11-May-2005 - David H. Brooks

This file describes the IDL procedures used for calculating 
the updated TRACE response functions in the subdirectories of 
this package, and the accompanying data files. 

IDL routines.
----------

trace_resp_spec - The procedure for calculating the isothermal
                  spectra needed for the TRACE response calculations
                  using CHIANTI. The output is used by trace_resp_calc.

trace_resp_calc - The procedure for calculating the response file read
                  by trace_t_resp. It uses output from trace_resp_spec.

trace_resp_comp - A procedure for comparing two response files.

trace_r_resp    - Updated version of the routine that returns the TRACE
                  EUV response at a given temperature.

Example of use:
---------------

The following example shows how to use these routines to calculate the
current default response file 
(SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.spec).
For an explanation of the name of this file, see descriptions below.

IDL> trace_resp_spec, pressure = 1.0E+15
;; 2 widgets will pop up to allow selection of the ionization equilibrium and
;; elemental abundance files. Select, Mazzotta_etal.ioneq & sun_coronal.abund 
;; (Feldman).
IDL> trace_resp_calc, 'SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.spec'
;; if you do not name a file, a widget will popup for selection.
IDL> old_file=!TRACE_RESPONSE+'/FELDMAN_RAYMOND_pe1E15.resp'
;; if you do not name a file, a widget will popup for selection. 
;; In this example, a response file from the central library 
;; is compared to one in the current working directory.
IDL> new_file='SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.resp'
IDL> trace_resp_comp, old_file, new_file, /jpeg
;; an onscreen plot is displayed and an output JPEG file s created. 
IDL> $ls
FELDMAN_RAYMOND_pe1E15_x_SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.jpg

Isothermal spectra saved in generic files (.genx).
----------

The naming convention is

ABUNDANCES_IONIZATION_EQUILIBRIUM_PRESSURE/DENSITY_CHIANTI_VERSION.spec

e.g. SUN_CORONAL_MAZZOTTA_ETAL_ne1.0E08_CHIANTI_v4.2.spec

SUN_CORONAL   - The coronal abundances of Feldman have been used.

MAZZOTTA_ETAL - The ionization fractions of Mazzotta et al. have been used.
ne1.0E08      - The results are calculated for an electron density of 
	        10^8 cm^-3
CHIANTI_v4.2  - CHIANTI version 4.2 has been used.

The following data files have been archived.      

SUN_CORONAL_MAZZOTTA_ETAL_ne1.0E08_CHIANTI_v4.2.spec
SUN_CORONAL_MAZZOTTA_ETAL_ne1.0E09_CHIANTI_v4.2.spec
SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.spec
SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E16_CHIANTI_v4.2.spec
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_ne1.0E08_CHIANTI_v4.2.spec
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_ne1.0E09_CHIANTI_v4.2.spec
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.spec
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_pe1.0E16_CHIANTI_v4.2.spec

TRACE response files.
----------

The naming convention is the same as for the spectra except that .spec
is replaced with .resp (these are .genx files)

The following data files have been archived.      

SUN_CORONAL_MAZZOTTA_ETAL_ne1.0E08_CHIANTI_v4.2.resp
SUN_CORONAL_MAZZOTTA_ETAL_ne1.0E09_CHIANTI_v4.2.resp
SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.resp
SUN_CORONAL_MAZZOTTA_ETAL_pe1.0E16_CHIANTI_v4.2.resp
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_ne1.0E08_CHIANTI_v4.2.resp
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_ne1.0E09_CHIANTI_v4.2.resp
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_pe1.0E15_CHIANTI_v4.2.resp
SUN_PHOTOSPHERIC_MAZZOTTA_ETAL_pe1.0E16_CHIANTI_v4.2.resp