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1. The JCMT BISTRO-2 survey : magnetic fields of the massive DR21 filament

Author

Tao-Chung Ching, Keping Qiu, Di Li, Zhiyuan Ren, Shih-Ping Lai, David Berry, Kate Pattle, Ray Furuya, Derek Ward-Thompson, Doug Johnstone, Patrick M. Koch, Chang Won Lee, Thiem Hoang, Tetsuo Hasegawa, Woojin Kwon, Pierre Bastien, Chakali Eswaraiah, Jia-Wei Wang, Kyoung Hee Kim, Jihye Hwang, Archana Soam, A-Ran Lyo, Junhao Liu, Valentin J. M. Le Gouellec, Doris Arzoumanian, Anthony Whitworth, James Di Francesco, Frédérick Poidevin, Tie Liu, Simon Coudé, Mehrnoosh Tahani, Hong-Li Liu, Takashi Onaka, Dalei Li, Motohide Tamura, Zhiwei Chen, Xindi Tang, Florian Kirchschlager, Tyler L. Bourke, Do-Young Byun, Mike Chen, Huei-Ru Vivien Chen, Wen Ping Chen, Jungyeon Cho, Yunhee Choi, Youngwoo Choi, Minho Choi, Antonio Chrysostomou, Eun Jung Chung, Y. Sophia Dai, Pham Ngoc Diep, Yasuo Doi, Yan Duan, Hao-Yuan Duan, David Eden, Lapo Fanciullo, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Saeko Hayashi, Martin Houde, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Vera Könyves, Ji-hyun Kang, Miju Kang, Janik Karoly, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Jongsoo Kim, Mi-Ryang Kim, Shinyoung Kim, Hyosung Kim, Kee-Tae Kim, Gwanjeong Kim, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Sang-Sung Lee, Hyeseung Lee, Jeong-Eun Lee, Chin-Fei Lee, Yong-Hee Lee, Guangxing Li, Hua-bai Li, Sheng-Jun Lin, Sheng-Yuan Liu, Xing Lu, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Mark Rawlings, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Sarah Sadavoy, Hiro Saito, Giorgio Savini, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jintai Wu, Jinjin Xie, Meng-Zhe Yang, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Chuan-Peng Zhang, Yapeng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, Stewart Eyres, Sam Falle, Jean-François Robitaille, Sven van Loo, National Natural Science Foundation of China, Chinese Academy of Sciences, Natural Sciences and Engineering Research Council of Canada, Ministerio de Ciencia, Innovación y Universidades (España), National Research Foundation of Korea, National Research, Japan Society for the Promotion of Science, Agencia Estatal de Investigación (España), Ching, Tao-Chung [0000-0001-8516-2532], Qiu, Keping [0000-0002-5093-5088], Li, Di [0000-0003-3010-7661], Ren, Zhiyuan [0000-0003-4659-1742], Lai, Shih-Ping [0000-0001-5522-486X], Berry, David [0000-0001-6524-2447], Pattle, Kate [0000-0002-8557-3582], Furuya, Ray [0000-0003-0646-8782], Ward-Thompson, Derek [0000-0003-1140-2761], Johnstone, Doug [0000-0002-6773-459X], Koch, Patrick M [0000-0003-2777-5861], Lee, Chang Won [0000-0002-3179-6334], Hoang, Thiem [0000-0003-2017-0982], Hasegawa, Tetsuo [0000-0003-1853-0184], Kwon, Woojin [0000-0003-4022-4132], Bastien, Pierre [0000-0002-0794-3859], Eswaraiah, Chakali [0000-0003-4761-6139], Wang, Jia-Wei [0000-0002-6668-974X], Kim, Kyoung Hee [0000-0001-9597-7196], Hwang, Jihye [0000-0001-7866-2686], Soam, Archana [0000-0002-6386-2906], Lyo, A-Ran [0000-0002-9907-8427], Liu, Junhao [0000-0002-4774-2998], Le Gouellec, Valentin JM [0000-0002-5714-799X], Arzoumanian, Doris [0000-0002-1959-7201], Whitworth, Anthony [0000-0002-1178-5486], Francesco, James Di [0000-0002-9289-2450], Poidevin, Frédérick [0000-0002-5391-5568], Liu, Tie [0000-0002-5286-2564], Coudé, Simon [0000-0002-0859-0805], Tahani, Mehrnoosh [0000-0001-8749-1436], Liu, Hong-Li [0000-0003-3343-9645], Onaka, Takashi [0000-0002-8234-6747], Tamura, Motohide [0000-0002-6510-0681], Chen, Zhiwei [0000-0003-0849-0692], Tang, Xindi [0000-0002-4154-4309], Kirchschlager, Florian [0000-0002-3036-0184], Bourke, Tyler L [0000-0001-7491-0048], Byun, Do-Young [0000-0003-1157-4109], Chen, Huei-Ru Vivien [0000-0002-9774-1846], Chen, Wen Ping [0000-0003-0262-272X], Cho, Jungyeon [0000-0003-1725-4376], Chrysostomou, Antonio [0000-0002-9583-8644], Chung, Eun Jung [0000-0003-0014-1527], Dai, Y Sophia [0000-0002-7928-416X], Diep, Pham Ngoc [0000-0002-2808-0888], Doi, Yasuo [0000-0001-8746-6548], Duan, Hao-Yuan [0000-0002-7022-4742], Eden, David [0000-0002-5881-3229], Fanciullo, Lapo [0000-0001-9930-9240], Fissel, Laura M [0000-0002-4666-609X], Franzmann, Erica [0000-0003-2142-0357], Friberg, Per [0000-0002-8010-8454], Friesen, Rachel [0000-0001-7594-8128], Fuller, Gary [0000-0001-8509-1818], Gledhill, Tim [0000-0002-2859-4600], Graves, Sarah [0000-0001-9361-5781], Greaves, Jane [0000-0002-3133-413X], Gu, Qilao [0000-0002-2826-1902], Hayashi, Saeko [0000-0001-5026-490X], Houde, Martin [0000-0003-4420-8674], Hull, Charles LH [0000-0002-8975-7573], Inoue, Tsuyoshi [0000-0002-7935-8771], Inutsuka, Shu-ichiro [0000-0003-4366-6518], Jeong, Il-Gyo [0000-0002-5492-6832], Könyves, Vera [0000-0002-3746-1498], Kang, Ji-hyun [0000-0001-7379-6263], Kang, Miju [0000-0002-5016-050X], Karoly, Janik [0000-0001-5996-3600], Kataoka, Akimasa [0000-0003-4562-4119], Kawabata, Koji [0000-0001-6099-9539], Kemper, Francisca [0000-0003-2743-8240], Kim, Jongsoo [0000-0002-1229-0426], Kim, Shinyoung [0000-0001-9333-5608], Kim, Kee-Tae [0000-0003-2412-7092], Kim, Gwanjeong [0000-0003-2011-8172], Kirk, Jason [0000-0002-4552-7477], Kobayashi, Masato IN [0000-0003-3990-1204], Kusune, Takayoshi [0000-0002-9218-9319], Kwon, Jungmi [0000-0003-2815-7774], Lacaille, Kevin [0000-0001-9870-5663], Law, Chi-Yan [0000-0003-1964-970X], Lee, Sang-Sung [0000-0002-6269-594X], Lee, Hyeseung [0000-0003-3465-3213], Lee, Jeong-Eun [0000-0003-3119-2087], Lee, Chin-Fei [0000-0002-3024-5864], Lee, Yong-Hee [0000-0001-6047-701X], Li, Guangxing [0000-0003-3144-1952], Li, Hua-bai [0000-0003-2641-9240], Lin, Sheng-Jun [0000-0002-6868-4483], Liu, Sheng-Yuan [0000-0003-4603-7119], Lu, Xing [0000-0003-2619-9305], Mairs, Steve [0000-0002-6956-0730], Matsumura, Masafumi [0000-0002-6906-0103], Matthews, Brenda [0000-0003-3017-9577], Moriarty-Schieven, Gerald [0000-0002-0393-7822], Nagata, Tetsuya [0000-0001-9264-9015], Nakamura, Fumitaka [0000-0001-5431-2294], Ngoc, Nguyen Bich [0000-0002-5913-5554], Ohashi, Nagayoshi [0000-0003-0998-5064], Park, Geumsook [0000-0001-8467-3736], Parsons, Harriet [0000-0002-6327-3423], Pyo, Tae-Soo [0000-0002-3273-0804], Qian, Lei [0000-0003-0597-0957], Rao, Ramprasad [0000-0002-1407-7944], Rawlings, Mark [0000-0002-6529-202X], Rawlings, Jonathan [0000-0001-5560-1303], Richer, John [0000-0002-9693-6860], Rigby, Andrew [0000-0002-3351-2200], Savini, Giorgio [0000-0003-4449-9416], Shimajiri, Yoshito [0000-0001-9368-3143], Shinnaga, Hiroko [0000-0001-9407-6775], Tang, Ya-Wen [0000-0002-0675-276X], Tomisaka, Kohji [0000-0003-2726-0892], Tram, Le Ngoc [0000-0002-6488-8227], Viti, Serena [0000-0001-8504-8844], Wang, Hongchi [0000-0003-0746-7968], Wu, Jintai [0000-0001-7276-3590], Xie, Jinjin [0000-0002-2738-146X], Yen, Hsi-Wei [0000-0003-1412-893X], Yoo, Hyunju [0000-0002-8578-1728], Yun, Hyeong-Sik [0000-0001-6842-1555], Zhang, Chuan-Peng [0000-0002-4428-3183], Zhang, Yapeng [0000-0002-5102-2096], Zhou, Jianjun [0000-0003-0356-818X], André, Philippe [0000-0002-3413-2293], Falle, Sam [0000-0002-9829-0426], Robitaille, Jean-François [0000-0001-5079-8573], van Loo, Sven [0000-0003-4746-8500], and Apollo - University of Cambridge Repository

