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Дата изменения: Thu Sep 15 17:22:53 2005 Дата индексирования: Sat Dec 22 08:33:22 2007 Кодировка: Поисковые слова: annular solar eclipse |
PROJECT
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME
CH_SS
PURPOSE:
Widget-based multi-purpose routine
to calculate CHIANTI line intensities and continua, to create a
synthetic spectrum, to make tables of lines, etc.
CALLING SEQUENCE:
IDL> ch_ss
PROCEDURE:
This routine calculates a synthetic spectrum by merging line
intensities and continua.
The widget is organised into four Sections:
SECTION 1:
-The Calculation of the CHIANTI line intensities.
This can be done in two ways:
1-Restore a save file with the CHIANTI line intensities already
calculated.
2-Calculate CHIANTI line intensities with a call to CH_SYNTHETIC.
In this case, A series of parameters must be set:
- Minimum and maximum wavelengths in Angstroms
- The model used for the calculation. Three are the options:
1) a constant density (cm^-3)
2) a constant pressure (cm^-3 K)
3) a general (Te,Ne) model. In this case, a file will be read.
This file should have two columns, one with the Te (K)
values, and one with the Ne (cm^-3) values.
- The ionization fraction file to be used. "*.ioneq" files
can be selected from either the CHIANTI database, the
working directory or selected via a widget.
- All ions ? If set to yes (default), then all the ions present in the
database will be included.
If set to no, then it is possible to select a list of ions
with a widget
- All lines ? If set to no (default), only the lines for which there are
observed energy levels are included
If set to yes, also the lines that do not have
corresponding observed energy levels are included. In this
case, the wavelengths are calculated from the theoretical
energy levels, and might not be very accurate.
- Isothermal ? If set to no (default), a DEM file must be selected.
"*.dem" files (i.e. files with a .dem extension)
can be selected from either the CHIANTI database, the
working directory or selected via a widget.
If set to yes, then the user is requested to enter one
or more temperatures (as logarithmic values - Log T )
and correspondent column emission measures EM
logarithmic values.
NOTE: if more than one value is entered, then the
sequence must be separated by commas (e.g.: 6.0,
6.5, 7.), and both Log T and Log EM must have the
same number of values
- Photoexcitation ?
If set to yes, you have to define:
Trad: The blackbody radiation field temperature
R/Ro: Distance from the centre of the star in stellar
radius units
Units: Photons or Ergs'
Protons: If set to Yes, the proton data are used to calculate the level population
Once all the parameters have been defined, the user should click on the
"Calculate intensities" button to start the calculation (which calls
CH_SYNTHETIC).
Once the calculation is finished, an IDL structure is loaded into
memory. It is then possible to save it for later use by clicking on the
"SAVE" button.
The RESTORE button is to restore previously saved files into an IDL
structure in memory.
Once the IDL structure with the line intensities is in the memory, it is
then possible to calculate and plot a spectrum (SECTION 2).
SECTION 2:
This section controls the parameters that are needed to fold the
line intensities and the continua into a synthetic
spectrum. These parameters are used by MAKE_CHIANTI_SPEC.
Before this is done, a set of line intensities MUST be in the
program memory. This is done either by calculating the
intensities or by restoring a save file with
previously calculated values (SECTION 1).
Setting the parameters:
-Minimum and maximum wavelengths in Angstroms
-spectrum bin size in Angstroms. Disallowed if an Effective area
file is used.
-instrumental FWHM: Setting this to a non-zero value broadens
each of the spectral lines with a Gaussian of
the specified FWHM (in Angstroms) so
mimicking the effects of instrumental
broadening.
-continuum: Add continua to the binned spectrum:
free-free, free-bound and two-photon.
Please note that the continuum calculation takes some
time and you may want to define a minimum abundance
value to speed the calculations.
- All lines ? If set to no (default), only the lines for which there are
observed energy levels are included.
If set to yes, the "unobserved lines" will be added, but
only if they are present in the structure.
