Search: id:"swepub:oai:research.chalmers.se:3697e367-a183-42e6-bde7-717e0a95259f" >
Astrochemical Diagn...
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Gorai, Prasanta,1991Gothenburg University,Göteborgs universitet,Institutionen för kemi och molekylärbiologi,Department of Chemistry and Molecular Biology
(author)
Astrochemical Diagnostics of the Isolated Massive Protostar G28.20-0.05
- Article/chapterEnglish2024
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2024
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LIBRIS-ID:oai:research.chalmers.se:3697e367-a183-42e6-bde7-717e0a95259f
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https://research.chalmers.se/publication/539469URI
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https://doi.org/10.3847/1538-4357/ad09bbDOI
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https://gup.ub.gu.se/publication/334546URI
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Language:English
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Summary in:English
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We study the astrochemical diagnostics of the isolated massive protostar G28.20-0.05. We analyze data from Atacama Large Millimeter/submillimeter Array 1.3 mm observations with a resolution of 0.″2 (∼1000 au). We detect emission from a wealth of species, including oxygen-bearing (e.g., H2CO, CH3OH, CH3OCH3), sulfur-bearing (SO2, H2S), and nitrogen-bearing (e.g., HNCO, NH2CHO, C2H3CN, C2H5CN) molecules. We discuss their spatial distributions, physical conditions, correlation between different species, and possible chemical origins. In the central region near the protostar, we identify three hot molecular cores (HMCs). HMC1 is part of a millimeter continuum ring-like structure, is closest in projection to the protostar, has the highest temperature of ∼300 K, and shows the most line-rich spectra. HMC2 is on the other side of the ring, has a temperature of ∼250 K, and is of intermediate chemical complexity. HMC3 is further away, ∼3000 au in projection, cooler (∼70 K), and is the least line-rich. The three HMCs have similar mass surface densities (∼10 g cm−2), number densities (n H ∼ 109 cm−3), and masses of a few solar masses. The total gas mass in the cores and in the region out to 3000 au is ∼25 M ⊙, which is comparable to that of the central protostar. Based on spatial distributions of peak line intensities as a function of excitation energy, we infer that the HMCs are externally heated by the protostar. We estimate column densities and abundances of the detected species and discuss the implications for hot core astrochemistry.
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Law, Chi Yan,1990Chalmers tekniska högskola,Chalmers University of Technology,European Southern Observatory (ESO)(Swepub:cth)ychi
(author)
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Tan, Jonathan,1973Chalmers tekniska högskola,Chalmers University of Technology,University of Virginia(Swepub:cth)tanj
(author)
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Zhang, YichenShanghai Jiao Tong University,University of Virginia
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Fedriani, Rubén,1991Chalmers tekniska högskola,Chalmers University of Technology,Instituto de Astrofisica de Andalucía (IAA),Institute of Astrophysics of Andalusia (IAA)(Swepub:cth)fedriani
(author)
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Tanaka, Kei E.I.Tokyo Institute of Technology
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Bonfand, MélisseUniversity of Virginia
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Cosentino, Giuliana,1990Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)giuliana
(author)
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Mardones, DiegoUniversidad de Chile (UCH),University of Chile (UCH)
(author)
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Beltrán, Maria T.Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory
(author)
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Garay, G.Universidad de Chile (UCH),University of Chile (UCH)
(author)
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Göteborgs universitetInstitutionen för kemi och molekylärbiologi
(creator_code:org_t)
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In:Astrophysical Journal960:21538-43570004-637X
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