QUIJOTE科学结果。II。银河系分子复合物W43和W47及超新星遗迹W44微波辐射的偏振测量
QUIJOTE Scientific Results. II. Polarisation Measurements of the Microwave Emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44
摘要：
我们目前的Q-U-I JOint TENERIFE（QUIJOTE）的强度和偏振图，在10-20 GHz的覆盖区域沿银河系平面24<1 <45度，|b| <8度。这些图由210小时的数据得到，具有~40 μ K/束的偏振灵敏度和~1度的角分辨率。我们的强度数据对于确认两个分子复合物W 43（22 σ）和W 47（8 σ）的异常微波发射（AME）的存在至关重要。我们还检测到与W 44相关的高显著性（6 σ）AME，这是对SNR的首次明确检测。新的QUIJOTE偏振数据与WMAP相结合，对于以下方面至关重要：i）确定W 44中同步辐射的光谱指数，beta_sync =-0.62 +/-0.03，一旦在拟合中包括自由-自由分量，则与从强度光谱推断的值非常一致。ii）用旋转测量值-404 +/-49 rad/m2在W 44方向上跟踪与法拉第旋转相关的偏振角的变化。和iii）设定Pi_AME <0.39%（95% C.L.）的W 43的极化的上限。从QUIJOTE 17 GHz的数据，和<0.22%，从WMAP 41 GHz的数据，这是最严格的限制有史以来获得的极化分数的AME。对于典型的物理条件（晶粒温度和磁场强度），并在晶粒和磁场之间的完美对齐的情况下，电或磁偶极子发射的模型预测较高的极化分数。
英文摘要：
We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10-20 GHz covering a region along the Galactic plane 24<l<45 deg, |b|<8 deg. These maps result from 210 h of data, have a sensitivity in polarisation of ~40 muK/beam and an angular resolution of ~1 deg. Our intensity data are crucial to confirm the presence of anomalous microwave emission (AME) towards the two molecular complexes W43 (22 sigma) and W47 (8 sigma). We also detect at high significance (6 sigma) AME associated with W44, the first clear detection of this emission towards a SNR. The new QUIJOTE polarisation data, in combination with WMAP, are essential to: i) Determine the spectral index of the synchrotron emission in W44, beta_sync =-0.62 +/-0.03, in good agreement with the value inferred from the intensity spectrum once a free-free component is included in the fit. ii) Trace the change in the polarisation angle associated with Faraday rotation in the direction of W44 with rotation measure -404 +/- 49 rad/m2. And iii) set upper limits on the polarisation of W43 of Pi_AME <0.39 per cent (95 per cent C.L.) from QUIJOTE 17~GHz, and <0.22 per cent from WMAP 41 GHz data, which are the most stringent constraints ever obtained on the polarisation fraction of the AME. For typical physical conditions (grain temperature and magnetic field strengths), and in the case of perfect alignment between the grains and the magnetic field, the models of electric or magnetic dipole emissions predict higher polarisation fractions.
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