects. The PDFs of C¹⁸O and ¹³CO are mostly lognormal up to A_v∼1-15, followed by excess up to A_v∼40. Above that value, all CO PDFs drop, which is most likely due to depletion. The high density tracers CS and N₂H⁺ exhibit only a power law distribution between A_v∼15 and 400, respectively. The PDF from dust is lognormal for A_v∼3-15 and has a power-law tail up to A_v∼500. Absolute values for the molecular line column densities are, however, rather uncertain because of abundance and excitation temperature variations. If we take the dust PDF at face value, we ``calibrate'' the molecular line PDF of CS to that of the dust and determine an abundance [CS]/[H₂] of 10^–9. The slopes of the power-law tails of the CS, N₂H⁺, and dust PDFs are -1.6, -1.4, and -2.3, respectively, and are thus consistent with free-fall collapse of filaments and clumps. A quasi static configuration of filaments and clumps can also possibly account for the observed N-PDFs, providing they have a sufficiently condensed density structure and external ram pressure by gas accretion is provided. The somehow flatter slopes of N₂H⁺ and CS can reflect an abundance change and/or subthermal excitation at low column densities.