Chemical Evolution of HC3N in Dense Molecular Clouds
arXiv:1910.07222 · doi:10.1093/mnras/stz2431
Abstract
We investigated the chemical evolution of HC3N in six dense molecular clouds, using archival available data from the Herschel infrared Galactic Plane Survey (Hi-GAL) and the Millimeter Astronomy Legacy Team Survey at 90 GHz (MALT90). Radio sky surveys of the Multi-Array Galactic Plane Imaging Survey (MAGPIS) and the Sydney University Molonglo Sky Survey (SUMSS) indicate these dense molecular clouds are associated with ultracompact HII (UCHII) regions and/or classical HII regions. We find that in dense molecular clouds associated with normal classical HII regions, the abundance of HC3N begins to decrease or reaches a plateau when the dust temperature gets hot. This implies UV photons could destroy the molecule of HC3N. On the other hand, in the other dense molecular clouds associated with UCHII regions, we find the abundance of HC3N increases with dust temperature monotonously, implying HC3N prefers to be formed in warm gas. We also find that the spectra of HC3N (10-9) in G12.804-0.199 and RCW 97 show wing emissions, and the abundance of HC3N in these two regions increases with its nonthermal velocity width, indicating HC3N might be a shock origin species. We further investigated the evolutionary trend of N(N2H+)/N(HC3N) column density ratio, and found this ratio could be used as a chemical evolutionary indicator of cloud evolution after the massive star formation is started.
References in corpus (29)
- Toward Understanding Massive Star Formation
- A Catalog of Extended Green Objects (EGOs) in the GLIMPSE Survey: A new sample of massive young stellar object outflow candidates
- ATLASGAL - Compact source catalogue: 330 < l < 21 degrees
- Chemistry in Infrared Dark Cloud Clumps: a Molecular Line Survey at 3 mm
- MALT90: The Millimetre Astronomy Legacy Team 90 GHz Survey
- Large-scale filaments associated with Milky Way spiral arms
- The Millimeter Astronomy Legacy Team 90 GHz (MALT90) Pilot Survey
- The data reduction pipeline for the Hi-GAL survey
- Modeling the Lukewarm Corino Phase - is L1527 unique?
- Trigonometric Parallaxes of Star Forming Regions in the Scutum Spiral Arm
- A Search for Carbon-Chain-Rich Cores in Dark Clouds
- Very compact radio emission from high-mass protostars. II. Dust disks and ionized accretion flows
- Trigonometric Parallaxes of Massive Star Forming Regions: G012.88+0.48 and W33
- MSX Mid infrared imaging of massive star birth environments. II: Giant HII regions
- Characterization of the MALT90 Survey and the Mopra Telescope at 90 GHz
- Diversity of chemistry and excitation conditions in the high-mass star forming complex W33
- Chemical modeling of water deuteration in IRAS16293-2422
- Survey Observations to Study Chemical Evolution from High-mass Starless Cores to High-mass Protostellar Objects I: HC3N and HC5N
- 13C Isotopic Fractionation of HC3N in Star-Forming Regions -Low-Mass Star Forming Region L1527 and High-Mass Star Forming Region G28.28-0.36-
- ATLASGAL --- Molecular fingerprints of a sample of massive star forming clumps
- Revealing the environs of the remarkable southern hot core G327.3-0.6
- A molecular line study towards massive extended green object clumps in the southern sky: chemical properties
- A search for Cyanopolyynes in L1157-B1
- Chemical evolution of Red MSX Sources in the southern sky
- G5.89: An Explosive Outflow Powered by a Proto-Stellar Merger?
- Chemical evolution of the HC3N and N2H+ molecules in dense cores of the Vela C giant molecular cloud complex
- Chemical evolution of N2H+ in six massive star-forming regions
- Investigating inner and large scale physical environments of IRAS 17008-4040 and IRAS 17009-4042 toward l = 345.5 deg, b = 0.3 deg
- Distribution of water in the G327.3-0.6 massive star-forming region