-elemental abundances
"*.abund" files (i.e. files with a .abund
extension) can be selected either from the CHIANTI database,
the working directory, or via a widget.
-select a minimum abundance value
If set not null, only the lines of those elements
which have an abundance greater than the value set are
selected. Also, the continuum is calculated only for
those elements which have an abundance greater than
the value set. This can significantly speed up the
calculations. By default, the minimum value in the
selected abundance file is used. To have an idea of
what minimum abundance should be set, the abundances
of Allen (1973) give:
abundance (H) = 1.
abundance (He) = 0.085
abundance (C) = 3.3e-4
abundance (O) = 6.6e-4
abundance (Si) = 3.3e-5
abundance (Fe) = 3.9e-5
Eff. Area: Yes/No
If you want to fold the spectrum with an effective area.
If set to Yes, you are requested to choose an input ascii file
with two columns, the wavelength and the effective area values
(cm^2).
The wavelenghts in the file (that might not be linear) are used
to create the spectrum, that is multiplied with the effective
area values.
Note that this option only works well if a sufficient number
of bins is given. The line intensities contributing to each
bin are summed, and subsequently convolved with a gaussian
of full-width-half-maximum FWHM, if FWHM is not set = 0.
Please note that the convolution might not work if a small
number of bins is defined.
Also note that to have the correct output units (counts s-1
bin-1) the appropiately scaled DEM (or EM) values must be provided.
After this, by clicking on the "Calculate and plot" button the
program calculates and plots the synthetic spectrum.
Once the spectrum is displayed, it is then possible to
view the details of the lines by clicking with the mouse in the
plot window, and to perform various operations by clicking on
the buttons in SECTION 3
SECTION 3:
This Section allows the user to select a few parameters for the
plotting, and to create different types of OUTPUT.
Labels ? : Setting this to yes plots a vertical line for each
spectral line in the spectrum, and also writes a label
above the strongest lines indicating the ion from
which the line arises.
Min.: Only lines which have an intensity greater than the
value set here will be listed and, if requested,
labelled and selected for inclusion in the various
outputs. Setting the value=0. will result in all
lines being listed and written in the outputs.
X,Y, XOOM, UNZOOM: It si possible to select a region of the
spectrum, by zooming with the use of the mouse
or by setting the X,Y ranges.
NOTE that only the line details and portion of
the spectrum shown will be output.
LINEAR/LOG To plot the spectrum in linear or log scale
Create PS file: A postscript file is created.
Hardcopy: the postscript file "idl.ps" is created and sent to the
default printer.
Save Line details (latex): The details of the lines shown in the
plot will be saved in a latex file.
Save Line details (ascii): The details of the lines shown in the
plot will be saved in an ascii file.
Save Spectrum (ascii): The X,Y values of the plot are saved in
an ascii file.
Save Spectrum (IDL/FITS): The details of all the lines and the arrays
of the X,Y values of the plot are saved into
an IDL or FITS file. The IDL structure
has the following tags:
.LAMBDA: The array of wavelength X values
.SPECTRUM: The array of spectrum Y values
.UNITS The units of LAMBDA, SPECTRUM
.INSTR_FWHM The Instrumental FWHM
.BIN_SIZE Width of the Bins (fixed) in angstroms
.ABUND_NAME The CHIANTI abundance file name
.ABUND The abundance values
.MIN_ABUND The minimum abundance value used
.ABUND_REF The references
.CONTINUUM The values of the continuum (if
calculated)
.EFFAREA The array of effective area
values (optional)
.FILE_EFFAREA The name of the effective area file used (optional).
.IONEQ_NAME The ion balance file used (full path).
.IONEQ_LOGT The Log10 T values associated.
.IONEQ_REF The references.
.DEM_NAME The differential emission measure file eventually used
(full path).
.DEM The Log10 DEM values
.DEM_LOGT The Log10 T values associated.
.DEM_REF The references.
.MODEL_NAME A string indicating the model used
(e.g. constant density or constant pressure).
.MODEL_NE the Ne value.
.MODEL_PE the Pe value.
.WVL_UNITS The wavelength units.
