论文标题
fildreams 2。应用四个赫歇尔场中细丝和磁场之间的相对方向的分析
FilDReaMS 2. Application to the analysis of the relative orientations between filaments and the magnetic field in four Herschel fields
论文作者
论文摘要
星际介质的模拟和观察结果都表明，对丝状结构和磁场之间的相对取向的研究可以使磁场在丝体形成和演化中所起的作用以及在恒星形成过程中所起的作用。我们提供了Fildreams的第一个应用，这是检测和分析细丝的新方法。我们的目标是研究检测到的丝和磁场之间的相对方向。我们将fildreams应用于以不同的银河环境和进化阶段为特征的四个Herschel场（G210，G300，G82，G202）的样本。首先，我们检查由不同条形宽度及其分层组织的细丝形成的网络。其次，我们将灯丝取向与从普朗克极化数据推断出的磁场方向，并首次将相对方向角的统计数据作为空间尺度和$ {\ rm H_2} $列列密度的函数。我们发现在四个Herschel场中的优先相对取向：低柱密度的小细丝比垂直于磁场的小丝略微平行，而大丝（高柱密度）的定向几乎垂直（或者在G202的情况下，几乎平行于G202）。在附近的两个田地（G210和G300）中，我们观察到从大部分平行到垂直的过渡，以$ n _ {\ rm H_2} \ simeq 1.1 $和$ 1.4 \ times10^{21}} \，$ cm $ $ cm $^{ - 2} $，分别与以前的研究相分为一致的研究。我们的结果证实了云尺度和细丝在较小尺度的磁场之间存在耦合。他们还说明了结合Herschel和Planck观察的潜力，并呼吁使用我们的专用方法进行进一步的统计分析。
Both simulations and observations of the interstellar medium show that the study of the relative orientations between filamentary structures and the magnetic field can bring new insight into the role played by magnetic fields in the formation and evolution of filaments and in the process of star formation. We provide a first application of FilDReaMS, the new method to detect and analyze filaments. Our goal is to investigate the relative orientations between the detected filaments and the magnetic field. We apply FilDReaMS to a sample of four Herschel fields (G210, G300, G82, G202) characterized by different Galactic environments and evolutionary stages. First, we examine the networks formed by filaments of different bar widths as well as their hierarchical organization. Second, we compare the filament orientations to the magnetic field orientation inferred from Planck polarization data and, for the first time, we study the statistics of the relative orientation angle as functions of both spatial scale and ${\rm H_2}$ column density. We find preferential relative orientations in the four Herschel fields: small filaments with low column densities are slightly more parallel than perpendicular to the magnetic field, while large filaments (higher column densities) are oriented nearly perpendicular (or, in the case of G202, nearly parallel). In the two nearby fields (G210 and G300), we observe a transition from mostly parallel to mostly perpendicular at an $N_{\rm H_2} \simeq 1.1$ and $1.4\times10^{21}\,$cm$^{-2}$, respectively, consistent with the results of previous studies. Our results confirm the existence of a coupling between magnetic fields at cloud scales and filaments at smaller scale. They also illustrate the potential of combining Herschel and Planck observations, and they call for further statistical analyses with our dedicated method.
