The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17

Tie Liu; Kee Tae Kim; Mika Juvela; Ke Wang; Ken'Ichi Tatematsu; James Di Francesco; Sheng Yuan Liu; Yuefang Wu; Mark Thompson; Gary Fuller; David Eden; Di Li; I. Ristorcelli; Sung Ju Kang; Yuxin Lin; D. Johnstone; J. H. He; P. M. Koch; Patricio Sanhueza; Sheng Li Qin; Q. Zhang; N. Hirano; Paul F. Goldsmith; Neal J. Evans; Glenn J. White; Minho Choi; Chang Won Lee; L. V. Toth; Steve Mairs; H. W. Yi; Mengyao Tang; Archana Soam; N. Peretto; Manash R. Samal; Michel Fich; Harriet Parsons; Jinghua Yuan; Chuan Peng Zhang; Johanna Malinen; George J. Bendo; A. Rivera-Ingraham; Hong Li Liu; Jan Wouterloot; Pak Shing Li; Lei Qian; Jonathan Rawlings; Mark G. Rawlings; Siyi Feng; Dana Alina; J. E. Lee

doi:10.3847/1538-4365/aaa3dd

The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17

Tie Liu
, Kee Tae Kim
, Mika Juvela
, Ke Wang
, Ken'Ichi Tatematsu
, James Di Francesco
, Sheng Yuan Liu
, Yuefang Wu
, Mark Thompson
, Gary Fuller
, David Eden
, Di Li
, I. Ristorcelli
, Sung Ju Kang
, Yuxin Lin
, D. Johnstone
, J. H. He
, P. M. Koch
, Patricio Sanhueza
, Sheng Li Qin

Q. Zhang, N. Hirano, Paul F. Goldsmith, Neal J. Evans, Glenn J. White, Minho Choi, Chang Won Lee, L. V. Toth, Steve Mairs, H. W. Yi, Mengyao Tang, Archana Soam, N. Peretto, Manash R. Samal, Michel Fich, Harriet Parsons, Jinghua Yuan, Chuan Peng Zhang, Johanna Malinen, George J. Bendo, A. Rivera-Ingraham, Hong Li Liu, Jan Wouterloot, Pak Shing Li, Lei Qian, Jonathan Rawlings, Mark G. Rawlings, Siyi Feng, Dana Alina, J. E. Lee

Korea Astronomy and Space Science Institute
East Asian Observatory
University of Helsinki
European Southern Observatory
National Institutes of Natural Sciences - National Astronomical Observatory of Japan
National Research Council of Canada
University of Victoria BC
Academia Sinica - Institute of Astronomy and Astrophysics
Peking University
University of Hertfordshire
University of Manchester
Liverpool John Moores University
CAS - National Astronomical Observatories
Chinese Academy of Sciences
Université Paul Sabatier Toulouse III
Max Planck Institute for Radio Astronomy
Universidad de Chile
Yunnan University
Center for Astrophysics | Harvard and Smithsonian
Jet Propulsion Laboratory, California Institute of Technology
University of Texas at Austin
Open University Milton Keynes
Rutherford Appleton Laboratory
University of Science and Technology UST
Eotvos Lorand University
Research Centre For Astronomy and Earth Sciences
Kyung Hee University
Cardiff University
National Central University
University of Waterloo
University of Cologne
European Space Astronomy Centre
Chinese University of Hong Kong
Universidad de Concepción
University of California at Berkeley
University College London
Max Planck Institute for Extraterrestrial Physics
School of Space Research

Research output: Contribution to journal › Article › peer-review

62 Citations (Scopus)

Abstract

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.

Original language	English
Article number	28
Journal	Astrophysical Journal, Supplement Series
Volume	234
Issue number	2
DOIs	https://doi.org/10.3847/1538-4365/aaa3dd
Publication status	Published - Feb 2018

Funding

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) 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.

