南峰太阳观测：校准数据和改进图像
The solar survey at Pic du Midi: calibrated data and improved images
摘要：
在Pic du Midi天文台，我们利用光球层、双折射和日冕的图像进行太阳调查。这次巡天被命名为CLIMSO（CLIchés Multiples du Soleil），在以下谱线中：Fe XIII日冕（1.075微米），H-alpha（656.3 nm）和He I（1.083微米）的光谱，H-alpha和Ca II（393.4 nm）的光球。所有帧覆盖太阳直径的1.3倍，角分辨率接近一弧秒。在天气允许的情况下，日冕和色球层的帧率是每分钟一个频道，而Fe XIII日冕的帧率是每小时一个频道。这项调查于2007年开始对圆盘和日冕进行调查，并于2015年开始对日冕进行调查。我们几乎已经完成了一个太阳活动周期，希望能覆盖更多的太阳活动周期，保持相同的波长或增加其他波长。目标：使CLIMSO图像更容易使用，并为科学界带来更多利润。方法：提供“科学就绪”数据。我们改进了日冕仪的对比度，除了以前的光谱通道外，现在还提供了Fe XIII日冕的图像。我们还实现了一个基于衍射菲涅耳阵列的自动导航系统，用于精确定位日冕面具后面的太阳。结果：数据（图像和影片）可通过虚拟观测站和专用网站（如http://climso.irap.omp.eu）公开获取和下载。对于H-α和Ca II通道，我们将数据校准为物理单位，与大气或仪器条件无关：我们提供了以W m^-2 sr^-1 nm^-1为单位的太阳光谱辐射图。本文介绍了仪器的改进和校准过程。
英文摘要：
At Pic du Midi observatory we carry out a solar survey with images of the photosphere, prominences and corona. This survey, named CLIMSO (CLIchés Multiples du SOleil), is in the following spectral lines: Fe XIII corona (1.075 micron), H-alpha (656.3 nm) and He I (1.083 micron) prominences, H-alpha and Ca II (393.4 nm) photosphere. All frames cover 1.3 times the diameter of the Sun with an angular resolution approaching one arc second. The frame rate is one per minute per channel (weather permitting) for the prominences and chromosphere, and one per hour for the Fe XIII corona. This survey started in 2007 for the disk and prominences, and in 2015 for the corona. We have almost completed one solar cycle, and hope to cover several more, keeping the same wavelengths or adding others. Aims: Make the CLIMSO images easier to use and more profitable for the scientific community. Methods: Providing 'science-ready' data. We have improved the contrast capabilities of our coronagraphs, which now provide images of the Fe XIII corona, in addition to the previous spectral channels. We have also implemented an autoguiding system based on a diffractive Fresnel array for precise positioning of the Sun behind the coronagraphic masks. Results: The data (images and films) are publicly available and downloadable through virtual observatories and dedicated sites: e.g. http://climso.irap.omp.eu. For the H-alpha and and Ca II channels we calibrate the data into physical units, independent of atmospheric or instrumental conditions: we provide solar maps of spectral radiances inW m^-2 sr^-1 nm^-1. The instrumental improvements and the calibration process are presented in this paper.
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