Magnetic Fields toward Ophiuchus-B Derived from SCUBA-2 Polarization Measurements
Magnetic Fields toward Ophiuchus-B Derived from SCUBA-2 Polarization Measurements
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DOI：
10.3847/1538-4357/aac4a6
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发表时间：
2018-05
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通讯作者：
A. Soam;K. Pattle;D. Ward-Thompson;C. Lee;S. Sadavoy;P. Koch;Gwanjeong Kim;J. Kwon;W. Kwon;D. Arzoumanian;D. Berry;Thiem C. Hoang;M. Tamura;Sang-Sung Lee;Tie Liu;Kee-Tae Kim;D. Johnstone;F. Nakamura;A. Lyo;T. Onaka;Jongsoo Kim;R. Furuya;T. Hasegawa;S. Lai;P. Bastien;E. Chung;Shinyoung Kim;H. Parsons;M. Rawlings;S. Mairs;S. Graves;J. Robitaille;Hongli Liu;A. Whitworth;C. Eswaraiah;R. Rao;H. Yoo;M. Houde;Ji-hyun Kang;Y. Doi;Minho Choi;Miju Kang;S. Coudé;Hua-b. Li;M. Matsumura;B. Matthews;A. Pon;J. Francesco;S. Hayashi;K. Kawabata;S. Inutsuka;K. Qiu;E. Franzmann;P. Friberg;J. Greaves;J. Kirk;Di Li;H. Shinnaga;S. Loo;Yusuke Aso;D. Byun;H. Chen;Mike Chen;W. Chen;T. Ching;Jungyeon Cho;A. Chrysostomou;E. Drabek-Maunder;S. Eyres;J. Fiege;R. Friesen;G. Fuller;T. Gledhill;M. Griffin;Q. Gu;J. Hatchell;W. Holland;T. Inoue;K. Iwasaki;Il-Gyo Jeong;Sung-ju Kang;F. Kemper;K. Kim;Mi-Ryang Kim;K. Lacaille;Jeong-Eun Lee;Da-lei Li;Junhao Liu;Sheng-Yuan Liu;G. Moriarty-Schieven;H. Nakanishi;N. Ohashi;N. Peretto;T. Pyo;L. Qian;B. Retter;J. Richer;A. Rigby;G. Savini;A. Scaife;Ya-wen Tang;K. Tomisaka;Hongchi Wang;Jia‐Wei Wang;Hsi-Wei Yen;Jinghua Yuan;Chuan-peng Zhang;Guoyin Zhang;Jianjun Zhou;Lei Zhu;P. Andre';C. Dowell;S. Falle;Y. Tsukamoto;Yoshihiro Kanamori;A. Kataoka;Masato I. N. Kobayashi;T. Nagata;H. Saito;M. Seta;J. Hwang;I. Han;Hyeseung Lee;T. Zenko
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文献类型：
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作者：
A. Soam;K. Pattle;D. Ward-Thompson;C. Lee;S. Sadavoy;P. Koch;Gwanjeong Kim;J. Kwon;W. Kwon;D. Arzoumanian;D. Berry;Thiem C. Hoang;M. Tamura;Sang-Sung Lee;Tie Liu;Kee-Tae Kim;D. Johnstone;F. Nakamura;A. Lyo;T. Onaka;Jongsoo Kim;R. Furuya;T. Hasegawa;S. Lai;P. Bastien;E. Chung;Shinyoung Kim;H. Parsons;M. Rawlings;S. Mairs;S. Graves;J. Robitaille;Hongli Liu;A. Whitworth;C. Eswaraiah;R. Rao;H. Yoo;M. Houde;Ji-hyun Kang;Y. Doi;Minho Choi;Miju Kang;S. Coudé;Hua-b. Li;M. Matsumura;B. Matthews;A. Pon;J. Francesco;S. Hayashi;K. Kawabata;S. Inutsuka;K. Qiu;E. Franzmann;P. Friberg;J. Greaves;J. Kirk;Di Li;H. Shinnaga;S. Loo;Yusuke Aso;D. Byun;H. Chen;Mike Chen;W. Chen;T. Ching;Jungyeon