Calibration procedures for the CHASE/HIS science data. (arXiv:2205.06075v1 [astro-ph.SR])

Calibration procedures for the CHASE/HIS science data. (arXiv:2205.06075v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Qiu_Y/0/1/0/all/0/1">Ye Qiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_S/0/1/0/all/0/1">ShiHao Rao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">Chuan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_C/0/1/0/all/0/1">Cheng Fang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ding_M/0/1/0/all/0/1">MingDe Ding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Z/0/1/0/all/0/1">Zhen Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ni_Y/0/1/0/all/0/1">YiWei Ni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_W/0/1/0/all/0/1">WenBo Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_J/0/1/0/all/0/1">Jie Hong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hao_Q/0/1/0/all/0/1">Qi Hao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_Y/0/1/0/all/0/1">Yu Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_P/0/1/0/all/0/1">PengFei Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wan_X/0/1/0/all/0/1">XiaoSheng Wan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Z/0/1/0/all/0/1">Zhi Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+You_W/0/1/0/all/0/1">Wei You</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_Y/0/1/0/all/0/1">Yuan Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tao_H/0/1/0/all/0/1">HongJiang Tao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">XianSheng Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_Y/0/1/0/all/0/1">YuKun He</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Q/0/1/0/all/0/1">Qiang Liu</a>

The H{alpha} line is an important optical line in solar observations
containing the information from the photosphere to the chromosphere. To study
the mechanisms of solar eruptions and the plasma dynamics in the lower
atmosphere, the Chinese H{alpha} Solar Explorer (CHASE) was launched into a
Sun-synchronous orbit on October 14, 2021. The scientific payload of the CHASE
satellite is the H{alpha} Imaging Spectrograph (HIS). The CHASE/HIS acquires,
for the first time, seeing-free H{alpha} spectroscopic observations with high
spectral and temporal resolutions. It consists of two observational modes. The
raster scanning mode provides full-Sun or region-of-interest spectra at
H{alpha} (6559.7-6565.9 {AA}) and Fe I (6567.8-6570.6 {AA}) wavebands. The
continuum imaging mode obtains full-Sun photospheric images at around 6689
{AA}. In this paper, we present detailed calibration procedures for the
CHASE/HIS science data, including the dark-field and flat-field correction,
slit image curvature correction, wavelength and intensity calibration, and
coordinate transformation. The higher-level data products can be directly used
for scientific research.

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