This page (revision-13) was last changed on 07-Dec-2016 14:14 by Peter Young

This page was created on 12-Nov-2009 15:08 by PeterYoung

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Page References

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EISPointing
EISPointing

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At line 19 changed one line
IDL> ycen=data->getycen(/raster)
IDL> ycen=data->getycen(wvl,/raster)
At line 22 added 2 lines
where WVL is the wavelength you are interested in. If WVL is not specified then 256.32 (the wavelength of the He II line) is assumed. Note that the raster center in solar-Y varies with wavelength by up to 18" due to the tilt of the EIS grating relative to the detector and a spatial offset between the two CCDs.
At line 26 removed one line
A further point to remember is that all coordinates are assumed to be correct for He II 256.32 only. To obtain the Y-pointing for a line at another wavelength, do:
At line 28 removed 6 lines
{{{
IDL> ycen = ycen - eis_ccd_offset(195.12)
}}}
for the example of the 195.12 line. The offset can be as large as 18" for lines in the short wavelength band of EIS.
At line 40 changed one line
IDL> ypos=data->getypos()
IDL> ypos=data->getypos(wvl)
At line 48 changed one line
IDL> ycen=data->getycen()
IDL> ycen=data->getycen(wvl)
At line 61 changed one line
In addition to the satellite jitter there also appears to be jitter internal to the EIS instrument. This can be measured by, e.g., looking a time series of slot images and comparing the jitter obtained by co-aligning the images to the satellite jitter: the residuals represent the instrument jitter. This jitter has not been characterized yet and no software tools exist to yield the jitter values. However the magnitude of the instrument jitter is believed to be smaller than the satellite jitter.
In addition to the satellite jitter there also appears to be jitter internal to the EIS instrument. This can be measured by, e.g., looking at a time series of slot images and comparing the jitter obtained by co-aligning the images to the satellite jitter: the residuals represent the instrument jitter. This jitter has not been characterized yet and no software tools exist to yield the jitter values. However the magnitude of the instrument jitter is believed to be smaller than the satellite jitter.
At line 66 changed one line
As with most solar data, the EIS data have a header that contains XCEN and YCEN values. These can be obtained by doing:
As with most solar data, an EIS data-set has a header that contains XCEN and YCEN values. These can be obtained by doing:
This page (revision-13) was last changed on 07-Dec-2016 14:14 by Peter YoungTop