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arXiv 1507.03310astro-ph.GA
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首次探测到射电大AGN的350微米偏振

First Detection of 350 Micron Polarization From a Radio-loud AGN

Sang-Sung Lee, Sincheol Kang, Do-Young Byun, Nicholas Chapman, Giles Novak, Sascha Trippe, Juan Carlos Algaba, Motoki Kino

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9 pages, 3 figures, 2 tables, ApJ Letter in press
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摘要：

我们报告的第一次检测到的线性偏振发射在350 $μ$米的观测波长从无线电响亮的活动星系核3C 279。我们在2014年3月13日和14日使用加州理工学院亚毫米波天文台的SHARP偏振仪对3C 279进行了偏振观测。首次探测到线偏振，偏振度为13.3 $\pm$ 3.4（$3.9σ$），电矢量位置角（EVPA）为34.7 $^\circ\pm5.6^\circ$。我们还在2014年3月6日（单碟）与韩国甚长基线干涉测量（VLBI）网络在13，7和3.5 mm双偏振下同时观测了3C~279，并在3月22日（VLBI）在13，7，3.5和2.3 mm下以毫角秒（mas）尺度成像。我们发现，在13 mm ~ 350 $μ$ m范围内，线偏振度从10%增加到13%，并且在质量尺度上，在$<10^\circ$范围内，所有观测频率下的EVPA都平行于喷流方向，这意味着在最里面的区域，积分磁场垂直于喷流方向。我们还发现，法拉第旋转措施RM是在一个范围内的$-6.5\times10^2 \sim -2.7\times10^3$ rad m $^{-2}$之间的13和3.5毫米，并缩放为波长的函数：$|{\rm RM}|\proptoλ^{-2.2}$。这些结果表明，在1~mas尺度范围内，致密射流中产生了毫米和亚毫米偏振辐射，并受到射流中或射流附近法拉第屏的影响。

英文摘要：

We report the first detection of linearly polarized emission at an observing wavelength of 350 $μ$m from the radio-loud Active Galactic Nucleus 3C 279. We conducted polarization observations for 3C 279 using the SHARP polarimeter in the Caltech Submillimeter Observatory on 2014 March 13 and 14. For the first time, we detected the linear polarization with the degree of polarization of 13.3\%$\pm$3.4\% ($3.9σ$) and the Electric Vector Position Angle (EVPA) of 34.7$^\circ\pm5.6^\circ$. We also observed 3C~279 simultaneously at 13, 7, and 3.5 mm in dual polarization with the Korean very long baseline interferometry (VLBI) Network on 2014 March 6 (single dish) and imaged in milliarcsecond (mas) scales at 13, 7, 3.5, and 2.3 mm on March 22 (VLBI). We found that the degree of linear polarization increases from 10\% to 13\% at 13 mm to 350 $μ$m and the EVPAs at all observing frequencies are parallel within $<10^\circ$ to the direction of the jet at mas scale, implying that the integrated magnetic fields are perpendicular to the jet in the innermost regions. We also found that the Faraday rotation measures RM are in a range of $-6.5\times10^2 \sim -2.7\times10^3$ rad m$^{-2}$ between 13 and 3.5 mm, and are scaled as a function of wavelength: $|{\rm RM}|\proptoλ^{-2.2}$. These results indicate that the mm and sub-mm polarization emission are generated in the compact jet within 1~mas scale and affected by a Faraday screen in or in the close proximity of the jet.

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