The ALMA-ATOMS survey: Vibrationally excited HC${}_3$N lines in hot cores

Abstract

Interstellar molecules are excellent tools for studying the physical and chemical environments of massive star-forming regions. In particular, vibrationally excited HC${}_3$N (HC${}_3$N*) lines are the key tracers for probing hot cores environments. We present the Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm observations of HC${}_3$N* lines in 60 hot cores, aiming to investigate how physical conditions affect the excitation of HC${}_3$N* transitions. We have used the XCLASS for line identification. Under the assumption of local thermodynamic equilibrium (LTE), we derived the rotation temperature and column density of HC${}_3$N* transitions in hot cores. Additionally, we calculated the H${}_2$ column density and number density, along with the abundance of HC${}_3$N* relative to H${}_2$, to enable a comparison of the physical properties of hot cores with different numbers of HC${}_3$N* states. We have detected HC${}_3$N* lines in 52 hot cores, in which 29 cores showing more than one vibrationally excited state. Hot cores with higher gas temperatures have more detections of these vibrationally excited lines. The excitation of HC${}_3$N* requires dense environments, with its spatial distribution influenced by the presence of UC Hii regions. The observed column density of HC${}_3$N* contributes to the number of HC${}_3$N* states in hot core environments. After analyzing the various factors influencing HC${}_3$N* excitation in hot cores, we conclude that the excitation of HC${}_3$N* is mainly driven by mid-IR pumping, while collisional excitation is ineffective.

arXiv comment14 pages, 9 figures

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