Subjects
STAR-FORMING REGIONS, SUBMILLIMETER POLARIZATION, HERSCHEL, FOS: Physical sciences, Astronomy and Astrophysics, MU-M POLARIZATION, MOLECULAR CLOUD, Astrophysics - Astrophysics of Galaxies, 1ST, Astrophysics - Solar and Stellar Astrophysics, Physics and Astronomy, 5101 Astronomical Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SCUBA-2, GOULD BELT SURVEY, DUST EMISSION, 51 Physical Sciences, Solar and Stellar Astrophysics (astro-ph.SR), FAR-INFRARED POLARIMETRY
Abstract

Tao-Chung Ching et al., We present 850 μm dust polarization observations of the massive DR21 filament from the B-fields In STar-forming Region Observations (BISTRO) survey, using the POL-2 polarimeter and the SCUBA-2 camera on the James Clerk Maxwell Telescope. We detect ordered magnetic fields perpendicular to the parsec-scale ridge of the DR21 main filament. In the subfilaments, the magnetic fields are mainly parallel to the filamentary structures and smoothly connect to the magnetic fields of the main filament. We compare the POL-2 and Planck dust polarization observations to study the magnetic field structures of the DR21 filament on 0.1–10 pc scales. The magnetic fields revealed in the Planck data are well-aligned with those of the POL-2 data, indicating a smooth variation of magnetic fields from large to small scales. The plane-of-sky magnetic field strengths derived from angular dispersion functions of dust polarization are 0.6–1.0 mG in the DR21 filament and ∼0.1 mG in the surrounding ambient gas. The mass-to-flux ratios are found to be magnetically supercritical in the filament and slightly subcritical to nearly critical in the ambient gas. The alignment between column density structures and magnetic fields changes from random alignment in the low-density ambient gas probed by Planck to mostly perpendicular in the high-density main filament probed by James Clerk Maxwell Telescope. The magnetic field structures of the DR21 filament are in agreement with MHD simulations of a strongly magnetized medium, suggesting that magnetic fields play an important role in shaping the DR21 main filament and subfilaments., This work is supported by National Natural Science Foundation of China (NSFC) grant Nos. 11988101, U1931117, 11725313, and 12073061 and the CAS International Partnership Program of Chinese Academy of Sciences grant No. 114A11KYSB20160008. T.-C.C. is funded by Chinese Academy of Sciences Taiwan Young Talent Program grant No. 2018TW2JB0002. T.-C.C. and C.E. were supported by Special Funding for Advanced Users, budgeted and administrated by Center for Astronomical Mega-Science (CAMS), Chinese Academy of Sciences. K.P. is a Royal Society University Research Fellow, supported by grant No. URF\R1\211322. D.J. is supported by the National Research Council of Canada and by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant. P.M.K. is supported by the Ministry of Science and Technology (MoST) in Taiwan through grants 109-2112-M-001-022 and 110-2112-M-001-057. C.W.L. is supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (NRF-2019R1A2C1010851), and by the Korea Astronomy and Space Science Institute grant funded by the Korea government (MSIT; Project No. 2022-1-840-05). T.H. is supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIT) through the Mid-career Research Program (2019R1A2C1087045). W.K. was supported by the NRF grant funded by the MSIT (2021R1F1A1061794). C.E. acknowledges the financial support from grant RJF/2020/000071 as a part of Ramanujan Fellowship awarded by the Science and Engineering Research Board (SERB), Department of Science and Technology (DST), Govt. of India. F.P. acknowledges support from the Spanish State Research Agency (AEI) under grant No. PID2019-105552RB-C43. M.T. is supported by JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. J.K. is supported by JSPS KAKENHI grant No. 19K14775. L.F. and F.K. acknowledge the support by the MoST in Taiwan through grant 107-2119-M-001-031-MY3 and Academia Sinica through grant AS-IA-106-M03. L.F. acknowledges the support by the MoST in Taiwan through grants 111-2811-M-005-007 and 109-2112-M-005-003-MY3. C.L.H.H. acknowledges the support of the NAOJ Fellowship and JSPS KAKENHI grants 18K13586 and 20K14527. F.K. is supported by the Spanish program Unidad de Excelencia María de Maeztu CEX2020-001058-M, financed by MCIN/AEI/10.13039/501100011033. K.Q. is partially supported by National Key R&D Program of China No. 2022YFA1603100, and acknowledges the National Natural Science Foundation of China (NSFC) grant U1731237. S.P.L. acknowledges grants from the Ministry of Science and Technology of Taiwan 106-2119-M-007-021-MY3 and 109-2112-M-007-010-MY3. Y.D. acknowledges the support of JSPS KAKENHI grants 25247016 and 18H01250. Y.S.D. is supported by the National Key R&D Program of China for grant No. 2022YFA1605300, and NSFC grants Nos. 12273051, 11933003.

