This page (revision-7) was last changed on 07-Dec-2016 14:14 by Terje Fredvik

This page was created on 14-Jun-2010 15:59 by PeterYoung

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Version Date Modified Size Author Changes ... Change note
7 07-Dec-2016 14:14 4 KB Terje Fredvik to previous
6 31-Mar-2011 10:21 4 KB Terje Fredvik to previous | to last
5 31-Mar-2011 10:19 4 KB Terje Fredvik to previous | to last
4 15-Jun-2010 15:05 4 KB PeterYoung to previous | to last
3 15-Jun-2010 15:04 4 KB PeterYoung to previous | to last
2 14-Jun-2010 16:11 4 KB PeterYoung to previous | to last
1 14-Jun-2010 15:59 4 KB PeterYoung to last

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At line 1 changed one line
!Correction for EIS Line Centre Variations Due To Orbital Motion Using Instrument Temperatures
!!!Correction for EIS Line Centre Variations Due To Orbital Motion Using Instrument Temperatures
At line 5 changed one line
(Click here to see a complete list of all new and modified SolarSoft routines)
(Click [here|http://folk.uio.no/tfredvik/astro/wavecorr/list.txt] to see a complete list of all new and modified SolarSoft routines)
At line 7 changed one line
The wavelength correction can be found using eis_wave_corr_hk.pro, the gethkwavecorr() method of the eis_data object or eis_prep.pro. All procedures use specially prepared house keeping data files that are distributed with SolarSoft in the directory $EIS_DATA/wave_corr. If the house keeping files that are needed for correcting a certain EIS raster are missing in your SolarSoft installation, the new routines will search for the files in $EIS_WAVE_CORR_HK_DATA (if this environment variable is set), and in the current working directory. If the files are not found, they will automatically be downloaded from the Oslo archive and saved in $EIS_WAVE_CORR_HK_DATA (if set) or to the current working directory (if not set).
The wavelength correction can be found using {{eis_wave_corr_hk.pro}}, the {{gethkwavecorr()}} method of the eis_data object or eis_prep.pro. All procedures use specially prepared house keeping data files that are distributed with SolarSoft in the directory {{$EIS_DATA/wave_corr}}. If the house keeping files that are needed for correcting a certain EIS raster are missing in your SolarSoft installation, the new routines will search for the files in {{$EIS_WAVE_CORR_HK_DATA}} (if this environment variable is set), and in the current working directory. If the files are not found, they will automatically be downloaded from the Oslo archive and saved in {{$EIS_WAVE_CORR_HK_DATA}} (if set) or to the current working directory (if not set).
At line 11 changed one line
This is simply a wrapper procedure calling the necessary methods of the eis_data object. It is called with the same parameters as the well known eis_wave_corr.pro:
This is simply a wrapper procedure calling the necessary methods of the {{eis_data}} object. It is called with the same parameters as the well known {{eis_wave_corr.pro}}:
At line 21 changed 3 lines
In addition eis_wave_corr_hk takes two keywords:
wvl_cube: If set to a named variable, wvl_cube will return a 3 dimensional wavelength cube in the format used by mk_analysis.pro of the Component Fitting System for IDL (cfit) package.
lam: the underlying methods of eis_data calculates the wavelength correction in pixels, and we assume that the shift in pixels is the same for all lines formed at any location on the two detectors. However, when measured in Angstroms the line centre variation and the slit tilt will vary slightly with wavelength. As default, eis_wave_corr_hk assumes that the corrections are to be calculated for the Fe XII 195 Å line, but the lam keyword may be set to the wavelength of the line you want to investigate.
In addition {{eis_wave_corr_hk}} takes two keywords:
At line 23 added 3 lines
* wvl_cube: If set to a named variable, wvl_cube will return a 3 dimensional wavelength cube in the format used by mk_analysis.pro of the Component Fitting System for IDL (cfit) package.
* lam: the underlying methods of eis_data calculates the wavelength correction in pixels, and we assume that the shift in pixels is the same for all lines formed at any location on the two detectors. However, when measured in Angstroms the line centre variation and the slit tilt will vary slightly with wavelength. As default, eis_wave_corr_hk assumes that the corrections are to be calculated for the Fe XII 195 Å line, but the lam keyword may be set to the wavelength of the line you want to investigate.
At line 40 changed one line
When creating an eis_data object, the aux_data will contain two new null pointers, hkpixcorrtilt and hkpixcorrtime:
When creating an {{eis_data}} object, the aux_data will contain two new null pointers, {{hkpixcorrtilt}} and {{hkpixcorrtime}}:
At line 47 changed one line
The two pointers will become valid when the method gethkwavecorr() is called (i.e. when you try to access the contents of the pointers):
The two pointers will become valid when the method {{gethkwavecorr()}} is called (i.e. when you try to access the contents of the pointers):
At line 55 changed one line
The gethkwavecorr() may be called with a wavelength as input parameter, or with the keyword wvl_cube set, to get the same functionality as for the eis_wave_corr_hk wrapper as explained above.
The {{gethkwavecorr()}} may be called with a wavelength as input parameter, or with the keyword {{wvl_cube}} set, to get the same functionality as for the {{eis_wave_corr_hk}} wrapper as explained above.
At line 66 changed one line
eis_prep.pro now accepts the keyword hkwavecorr. If set, the resulting level 1 file will contain the wavelength correction information.
{{eis_prep.pro}} now accepts the keyword {{hkwavecorr}}. If set, the resulting level 1 file will contain the wavelength correction information.
At line 75 removed one line
This page (revision-7) was last changed on 07-Dec-2016 14:14 by Terje FredvikTop