用电荷重排和白天天空测量校准和稳定分光偏振计
Calibrating and Stabilizing Spectropolarimeters with Charge Shuffling and Daytime Sky Measurements
摘要：
在分辨率为$R>$ 10，000的情况下，校准良好的分光偏振法研究在单个谱线轮廓上的信噪比（SNR）优于0.01\%，这在大孔径望远镜中变得越来越普遍。光谱偏振研究需要高信噪比的观测，并且经常受到仪器系统误差的限制。作为一个例子，结合先进的线组合算法的光纤偏振分光光度计可以达到0.001\%的统计误差限制在测量的谱线轮廓参考的连续。这种观测的校准通常需要用于串扰和连续偏振。这并不简单，因为望远镜串扰误差很少小于$\sim$ 1\%。在太阳能仪器中，如丹尼尔K。Inouye太阳望远镜（DKIST），需要更严格的校准，望远镜光学设计包含大量的内在偏振伪影。本文介绍了一些普遍有用的技术，我们已经应用到HiVIS分光偏振仪在3.7米AEOS望远镜的哈雷阿卡拉。HiVIS现在产生精确的偏振谱线轮廓，在我们的全光谱分辨率为10，000，光谱采样为$\sim$ 100，000时，散粒噪声限制在0.01\% SNR水平。我们展示了在一个偏振串扰水平基本上为100%的系统中的串扰和连续偏振的绝对分光偏振校准的线轮廓。在这些数据中，连续偏振可以恢复到百分之一的精度，因为同步电荷洗牌模型现在与我们的CCD检测器。这些技术可以应用于其他望远镜上的分光偏振计，用于夜间和白天的应用，如DKIST，TMT和ELT，它们具有折叠的非轴对称焦点。
英文摘要：
Well-calibrated spectropolarimetry studies at resolutions of $R>$10,000 with signal-to-noise ratios (SNRs) better than 0.01\% across individual line profiles, are becoming common with larger aperture telescopes. Spectropolarimetric studies require high SNR observations and are often limited by instrument systematic errors. As an example, fiber-fed spectropolarimeters combined with advanced line-combination algorithms can reach statistical error limits of 0.001\% in measurements of spectral line profiles referenced to the continuum. Calibration of such observations is often required both for cross-talk and for continuum polarization. This is not straightforward since telescope cross-talk errors are rarely less than $\sim$1\%. In solar instruments like the Daniel K. Inouye Solar Telescope (DKIST), much more stringent calibration is required and the telescope optical design contains substantial intrinsic polarization artifacts. This paper describes some generally useful techniques we have applied to the HiVIS spectropolarimeter at the 3.7m AEOS telescope on Haleakala. HiVIS now yields accurate polarized spectral line profiles that are shot-noise limited to 0.01\% SNR levels at our full spectral resolution of 10,000 at spectral sampling of $\sim$100,000. We show line profiles with absolute spectropolarimetric calibration for cross-talk and continuum polarization in a system with polarization cross-talk levels of essentially 100\%. In these data the continuum polarization can be recovered to one percent accuracy because of synchronized charge-shuffling model now working with our CCD detector. These techniques can be applied to other spectropolarimeters on other telescopes for both night and day-time applications such as DKIST, TMT and ELT which have folded non-axially symmetric foci.
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