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At line 1 removed 2 lines
[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
At line 8 changed one line
IDL> eis_auto_fit, wd, fit
IDL> eis_wave_corr, l1name, offset
IDL> eis_auto_fit, wd, fit, offset=offset
At line 10 added 4 lines
The first command is used to determine the wavelength offset at each spatial pixel due to the tilt of the EIS slit and orbit variation of emission line centroids. Correcting for these effects yields a much more accurate velocity map.
Alternatively, you may use ''eis_wave_corr_hk'' instead of ''eis_wave_corr'' to correct the orbital variation by using instrumental temperature. This method is suitable for active regions (details are described [here|HKmethod]).
At line 14 changed 3 lines
int=eis_get_fitdata(fit,/int,calib=calib)
vel=eis_get_fitdata(fit,/vel,calib=calib)
wid=eis_get_fitdata(fit,/wid,calib=calib)
int=eis_get_fitdata(fit,/int)
vel=eis_get_fitdata(fit,/vel)
wid=eis_get_fitdata(fit,/wid)
At line 19 changed one line
The optional input 'calib' specifies which radiometric calibration to apply to the data. Please check the [calibration discussion page|EISCalibration] for more details. The recommended options are 1 or 3 for the Del Zanna (2013) or Warren et al. (2014) calibrations. Neglecting to specify calib means that the original laboratory calibration (as performed in the call to eis_prep) will be retained. Although 'calib' does not need to be specified for the velocity and line width arrays, it's good practice to always specify it.
Error arrays for each parameter can be obtained by adding the optional output 'error=error':
At line 21 removed 2 lines
Error arrays for each parameter can be obtained by adding the optional output 'error=error'. Make sure that 'calib' takes the same value as it did when you extracted the intensity array.
At line 24 changed one line
int=eis_get_fitdata(fit,/int,error=int_error,calib=calib)
int=eis_get_fitdata(fit,/int,error=int_error)
At line 27 changed one line
This example shows the most simple use for eis_auto_fit. The routine can also be used to perform multiple Gaussian fits and a full description of the capabilities are given in two documents: '[Gaussian fitting for the Hinode/EIS mission|ftp://sohoftp.nascom.nasa.gov/solarsoft/hinode/eis/doc/eis_notes/16_AUTO_FIT/eis_swnote_16.pdf]' and '[Gaussian fitting examples using eis_auto_fit|https://ftp://sohoftp.nascom.nasa.gov/solarsoft/hinode/eis/doc/eis_notes/17_AUTO_FIT_EXAMPLES/eis_swnote_17.pdf]'.
This example shows the most simple use for eis_auto_fit. The routine can also be used to perform multiple Gaussian fits and a full description of the capabilities are given in two documents: '[Gaussian fitting for the Hinode/EIS mission|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/fitting/eis_auto_fit.pdf]' and '[Gaussian fitting examples using eis_auto_fit|https://hyperion.nascom.nasa.gov/svn/eis/release/doc/fitting/eis_auto_fit_examples.pdf]'.
At line 32 changed one line
# When the line width array is extracted with eis_get_fitdata, it is automatically corrected for the instrumental line width. To keep the instrumental component, use the /keep_inst_width keyword. The thermal component of the line width can be removed by using the thermal_wid= optional input - see the routine header for details on how to use this keyword.
# The Gaussian line widths include a significant instrumental component of approximately 55 mA.
This page (revision-12) was last changed on 27-Nov-2017 16:52 by Peter YoungTop