YNAO OpenIR  > 大样本恒星演化研究组
Herschel and SCUBA-2 observations of dust emission in a sample of Planck cold clumps
Juvela, Mika1; He JH(何金华)2,3,4,5; Pattle, Katherine6; Liu, Tie7,8; Bendo, George9; Eden, David J.10; Fehér, Orsolya11,12; Michel, Fich13; Fuller, Gary9; Hirano, Naomi14; Kim, Kee-Tae7; Li, Di15,16; Liu, Sheng-Yuan14; Malinen, Johanna17; Marshall, Douglas J.18; Paradis, Deborah19,20; Parsons, Harriet8; Pelkonen, Veli-Matti1; Rawlings, Mark G.8; Ristorcelli, Isabelle19,20; Samal, Manash R.21; Tatematsu, Ken'Ichi22; Thompson, Mark23; Traficante, Alessio24; Wang, Ke25; Ward-Thompson, Derek6; Wu, Yuefang26; Yi, Hee-Weon27; Yoo, Hyunju28
发表期刊ASTRONOMY & ASTROPHYSICS
2018-04-27
卷号612
DOI10.1051/0004-6361/201731921
产权排序第2完成单位
收录类别SCI ; EI
关键词Ism: Clouds Infrared: Ism Submillimetre: Ism Stars: Formation Stars: protoStars Dust Extinction
摘要Context. Analysis of all-sky Planck submillimetre observations and the IRAS 100 mu m data has led to the detection of a population of Galactic cold clumps. The clumps can be used to study star formation and dust properties in a wide range of Galactic environments.

Aims. Our aim is to measure dust spectral energy distribution ( SED) variations as a function of the spatial scale and the wavelength.

Methods. We examined the SEDs at large scales using IRAS, Planck, and Herschel data. At smaller scales, we compared JCMT/SCUBA-2 850 mu m maps with Herschel data that were filtered using the SCUBA-2 pipeline. Clumps were extracted using the Fellwalker method, and their spectra were modelled as modified blackbody functions.

Results. According to IRAS and Planck data, most fields have dust colour temperatures T-C similar to 14-18K and opacity spectral index values of beta = 1.5-1.9. The clumps and cores identified in SCUBA-2 maps have T similar to 13K and similar beta values. There are some indications of the dust emission spectrum becoming flatter at wavelengths longer than 500 mu m. In fits involving Planck data, the significance is limited by the uncertainty of the corrections for CO line contamination. The fits to the SPIRE data give a median beta value that is slightly above 1.8. In the joint SPIRE and SCUBA-2 850 mu m fits, the value decreases to beta similar to 1.6. Most of the observed T-beta anticorrelation can be explained by noise.

