NAOC Open IR
Physical and chemical structure of high-mass star-forming regions Unraveling chemical complexity with CORE: the NOEMA large program
Gieser, C.1,2; Beuther, H.2; Semenov, D.2,3; Ahmadi, A.4; Suri, S.2; Moeller, T.5; Beltran, M. T.6; Klaassen, P.7; Zhang, Q.8; Urquhart, J. S.9; Henning, Th.2; Feng, S.10,11,12; Galvan-Madrid, R.13; Magalhaes, V. de Souza14; Moscadelli, L.; Longmore, S.15; Leurini, S.16; Kuiper, R.17; Peters, T.18; Menten, K. M.19; Csengeri, T.20; Fuller, G.21; Wyrowski, F.19; Lumsden, S.22; Sanchez-Monge, A.5; Maud, L.23; Linz, H.2; Palau, A.; Schilke, P.5; Pety, J.24; Pudritz, R.25; Winters, J. M.; Pietu, V.
2021-04-15
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume648Pages:68
AbstractAims. Current star formation research centers the characterization of the physical and chemical properties of massive stars, which are in the process of formation, at the spatial resolution of individual high-mass cores. Methods. We use sub-arcsecond resolution (similar to 0 ''.4) observations with the NOrthern Extended Millimeter Array at 1.37 mm to study the dust emission and molecular gas of 18 high-mass star-forming regions. With distances in the range of 0.7-5.5 kpc, this corresponds to spatial scales down to 300-2300 au that are resolved by our observations. We combined the derived physical and chemical properties of individual cores in these regions to estimate their ages. The temperature structures of these regions are determined by fitting the H2CO and CH3CN line emission. The density profiles are inferred from the 1.37 mm continuum visibilities. The column densities of 11 different species are determined by fitting the emission lines with XCLASS. Results. Within the 18 observed regions, we identified 22 individual cores with associated 1.37 mm continuum emission and with a radially decreasing temperature profile. We find an average temperature power-law index of q = 0.4 +/- 0.1 and an average density power-law index of p = 2.0 +/- 0.2 on scales that are on the order of several 1000 au. Comparing these results with values of p derived from the literature presumes that the density profiles remain unchanged from clump to core scales. The column densities relative to N((CO)-O-18) between pairs of dense gas tracers show tight correlations. We applied the physical-chemical model MUlti Stage ChemicaL codE to the derived column densities of each core and find a mean chemical age of similar to 60 000 yr and an age spread of 20 000-100 000 yr. With this paper, we release all data products of the CORE project. Conclusions. The CORE sample reveals well-constrained density and temperature power-law distributions. Furthermore, we characterized a large variety in molecular richness that can be explained by an age spread that is then confirmed by our physical-chemical modeling. The hot molecular cores show the greatest number of emission lines, but we also find evolved cores at an evolutionary stage in which most molecules are destroyed and, thus, the spectra appear line-poor once again.
Keywordastrochemistry ISM: molecules stars: formation
Funding OrganizationINSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP ; INSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP ; INSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP ; INSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP
DOI10.1051/0004-6361/202039670
WOS KeywordORGANIC-MOLECULES ; DUST CONTINUUM ; CIRCUMSTELLAR ENVIRONMENTS ; PROTOSTELLAR CANDIDATES ; MILLIMETER CONTINUUM ; SELF-CALIBRATION ; EARLY PHASES ; HOT CORES ; FRAGMENTATION ; DISK
Language英语
Funding ProjectINSU/CNRS (France) ; MPG (Germany) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme[CSF-648505] ; Deutsche Forschungsgemeinschaft[SE 1962/6-1] ; UNAM-PAPIIT[IN113119] ; UNAM-PAPIIT[IN104319] ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG)[KU 2849/3-1] ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG)[KU 2849/3-2] ; Deutsche Forschungsgemeinschaft (DFG)[184018 867] ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CEA ; INC/INP ; [L14AB]
Funding OrganizationINSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP ; INSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP ; INSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP ; INSU/CNRS (France) ; INSU/CNRS (France) ; MPG (Germany) ; MPG (Germany) ; IGN (Spain) ; IGN (Spain) ; European Research Council under the Horizon 2020 Framework Programme ; European Research Council under the Horizon 2020 Framework Programme ; Deutsche Forschungsgemeinschaft ; Deutsche Forschungsgemeinschaft ; UNAM-PAPIIT ; UNAM-PAPIIT ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Emmy Noether Research Group on Accretion Flows and Feedback in Realistic Models of Massive Star Formation - German Research Foundation (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; Deutsche Forschungsgemeinschaft (DFG) ; CONACyT ; CONACyT ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; Programme National "Physique et Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU ; CNES ; CNES ; CEA ; CEA ; INC/INP ; INC/INP
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000647068900001
PublisherEDP SCIENCES S A
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/77990
Collection中国科学院国家天文台
Corresponding AuthorGieser, C.
Affiliation1.Univ Heidelberg IMPRS HD, Int Max Planck Res Sch Astron & Cosm Phys, Heidelberg, Germany
2.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
3.Ludwig Maximilians Univ Munchen, Dept Chem, Butenandtstr 5-13, D-81377 Munich, Germany
4.Leiden Univ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands
5.Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany
6.INAF, Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy
7.Royal Observ Edinburgh, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland
8.Harvard Smithsonian, Astrophys, 60 Garden St, Cambridge, MA 02138 USA
9.Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England
10.Acad Sinica, Inst Astron & Astrophys, Sec 4,Roosevelt Rd, Taipei 10617, Taiwan
11.Chinese Acad Sci, CAS Key Lab FAST, Natl Astron Observ, Beijing 100101, Peoples R China
12.Natl Astron Observ Japan, Natl Inst Nat Sci, 21-1 Osawa, Mitaka, Tokyo 1818588, Japan
13.UNAM, Inst Radioastron Astrofis IRyA, Apdo Postal 72-3 Xangari, Morelia, Michoacan 58089, Mexico
14.Inst Radioastron Millimetr IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France
15.Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England
16.INAF, Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy
17.Univ Tubingen, Inst Astron & Astrophys, Morgenstelle 10, D-72076 Tubingen, Germany
18.Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany
19.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
20.Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, B18N,Allee Geoffroy St Hilaire, F-33615 Pessac, France
21.Univ Manchester, Dept Phys, POB 88, Manchester M60 1QD, Lancs, England
22.Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
23.European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany
24.PSL Res Univ, Observ Paris, Sorbonne Univ, CNRS, F-75014 Paris, France
25.McMaster Univ, Dept Phys & Astron, 1280 Main St W, Hamilton, ON L8S 4M1, Canada
Recommended Citation
GB/T 7714
Gieser, C.,Beuther, H.,Semenov, D.,et al. Physical and chemical structure of high-mass star-forming regions Unraveling chemical complexity with CORE: the NOEMA large program[J]. ASTRONOMY & ASTROPHYSICS,2021,648:68.
APA Gieser, C..,Beuther, H..,Semenov, D..,Ahmadi, A..,Suri, S..,...&Pietu, V..(2021).Physical and chemical structure of high-mass star-forming regions Unraveling chemical complexity with CORE: the NOEMA large program.ASTRONOMY & ASTROPHYSICS,648,68.
MLA Gieser, C.,et al."Physical and chemical structure of high-mass star-forming regions Unraveling chemical complexity with CORE: the NOEMA large program".ASTRONOMY & ASTROPHYSICS 648(2021):68.
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