B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main
B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main
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DOI：
10.3847/1538-4357/ac4bbe
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发表时间：
2022-01
期刊：
影响因子：
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通讯作者：
W. Kwon;K. Pattle;S. Sadavoy;C. Hull;D. Johnstone;D. Ward-Thompson;J. Francesco;P. Koch;R. Furuya;Y. Doi;Valentin J. M. Le Gouellec;J. Hwang;A. Lyo;A. Soam;Xindi Tang;T. Hoang;F. Kirchschlager;C. Eswaraiah;L. Fanciullo;K. Kim;T. Onaka;V. Könyves;Ji-hyun Kang;Chang Won 창원 Lee 이;Motohide Tamura;P. Bastien;Tetsuo 川哲夫 Hasegawa 長谷;S. Lai;K. Qiu;D. Berry;D. Arzoumanian;T. Bourke;D. Byun;W. Chen;H. Chen;Mike Chen;Zhiwei Chen;Tao-Chung 道沖 Ching 慶;Jungyeon Cho;Yunhee Choi;Minho Choi;A. Chrysostomou;E. Chung;S. Coudé;S. Dai;P. Diep;Y. Duan;H. Duan;D. Eden;J. Fiege;L. Fissel;E. Franzmann;P. Friberg;R. Friesen;G. Fuller;T. Gledhill;S. Graves;J. Greaves;M. Griffin;Q. Gu;I. Han;J. Hatchell;S. Hayashi;M. Houde;T. Inoue;S. Inutsuka;K. Iwasaki;Il-Gyo Jeong;Miju Kang;J. Karoly;A. Kataoka;K. Kawabata;F. Kemper;Kee-Tae Kim;Gwanjeong Kim;Mi-Ryang Kim;Shinyoung Kim;Jongsoo Kim;J. Kirk;Masato I. N. Kobayashi;Takayoshi Kusune;J. Kwon;K. Lacaille;C. Law;Chin-Fei Lee;Yong-Hee Lee;Hyeseung Lee;Jeong-Eun Lee;Sang-Sung Lee;Da-lei Li;Di Li;Hua-b. Li;S. Lin 林;Sheng-Yuan Liu;Hongli Liu;J. Liu 刘;T. Liu 刘;Xing Lu;S. Mairs;Masafumi 雅文 Matsumura 松村;B. Matthews;G. Moriarty-Schieven;T. Nagata;F. Nakamura;H. Nakanishi;N. B. Ngoc;N. Ohashi;Geumsook Park;H. Parsons;N. Peretto;F. Priestley;T. Pyo;L. Qian;R. Rao;J. Rawlings;M. Rawlings;B. Retter;J. Richer;A. Rigby;H. Saito;G. Savini;M. Seta;Y. Shimajiri;H. Shinnaga;M. Tahani;Ya-wen Tang;K. Tomisaka;L. Tram;Y. Tsukamoto;S. Viti;Hongchi Wang;Jia-Wei Wang;A. Whitworth;Jin-An Wu;Jinjin 津津 Xie 謝;Hsi-Wei Yen;H. Yoo;Jinghua Yuan;H. Yun;T. Zenko;Yapeng Zhang;Chuan-peng Zhang;Guo-Yin Zhang;Jianjun Zhou;Lei Zhu;I. D. Looze;Philippe André;C. Dowell;S. Eyres;S. Falle;J. Robitaille;S. Loo
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文献类型：
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作者：