Published
2022

2. The JCMT BISTRO Survey: An 850/450$\mu$m Polarization Study of NGC 2071IR in OrionB

Author

A-Ran Lyo, Jongsoo Kim, Sarah Sadavoy, Doug Johnstone, David Berry, Kate Pattle, Woojin Kwon, Pierre Bastien, Takashi Onaka, James Di Francesco, Ji-Hyun Kang, Ray Furuya, Charles L. H. Hull, Motohide Tamura, Patrick M. Koch, Derek Ward-Thompson, Tetsuo Hasegawa, Thiem Hoang, Doris Arzoumanian, Chang Won Lee, Chin-Fei Lee, Do-Young Byun, Florian Kirchschlager, Yasuo Doi, Kee-Tae Kim, Jihye Hwang, Pham Ngoc Diep, Lapo Fanciullo, Sang-Sung Lee, Geumsook Park, Hyunju Yoo, Eun Jung Chung, Anthony Whitworth, Steve Mairs, Archana Soam, Tie Liu, Xindi Tang, Simon Coudé, Philippe André, Tyler L. Bourke, Huei-Ru Vivien Chen, Zhiwei Chen, Wen Ping Chen, Mike Chen, Tao-Chung Ching, Jungyeon Cho, Minho Choi, Yunhee Choi, Antonio Chrysostomou, Sophia Dai, C. Darren Dowell, Hao-Yuan Duan, Yan Duan, David Eden, Chakali Eswaraiah, Stewart Eyres, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Jannifer Hatchell, Saeko Hayashi, Martin Houde, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Miju Kang, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Gwanjeong Kim, Mi-Ryang Kim, Shinyoung Kim, Kyoung Hee Kim, Jason Kirk, Masato I. N. Kobayashi, Vera Könyves, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Shih-Ping Lai, Chi-Yan Law, Jeong-Eun Lee, Yong-Hee Lee, Hyeseung Lee, Dalei Li, Di Li, Hua-Bai Li, Hong-Li Liu, Junhao Liu, Sheng-Yuan Liu, Xing Lu, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-soo Pyo, Lei Qian, Keping Qiu, Ramprasad Rao, Jonathan Rawlings, Mark G. Rawlings, Brendan Retter, John Richer, Andrew Rigby, Hiro Saito, Giorgio Savini, Anna Scaife, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Mehrnoosh Tahani, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Jia-Wei Wang, Hongchi Wang, Jinjin Xie, Hsi-Wei Yen, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Guoyin Zhang, Chuan-Peng Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Sam Falle, Jean-François Robitaille, Sven van Loo, Lyo, A-Ran [0000-0002-9907-8427], Kim, Jongsoo [0000-0002-1229-0426], Johnstone, Doug [0000-0002-6773-459X], Pattle, Kate [0000-0002-8557-3582], Kwon, Woojin [0000-0003-4022-4132], Bastien, Pierre [0000-0002-0794-3859], Onaka, Takashi [0000-0002-8234-6747], Kang, Ji-Hyun [0000-0001-7379-6263], Furuya, Ray [0000-0003-0646-8782], Hull, Charles L. H. [0000-0002-8975-7573], Tamura, Motohide [0000-0002-6510-0681], Koch, Patrick M. [0000-0003-2777-5861], Ward-Thompson, Derek [0000-0003-1140-2761], Hoang, Thiem [0000-0003-2017-0982], Arzoumanian, Doris [0000-0002-1959-7201], Lee, Chin-Fei [0000-0002-3024-5864], Byun, Do-Young [0000-0003-1157-4109], Kirchschlager, Florian [0000-0002-3036-0184], Doi, Yasuo [0000-0001-8746-6548], Kim, Kee-Tae [0000-0003-2412-7092], Hwang, Jihye [0000-0001-7866-2686], Lee, Sang-Sung [0000-0002-6269-594X], Park, Geumsook [0000-0001-8467-3736], Yoo, Hyunju [0000-0002-8578-1728], Chung, Eun Jung [0000-0003-0014-1527], Mairs, Steve [0000-0002-6956-0730], Soam, Archana [0000-0002-6386-2906], Liu, Tie [0000-0002-5286-2564], Tang, Xindi [0000-0002-4154-4309], Coudé, Simon [0000-0002-0859-0805], André, Philippe [0000-0002-3413-2293], Bourke, Tyler L. [0000-0001-7491-0048], Chen, Zhiwei [0000-0003-0849-0692], Ping Chen, Wen [0000-0002-5519-0628], Ching, Tao-Chung [0000-0001-8516-2532], Cho, Jungyeon [0000-0003-1725-4376], Chrysostomou, Antonio [0000-0002-9583-8644], Eden, David [0000-0002-5881-3229], Franzmann, Erica [0000-0003-2142-0357], Friberg, Per [0000-0002-8010-8454], Friesen, Rachel [0000-0001-7594-8128], Fuller, Gary [0000-0001-8509-1818], Gledhill, Tim [0000-0002-2859-4600], Graves, Sarah [0000-0001-9361-5781], Gu, Qilao [0000-0002-2826-1902], Hatchell, Jannifer [0000-0002-4870-2760], Houde, Martin [0000-0003-4420-8674], Inoue, Tsuyoshi [0000-0002-7935-8771], Inutsuka, Shu-ichiro [0000-0003-4366-6518], Iwasaki, Kazunari [0000-0002-2707-7548], Kang, Miju [0000-0002-5016-050X], Kataoka, Akimasa [0000-0003-4562-4119], Kawabata, Koji [0000-0001-6099-9539], Kemper, Francisca [0000-0003-2743-8240], Kim, Gwanjeong [0000-0003-2011-8172], Kim, Mi-Ryang [0000-0002-1408-7747], Kim, Shinyoung [0000-0001-9333-5608], Kirk, Jason [0000-0002-4552-7477], Kobayashi, Masato I. N. [0000-0003-3990-1204], Könyves, Vera [0000-0002-3746-1498], Kusune, Takayoshi [0000-0002-9218-9319], Kwon, Jungmi [0000-0003-2815-7774], Lacaille, Kevin [0000-0001-9870-5663], Lai, Shih-Ping [0000-0001-5522-486X], Law, Chi-Yan [0000-0003-1964-970X], Lee, Jeong-Eun [0000-0003-3119-2087], Lee, Yong-Hee [0000-0001-6047-701X], Lee, Hyeseung [0000-0003-3465-3213], Li, Di [0000-0003-3010-7661], Li, Hua-Bai [0000-0003-2641-9240], Liu, Junhao [0000-0002-4774-2998], Liu, Sheng-Yuan [0000-0003-4603-7119], Lu, Xing [0000-0003-2619-9305], Matsumura, Masafumi [0000-0002-6906-0103], Matthews, Brenda [0000-0003-3017-9577], Moriarty-Schieven, Gerald [0000-0002-0393-7822], Nagata, Tetsuya [0000-0001-9264-9015], Nakamura, Fumitaka [0000-0001-5431-2294], Ohashi, Nagayoshi [0000-0003-0998-5064], Parsons, Harriet [0000-0002-6327-3423], Pyo, Tae-soo [0000-0002-3273-0804], Qian, Lei [0000-0003-0597-0957], Qiu, Keping [0000-0002-5093-5088], Rao, Ramprasad [0000-0002-1407-7944], Rawlings, Jonathan [0000-0001-5560-1303], Rawlings, Mark G. [0000-0002-6529-202X], Richer, John [0000-0002-9693-6860], Rigby, Andrew [0000-0002-3351-2200], Savini, Giorgio [0000-0003-4449-9416], Shimajiri, Yoshito [0000-0001-9368-3143], Shinnaga, Hiroko [0000-0001-9407-6775], Tang, Ya-Wen [0000-0002-0675-276X], Tomisaka, Kohji [0000-0003-2726-0892], Tram, Le Ngoc [0000-0002-6488-8227], Viti, Serena [0000-0001-8504-8844], Wang, Jia-Wei [0000-0002-6668-974X], Wang, Hongchi [0000-0003-0746-7968], Yen, Hsi-Wei [0000-0003-1412-893X], Yun, Hyeong-Sik [0000-0001-6842-1555], Zhang, Chuan-Peng [0000-0002-4428-3183], and Apollo - University of Cambridge Repository

