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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CCDOffset
CCDOffset

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[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
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The variation with wavelength mentioned above is due to the tilt of the grating relative to the CCD axes. An estimate of this tilt for the SW band has been made by Young et al. (2008; astro-ph 0805.0958). Combining with the offset between the two CCDs it is possible to estimate the offset relative to the EIS reference line (He II 256) for any wavelength. A routine has been written to give this estimate, and it is called as:
IDL> offset=eis_ccd_offset(195.12)
where offset is the offset, in pixels, of the Fe XII 195.12 image from the He II 256 image. I.e., if the same feature is seen in both 256 and 195, then the 195 feature will be 'offset' pixels higher on the CCD than the 256 feature.
The routine does the following:
- assume the tilt measured for the SW band is the same as for the LW band
- the offset between SW and LW has been obtained by co-aligning images in Fe VIII 185.21 and Si VII 275.35
-- PeterYoung, 18-Aug-2008
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Wavelength dependent Y-offset has been determined from Mercury transit on November 8, 2006.
[yoffset.pdf]
--[SKamio|http://null], 19-Aug-2008
This page (revision-6) was last changed on 07-Dec-2016 14:14 by SKamioTop