Extended HNCO, SiO, and HC3N Emission in 43 Southern Star-forming Regions
He,Yu-Xin1,2,3,4; Henkel,Christian1,5,6; Zhou,Jian-Jun1,2; Esimbek,Jarken1,2; Stutz,Amelia M.4,7; Liu,Hong-Li4,8; Ji,Wei-Guang1,2; Li,Da-Lei1,2; Wu,Gang1,2; Tang,Xin-Di1,2; Komesh,Toktarkhan1,9,10; Sailanbek,Serikbek1,9,10
Source PublicationThe Astrophysical Journal Supplement Series
AbstractAbstract We have selected 43 southern massive star-forming regions to study the spatial distribution of HNCO 404–303, SiO 2–1, and HC3N 10–9 line emission and to investigate their spatial association with the dust emission. The morphology of HNCO 404–303 and HC3N 10–9 agrees well with the dust emission. HC3N 10–9 tends to originate from more compact regions than HNCO 404–303 and SiO 2–1. We divided our sources into three groups: those in the Central Molecular Zone (CMZ), those associated with bubbles (Bubble), and the remaining sources, which are termed “normal star-forming regions” (NMSFR). These three groups, subdivided into three different categories with respect to line widths, integrated intensities, and column densities, hint at the presence of different physical and chemical processes. We find that the dust temperature Td, and the abundance ratios NHNCO/NSiO and NHNCO/NHC3N show a decreasing trend toward the central dense regions of CMZ sources, while NHC3N/NSiO moves in the opposite direction. Moreover, a better agreement is found between Td and NHC3N/NSiO in Bubble and NMSFR category sources. Both outflow and inflow activities have been found in eight of the 16 bubble and NMSFR sources. The low outflow detection rate indicates either that in these sources the SiO 2–1 line wing emission is below our sensitivity limit or that the bulk of the SiO emission may be produced by the expansion of an H ii region or supernova remnant, which has pushed molecular gas away, forming a shock and yielding SiO.
KeywordAstrochemistry Molecular clouds Star formation Radio astronomy Millimeter astronomy
WOS IDIOP:0067-0049-253-1-abd0fb
PublisherThe American Astronomical Society
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Document Type期刊论文
Corresponding AuthorHe,Yu-Xin
Affiliation1.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, People’s Republic of China
2.Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi 830011, People’s Republic of China
3.Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100012, People’s Republic of China
4.Departmento de Astronomía, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción, Concepción, Chile
5.Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
6.Astron. Dept., King Abdulaziz University, P.O. Box 80203, 21589 Jeddah, Saudi Arabia
7.Max-Planck-Institute for Astronomy, K?nigstuhl 17, D-69117 Heidelberg, Germany
8.Department of Astronomy, Yunnan University, Kunming, 650091, People’s Republic of China
9.Department of Solid State Physics and Nonlinear Physics, Faculty of Physics and Technology, Al-Farabi Kazakh National University, Almaty, 050040, Kazakhstan
10.University of the Chinese Academy of Sciences, Beijing 100080, People’s Republic of China
Recommended Citation
GB/T 7714
He,Yu-Xin,Henkel,Christian,Zhou,Jian-Jun,et al. Extended HNCO, SiO, and HC3N Emission in 43 Southern Star-forming Regions[J]. The Astrophysical Journal Supplement Series,2021,253(1).
APA He,Yu-Xin.,Henkel,Christian.,Zhou,Jian-Jun.,Esimbek,Jarken.,Stutz,Amelia M..,...&Sailanbek,Serikbek.(2021).Extended HNCO, SiO, and HC3N Emission in 43 Southern Star-forming Regions.The Astrophysical Journal Supplement Series,253(1).
MLA He,Yu-Xin,et al."Extended HNCO, SiO, and HC3N Emission in 43 Southern Star-forming Regions".The Astrophysical Journal Supplement Series 253.1(2021).
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