Subjects
Young stellar object, FAR-INFRARED POLARIZATION, Astrophysics, F500, IMAGING POLARIMETRY, MAGNETIC-FIELDS, Gravitational energy, STAR-FORMATION, interstellar magnetic fields, Bipolar outflow, SCUBA-2, FORMING MOLECULAR CLOUDS, GOULD BELT SURVEY, James Clerk Maxwell Telescope, polarimetry, Physics, interstellar medium, SUBMILLIMETER POLARIZATION, Magnetic energy, Center (category theory), Interstellar Matter and the Local Universe, CORES, Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Magnetic field, Physics and Astronomy, BIPOLAR OUTFLOW, Space and Planetary Science, star forming regions
Abstract

We present the results of simultaneous 450 $\mu$m and 850 $\mu$m polarization observations toward the massive star forming region NGC 2071IR, a target of the BISTRO (B-fields in Star-Forming Region Observations) Survey, using the POL-2 polarimeter and SCUBA-2 camera mounted on the James Clerk Maxwell Telescope. We find a pinched magnetic field morphology in the central dense core region, which could be due to a rotating toroidal disk-like structure and a bipolar outflow originating from the central young stellar object, IRS 3. Using the modified Davis-Chandrasekhar-Fermi method, we obtain a plane-of-sky magnetic field strength of 563$\pm$421 $\mu$G in the central $\sim$0.12 pc region from 850 $\mu$m polarization data. The corresponding magnetic energy density of 2.04$\times$10$^{-8}$ erg cm$^{-3}$ is comparable to the turbulent and gravitational energy densities in the region. We find that the magnetic field direction is very well aligned with the whole of the IRS 3 bipolar outflow structure. We find that the median value of polarization fractions, 3.0 \%, at 450 $\mu$m in the central 3 arcminute region, which is larger than the median value of 1.2 \% at 850 $\mu$m. The trend could be due to the better alignment of warmer dust in the strong radiation environment. We also find that polarization fractions decrease with intensity at both wavelengths, with slopes, determined by fitting a Rician noise model, of $0.59 \pm 0.03$ at 450 $\mu$m and $0.36 \pm 0.04$ at 850 $\mu$m, respectively. We think that the shallow slope at 850 $\mu$m is due to grain alignment at the center being assisted by strong radiation from the central young stellar objects., Comment: 17 pages, 11 figures, 4 tables

Published
2021

3. Characterization of dense Planck clumps observed with Herschel and SCUBA-2

Author

E. Mannfors, Leonardo Bronfman, Hsien Shang, Miikka S. Väisälä, Archana Soam, Mika Juvela, Jinhua He, Gwanjeon Kim, Alessio Traficante, Patricio Sanhueza, Chang Won Lee, Kee-Tae Kim, H. Kirppu, Harriet Parsons, David Eden, J. Montillaud, Tie Liu, Ken'ichi Tatematsu, Particle Physics and Astrophysics, and Department of Physics

Subjects
Opacity, Young stellar object, Milky Way, Extinction (astronomy), MU-M, PHYSICAL-PROPERTIES, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, MOLECULAR CLOUD, ISM: clouds, 01 natural sciences, PIXEL BOLOMETER CAMERA, MAGNETIC-FIELDS, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, GOULD BELT SURVEY, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: general, infrared: ISM, STAR-FORMING REGIONS, Physics, HI-GAL, stars: formation, 010308 nuclear & particles physics, Star formation, Molecular cloud, Galactic Center, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), GALACTIC COLD CLUMPS, dust, extinction, methods: observational, OPHIUCHI MAIN CLOUD
Abstract

We aim to characterize a diverse selection of dense, potentially star-forming cores, clumps, and clouds within the Milky Way in terms of their dust emission and SF activity. We studied 53 fields that have been observed in the JCMT SCUBA-2 continuum survey SCOPE and have been mapped with Herschel. We estimated dust properties by fitting Herschel observations with modified blackbody functions, studied the relationship between dust temperature and dust opacity spectral index $\beta$, and estimated column densities. We extracted clumps from the SCUBA-2 850 $\mu$m maps with the FellWalker algorithm and examined their masses and sizes. Clumps are associated with young stellar objects found in several catalogs. We estimated the gravitational stability of the clumps with virial analysis. The clumps are categorized as unbound starless, prestellar, or protostellar. We find 529 dense clumps, typically with high column densities from (0.3-4.8)$\times 10^{22}$ cm$^{-2}$, with a mean of (1.5$\pm$0.04)$\times10^{22}$ cm$^{-2}$, low temperatures ($T\sim $10-20 K), and estimated submillimeter $\beta$ =1.7$\pm$0.1. We detect a slight increase in opacity spectral index toward millimeter wavelengths. Masses of the sources range from 0.04 $M_\odot$ to 4259 $M_\odot$. Mass, linear size, and temperature are correlated with distance. Furthermore, the estimated gravitational stability is dependent on distance, and more distant clumps appear more virially bound. Finally, we present a catalog of properties of the clumps.Our sources present a large array of SF regions, from high-latitude, nearby diffuse clouds to large SF complexes near the Galactic center. Analysis of these regions will continue with the addition of molecular line data, which will allow us to study the densest regions of the clumps in more detail., Comment: 60 pages (article 18 pages), 73 figures To be published in A&A

Published
2021

4. The JCMT BISTRO Survey:The Magnetic Field of the Barnard 1 Star-forming Region

Author

Coude, S, Bastien, P, Houde, M, Sadavoy, S, Friesen, R, Di Francesco, J, Johnstone, D, Mairs, S, Hasegawa, T, Kwon, W, Lai, S-P, Qiu, K, Ward-Thompson, D, Berry, D, Chen, MC-Y, Fiege, J, Franzmann, E, Hatchell, J, Lacaille, K, Matthews, BC, Moriarty-Schieven, GH, Pon, A, Andre, P, Arzoumanian, D, Aso, Y, Byun, D-Y, Eswaraiah, C, Chen, H-R, Chen, WP, Ching, T-C, Cho, J, Choi, M, Chrysostomou, A, Chung, EJ, Doi, Y, Drabek-Maunder, E, Dowell, CD, Eyres, SPS, Falle, S, Friberg, P, Fuller, G, Furuya, RS, Gledhill, T, Graves, SF, Greaves, JS, Griffin, MJ, Gu, Q, Hayashi, SS, Hoang, T, Holland, W, Inoue, T, Inutsuka, S-I, Iwasaki, K, Jeong, I-G, Kanamori, Y, Kataoka, A, Kang, J-H, Kang, M, Kang, S-J, Kawabata, KS, Kemper, F, Kim, G, Kim, J, Kim, K-T, Kim, KH, Kim, M-R, Kim, S, Kirk, JM, Kobayashi, MIN, Koch, PM, Kwon, J, Lee, J-E, Lee, CW, Lee, S-S, Li, D, Li, H-B, Liu, H-L, Liu, J, Liu, S-Y, Liu, T, van Loo, S, Lyo, A-R, Matsumura, M, Nagata, T, Nakamura, F, Nakanishi, H, Ohashi, N, Onaka, T, Parsons, H, Pattle, K, Peretto, N, Pyo, T-S, Qian, L, Rao, R, Rawlings, MG, Retter, B, Richer, J, Rigby, A, Robitaille, J-F, Saito, H, Savini, G, Scaife, AMM, Seta, M, Shinnaga, H, Soam, A, Tamura, M, Tang, Y-W, Tomisaka, K, Tsukamoto, Y, Wang, H, Wang, J-W, Whitworth, AP, Yen, H-W, Yoo, H, Yuan, J, Zenko, T, Zhang, C-P, Zhang, G, Zhou, J, Zhu, L, and The BISTRO Collaboration