W. Kwon;K. Pattle;S. Sadavoy;C. Hull;D. Johnstone;D. Ward-Thompson;J. Francesco;P. Koch;R. Furuya;Y. Doi;Valentin J. M. Le Gouellec;J. Hwang;A. Lyo;A. Soam;Xindi Tang;T. Hoang;F. Kirchschlager;C. Eswaraiah;L. Fanciullo;K. Kim;T. Onaka;V. Könyves;Ji-hyun Kang;Chang Won 창원 Lee 이;Motohide Tamura;P. Bastien;Tetsuo 川哲夫 Hasegawa 長谷;S. Lai;K. Qiu;D. Berry;D. Arzoumanian;T. Bourke;D. Byun;W. Chen;H. Chen;Mike Chen;Zhiwei Chen;Tao-Chung 道沖 Ching 慶;Jungyeon Cho;Yunhee Choi;Minho Choi;A. Chrysostomou;E. Chung;S. Coudé;S. Dai;P. Diep;Y. Duan;H. Duan;D. Eden;J. Fiege;L. Fissel;E. Franzmann;P. Friberg;R. Friesen;G. Fuller;T. Gledhill;S. Graves;J. Greaves;M. Griffin;Q. Gu;I. Han;J. Hatchell;S. Hayashi;M. Houde;T. Inoue;S. Inutsuka;K. Iwasaki;Il-Gyo Jeong;Miju Kang;J. Karoly;A. Kataoka;K. Kawabata;F. Kemper;Kee-Tae Kim;Gwanjeong Kim;Mi-Ryang Kim;Shinyoung Kim;Jongsoo Kim;J. Kirk;Masato I. N. Kobayashi;Takayoshi Kusune;J. Kwon;K. Lacaille;C. Law;Chin-Fei Lee;Yong-Hee Lee;Hyeseung Lee;Jeong-Eun Lee;Sang-Sung Lee;Da-lei Li;Di Li;Hua-b. Li;S. Lin 林;Sheng-Yuan Liu;Hongli Liu;J. Liu 刘;T. Liu 刘;Xing Lu;S. Mairs;Masafumi 雅文 Matsumura 松村;B. Matthews;G. Moriarty-Schieven;T. Nagata;F. Nakamura;H. Nakanishi;N. B. Ngoc;N. Ohashi;Geumsook Park;H. Parsons;N. Peretto;F. Priestley;T. Pyo;L. Qian;R. Rao;J. Rawlings;M. Rawlings;B. Retter;J. Richer;A. Rigby;H. Saito;G. Savini;M. Seta;Y. Shimajiri;H. Shinnaga;M. Tahani;Ya-wen Tang;K. Tomisaka;L. Tram;Y. Tsukamoto;S. Viti;Hongchi Wang;Jia-Wei Wang;A. Whitworth;Jin-An Wu;Jinjin 津津 Xie 謝;Hsi-Wei Yen;H. Yoo;Jinghua Yuan;H. Yun;T. Zenko;Yapeng Zhang;Chuan-peng Zhang;Guo-Yin Zhang;Jianjun Zhou;Lei Zhu;I. D. Looze;Philippe André;C. Dowell;S. Eyres;S. Falle;J. Robitaille;S. Loo
作为恒星形成区B场观测调查的一部分，我们使用詹姆斯·克拉克麦克斯韦望远镜上的POL-2偏振计对巨蛇座主分子云进行了850 μm偏振观测。这些观测探测了巨蛇座主分子云在大约6000 Au尺度上的磁场形态，该分子云由具有不同物理性质（如密度和星星形成活动）的核心和六个细丝组成。利用相对取向直方图（HRO）技术，我们发现在NH 2 <0.93×1022 cm−2的低密度星系结构中，磁场平行于细丝（磁场垂直于密度梯度），而在具有星星形成活动的致密星系结构中，磁场垂直于细丝（磁场平行于密度梯度）。此外，将HRO技术应用于更致密的核心区域，我们发现磁场方向在NH 2 = 4.6×1022 cm−2处再次变为垂直于密度梯度。这可以解释为核心形成的标志。在NH 2 = 16×1022 cm−2时，磁场又变回平行于密度梯度，这可以理解为是由于磁场被下落的物质拉入。此外，我们还用Davis-Brachasekhar-Fermi方法估算了暗条的磁场强度（B POS = 60-300 μG），并根据磁场和湍流能量密度讨论了暗条是否是引力不稳定的.
We present 850 μm polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope as part of the B-fields In STar-forming Region Observations survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less-dense filamentary structures where NH2<0.93×1022 cm−2 (magnetic fields perpendicular to density gradients), while they are perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at NH2≈4.6×1022 cm−2. This can be interpreted as a signature of core formation. At NH2≈16×1022 cm−2, magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments (B POS = 60–300 μG)) using the Davis–Chandrasekhar–Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities.