ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions – XXI. A large-sample observational study of ethanol and dimethyl ether in hot cores

ABSTRACT Hot cores, as a stage of massive star formation, exhibit abundant line emissions of complex organic molecules (COMs). We present a deep line survey of two isomers of C$_2$H$_6$O: ethanol (C$_2$H$_5$OH; EA), and dimethyl ether (CH$_3$OCH$_3$; DE) as well as their possible precursor CH$_3$OH towards 60 hot cores by using the Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm line observations. EA is detected in 40 hot cores and DE is detected in 59 hot cores. Of these, EA and DE are simultaneously detected in 39 hot cores. We calculate rotation temperatures and column densities of EA and DE by using the eXtended CASA Line Analysis Software Suite (xclass) software. The average rotation temperature of EA is higher than that of DE, whereas the average column density of EA is lower than that of DE. Combined with previous studies of hot cores and hot corinos, we find strong column density correlations among EA and DE ($\rho$ = 0.92), EA and CH$_3$OH ($\rho$ = 0.82), as well as DE and CH$_3$OH ($\rho$ = 0.80). The column density ratios of EA/DE versus the column densities of CH$_3$OH remain nearly constant with values within ~1 order of magnitude. These strong correlations and the stable ratios, suggest that EA, DE, and CH$_3$OH could be chemically linked, with CH$_3$OH potentially serving as a precursor for EA and DE. Compared with chemical models, the three different warm-up time-scale models result in the systematic overproduction of EA and the systematic underproduction of DE. Therefore, our large sample observations can provide crucial constraints on chemical models.

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Journal
Monthly Notices of the Royal Astronomical Society
Published
2025-03-11
DOI
https://doi.org/10.1093/mnras/staf408
Citations
5
Primary Topic
Astrophysics and Star Formation Studies
Type
article
Field-Weighted Citation Impact
5.77
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article

ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions – XXI. A large-sample observational study of ethanol and dimethyl ether in hot cores

Xindi Tang, Patricio Sanhueza, Xunchuan Liu, Emma Mannfors et al.
5 citations
Monthly Notices of the Royal Astronomical Society
Astrophysics and Star Formation Studies
5.77
article

ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions – XXI. A large-sample observational study of ethanol and dimethyl ether in hot cores

Xindi Tang, Patricio Sanhueza, Xunchuan Liu, Emma Mannfors, L. K. Dewangan, Long-Fei Chen, Prasanta Gorai, M. Juvela, Yaping Peng, Xiaohu Li, L. Bronfman, James O. Chibueze, Sheng‐Li Qin, Pablo García, L. Viktor Tóth, Swagat R. Das, Dongting Yang, Li Chen, Hongli Liu, Ziyang Li, J. H. Zou, Guido Garay, Zhiping Kou, Tie Liu
article en
5 citations

Abstract

ABSTRACT Hot cores, as a stage of massive star formation, exhibit abundant line emissions of complex organic molecules (COMs). We present a deep line survey of two isomers of C$_2$H$_6$O: ethanol (C$_2$H$_5$OH; EA), and dimethyl ether (CH$_3$OCH$_3$; DE) as well as their possible precursor CH$_3$OH towards 60 hot cores by using the Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm line observations. EA is detected in 40 hot cores and DE is detected in 59 hot cores. Of these, EA and DE are simultaneously detected in 39 hot cores. We calculate rotation temperatures and column densities of EA and DE by using the eXtended CASA Line Analysis Software Suite (xclass) software. The average rotation temperature of EA is higher than that of DE, whereas the average column density of EA is lower than that of DE. Combined with previous studies of hot cores and hot corinos, we find strong column density correlations among EA and DE ($\rho$ = 0.92), EA and CH$_3$OH ($\rho$ = 0.82), as well as DE and CH$_3$OH ($\rho$ = 0.80). The column density ratios of EA/DE versus the column densities of CH$_3$OH remain nearly constant with values within ~1 order of magnitude. These strong correlations and the stable ratios, suggest that EA, DE, and CH$_3$OH could be chemically linked, with CH$_3$OH potentially serving as a precursor for EA and DE. Compared with chemical models, the three different warm-up time-scale models result in the systematic overproduction of EA and the systematic underproduction of DE. Therefore, our large sample observations can provide crucial constraints on chemical models.

Monthly Notices of the Royal Astronomical SocietyVol. 538(4)
Eötvös Loránd University (HU), Kunming University of Science and Technology (CN), University of Nigeria (NG), Physical Research Laboratory (IN), University of Debrecen (HU), University of Helsinki (FI), Pioneer (United States) (US), Guizhou Normal University (CN), University of South Africa (ZA), University of Oslo (NO), Yunnan University (CN), National Institutes of Natural Sciences (JP), The Graduate University for Advanced Studies, SOKENDAI (JP), North-West University (ZA), Shanghai Astronomical Observatory (CN), Helsinki Institute of Physics (FI), Xinjiang Astronomical Observatory (CN), Universidad Católica del Norte (CL), National Astronomical Observatory of Japan (JP), National Astronomical Observatories (CN), University of Chinese Academy of Sciences (CN), University of Chile (CL)
Openalex Percentile: Top 5%
Astrophysics and Star Formation Studies
5.77
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