Subjects
010504 meteorology & atmospheric sciences, INFRARED POLARIMETRY, RADIATIVE TORQUES, FOS: Physical sciences, Astrophysics, F500, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, ISM: clouds, MOLECULAR, 0103 physical sciences, POLARIZATION MEASUREMENTS, SCUBA-2, GOULD BELT SURVEY, ISM: individual objects (Barnard 1), individual objects (Barnard 1) [ISM], ISM [submillimeter], 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, LINEAR-POLARIZATION, polarization, stars: formation, formation [stars], Magnetic energy, Linear polarization, Molecular cloud, F510, CLOUDS, magnetic fields [ISM], Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, H2O MASERS, Magnetic field, ALIGNMENT, Amplitude, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, ISM: magnetic fields, INTERSTELLAR GRAINS, clouds [ISM]
Abstract

著者人数: The B-fields In STar-forming Regions Observations (BISTRO) Collaboration 121名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 權, 靜美), Number of authors: The B-fields In STar-forming Regions Observations (BISTRO) Collaboration 121 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Kwon, Jungmi), Accepted: 2019-04-18, 資料番号: SA1190042000

Published
2019
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5. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution – Survey Description and Compact Source Catalogue

Author

Karine Demyk, Mark G. Rawlings, Giuseppe Cosentino, Lixia Yuan, Gwanjeong Kim, Dimitris Stamatellos, Satoshi Ohashi, Dalei Li, Yasuo Doi, L. Harvey-Smith, Archana Soam, Anthony Peter Whitworth, Mark Thompson, Izaskun Jiménez-Serra, Gary A. Fuller, Huei-Ru Chen, Tae-Geun Ji, Oscar Morata, Chakali Eswaraiah, Jinyi Yang, Takeshi Sakai, Y. L. Yuan, Hiroko Shinnaga, David Cornu, Jonathan Rawlings, Walter Kieran Gear, Shaila Akhter, Yuri Aikawa, A. Chrysostomou, Fanyi Meng, Andrew Walsh, Christine D. Wilson, P. M. McGehee, M. Chen, Tomoya Hirota, Carsten Henkel, You-Hua Chu, E. Falgarone, S. Kim, Yuxin He, Johanna Malinen, Sung-ju Kang, Chin-Fei Lee, Xuepeng Chen, Miju Kang, Annie Hughes, V.-M. Pelkonen, Graham S. Bell, Woojin Kwon, Huawei Zhang, Bon-Chul Koo, E. Jarken, Glenn J. White, J. X. Ge, Andrew Rigby, A-Ran Lyo, Wayne S. Holland, Hong-Li Liu, Geumsook Park, Mengyao Tang, Emily Drabek-Maunder, Hee-Weon Yi, M. Liu, Tie Liu, Rebeka Bögner, J.-P. Bernard, C. P. Zhang, B. S. Wang, Manash R. Samal, Harriet Parsons, Mika Juvela, Toby J. T. Moore, Lei Zhu, Ya-Wen Tang, Guobao Zhang, Leonardo Bronfman, George J. Bendo, S. Mairs, Serena Viti, H. Wang, Tetsuo Hasegawa, Yuxin Lin, Minho Choi, Zhiyuan Ren, Ke Wang, Yi-Jehng Kuan, David Eden, I. Ristorcelli, Lei Qian, X. Chen, Paul F. Goldsmith, Jinhua He, Diego Mardones, Shih-Ping Lai, Di Li, Soojong Pak, Qizhou Zhang, Ken'ichi Tatematsu, L. Montier, Yuefang Wu, C. Zhou, Guido Garay, Patricio Sanhueza, A. Rivera-Ingraham, Nicolas Peretto, Keping Qiu, Siyi Feng, Patrick M. Koch, Neal J. Evans, Jeong-Eun Lee, Andrew Blain, A. P. Marston, Hua-bai Li, M. Fich, Chao Zhang, Eun Jung Chung, G. Luo, J. Montillaud, Derek Ward-Thompson, Jianjun Zhou, Maria Cunningham, Jungha Kim, N. Lo, Roberta Paladini, J. Di Francesco, Jongsoo Kim, Ye Xu, Xing Lu, Charlotte Vastel, Chang Won Lee, Pak Shing Li, John A. P. Lopez, Per Friberg, Sheng-Li Qin, Gerald Moriarty-Schieven, D. Alina, G. Pech, Wen Ping Chen, O. Fehér, Pei Zuo, Sheng-Yuan Liu, Jinghua Yuan, Scott Chapman, Alessio Traficante, Doug Johnstone, Jane Greaves, Do-Young Byun, Naomi Hirano, Helen J. Fraser, Jiali Wang, Koji S. Kawabata, J. G. A. Wouterloot, X. Guan, Hsien Shang, Annie Zavagno, John Richer, Kee-Tae Kim, Sarolta Zahorecz, Kate Pattle, Y. Lee, L. V. Toth, Kevin Lacaille, Department of Physics, Particle Physics and Astrophysics, Liverpool John Moores University (LJMU), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Arizona, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), and Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Milky Way, Continuum (design consultancy), SPIRAL ARMS, FOS: Physical sciences, F800, Astrophysics, 01 natural sciences, ISM: clouds, Luminosity, STAR-FORMATION, CLUMP IDENTIFICATION, symbols.namesake, surveys, 0103 physical sciences, Planck, GOULD BELT SURVEY, 010303 astronomy & astrophysics, James Clerk Maxwell Telescope, Solar and Stellar Astrophysics (astro-ph.SR), QC, QB, Physics, LEGACY SURVEY, Spiral galaxy, stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ATLASGAL, Astronomy and Astrophysics, Galactic plane, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, CLOUD, submillimetre: ISM, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], GAS, Astrophysics of Galaxies (astro-ph.GA), symbols, MILKY-WAY, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], COMPLETE SAMPLE
Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-um continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of $N_{H_{2}}$ $>$ 5 $\times$ 10$^{21}$ cm$^{-2}$. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other., 16 pages, 13 figures, 1 table. Accepted for publication in MNRAS

Published
2019
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6. SCUBA-2 Continuum Observations of Pre-protostellar Evolution - survey description and compact source catalogue

Author

Eden, D. J., Liu, Tie, Kim, Kee-Tae, Juvela, M., Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans, N. J., Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, M., Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. -E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhou, J., Zhu, L., Zuo, P., University of Helsinki, Department of Physics, and University of Helsinki, Particle Physics and Astrophysics

Subjects
LEGACY SURVEY, stars: formation, ATLASGAL, SPIRAL ARMS, 115 Astronomy, Space science, ISM: clouds, CLOUD, STAR-FORMATION, submillimetre: ISM, CLUMP IDENTIFICATION, surveys, GAS, MILKY-WAY, COMPLETE SAMPLE, GOULD BELT SURVEY
Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850 mu m continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353 GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having three or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of N-H2 > 5 x10(21) cm(-2). By positionally associating the SCOPE compact sources with young stellar objects, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other.

