摘要
The low dust temperatures (<14 K) of Planck Galactic cold clumps (PGCCs) make them ideal targets to probe the initial conditions and very early phase of star formation. "TOP-SCOPE" is a joint survey program targeting ∼2000 PGCCs in J = 1-0 transitions of CO isotopologues and ∼1000 PGCCs in 850 μm continuum emission. The objective of the "TOP-SCOPE" survey and the joint surveys (SMT 10 m, KVN 21 m, and NRO 45 m) is to statistically study the initial conditions occurring during star formation and the evolution of molecular clouds, across a wide range of environments. The observations, data analysis, and example science cases for these surveys are introduced with an exemplar source, PGCC G26.53+0.17 (G26), which is a filamentary infrared dark cloud (IRDC). The total mass, length, and mean line mass (M/L) of the G26 filament are ∼6200 M, ∼12 pc, and ∼500 Mpc-1, respectively. Ten massive clumps, including eight starless ones, are found along the filament. The most massive clump as a whole may still be in global collapse, while its denser part seems to be undergoing expansion owing to outflow feedback. The fragmentation in the G26 filament from cloud scale to clump scale is in agreement with gravitational fragmentation of an isothermal, nonmagnetized, and turbulent supported cylinder. A bimodal behavior in dust emissivity spectral index (β) distribution is found in G26, suggesting grain growth along the filament. The G26 filament may be formed owing to large-scale compression flows evidenced by the temperature and velocity gradients across its natal cloud.
原文 | 英語 |
---|---|
文章編號 | 28 |
期刊 | Astrophysical Journal, Supplement Series |
卷 | 234 |
發行號 | 2 |
DOIs | |
出版狀態 | 已發佈 - 2018 2月 |
ASJC Scopus subject areas
- 天文和天體物理學
- 空間與行星科學
指紋
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於: Astrophysical Journal, Supplement Series, 卷 234, 編號 2, 28, 02.2018.
研究成果: 雜誌貢獻 › 期刊論文 › 同行評審
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TY - JOUR
T1 - The TOP-SCOPE Survey of Planck Galactic Cold Clumps
T2 - Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17
AU - Liu, Tie
AU - Kim, Kee Tae
AU - Juvela, Mika
AU - Wang, Ke
AU - Tatematsu, Ken'Ichi
AU - Francesco, James Di
AU - Liu, Sheng Yuan
AU - Wu, Yuefang
AU - Thompson, Mark
AU - Fuller, Gary
AU - Eden, David
AU - Li, Di
AU - Ristorcelli, I.
AU - Kang, Sung Ju
AU - Lin, Yuxin
AU - Johnstone, D.
AU - He, J. H.
AU - Koch, P. M.
AU - Sanhueza, Patricio
AU - Qin, Sheng Li
AU - Zhang, Q.
AU - Hirano, N.
AU - Goldsmith, Paul F.
AU - Evans, Neal J.
AU - White, Glenn J.
AU - Choi, Minho
AU - Lee, Chang Won
AU - Toth, L. V.
AU - Mairs, Steve
AU - Yi, H. W.
AU - Tang, Mengyao
AU - Soam, Archana
AU - Peretto, N.
AU - Samal, Manash R.
AU - Fich, Michel
AU - Parsons, Harriet
AU - Yuan, Jinghua
AU - Zhang, Chuan Peng
AU - Malinen, Johanna
AU - Bendo, George J.
AU - Rivera-Ingraham, A.
AU - Liu, Hong Li
AU - Wouterloot, Jan
AU - Li, Pak Shing
AU - Qian, Lei
AU - Rawlings, Jonathan
AU - Rawlings, Mark G.
AU - Feng, Siyi
AU - Aikawa, Yuri
AU - Akhter, S.
AU - Alina, Dana
AU - Bell, Graham
AU - Bernard, J. P.
AU - Blain, Andrew
AU - Bogner, Rebeka
AU - Bronfman, L.
AU - Byun, D. Y.
AU - Chapman, Scott
AU - Chen, Huei Ru
AU - Chen, M.
AU - Chen, Wen Ping
AU - Chen, X.
AU - Chen, Xuepeng
AU - Chrysostomou, A.
AU - Cosentino, Giuliana
AU - Cunningham, M. R.