.WVL_LIMITS The wavelength limits specified by the user.
.INT_UNITS The intensity units
.LOGT_ISOTHERMAL
The Log10(T) values used.
.LOGEM_ISOTHERMAL
The Log10(EM) values used.
.TIME The date and time when the structure was created.
.VERSION The version number of the CHIANTI database used.
.ADD_PROTONS
A flag (0/1) to indicate whether proton data were used (1)
or not (0) to calculate the level population.
.PHOTOEXCITATION
A flag (0/1) to indicate if photoexcitation was included (1)
or not (0).
.RADTEMP
The blackbody radiation field temperature used (if
photoexcitation was included).
.RPHOT
Distance from the centre of the star in stellar radius units
(if photoexcitation was included).
THEN, FOR EACH LINE USED TO CALCULATE THE
SPECTRUM:
.LINES A structure containing information about the lines.
Its size is the number of lines in the spectrum. The
tags are:
.peak The peak intensity value
.iz The atomic number of the elements (e.g., 26=Fe)
.ion The ionisation stage (e.g., 13=XIII)
.snote The identification of the ion (e.g., 'Fe XXIV d')
.ident The identification of the transition, configuration
and terms in text form.
.ident_latex
The identification of the transition, configuration
and terms in latex form.
.lvl1 The lower level of the transition (see .elvlc
file for ion)
.lvl2 The upper level for transition.
.tmax The temperature of maximum emission of the line
(i.e., the temperature at which the product of
the emissivity and the ion fraction has its
maximum). Rounded to nearest 0.1, and zero in case
the isothermal approximation is used.
.fwhm
.wvl Wavelength of the transition, in Angstroms.
.flag A flag, =-1 if the line has only theoretical energy
levels. Otherwise flag=0.
.int Intensity of line (with the abundance factor multiplied)
Save Spectrum (FITS): The entire information contained in the
IDL structure is stored in a FITS file.
SECTION 4:
Here, text information messages are printed.
INPUTS
None.
OPTIONAL INPUTS:
The font
OUTPUTS:
Many.
KEYWORD PARAMETERS:
FONT the font to be used. Can be useful to customize the appearance of
the widget.
CALLS:
CH_SYNTHETIC, CH_LINE_LIST, CH_DRAWBOX, MAKE_CHIANTI_SPEC, CH_XMENU_SEL,
plus many other CHIANTI and SolarSoft routines.
PROGRAMMING NOTES
Within CH_SS, there are several other routines which are:
OPLOT_LINES This overplots lines and a label on the displayed
spectrum.
SYN_CURSOR When the mouse is clicked when on the spectrum window,
this routine prints out the list of nearby lines and
their IDs in the text window.
CALC_SYN_SPECTRUM
Calculates line intensities with a call to CH_SYNTHETIC
PLOT_SYN_SPECTRUM This calls make_chianti_spec to produce the
intensity vs. wavelength plot.
SYN_MAIN_EVENT This handles the widget operations
SYN_WID This creates the widgets.
COMMON BLOCKS:
many
RESTRICTIONS:
SIDE EFFECTS:
EXAMPLE:
IDL> ch_ss
CATEGORY:
spectral synthesis.
WRITTEN :
Ver.1, 7-Nov-01, Giulio Del Zanna (GDZ) and Peter Young (PRY)
MODIFICATION HISTORY:
V.2, 7-Nov-01, GDZ . Fixed a small bug (now the spectrum plot is always
plotted within the widget), and modified the option to add continua.
Changed the suggested names of the outputs.
Corrected a bug when creating an IDL save file with the spectrum, when
no line details are present.
V.3 28-Jan-02 GDZ
fixed a bug in the density text widget, added a few buttons
and options, including the effective area.
Added noprot, rphot, radtemp keywords to the call to ch_synthetic
V 4, 18-Apr-2002, GDZ
Added photoexcitation, changed IDL save files to FITS files,
V.5, 21-May-2002, GDZ
fixed a few small bugs: checking min_abund before calculating the
spectrum; checking the ioneq file when
restoring the structure; changed the status of
all lines; chnaged the font system.
generalized directory concatenation to work for
Unix, Windows and VMS.
