COMPLEX SCATTERED RADIATION FIELDS AND MULTIPLE MAGNETIC FIELDS IN THE PROTOSTELLAR CLUSTER IN NGC 2264
COMPLEX SCATTERED RADIATION FIELDS AND MULTIPLE MAGNETIC FIELDS IN THE PROTOSTELLAR CLUSTER IN NGC 2264
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DOI：
10.1088/0004-637x/741/1/35
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发表时间：
2011-08
期刊：
影响因子：
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通讯作者：
J. Kwon;M. Tamura;R. Kandori;N. Kusakabe;J. Hashimoto;Y. Nakajima;F. Nakamura;T. Nagayama;T. Nagata;J. Hough;M. Werner;P. Teixeira
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文献类型：
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作者：
J. Kwon;M. Tamura;R. Kandori;N. Kusakabe;J. Hashimoto;Y. Nakajima;F. Nakamura;T. Nagayama;T. Nagata;J. Hough;M. Werner;P. Teixeira
对麒麟座OB 1分子云中NGC 2264 IRS 2周围的原星团区域进行了J、H和Ks波段的近红外成像偏振测量。探测到了与NGC 2264 IRS 2和IRAS 12 S1核心有关的各种红外反射星云团（IRNC），以及局部红外反射星云（IRNe）。红外Ne的照明源被确定为已知或新的近红外和中红外源。此外，在所有三个波段中检测到314个点状源，并对其孔径偏振进行了研究。利用色图，红化场星和无盘前主序星被选择来追踪分子云的磁场（MF）结构。点源的偏振位置角在团核内为81° ± 29°，在团核周边为58° ± 24°，这可解释为MF在云观测区的天空投影方向。根据费米子-拉塞卡法的粗略估计，磁场强度约为100 μG。最近的数值模拟的集群形成的比较意味着云动力学控制的相对较强的MF。局部MF方向与IRAS 12 S1的CO流出方向有很好的相关性，并且与亚毫米偏振测量推断的方向一致。相反，本地MF方向大致垂直于银河MF方向。
Near-infrared imaging polarimetry in the J, H, and Ks bands has been carried out for the protostellar cluster region around NGC 2264 IRS 2 in the Monoceros OB1 molecular cloud. Various infrared reflection nebula clusters (IRNCs) associated with NGC 2264 IRS 2 and the IRAS 12 S1 core, as well as local infrared reflection nebulae (IRNe), were detected. The illuminating sources of the IRNe were identified with known or new near- and mid-infrared sources. In addition, 314 point-like sources were detected in all three bands and their aperture polarimetry was studied. Using a color–color diagram, reddened field stars and diskless pre-main-sequence stars were selected to trace the magnetic field (MF) structure of the molecular cloud. The mean polarization position angle of the point-like sources is 81° ± 29° in the cluster core, and 58° ± 24° in the perimeter of the cluster core, which is interpreted as the projected direction on the sky of the MF in the observed region of the cloud. The Chandrasekhar–Fermi method gives a rough estimate of the MF strength to be about 100 μG. A comparison with recent numerical simulations of the cluster formation implies that the cloud dynamics is controlled by the relatively strong MF. The local MF direction is well associated with that of CO outflow for IRAS 12 S1 and consistent with that inferred from submillimeter polarimetry. In contrast, the local MF direction runs roughly perpendicular to the Galactic MF direction.