AU - Demyk, K.
AU - Drabek-Maunder, Emily
AU - Doi, Yasuo
AU - Eswaraiah, C.
AU - Falgarone, Edith
AU - Fehér, O.
AU - Fraser, Helen
AU - Friberg, Per
AU - Garay, G.
AU - Ge, J. X.
AU - Gear, W. K.
AU - Greaves, Jane
AU - Guan, X.
AU - Harvey-Smith, Lisa
AU - Hasegawa, Tetsuo
AU - Hatchell, J.
AU - He, Yuxin
AU - Henkel, C.
AU - Hirota, T.
AU - Holland, W.
AU - Hughes, A.
AU - Jarken, E.
AU - Ji, Tae Geun
AU - Jimenez-Serra, Izaskun
AU - Kang, Miju
AU - Kawabata, Koji S.
AU - Kim, Gwanjeong
AU - Kim, Jungha
AU - Kim, Jongsoo
AU - Kim, Shinyoung
AU - Koo, B. C.
AU - Kwon, Woojin
AU - Kuan, Yi Jehng
AU - Lacaille, K. M.
AU - Lai, Shih Ping
AU - Lee, C. F.
AU - Lee, J. E.
AU - Lee, Y. U.
AU - Li, Dalei
AU - Li, Hua Bai
AU - Lo, N.
AU - Lopez, John A.P.
AU - Lu, Xing
AU - Lyo, A. Ran
AU - Mardones, D.
AU - Marston, A.
AU - McGehee, P.
AU - Meng, F.
AU - Montier, L.
AU - Montillaud, Julien
AU - Moore, T.
AU - Morata, O.
AU - Moriarty-Schieven, Gerald H.
AU - Ohashi, S.
AU - Pak, Soojong
AU - Park, Geumsook
AU - Paladini, R.
AU - Pattle, Kate M.
AU - Pech, Gerardo
AU - Pelkonen, V. M.
AU - Qiu, K.
AU - Ren, Zhi Yuan
AU - Richer, John
AU - Saito, M.
AU - Sakai, Takeshi
AU - Shang, H.
AU - Shinnaga, Hiroko
AU - Stamatellos, Dimitris
AU - Tang, Y. W.
AU - Traficante, Alessio
AU - Vastel, Charlotte
AU - Viti, S.
AU - Walsh, Andrew
AU - Wang, Bingru
AU - Wang, Hongchi
AU - Wang, Junzhi
AU - Ward-Thompson, D.
AU - Whitworth, Anthony
AU - Xu, Ye
AU - Yang, J.
AU - Yang, Yao Lun
AU - Yuan, Lixia
AU - Zavagno, A.
AU - Zhang, Guoyin
AU - Zhang, H. W.
AU - Zhou, Chenlin
AU - Zhou, Jianjun
AU - Zhu, Lei
AU - Zuo, Pei
AU - Zhang, Chao
N1 - Funding Information: L. was supported by the Basic Science Research Program though the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science, and Technology (NRF-2016R1A2B4012593). Miju Kang was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science, ICT, and Future Planning (no. NRF-2015R1C1A1A01052160). The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of the National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China, and the Chinese Academy of Sciences (grant no. XDB09000000) Funding Information: Tie Liu is supported by the KASI fellowship and EACOA fellowship. Ke Wang is supported by grant WA3628-1/1 of the German Research Foundation (DFG) through the priority program 1573 (“Physics of the Interstellar Medium”). S.-.L.Q. is supported by the Joint Research Fund in Astronomy (U1631237) under cooperative agreement between the National Natural Science Foundation of China (NSFC) and Chinese Academy of Sciences (CAS), by the Top Talents Program of Yunnan Province (2015HA030). M.J. and V.-M.P. acknowledge the support of the Academy of Finland grant no. 285769. J.Ma. acknowledges the support of ERC-2015-STG No. 679852 RADFEEDBACK. C.W. L. was supported by the Basic Science Research Program though the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science, and Technology (NRF-2016R1A2B4012593). Miju Kang was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science, ICT, and Future Planning (no. NRF-2015R1C1A1A01052160). The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of the National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China, and the Chinese Academy of Sciences (grant no. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. The data presented in this paper are based on the ESO-ARO program ID 196.C-0999(A). D.M., G.G., and L.B. acknowledge support from CONICYT Project PFB-06. S.P.L. acknowledges support from the Ministry of Science and Technology of Taiwan with grants MOST 105-2119-M-007-024 and MOST 106-2119-M-007-021-MY3. J.E.L. was supported by the Basic Science Research Program through the National Research Foundation of Korea (grant No. NRF-2015R1A2A2A01004769) and the Korea Astronomy and Space Science Institute under the R&D program supervised by the Ministry of Science, ICT and Future Planning. V.-M.P. acknowledges the financial support from the European Research Council, Advanced grant No. 320773 SAEMPL. D.L. is part of the CAS Interdisciplinary Innovation Team team. Publisher Copyright: © 2018. The American Astronomical Society. All rights reserved..