Cho;A. Chrysostomou;E. Drabek-Maunder;S. Eyres;J. Fiege;R. Friesen;G. Fuller;T. Gledhill;M. Griffin;Q. Gu;J. Hatchell;W. Holland;T. Inoue;K. Iwasaki;Il-Gyo Jeong;Sung-ju Kang;F. Kemper;K. Kim;Mi-Ryang Kim;K. Lacaille;Jeong-Eun Lee;Da-lei Li;Junhao Liu;Sheng-Yuan Liu;G. Moriarty-Schieven;H. Nakanishi;N. Ohashi;N. Peretto;T. Pyo;L. Qian;B. Retter;J. Richer;A. Rigby;G. Savini;A. Scaife;Ya-wen Tang;K. Tomisaka;Hongchi Wang;Jia‐Wei Wang;Hsi-Wei Yen;Jinghua Yuan;Chuan-peng Zhang;Guoyin Zhang;Jianjun Zhou;Lei Zhu;P. Andre';C. Dowell;S. Falle;Y. Tsukamoto;Yoshihiro Kanamori;A. Kataoka;Masato I. N. Kobayashi;T. Nagata;H. Saito;M. Seta;J. Hwang;I. Han;Hyeseung Lee;T. Zenko
我们提出的尘埃排放偏振测量的Ophiuchus-B（Oph-B）进行使用的亚毫米波公共用户测辐射热仪阵列2（SCUBA-2）相机及其相关的偏振计（POL-2）的詹姆斯克拉克麦克斯韦望远镜在夏威夷的结果。这项工作是恒星形成区观测调查中的B场的一部分，该调查旨在了解磁场在附近恒星形成分子云的星星形成中的作用。我们提出了第一次看在Oph-B的磁场的几何形状和强度。在100.2pc上追踪场几何形状，清楚地检测到Oph-B的两个子块。场模式在子丛Oph-B1中出现显著紊乱。Oph-B2中的场几何形状更有序，倾向于沿着团块的主轴，平行于团块所在的沉积结构。在两个子块中，偏振度朝向致密的芯材料系统地减小。低密度材料沿着周边的磁力线与近红外偏振观测探测到的大尺度磁场平滑地结合在一起。我们使用Davis-Erasekhar-Fermi分析估计Oph-B2子团的磁场强度为630 ± 410 μG。在此磁场强度下，我们发现质量通量比λ = 1.6 ± 1.1，这表明Oph-B2团簇是轻微的磁超临界。
We present the results of dust emission polarization measurements of Ophiuchus-B (Oph-B) carried out using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) camera with its associated polarimeter (POL-2) on the James Clerk Maxwell Telescope in Hawaii. This work is part of the B-fields in Star-forming Region Observations survey initiated to understand the role of magnetic fields in star formation for nearby star-forming molecular clouds. We present a first look at the geometry and strength of magnetic fields in Oph-B. The field geometry is traced over ∼0.2 pc, with clear detection of both of the sub-clumps of Oph-B. The field pattern appears significantly disordered in sub-clump Oph-B1. The field geometry in Oph-B2 is more ordered, with a tendency to be along the major axis of the clump, parallel to the filamentary structure within which it lies. The degree of polarization decreases systematically toward the dense core material in the two sub-clumps. The field lines in the lower density material along the periphery are smoothly joined to the large-scale magnetic fields probed by NIR polarization observations. We estimated a magnetic field strength of 630 ± 410 μG in the Oph-B2 sub-clump using a Davis–Chandrasekhar–Fermi analysis. With this magnetic field strength, we find a mass-to-flux ratio λ = 1.6 ± 1.1, which suggests that the Oph-B2 clump is slightly magnetically supercritical.