This respository stores Jupyter notebooks and IDL codes to analyze spectroscopic observations of the solar corona during the 2017 total solar eclipse (TSE). The observation was obtained by a three-channel PArtially Multiplexed Imaging Spectrometer (3PAMIS). Many thanks to Prof. Shadia Habbal, Prof. Adalbert Ding, Dr. Michael Nassir, and their team for developing the instrument, organized the expedition, making the observations, and sharing the data. Special gratitudes to Bryan Yamashiro for helping me on data reduction and calibration. 3PAMIS observations were compared to EIS and CoMP observations, and the results are summarized in a manuscript submitted to ApJ.

Some Jupyter notebooks use my naive Python scripts. The HTML exports of the Jupyter notebooks are available in the ipynb_html directory.

Links to the Jupyter notebooks for each Figure (Recommend to open these notebooks in nbviewer to enable the internal hyperlinks in notebooks):

Figure 1: FOV of 3PAMIS observations during the TSE.

Figure 2: Examples of spectral line profiles observed by 3PAMIS.

Figure 3: Fitting results of Fe X (red) and Fe XIV (green) lines observed by 3PAMIS.

Figure 4: Variation of Fe X and Fe XIV line intensities and line widths observed by 3PAMIS.

Figure 5: Line intensities observed by EIS in a polar coronal hole and the quiet Sun.

Figure 6: Effective temperatures in a polar coronal hole observed by EIS.

Figure 7: Effective temperatures in the quiet Sun observed by EIS.

Figure 8: Comparison between the Doppler velocities and line widths observed by 3PAMIS and CoMP.

Figure 9: Comparison between line widths observed by 3PAMIS and reported by Koutchmy et al. (2019) during the 2017 TSE.

Figure 10: Comparison between line widths observed by 3PAMIS during the 2017 TSE and other spectroscopic observations.

Figure 11: Electron density measured by CoMP and populations into the upper level of Fe XIV 530.3 nm line calculated by CHIANTI.

Figure 12: Nonthermal velocity measured by 3PAMIS. Derived using the electron temperature reported by Boe et al. (2020).

Figure 13: An example of the spectral line curvature correction of the 3PAMIS red detector.

Figure 14: 1-D flatfield curve of the 3PAMIS red detector near the Fe X 637.4 nm line at the 52nd order.

Figures 15a and 15b: Wavelength calibration of 3PAMIS red and green detectors.

Figure 16: Absolute wavelength calibration of the 3PAMIS red detector.

Figure 17: Instrumental broadening of 3PAMIS red and green detectors.

Figure 18: Pointing of 3PAMIS during the totality.

Figure 19: Comparison of Fe XIV profiles in different orders observed by 3PAMIS.