This page (revision-6) was last changed on 07-Dec-2016 14:14 by SKamio

This page was created on 14-May-2007 13:06 by Louise Harra

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Version Date Modified Size Author Changes ... Change note
6 07-Dec-2016 14:14 2 KB SKamio to previous Comment by SKamio
5 18-Aug-2008 16:20 2 KB PeterYoung to previous | to last
4 04-Dec-2007 13:56 1 KB PeterYoung to previous | to last
3 05-Jul-2007 15:27 889 bytes PeterYoung to previous | to last
2 05-Jul-2007 15:26 902 bytes PeterYoung to previous | to last Comment by PeterYoung
1 14-May-2007 13:06 154 bytes Louise Harra to last

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At line 2 added 13 lines
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Just to comment further on this... solar features imaged in the short wavelength band will occur at higher Y-pixel numbers than those imaged in the long wavelength band. Thus if you see a brightening at Y-pixel 100 in the Fe XII 195 line, then it corresponds to Y-pixel 84 in the long wavelength band.
The offset between the bands seems to vary with wavelength, with different people reporting offsets of between 16 and 20 pixels.
Note that the heliocentric coordinates stored in the fits headers and returned by the EIS software apply to the long wavelength band, not the short wavelength band. This is because the He II 256 line was used to co-align with the SOT data.
Peter Young
--[PeterYoung|http://null], 05-Jul-2007
This page (revision-6) was last changed on 07-Dec-2016 14:14 by SKamioTop