This page (revision-14) was last changed on 27-Nov-2017 16:38 by Peter Young

This page was created on 08-Oct-2013 20:24 by Peter Young

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EISCalibration
EISCalibration

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At line 19 changed one line
We then use very deep observations taken above the limb to fit a mode that includes both an emission measure distribution and potential modifications to the effective areas. The effective area near 195 is fixed to lie on the EIS-EVE curve shown above. Here is an example of this analysis.
We then use very deep observations taken above the limb to fit a model that includes both an emission measure distribution and potential modifications to the effective areas. The effective area near 195 is fixed to lie on the EIS-EVE curve shown above. Here is an example of this applied to some off-limb spectra taken in 2007.
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[{Image src = 'eis_spec_20071104_202810_256_129.dem.jpg' width='600'}]
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By repeating this analysis for several periods during the mission we are able to infer the effective areas as a function of wavelength and time. Details are given in this paper recently submitted to astro-ph [link pending].
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There is software distributed in SSW that computes the new effective areas. Perhaps the most useful routine is [eis_recalibrate_intensity.pro|http://sohowww.nascom.nasa.gov/solarsoft/hinode/eis/idl/atest/hwarren/calibration/eis_recalibrate_intensity.pro]
This page (revision-14) was last changed on 27-Nov-2017 16:38 by Peter YoungTop