This page (revision-17) was last changed on 13-May-2025 18:49 by Peter Young

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

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Page References

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EISCalibration
EISCalibration

Version management

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At line 6 added 2 lines
UPDATE, 13-May-2025: All EIS users are now recommended to use the calibration described in Del Zanna et al. (2025, ApJS, 276, 42). See below under "The 2025 update".
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Re-assessments of the EIS calibration have been performed by G. Del Zanna and H. Warren, and these are described below along with software routines that implement the calibrations.
Re-assessments of the EIS calibration were performed independently by G. Del Zanna and H. Warren around 2013-2014, and these are described below along with software routines that implement the calibrations. These two authors collaborated to yield the new calibration in 2025.
At line 10 changed one line
The new calibrations are still subject to testing and so eis_prep has not been updated. The recommendation is to run eis_prep ''without'' the /correct_sensitivity keyword (thus implementing the original laboratory calibration) and then performing a post facto correction with one of the methods described below.
The recommendation for users is to run eis_prep with the default options, yielding intensities computed with the original laboratory calibration. The intensities can then be modified to the newer calibrations as described below.
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!!G. Del Zanna method
!!The 2025 update
At line 18 added 13 lines
The 2025 calibration is implemented through the routine interpol_eis_ea. The following call shows how to generate the effective area on 1-May-2020 for the EIS SW channel:
{{IDL> wvl=findgen(41)+170.\\
IDL> ea=interpol_eis_ea('1-may-2020',wvl}}
There is also the routine eis_recalibrate_intensity_new that is useful for converting an intensity from the original laboratory calibration to the new calibration. For example, if the old intensity for the 195.12 line was 100, then the new intensity is given by
{{IDL> int=eis_recalibrate_intensity_new('1-may-2020',195.12,100.)}}
If you use the routines EIS_AUTO_FIT and/or EIS_MASK_SPECTRUM, then see the instructions at the bottom of this page.
!!G. Del Zanna method (2013)
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!!Warren, Ugarte-Urra, and Landi method
!!Warren, Ugarte-Urra, and Landi method (2014)
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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 a paper recently submitted to [astro-ph|http://arxiv.org/pdf/1310.5324v2.pdf].
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 the paper [Warren, Ugarte-Urra & Landi (2014)|https://ui.adsabs.harvard.edu/abs/2014ApJS..213...11W/abstract].
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!!Applying the new calibrations to the output from EIS_AUTO_FIT
!!Applying the new calibrations to the output from EIS_AUTO_FIT and EIS_MASK_SPECTRUM
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4 - /correct_sensitivity is "undone" and the Warren et al. (2014) calibration is applied
4 - /correct_sensitivity is "undone" and the Warren et al. (2014) calibration is applied\\
5 - the Del Zanna et al. (2025) calibration is applied\\
6 - /correct_sensitivity is "undone" and the Del Zanna et al. (2025) calibration is applied\\
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Similarly, if you use the routine EIS_MASK_SPECTRUM to derive a spectrum from a pixel mask, then you can specify the calibration using the CALIB= keyword. For example:
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{{IDL> eis_mask_spectrum,file,mask,swspec=swspec,lwspec=lwspec,calib=5,/refill}}
This page (revision-17) was last changed on 13-May-2025 18:49 by Peter YoungTop