Published
2019

7. Detection of Interstellar Ortho-D2H+ with SOFIA

Author

University of Helsinki, Department of Physics, Harju, Jorma, Sipilä, Olli, Brunken, Sandra, Schlemmer, Stephan, Caselli, Paola, Juvela, Mika, Menten, Karl M., Stutzki, Juergen, Asvany, Oskar, Kaminski, Tomasz, Okada, Yoko, Higgins, Ronan, University of Helsinki, Department of Physics, Harju, Jorma, Sipilä, Olli, Brunken, Sandra, Schlemmer, Stephan, Caselli, Paola, Juvela, Mika, Menten, Karl M., Stutzki, Juergen, Asvany, Oskar, Kaminski, Tomasz, Okada, Yoko, and Higgins, Ronan

Abstract

We report on the detection of the ground-state rotational line of ortho-D2H+ at 1.477 THz (203 mu m) using the German REceiver for Astronomy at Terahertz frequencies (GREAT) on. board the Stratospheric Observatory For Infrared Astronomy (SOFIA). The line is seen in absorption against. far-infrared continuum from the protostellar binary IRAS 16293-2422 in Ophiuchus. The para-D2H+ line at 691.7 GHz was not detected with the APEX telescope toward this position. These D2H+ observations complement our previous detections of para-H2D+ and ortho-H2D+ using SOFIA and APEX. By modeling chemistry and radiative transfer in the dense core surrounding the protostars, we find that the ortho-D2H+ and para-H2D+ absorption features mainly originate in the cool (T <18 K) outer envelope of the core. In contrast, the ortho-H2D+ emission from the core is significantly absorbed by the ambient molecular cloud. Analyses of the combined D2H+ and H2D+ data result in an age estimate of similar to 5. x. 10(5) yr for the core, with an uncertainty of similar to 2. x. 10(5) yr. The core material has probably been pre-processed for another 5. x. 10(5) years in conditions corresponding to those in the ambient molecular cloud. The inferred timescale is more than 10 times the age of the embedded protobinary. The D2H+ and H2D+ ions have large and nearly equal total (ortho+ para) fractional abundances of similar to 10(-9) in the outer envelope. This confirms the central role of H-3 + in the deuterium chemistry in cool, dense gas, and adds support to the prediction of chemistry models that also D-3(+) should be abundant in these conditions.

Published
2017

8. Star Formation and Feedback: A Molecular Outflow-Prestellar Core Interaction in L1689N

Author

Laurent Pagani, Evelyne Roueff, C. M. Walmsley, Charlotte Vastel, F. F. S. van der Tak, Maryvonne Gerin, Dariusz C. Lis, H. A. Wootten, Astronomy, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France, Centre Etud Spatiale Rayonnements Toulouse, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, Astrophysics, INITIAL CONDITIONS, 01 natural sciences, IRAS 16293-2422, 0103 physical sciences, Protostar, PHYSICAL CONDITIONS, GOULD BELT SURVEY, PRE-STELLAR CORE, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], HERSCHEL, stars: formation, INTERSTELLAR-MEDIUM, 010308 nuclear & particles physics, Star formation, TRIPLY DEUTERATED AMMONIA, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM: molecules, Interstellar medium, Caltech Submillimeter Observatory, DEUTERIUM FRACTIONATION, 13. Climate action, Space and Planetary Science, techniques: interferometric, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, CLOUD CORES, Outflow, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Dust emission
Abstract

We present Herschel, ALMA Compact Array (ACA), and Caltech Submillimeter Observatory (CSO) observations of the prestellar core in L1689N, which has been suggested to be interacting with a molecular outflow driven by the nearby solar type protostar IRAS 16293-2422. This source is characterized by some of the highest deuteration levels seen in the interstellar medium. The change in the NH2D line velocity and width across the core provides clear evidence of an interaction with the outflow, traced by the high-velocity water emission. Quiescent, cold gas, characterized by narrow line widths is seen in the NE part of the core, while broader, more disturbed line profiles are seen in the W/SW part. Strong N2D+ and ND3 emission is detected with the ACA, extending S/SW from the peak of the single-dish NH2D emission. The ACA data also reveal the presence a compact dust continuum source, with a mean size of ~1100 au, a central density of (1-2) 10^7 cm-3, and a mass of 0.2-0.4 Msun. The dust emission peak is displaced ~5" to the south with respect to the N2D+ and ND3 emission, as well as the single-dish dust continuum peak, suggesting that the northern, quiescent part of the core is characterized by spatially extended continuum emission, which is resolved out by the interferometer. We see no clear evidence of fragmentation in this quiescent part of the core, which could lead to a second generation of star formation, although a weak dust continuum source is detected in this region in the ACA data., Accepted for publication in the Astrophysical Journal, 20 pages, 10 figures, 2 tables

Published
2016
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9. Deuteration of ammonia in the starless core Ophiuchus/H-MM1

Author

Erik Rosolowsky, Jaime E. Pineda, Olli Sipilä, Paola Caselli, Stephan Schlemmer, Anna Punanova, Jorma Harju, Philip C. Myers, Rachel Friesen, F. Daniel, Alexandre Faure, Rolf Güsten, Yancy L. Shirley, Claire Rist, Pierre Hily-Blant, Laurent Wiesenfeld, and Department of Physics

Subjects
NITROGEN HYDRIDES, Astrochemistry, PRE-PROTOSTELLAR COLLAPSE, FOS: Physical sciences, Astrophysics, MOLECULAR CLOUD, ISM: clouds, 01 natural sciences, ISM: abundances, PRESTELLAR CORES, RADIO-ASTRONOMICAL SPECTROSCOPY, 0103 physical sciences, GOULD BELT SURVEY, 010303 astronomy & astrophysics, Hyperfine structure, Physics, 010304 chemical physics, astrochemistry, European research, Molecular cloud, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, ISM: molecules, DARK CLOUDS, Core (optical fiber), DEUTERIUM FRACTIONATION, 13. Climate action, Space and Planetary Science, Extraterrestrial life, Astrophysics of Galaxies (astro-ph.GA), HYPERFINE-STRUCTURE, Ophiuchus, BONNOR-EBERT SPHERES
Abstract

Ammonia and its deuterated isotopologues probe physical conditions in dense molecular cloud cores. With the aim of testing the current understanding of the spin-state chemistry of these molecules, we observed spectral lines of NH3, NH2D, NHD2, ND3, and N2D+ towards a dense, starless core in Ophiuchus with the APEX, GBT, and IRAM 30-m telescopes. The observations were interpreted using a gas-grain chemistry model combined with radiative transfer calculations. The chemistry model distinguishes between the different nuclear spin states of light hydrogen molecules, ammonia, and their deuterated forms. High deuterium fractionation ratios with NH2D/NH3=0.4, NHD2/NH2D=0.2, and ND3/NHD2=0.06 were found in the core. The observed ortho/para ratios of NH2D and NHD2 are close to the corresponding nuclear spin statistical weights. The chemistry model can approximately reproduce the observed abundances, but predicts uniformly too low ortho/para-NH2D, and too large ortho/para-NHD2 ratios. The longevity of N2H+ and NH3 in dense gas, which is prerequisite to their strong deuteration, can be attributed to the chemical inertia of N2 on grain surfaces. The discrepancies between the chemistry model and the observations are likely to be caused by the fact that the model assumes complete scrambling in principal gas-phase deuteration reactions of ammonia, which means that all the nuclei are mixed in reactive collisions. If, instead, these reactions occur through proton hop/hydrogen abstraction processes, statistical spin ratios are to be expected. The present results suggest that while the deuteration of ammonia changes with physical conditions and time, the nuclear spin ratios of ammonia isotopologues do not probe the evolutionary stage of a cloud., Comment: to appear in Astronomy & Astrophysics

