HI Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament

Abstract

Using the HI self-absorption data from the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we perform a study of the cold atomic gas in the Cygnus-X North region. The most remarkable HI cloud is characterized by a filamentary structure, associated in space and in velocity with the principle molecular filament in the Cygnus-X North region. We investigate the transition from the atomic filament to the molecular filament. We find that the HII regions Cygnus OB2 and G081.920+00.138 play a critical role in compressing and shaping the atomic Cygnus-X North filament, where the molecular filament subsequently forms. The cold HI in the DR21 filament has a much larger column density (N(HI) $\sim$ 1 $\times$ 10${}^{20}$ cm${}^{-2}$) than the theoretical value of the residual atomic gas ($\sim$ 1 $\times$ 10${}^{19}$ cm${}^{-2}$), suggesting that the HI-to-H${}_2$ transition is still in progress. The timescale of the HI-to-H${}_2$ transition is estimated to be 3 $\times$ 10${}^5$ yr, which approximates the ages of massive protostars in the Cygnus-X North region. This implies that the formation of molecular clouds and massive stars may occur almost simultaneously in the DR21 filament, in accord with a picture of rapid and dynamic cloud evolution.

arXiv comment10 pages, 7 figures

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