The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region
The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region
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DOI：
10.3847/1538-4357/ab1b23
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发表时间：
2019-04
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影响因子：
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通讯作者：
S. Coud'e;P. Bastien;M. Houde;S. Sadavoy;R. Friesen;J. Francesco;D. Johnstone;S. Mairs;T. Hasegawa;W. Kwon;S. Lai;K. Qiu;D. Ward-Thompson;D. Berry;M. C. Chen;J. Fiege;E. Franzmann;J. Hatchell;K. Lacaille;B. Matthews;G. Moriarty-Schieven;A. Pon;P. Andr'e;D. Arzoumanian;Yusuke Aso;D. Byun;Eswaraiah Chakali;H. Chen;W. Chen;T. Ching;Jungyeon Cho;Minho Choi;A. Chrysostomou;E. Chung;Y. Doi;E. Drabek-Maunder;C. Dowell;S. Eyres;S. Falle;P. Friberg;G. Fuller;R. Furuya;T. Gledhill;S. Graves;J. Greaves;M. Griffin;Q. Gu;S. Hayashi;Thiem C. Hoang;W. Holland;T. Inoue;S. Inutsuka;K. Iwasaki;Il-Gyo Jeong;Yoshihiro Kanamori;A. Kataoka;Ji-hyun Kang;Miju Kang;Sung-ju Kang;K. Kawabata;F. Kemper;Gwanjeong Kim;Jongsoo Kim;Kee-Tae Kim;K. Kim;Mi-Ryang Kim;Shinyoung Kim;J. Kirk;Masato I. N. Kobayashi;P. Koch;J. Kwon;Jeong-Eun Lee;C. Lee;Sang-Sung Lee;Da-lei Li;Di Li;Hua-b. Li;Hongli Liu;Junhao Liu;Sheng-Yuan Liu;Tie Liu;S. Loo;A. Lyo;M. Matsumura;T. Nagata;F. Nakamura;H. Nakanishi;N. Ohashi;T. Onaka;H. Parsons;K. Pattle;N. Peretto;T. Pyo;L. Qian;R. Rao;M. Rawlings;B. Retter;J. Richer;A. Rigby;J. Robitaille;H. Saito;G. Savini;A. Scaife;M. Seta;H. Shinnaga;A. Soam;M. Tamura;Ya-wen Tang;K. Tomisaka;Y. Tsukamoto;Hongchi Wang;Jia‐Wei Wang;A. Whitworth;Hsi-Wei Yen;H. Yoo;Jinghua Yuan;T. Zenko;Chuan-peng Zhang;Guoyin Zhang;Jianjun Zhou;Lei Zhu
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文献类型：
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作者：
S. Coud'e;P. Bastien;M. Houde;S. Sadavoy;R. Friesen;J. Francesco;D. Johnstone;S. Mairs;T. Hasegawa;W. Kwon;S. Lai;K. Qiu;D. Ward-Thompson;D. Berry;M. C. Chen;J. Fiege;E. Franzmann;J. Hatchell;K. Lacaille;B. Matthews;G. Moriarty-Schieven;A. Pon;P. Andr'e;D. Arzoumanian;Yusuke Aso;D. Byun;Eswaraiah Chakali;H. Chen;W. Chen;T. Ching;Jungyeon Cho;Minho Choi;A. Chrysostomou;E. Chung;Y. Doi;E. Drabek-Maunder;C. Dowell;S. Eyres;S. Falle;P. Friberg;G. Fuller;R. Furuya;T. Gledhill;S. Graves;J. Greaves;M. Griffin;Q. Gu;S. Hayashi;Thiem C. Hoang;W. Holland;T. Inoue;S. Inutsuka;K. Iwasaki;Il-Gyo Jeong;Yoshihiro Kanamori;A. Kataoka;Ji-hyun Kang;Miju Kang;Sung-ju Kang;K. Kawabata;F. Kemper;Gwanjeong Kim;Jongsoo Kim;Kee-Tae Kim;K. Kim;Mi-Ryang Kim;Shinyoung Kim;J. Kirk;Masato I. N. Kobayashi;P. Koch;J. Kwon;Jeong-Eun Lee;C. Lee;Sang-Sung Lee;Da-lei Li;Di Li;Hua-b. Li;Hongli Liu;Junhao Liu;Sheng-Yuan Liu;Tie Liu;S. Loo;A. Lyo;M. Matsumura;T. Nagata;F. Nakamura;H. Nakanishi;N. Ohashi;T. Onaka;H. Parsons;K. Pattle;N. Peretto;T. Pyo;L. Qian;R. Rao;M. Rawlings;B. Retter;J. Richer;A. Rigby;J. Robitaille;H. Saito;G. Savini;A. Scaife;M. Seta;H. Shinnaga;A. Soam;M. Tamura;Ya-wen Tang;K. Tomisaka;Y. Tsukamoto;Hongchi Wang;Jia‐Wei Wang;A. Whitworth;Hsi-Wei Yen;H. Yoo;Jinghua Yuan;T. Zenko;Chuan-peng Zhang;Guoyin Zhang;Jianjun Zhou;Lei Zhu
我们展示了来自詹姆斯·克拉克·麦克斯韦望远镜的恒星形成区磁场观测（B-fields In STar-forming Region Observations，简称BISTRO）项目中，英仙座分子云复合体中巴纳德1团块在850μm波段的POL - 2线偏振图。我们发现偏振率随总强度呈下降趋势，我们将其与朝向云的高密度区域的消偏振效应相关联。然后，我们利用850μm波段的偏振数据来推断巴纳德1中大规模磁场的天空平面取向。该磁场在大部分云团中呈南北走向，但在B1 - c区域除外，在那里它更偏向东西走向。根据偏振角的离散度，我们计算出云内的湍流相关长度为5.0±2.″5（1500天文单位），湍流与总磁场能量之比为0.5±0.3。我们将这个湍流与总磁场能量之比与来自绿岸氨巡天（Green Bank Ammonia Survey）的NH₃分子谱线观测结果相结合，通过戴维斯 - 钱德拉塞卡 - 费米方法来估算磁场天空平面分量的强度。天空平面振幅为120±60μG，临界标准λc = 3.0±1.5，我们发现巴纳德1是一个超临界分子云，其磁场几乎由湍流分量主导。
We present the POL-2 850 μm linear polarization map of the Barnard 1 clump in the Perseus molecular cloud complex from the B-fields In STar-forming Region Observations survey at the James Clerk Maxwell Telescope. We find a trend of decreasing polarization fraction as a function of total intensity, which we link to depolarization effects toward higher-density regions of the cloud. We then use the polarization data at 850 μm to infer the plane-of-sky orientation of the large-scale magnetic field in Barnard 1. This magnetic field runs north–south across most of the cloud, with the exception of B1-c, where it turns more east–west. From the dispersion of polarization angles, we calculate a turbulence correlation length of 5.0 ± 2.″5 (1500 au) and a turbulent-to-total magnetic energy ratio of 0.5 ± 0.3 inside the cloud. We combine this turbulent-to-total magnetic energy ratio with observations of NH3 molecular lines from the Green Bank Ammonia Survey to estimate the strength of the plane-of-sky component of the magnetic field through the Davis–Chandrasekhar–Fermi method. With a plane-of-sky amplitude of 120 ± 60 μG and a criticality criterion λc = 3.0 ± 1.5, we find that Barnard 1 is a supercritical molecular cloud with a magnetic field nearly dominated by its turbulent component.