Published
2016
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10. Planck intermediate results XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Alves, M. I. R., Arnaud, M., Arzoumanian, D., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keskitalo, R., Kisner, T. S., Knoche, J., Kunz, M., Kurki-Suonio, H., Macías-Pérez, J. F., Tristram, M., Lagache, G., Lamarre, J. -M., Lasenby, A., Maffei, B., Battaner, E., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Tucci, M., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Benabed, K., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., VALENZIANO, LUCA, Moneti, A., Montier, L., MORGANTE, GIANLUCA, Mortlock, D., Munshi, D., Murphy, J. A., Benoit-Lévy, A., Naselsky, P., Nati, F., Natoli, P., Valiviita, J., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Pagano, L., Pajot, F., Bernard, J. -P., Paladini, R., PAOLETTI, DANIELA, Van Tent, B., Pasian, F., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Berné, O., Pointecouteau, E., Vielva, P., Polenta, G., Pratt, G. W., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Bersanelli, M., VILLA, FABRIZIO, RICCIARDI, SARA, Ristorcelli, I., Rocha, G., Rosset, C., ROSSETTI, MARIACHIARA, Roudier, G., Rubiño-Martín, J. A., Rusholme, B., SANDRI, MAURA, Savelainen, M., Wade, L. A., Bielewicz, P., Savini, G., Scott, D., Soler, J. D., Stolyarov, V., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., TERENZI, LUCA, Wandelt, B. D., Toffolatti, L., Bonaldi, A., Tomasi, M., Bonavera, L., Lawrence, C. R., Yvon, D., ZACCHEI, Andrea, Zonca, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., BURIGANA, CARLO, Calabrese, E., Leonardi, R., Cardoso, J. -F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Levrier, F., Crill, B. P., Curto, A., CUTTAIA, FRANCESCO, Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., De Rosa, A., de Zotti, G., Delabrouille, J., Liguori, M., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Lilje, P. B., Falgarone, E., Ferrière, K., FINELLI, FABIO, Forni, O., FRAILIS, Marco, Fraisse, A. A., FRANCESCHI, ENRICO, Frejsel, A., GALEOTTA, Samuele, Galli, S., Linden-Vørnle, M., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., GRUPPUSO, ALESSANDRO, Guillet, V., López-Caniego, M., Hansen, F. K., Hanson, D., Harrison, D. L., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Huffenberger, K. M., Lubin, P. M., Hurier, G., Ade, P, Aghanim, N, Alves, M, Arnaud, M, Arzoumanian, D, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Battaner, E, Benabed, K, Benoit-Lévy, A, Bernard, J, Berné, O, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bracco, A, Burigana, C, Calabrese, E, Cardoso, J, Catalano, A, Chamballu, A, Chiang, H, Christensen, P, Clements, D, Colombi, S, Colombo, L, Combet, C, Couchot, F, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Elsner, F, Enßlin, T, Eriksen, H, Falgarone, E, Ferrière, K, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Héraud, Y, Gjerløw, E, González-Nuevo, J, Górski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Hanson, D, Harrison, D, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Huffenberger, K, Hurier, G, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keskitalo, R, Kisner, T, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden-Vørnle, M, López-Caniego, M, Lubin, P, Macías-Pérez, J, Maffei, B, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martínez-González, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville-Deschênes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Nørgaard-Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Oppermann, N, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Pasian, F, Perrotta, F, Pettorino, V, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Pratt, G, Puget, J, Rachen, J, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ricciardi, S, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rubiño-Martín, J, Rusholme, B, Sandri, M, Savelainen, M, Savini, G, Scott, D, Soler, J, Stolyarov, V, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, L, Wandelt, B, Yvon, D, Zacchei, A, Zonca, A, Junta de Andalucía, European Space Agency, Centre National de la Recherche Scientifique (France), Istituto Nazionale di Astrofisica, Consejo Superior de Investigaciones Científicas (España), Ministerio de Economía y Competitividad (España), European Commission, European Research Council, National Aeronautics and Space Administration (US), Science and Technology Facilities Council (UK), Academy of Finland, Center for Science (Finland), Agenzia Spaziale Italiana, Department of Energy (US), UK Space Agency, Fundação para a Ciência e a Tecnologia (Portugal), Science Foundation Ireland, DTU Space (Denmark), Swiss Space Office, Max Planck Society, German Centre for Air and Space Travel, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), European Project: 267934,EC:FP7:ERC,ERC-2010-AdG_20100224,MISTIC(2011), Science and Technology Facilities Council (STFC), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Ade, P. A. R., Aghanim, N., Alves, M. I. R., Arnaud, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Berné, O., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Calabrese, E., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Guillet, V., Hansen, F. K., Hanson, D., Harrison, D. L., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keskitalo, R., Kisner, T. S., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Pratt, G. W., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ricciardi, S., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Savelainen, M., Savini, G., Scott, D., Soler, J. D., Stolyarov, V., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
010504 meteorology & atmospheric sciences, magnetic field [ISM], Astronomy, Astrophysics, 7. Clean energy, 01 natural sciences, IMAGING POLARIMETRY, Interstellar filaments, Protein filament, dust, extinction, ISM: magnetic fields, polarization, submillimeter: ISM, Astronomy and Astrophysics, Space and Planetary Science, PRESTELLAR CORES, Polarization, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), media_common, Physics, extinction, Polarization (waves), 3. Good health, Magnetic field, Physical Sciences, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], dust, Astrophysics::Earth and Planetary Astrophysics, dust, magnetic fields, turbulence [ISM], GRAIN ALIGNMENT, INFRARED POLARIMETRY, RADIATIVE TORQUES, media_common.quotation_subject, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy & Astrophysics, Intrinsic polarization, DARK-CLOUDS, STAR-FORMATION, NO, symbols.namesake, ISM: magnetic field, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Planck, ISM [submillimeter], GOULD BELT SURVEY, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ISM [Submillimetre], Science & Technology, magnetic fields [ISM], TAURUS MOLECULAR CLOUD, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, 0201 Astronomical And Space Sciences, Sky, Astrophysics of Galaxies (astro-ph.GA), SUPRATHERMAL ROTATION, Dust emission
Abstract

Interstellar and circumstellar matter.-- et al., Planck observations at 353 GHz provide the first fully sampled maps of the polarized dust emission towards interstellar filaments and their backgrounds (i.e., the emission observed in the surroundings of the filaments). The data allow us to determine the intrinsic polarization properties of the filaments and therefore to provide insight into the structure of their magnetic field (B). We present the polarization maps of three nearby (several parsecs long) star-forming filaments of moderate column density (NH about 1022 cm-2): Musca, B211, and L1506. These three filaments are detected above the background in dust total and polarized emission. We use the spatial information to separate Stokes I, Q, and U of the filaments from those of their backgrounds, an essential step in measuring the intrinsic polarization fraction (p) and angle (ψ) of each emission component. We find that the polarization angles in the three filaments (ψfil) are coherent along their lengths and not the same as in their backgrounds (ψbg). The differences between ψfil and ψbg are 12° and 54° for Musca and L1506, respectively, and only 6° in the case of B211. These differences forMusca and L1506 are larger than the dispersions of ψ, both along the filaments and in their backgrounds. The observed changes of ψ are direct evidence of variations of the orientation of the plane of the sky (POS) projection of the magnetic field. As in previous studies, we find a decrease of several per cent in p with NH from the backgrounds to the crest of the filaments. We show that the bulk of the drop in p within the filaments cannot be explained by random fluctuations of the orientation of the magnetic field because they are too small (σψ< 10°). We recognize the degeneracy between the dust alignment efficiency (by, e.g., radiative torques) and the structure of the B-field in causing variations in p, but we argue that the decrease in p from the backgrounds to the filaments results in part from depolarization associated with the 3D structure of the B-field: both its orientation in the POS and with respect to the POS. We do not resolve the inner structure of the filaments, but at the smallest scales accessible with Planck (~0.2 pc), the observed changes of ψ and p hold information on the magnetic field structure within filaments. They show that both the mean field and its fluctuations in the filaments are different from those of their backgrounds, which points to a coupling between the matter and the B-field in the filament formation process., The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.

