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[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
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IDL maps are a widely used means of storing and using solar image data, and are very useful for comparing data-sets from different instruments. The sections below describe different ways of creating maps from EIS data. Please check Dominic Zarro's [IDL map webpage|http://hesperia.gsfc.nasa.gov/~zarro/idl/maps/maps.html] for more details on how to use maps. A basic operation is to plot a map:
IDL maps are a widely used means of storing and using solar image data, and are very useful for comparing data-sets from different instruments. The sections below describe different ways of creating maps from EIS data. Please check Dominic Zarro's [IDL map webpage|https://hesperia.gsfc.nasa.gov/rhessidatacenter/complementary_data/maps/] for more details on how to use maps. A basic operation is to plot a map:
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!!Creating a map from the eis_auto_fit output
The Gaussian fitting routine EIS_AUTO_FIT is described in [EIS Software Note No. 16|ftp://sohoftp.nascom.nasa.gov/solarsoft/hinode/eis/doc/eis_notes/16_AUTO_FIT/eis_swnote_16.pdf], and it returns a structure containing the fit results. Maps can be created from this structure using the routine EIS_GET_FITDATA and specifying the /MAP keyword:
{{{
IDL> intmap=eis_get_fitdata(fitdata,/int,/map)
IDL> velmap=eis_get_fitdata(fitdata,/vel,/map)
IDL> widmap=eis_get_fitdata(fitdata,/wid,/map)
}}}
!!Technical details for generating a map
An IDL map is generated through the command:
{{{
map=make_map(array,xc=xc,yc=yc,dx=dx,dy=dy,time=time)
}}}
where xc and yc give the X and Y coordinates of the image center, dx and dy give the size of the pixels in arcsecs, and time is the time of the observation.
This information can be obtained from the windata structure (produced by EIS_GETWINDATA):
{{{
xc=windata.xcen
yc=windata.ycen
dx=windata.scale[0]
dy=windata.scale[1]
time=windata.date_obs
}}}
This page (revision-4) was last changed on 18-Feb-2020 16:54 by Peter YoungTop