The second argument is the spectral window list that you want to study, in this example we’ve chosen, or C II, Si IV, Mg II h&k. IDL> iris_make_fits_level3, f,, /sp, sjifile=s, $ with keyword /all instead of the array with window indices we choose C II, Si IV 1403, and Mg II k. files will be written, current directory is the default. list the spectral windows possible, wdir is the directory where the level3 iris_files prints the file-names of all the raster files the variable f is an array of raster files for that observation where the environment variable IRIS_DATA should be the path to your IRIS data The different spectral windows of level 2 files are merged into the nwave dimension of the level 3 files.īesides the primary HDU, level 3 files have three extensions, see below: Ext. For rasters with only one repeat ( ntime = 1) the sp files are unnecessary and therefore not created. Here ny is the number of pixels along the slit, and nx the number of steps in the raster when rotation is used these are not aligned with solar (x, y) coordinates. The im files have the dimensions of ( nx, ny, nwave, ntime), while the sp files have the dimensions of ( nwave, ntime, nx, ny). The files are standard FITS files and the data is written in the primary Header Data Unit (HDU). They contain the same data, but one is the transpose of the other (this is to speed up access for visualization). ![]() There are two types of level 3 files: im and sp. include all the lines, only the NUV lines, or a selection), and so multiple level 3 files can be created from the same level 2 files. The user can decide which spectral line windows to include in the level 3 file (e.g. For a given observation, it combines multiple level 2 raster files into one or two level 3 files. Level 3 data can exist in a variety of configurations. ![]() ![]() Coalignment between channels and SJI/spectra
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