Published
2016
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11. Dust spectrum and polarisation at 850 μm in the massive IRDC G035.39-00.33

Author

Juvela, Mika, Guillet, V., Liu, Tie, Ristorcelli, Isabelle, Pelkonen, Veli-Matti, Alina, Dana, Bronfman, Leonardo, Eden, David J., Kim, Kee Tae, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Malinen, Johanna, Micelotta, Elisabetta, Montillaud, Julien, Rawlings, Mark G., Sanhueza, Patricio, Soam, Archana, Traficante, Alessio, Ysard, Nathalie, Zhang, Chuan-Peng, Eden, David, Koch, Patrick, Rawlings, Mark, Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Department of Plant Biology [Carnegie] (DPB), Carnegie Institution for Science, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Liverpool John Moores University (LJMU), Academia Sinica, Div Life Sci, Lab Proteome Anal & Mol Physiol, Gyeongsang Natl Univ, University of Cologne, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of Hawai'i [Hilo], NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), Chinese Academy of Sciences [Beijing] (CAS), University of Helsinki, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Carnegie Institution for Science [Washington], Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, University of Helsinki-University of Helsinki, Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Department of Physics

Subjects
GRAIN ALIGNMENT, Opacity, RADIATIVE TORQUES, SCUBA-2 OBSERVATIONS, INFRARED OBSERVATIONS, Extinction (astronomy), FOS: Physical sciences, Context (language use), Astrophysics, MOLECULAR CLOUD, POLARIMETRY, ISM: clouds, 01 natural sciences, Molecular physics, Protein filament, DARK CLOUD, 0103 physical sciences, Radiative transfer, TAURUS, GOULD BELT SURVEY, 010303 astronomy & astrophysics, QC, ComputingMilieux_MISCELLANEOUS, QB, infrared: ISM, Physics, Spectral index, stars: formation, stars: protostars, extinction, 010308 nuclear & particles physics, Molecular cloud, MAGNETIC-FIELD, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Magnetic field, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, dust, extinction, dust, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The dust sub-millimetre polarisation of star-forming clouds carries information on dust and the role of magnetic fields in cloud evolution. With observations of a dense filamentary cloud G035.39-00.33, we aim to characterise the dust emission properties and the variations of the polarisation fraction. JCMT SCUBA-2/POL-2 data at 850um are combined with Planck 850um (353GHz) data to map polarisation fractions. With previous SCUBA-2 observations (450um and 850um) and Herschel data, the column densities are determined via modified blackbody fits and via radiative transfer modelling. Models are constructed to examine how the polarisation angles and fractions depend on potential magnetic field geometries and grain alignment. POL-2 data show clear changes in the magnetic field orientation. The filament has a peak column density of N(H2)~7 10^22 cm-2, a minimum dust temperature of T~12 K, and a mass of some 4300Msun for the area N(H2)> 5 10^21 cm-2. The estimated average value of the dust opacity spectral index is beta ~ 1.9. The ratio of sub-millimetre and J band optical depths is tau(250 um)/tau(J) ~ 2.5 10^-3, more than four times the typical values for diffuse medium. The polarisation fraction decreases as a function of column density to p ~ 1% in the central filament. Because of noise, the observed decrease of p(N) is significant only at N(H2)>2 10^22 cm-2. The observations suggest that the grain alignment is not constant. Although the data can be explained with a complete loss of alignment at densities above ~ 10^4 cm-3 or using the predictions of radiative torques alignment, the uncertainty of the field geometry and the spatial filtering of the SCUBA-2 data prevent strong conclusions. G035.39-00.33 shows strong signs of dust evolution and the low polarisation fraction is suggestive of a loss of polarised emission from its densest parts., accepted for publication in Astronomy and Astrophysics

Published
2018
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12. The TOP-SCOPE Survey of PGCCs: PMO and SCUBA-2 Observations of 64 PGCCs in the Second Galactic Quadrant

Author

Xiao-Lan Liu, A. Marston, Manash R. Samal, Patricio Sanhueza, Yuefang Wu, Tianwei Zhang, D. Alina, Di Li, Guang-Xing Li, Chang Won Lee, Tie Liu, David Eden, Chuan-Peng Zhang, Jun-Jie Wang, Paul F. Goldsmith, Mika Juvela, Ken'ichi Tatematsu, Jin-Long Xu, Ke Wang, Patrick M. Koch, Alessio Traficante, Jinghua Yuan, Jianjun Zhou, Pak Shing Li, L. V. Toth, Kee-Tae Kim, Department of Physics, and Doctoral Programme in Particle Physics and Universe Sciences

Subjects
Milky Way, ISM: structure, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, INITIAL CONDITIONS, 01 natural sciences, ISM: clouds, 114 Physical sciences, Virial theorem, symbols.namesake, Core formation, 0103 physical sciences, Gravitational collapse, Astrophysics::Solar and Stellar Astrophysics, PHYSICAL CONDITIONS, Planck, GOULD BELT SURVEY, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB, Physics, stars: formation, 010308 nuclear & particles physics, Star formation, Molecular cloud, Galactic quadrant, GIANT MOLECULAR CLOUD, FORMING CLUMPS, Astronomy and Astrophysics, 115 Astronomy, Space science, GRAVITATIONAL COLLAPSE, STELLAR CLUSTERS, Space and Planetary Science, symbols, dust, extinction, MASSIVE STAR-FORMATION, COMPLETE SAMPLE, INFRARED DARK CLOUDS
Abstract

In order to understand the initial conditions and early evolution of star formation in a wide range of Galactic environments, we carried out an investigation of 64 Planck Galactic cold clumps (PGCCs) in the second quadrant of the Milky Way. Using the 13CO and C18O J = 1-0 lines and 850 μm continuum observations, we investigated cloud fragmentation and evolution associated with star formation. We extracted 468 clumps and 117 cores from the 13CO line and 850 μm continuum maps, respectively. We made use of the Bayesian distance calculator and derived the distances of all 64 PGCCs. We found that in general, the mass-size plane follows a relation of m ̃ r 1.67. At a given scale, the masses of our objects are around 1/10 of that of typical Galactic massive star-forming regions. Analysis of the clump and core masses, virial parameters, densities, and mass- size relation suggests that the PGCCs in our sample have a low core formation efficiency (̃3.0%), and most PGCCs are likely low-mass star- forming candidates. Statistical study indicates that the 850 μm cores are more turbulent, more optically thick, and denser than the 13CO clumps for star formation candidates, suggesting that the 850 μm cores are likely more appropriate future star formation candidates than the 13CO clumps.

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