PY - 2018/2
Y1 - 2018/2
N2 - The low dust temperatures (<14 K) of Planck Galactic cold clumps (PGCCs) make them ideal targets to probe the initial conditions and very early phase of star formation. "TOP-SCOPE" is a joint survey program targeting ∼2000 PGCCs in J = 1-0 transitions of CO isotopologues and ∼1000 PGCCs in 850 μm continuum emission. The objective of the "TOP-SCOPE" survey and the joint surveys (SMT 10 m, KVN 21 m, and NRO 45 m) is to statistically study the initial conditions occurring during star formation and the evolution of molecular clouds, across a wide range of environments. The observations, data analysis, and example science cases for these surveys are introduced with an exemplar source, PGCC G26.53+0.17 (G26), which is a filamentary infrared dark cloud (IRDC). The total mass, length, and mean line mass (M/L) of the G26 filament are ∼6200 M, ∼12 pc, and ∼500 Mpc-1, respectively. Ten massive clumps, including eight starless ones, are found along the filament. The most massive clump as a whole may still be in global collapse, while its denser part seems to be undergoing expansion owing to outflow feedback. The fragmentation in the G26 filament from cloud scale to clump scale is in agreement with gravitational fragmentation of an isothermal, nonmagnetized, and turbulent supported cylinder. A bimodal behavior in dust emissivity spectral index (β) distribution is found in G26, suggesting grain growth along the filament. The G26 filament may be formed owing to large-scale compression flows evidenced by the temperature and velocity gradients across its natal cloud.
AB - The low dust temperatures (<14 K) of Planck Galactic cold clumps (PGCCs) make them ideal targets to probe the initial conditions and very early phase of star formation. "TOP-SCOPE" is a joint survey program targeting ∼2000 PGCCs in J = 1-0 transitions of CO isotopologues and ∼1000 PGCCs in 850 μm continuum emission. The objective of the "TOP-SCOPE" survey and the joint surveys (SMT 10 m, KVN 21 m, and NRO 45 m) is to statistically study the initial conditions occurring during star formation and the evolution of molecular clouds, across a wide range of environments. The observations, data analysis, and example science cases for these surveys are introduced with an exemplar source, PGCC G26.53+0.17 (G26), which is a filamentary infrared dark cloud (IRDC). The total mass, length, and mean line mass (M/L) of the G26 filament are ∼6200 M, ∼12 pc, and ∼500 Mpc-1, respectively. Ten massive clumps, including eight starless ones, are found along the filament. The most massive clump as a whole may still be in global collapse, while its denser part seems to be undergoing expansion owing to outflow feedback. The fragmentation in the G26 filament from cloud scale to clump scale is in agreement with gravitational fragmentation of an isothermal, nonmagnetized, and turbulent supported cylinder. A bimodal behavior in dust emissivity spectral index (β) distribution is found in G26, suggesting grain growth along the filament. The G26 filament may be formed owing to large-scale compression flows evidenced by the temperature and velocity gradients across its natal cloud.
KW - ISM: abundances
KW - ISM: clouds
KW - ISM: kinematics and dynamics
KW - stars: formation
KW - surveys
UR - http://www.scopus.com/inward/record.url?scp=85042529579&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85042529579&partnerID=8YFLogxK
U2 - 10.3847/1538-4365/aaa3dd
DO - 10.3847/1538-4365/aaa3dd
M3 - Article
AN - SCOPUS:85042529579
SN - 0067-0049
VL - 234
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
M1 - 28
ER -