论文标题
用长波长阵列检测到低于100 MHz的脉冲星极化
Detecting Pulsar Polarization below 100 MHz with the Long Wavelength Array
论文作者
论文摘要
使用长波长阵列的第一个站（LWA1），我们检查了25至88 MHz之间的极化脉冲星的发射。脉冲星的极化光经过法拉第旋转，因为它通过磁化的星际介质。低频望远镜的观察是获得精确旋转措施（RMS）的理想选择，因为法拉第旋转的效果与观测波长的平方成正比。使用这些RMS，我们获得了极化脉冲曲线，以查看极化如何在25-88 MHz范围内变化。 RMS还用于得出沿视线的电子密度加权平均银河磁场的值。我们提出了使用LWA1数据获取的15个脉冲星的旋转度量和极化曲线。这些结果为低频极化特性和脉冲星的发射高度提供了新的见解，并在较高频率下进行了补体测量。
Using the first station of the Long Wavelength Array (LWA1), we examine polarized pulsar emission between 25 and 88 MHz. Polarized light from pulsars undergoes Faraday rotation as it passes through the magnetized interstellar medium. Observations from low frequency telescopes are ideal for obtaining precise rotation measures (RMs) because the effect of Faraday rotation is proportional to the square of the observing wavelength. With these RMs, we obtained polarized pulse profiles to see how polarization changes in the 25-88 MHz range. The RMs were also used to derive values for the electron density weighted average Galactic magnetic field along the line of sight. We present rotation measures and polarization profiles of 15 pulsars acquired using data from LWA1. These results provide new insight into low-frequency polarization characteristics and pulsar emission heights, and complement measurements at higher frequencies.
