This page (revision-12) was last changed on 27-Nov-2017 16:52 by Peter Young

This page was created on 17-Mar-2010 21:30 by PeterYoung

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At line 3 changed one line
Generally the EIS emission lines have a Gaussian shape and, by fitting a Gaussian function to the spectrum, one can derive line intensity, line width and velocity maps. The high sensitivity of EIS means that for many lines it is possible to perform good quality fits at each pixel in the image. The routine eis_auto_fit in Solarsoft takes the output from eis_getwindata (Worksheet 5) and fits a single Gaussian to each pixel in the image. The calling procedure is:
Generally the EIS emission lines have a Gaussian shape and, by fitting a Gaussian function to the spectrum, one can derive line intensity, line width and velocity maps. The high sensitivity of EIS means that for many lines it is possible to perform good quality fits at each pixel in the image. The routine EIS_AUTO_FIT in Solarsoft takes the output from eis_getwindata (Worksheet 5) and fits a single Gaussian to each pixel in the image. The calling procedure is:
At line 12 changed one line
The output from eis_auto_fit is an IDL structure called 'fit'. Intensity, velocity and line width arrays can be extracted from fit by doing:
The output from EIS_AUTO_FIT is an IDL structure called FIT. Intensity, velocity and line width arrays can be extracted from FIT by doing:
At line 28 removed 5 lines
!!Exercise
#Some horizontal stripes can be seen in the velocity and line width maps. What could be causing these?
#Use eis_fit_viewer to find the approximate variation in line centroid position caused by the orbital motion of Hinode.
This page (revision-12) was last changed on 27-Nov-2017 16:52 by Peter YoungTop