Conclusions. The typical submillimetre opacity spectral index fi of cold clumps is found to be similar to 1.7. This is above the values of diffuse clouds, but lower than in some previous studies of dense clumps. There is only tentative evidence of a T-beta anticorrelation and beta decreasing at millimetre wavelengths.
项目资助者Chinese Academy of Sciences(XDB09000000) ; Science and Technology Facilities Council of the United Kingdom ; Canada Foundation for Innovation ; National Aeronautics and Space Administration's Earth Science Technology Office(NCC5-626) ; ESO-ARO programme(196.C-0999(A)) ; Academy of Finland(285769) ; KASI fellowship ; EACOA fellowship ; ERC-STG(679852 RADFEEDBACK) ; European Research Council(320773)
语种英语
学科领域天文学
文章类型Article
ISSN1432-0746
URL查看原文
WOS记录号WOS:000430955300006
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]SPECTRAL INDEX ; TEMPERATURE-DEPENDENCE ; DARK CLOUDS ; DENSE CORES ; JCMT ; FIELD ; CATALOG ; MASSES ; NOISE ; MAPS
引用统计
被引频次:3[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/12160
专题大样本恒星演化研究组
中国科学院天体结构与演化重点实验室
作者单位1.Department of Physics, University of Helsinki, PO Box 64, 00014, Finland
2.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming; 650216, China
3.Chinese Academy of Sciences South America Center for Astronomy, China-Chile Joint Center for Astronomy, Camino El Observatorio 1515, Las Condes, Santiago, Chile
4.Eövös Loránd University, Department of Astronomy, Pazmany Peter setany 1/A, Budapest; 1117, Hungary
5.Department of Physics and Astronomy, University of Waterloo, Waterloo; ON; N2L 3G1, Canada
6.Institute of Astronomy and Astrophysics, Academia Sinica, AS/NTU No.1 Sec. 4 Roosevelt Rd, Taipei; 10617, Taiwan
7.National Astronomical Observatories, Chinese Academy of Sciences, Beijing; 100012, China
8.Key Laboratory of Radio Astronomy, Chinese Academy of Science, Nanjing; 210008, China
9.Institute of Physics i, University of Cologne, Cologne, Germany
10.Laboratoire AIM, IRFU/Service d'Astrophysique - CEA/DSM, CNRS - Université Paris Diderot, Bât. 709, Gif-sur-Yvette Cedex; 91191, France
11.Université de Toulouse, UPS-OMP, IRAP, Toulouse Cedex 4; 31028, France
12.CNRS, IRAP, 9 av. colonel Roche, Toulouse Cedex 4; 31028, France
13.Graduate Institute of Astronomy, National Central University 300, Jhongli, Taoyuan; 32001, Taiwan
14.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming; 650216, China
15.Nobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 462-2 Nobeyama, Minamimaki, Minamisaku, Nagano; 384-1305, Japan
16.Centre for Astrophysics Research, School of Physics Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield; AL10 9AB, United Kingdom
17.IAPS - INAF, via Fosso del Cavaliere, 100, Rome; 00133, Italy
18.European Southern Observatory, Karl-Schwarzschild-Str.2, Garching bei München; 85748, Germany
19.Department of Astronomy, Peking University, Beijing; 100871, China Department of Astronomy, Peking University, Beijing; 100871, China Department of Astronomy, Peking University, Beijing; 100871, China Department of Astronomy, Peking University, Beijing; 100871, China
20.School of Space Research, Kyung Hee University, 1732 Deogyeong-daero, Giheung-gu, Yongin-si, Gyeonggi-do, Korea, Republic of
21.Department of Astronomy and Space Science, Chungnam National University, 99 Daehak-ro, Yuseong-gu, Daejeon; 34134, Korea, Republic of
22.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing; 100012, China
23.Jeremiah Horrocks Institute, University of Central Lancashire, Preston; PR1 2HE, United Kingdom
24.Korea Astronomy and Space Science Institute, 776 Daedeokdaero, Yuseong-gu, Daejeon; 34055, Korea, Republic of
25.East Asian Observatory, 660 N. A'ohoku Place, Hilo; HI; 96720-2700, United States
26.UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester; M13 9PL, United Kingdom
27.Astrophysics Research Institute, Liverpool John Moores University, Ic2, Liverpool Science Park, 146 Brownlow Hill, Liverpool; L3 5RF, United Kingdom
28.Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly Thege Miklós út 15-17, Budapest; 1121, Hungary
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GB/T 7714
Juvela, Mika,He JH,Pattle, Katherine,et al. Herschel and SCUBA-2 observations of dust emission in a sample of Planck cold clumps[J]. ASTRONOMY & ASTROPHYSICS,2018,612.
APA Juvela, Mika.,He JH.,Pattle, Katherine.,Liu, Tie.,Bendo, George.,...&Yoo, Hyunju.(2018).Herschel and SCUBA-2 observations of dust emission in a sample of Planck cold clumps.ASTRONOMY & ASTROPHYSICS,612.
MLA Juvela, Mika,et al."Herschel and SCUBA-2 observations of dust emission in a sample of Planck cold clumps".ASTRONOMY & ASTROPHYSICS 612(2018).
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