Probing the role of magnetic fields in star-forming filaments: NIKA2-Pol commissioning results toward OMC-1
Probing the role of magnetic fields in star-forming filaments: NIKA2-Pol commissioning results toward OMC-1
复制标题
DOI：
10.1051/epjconf/202225700002
复制
发表时间：
2021-11
影响因子：
--
通讯作者：
H. Ajeddig;R. Adam;P. Ade;P. Andr'e;E. Artis;H. Aussel;A. Beelen;A. Benoit;S. Berta;L. Bing;O. Bourrion;M. Calvo;A. Catalano;M. Petris;F. D'esert;S. Doyle;E. Driessen;A. Gomez;J. Goupy;F. K'eruzor'e;C. Kramer;B. Ladjelate;G. Lagache;S. Leclercq;J. Lestrade;J. Mac'ias-P'erez;A. Maury;P. Mauskopf;F. Mayet;A. Monfardini;M. Munoz-Echeverr'ia;L. Perotto;G. Pisano;N. Ponthieu;V.Rev'eret;A. Rigby;A. Ritacco;C. Romero;H. Roussel;F. Ruppin;K. Schuster;S. Shu;A. Sievers;C. Tucker;R. Zylka;Y. Shimajiri
中科院分区：
文献类型：
--
作者：
H. Ajeddig;R. Adam;P. Ade;P. Andr'e;E. Artis;H. Aussel;A. Beelen;A. Benoit;S. Berta;L. Bing;O. Bourrion;M. Calvo;A. Catalano;M. Petris;F. D'esert;S. Doyle;E. Driessen;A. Gomez;J. Goupy;F. K'eruzor'e;C. Kramer;B. Ladjelate;G. Lagache;S. Leclercq;J. Lestrade;J. Mac'ias-P'erez;A. Maury;P. Mauskopf;F. Mayet;A. Monfardini;M. Munoz-Echeverr'ia;L. Perotto;G. Pisano;N. Ponthieu;V.Rev'eret;A. Rigby;A. Ritacco;C. Romero;H. Roussel;F. Ruppin;K. Schuster;S. Shu;A. Sievers;C. Tucker;R. Zylka;Y. Shimajiri
尘埃偏振观测是探测恒星形成区域磁场几何形状(在某种程度上也是磁场强度)的强大而实用的工具。特别是，普朗克极化数据揭示了分子云中大尺度磁场的重要性。然而，由于分辨率不足，普朗克观测无法在恒星前和原恒星尺度上约束B场几何。NIKA2-POL1.15 mm偏振成像提供了11.7角秒的高角度分辨率，相当于猎户座分子云(OMC)距离的0.02pc，这使得我们有可能推进对恒星形成细丝和致密核中B场形态的理解(IRAM 30M大程序B-FUN)。NIKA2-POL仪器的调试带来了几个具有挑战性的问题，特别是仪器极化或强度-极化“泄漏”效应。在这篇文章中，我们说明了如何纠正这种影响，从而在结构化的、可扩展的源(如OMC-1)中产生可靠的可利用数据。我们给出了NIKA2-POL和SCUBA2-Pol2在OMC-1区域的统计比较结果。我们还提出了猎户座-KL附近B场线局部收缩的初步证据，表现为一种新的小尺度沙漏图案，以及其他仪器如Pol2已经看到的更大尺度的沙漏。
Dust polarization observations are a powerful, practical tool to probe the geometry (and to some extent, the strength) of magnetic fields in starforming regions. In particular, Planck polarization data have revealed the importance of magnetic fields on large scales in molecular clouds. However, due to insufficient resolution, Planck observations are unable to constrain the B-field geometry on prestellar and protostellar scales. The high angular resolution of 11.7 arcsec provided by NIKA2-Pol 1.15 mm polarimetric imaging, corresponding to 0.02 pc at the distance of the Orion molecular cloud (OMC), makes it possible to advance our understanding of the B-field morphology in star-forming filaments and dense cores (IRAM 30m large program B-FUN). The commissioning of the NIKA2-Pol instrument has led to several challenging issues, in particular, the instrumental polarization or intensity-to-polarization “leakage” effect. In the present paper, we illustrate how this effect can be corrected for, leading to reliable exploitable data in a structured, extended source such as OMC-1. We present a statistical comparison between NIKA2-Pol and SCUBA2-Pol2 results in the OMC-1 region. We also present tentative evidence of local pinching of the B-field lines near Orion-KL, in the form of a new small-scale hourglass pattern, in addition to the larger-scale hourglass already seen by other instruments such as Pol2.