Keywords

ISM: abundances
ISM: clouds
ISM: kinematics and dynamics
stars: formation
surveys

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-4365/aaa3dd

Cite this

Liu, T., Kim, K. T., Juvela, M., Wang, K., Tatematsu, KI., Francesco, J. D., Liu, S. Y., Wu, Y., Thompson, M., Fuller, G., Eden, D., Li, D., Ristorcelli, I., Kang, S. J., Lin, Y., Johnstone, D., He, J. H., Koch, P. M., Sanhueza, P., ... Lee, J. E. (2018). The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17. Astrophysical Journal, Supplement Series, 234(2), Article 28. https://doi.org/10.3847/1538-4365/aaa3dd

Liu, T, Kim, KT, Juvela, M, Wang, K, Tatematsu, KI, Francesco, JD, Liu, SY, Wu, Y, Thompson, M, Fuller, G, Eden, D, Li, D, Ristorcelli, I, Kang, SJ, Lin, Y, Johnstone, D, He, JH, Koch, PM, Sanhueza, P, Qin, SL, Zhang, Q, Hirano, N, Goldsmith, PF, Evans, NJ, White, GJ, Choi, M, Lee, CW, Toth, LV, Mairs, S, Yi, HW, Tang, M, Soam, A, Peretto, N, Samal, MR, Fich, M, Parsons, H, Yuan, J, Zhang, CP, Malinen, J, Bendo, GJ, Rivera-Ingraham, A, Liu, HL, Wouterloot, J, Li, PS, Qian, L, Rawlings, J, Rawlings, MG, Feng, S, Alina, D & Lee, JE 2018, 'The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17', Astrophysical Journal, Supplement Series, vol. 234, no. 2, 28. https://doi.org/10.3847/1538-4365/aaa3dd

@article{eb66e5c198e8440fa6ef3243bc17fb7b,

title = "The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17",

abstract = "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.",

keywords = "ISM: abundances, ISM: clouds, ISM: kinematics and dynamics, stars: formation, surveys",

author = "Tie Liu and Kim, \{Kee Tae\} and Mika Juvela and Ke Wang and Ken'Ichi Tatematsu and Francesco, \{James Di\} and Liu, \{Sheng Yuan\} and Yuefang Wu and Mark Thompson and Gary Fuller and David Eden and Di Li and I. Ristorcelli and Kang, \{Sung Ju\} and Yuxin Lin and D. Johnstone and He, \{J. H.\} and Koch, \{P. M.\} and Patricio Sanhueza and Qin, \{Sheng Li\} and Q. Zhang and N. Hirano and Goldsmith, \{Paul F.\} and Evans, \{Neal J.\} and White, \{Glenn J.\} and Minho Choi and Lee, \{Chang Won\} and Toth, \{L. V.\} and Steve Mairs and Yi, \{H. W.\} and Mengyao Tang and Archana Soam and N. Peretto and Samal, \{Manash R.\} and Michel Fich and Harriet Parsons and Jinghua Yuan and Zhang, \{Chuan Peng\} and Johanna Malinen and Bendo, \{George J.\} and A. Rivera-Ingraham and Liu, \{Hong Li\} and Jan Wouterloot and Li, \{Pak Shing\} and Lei Qian and Jonathan Rawlings and Rawlings, \{Mark G.\} and Siyi Feng and Dana Alina and Lee, \{J. E.\}",

note = "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 ({\textquotedblleft}Physics of the Interstellar Medium{\textquotedblright}). 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: {\textcopyright} 2018. The American Astronomical Society. All rights reserved..",

year = "2018",

month = feb,

doi = "10.3847/1538-4365/aaa3dd",

language = "English",

volume = "234",

journal = "Astrophysical Journal, Supplement Series",

issn = "0067-0049",

publisher = "American Astronomical Society",

number = "2",

}

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 - Alina, Dana

AU - Lee, J. E.

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 - https://www.scopus.com/pages/publications/85042529579

UR - https://www.scopus.com/pages/publications/85042529579#tab=citedBy

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 -

The TOP-SCOPE Survey of Planck Galactic Cold Clumps: Survey Overview and Results of an Exemplar Source, PGCC G26.53+0.17

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