V.6, 15-July-2002, GDZ - New major revision.
Changed the chianti top directory (for Effective areas).
Changed Linear/Log button.
Rearranged the sizes of the buttons and added a special cursor to
highlight the area where details of the lines will be given. Works
only in linear scale.
Added quite a lot of new checks to avoid crashes and
fixed the problem with the zoom/unzoom/change units.
V.7, 2-Aug-02, GDZ
Modified the output labels on the plot, inside and on the axis.
Also modified a few minor things like the appearance of the Log T,EM
values.
Fixed a bug when creating the latex output.
Now it restores at the end previous colors and settings.
V.8, 8-Aug-02, GDZ
Changed the CHIANTI system variables. Fixed.
Also fixed a problem with the element ab. file.
V.9, 13-Aug-02, GDZ
Restored the correct use of ch_line_int, now only the lines in the
plot window are listed, and the ALL keyword is in use.
Now the correct xrange is loaded into COMMON when line int. are
restored. Now it checks if all ions were in the structure, when
restoring the line intensities, and flags the widget button accordingly.
Added a device,decomposed=0. to remove problems with colors.
Corrected the use of the DEM, IONEQ and ABUND pulldown menus,
avoiding conflicts between files in the working and CHIANTI
directory having the same name.
Added printing of references for ancillary files, and a check on the
element abundances vs. the elements present in the structure.
V.10, 7-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
Replaced f9.4 with f11.4 format for the wavelengths.
Some minor modifications to the widget.
Added extended details in the ascii output spectrum.
Added more explanations in the HELP buttons.
V.11, 22-Jul-2005 GDZ
-Added keV option and a few more extra checks.
V.12, 2-Aug-2005 GDZ
put RETAIN=2 in the main plotting window.
TO DO LIST:
Control the range of Angstroms when clicking
kev
Allow plots in intensities instead of intensities A-1
VERSION : V.12, 2-Aug-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
CH_SYNTHETIC
PURPOSE:
to calculate CHIANTI line intensities or G(T) and output an IDL structure.
PROCEDURE:
This routine calculates as default line intensities for a user-specified
differential emission measure and ionisation balance. The actual
creation of a synthetic spectrum (i.e., wavelength vs. intensity)
is performed by other routines - see CH_SS.PRO and
MAKE_CHIANTI_SPEC.PRO.
Note that this routine does not include the element abundances
in the line intensities, as this will be performed by
make_chianti_spec. One of the reasons why element abundances are not
included in the line intensities calculation is so that it is easier
for the user to see how modifying abundances affects their spectra in
e.g. CH_SS.PRO.
The calculations are performed at constant pressure or
at constant density.
The routine can also output line intensities calculated with an
isothermal approximation.
If the isothermal approximation is not used, then the user will be asked
to select two files, that can either be in the
standard CHIANTI database or in the working directory.
These files are:
- an ionization fraction file
- a differential emission measure (DEM) file.
The routine can also output the contribution functions G(T) of the lines,
instead of the intensities, if the keyword GOFT is used. In this case,
only the ionization equilibrium file needs to be selected.
The G(T), or intensity per emission measure, is calculated as:
G=(hc/lambda_ij)*A_ji*(N_j(X^+m)/N(X^+m))*(N(X^+m)/N(X))/ N_e /(4.*!pi)
where A_ji is the A-value of the transition;
(N_j(X^+m)/N(X^+m)) is the population of the upper level,
calculated by solving the statistical equilibrium equations;
(N(X^+m)/N(X)) is the ionization equilibrium
N_e is the electron density.
unless /PHOTONS is set, in which case the (hc/lambda_ij) factor
is not included.
If not specified otherwise, with the use of the MASTERLIST or SNG_ION
keywords, then the standard masterlist of the ions, which has
all the ions in the current CHIANTI database, is used.
PROGRAMMING NOTES
The DEM is not assumed to be specified at 0.1 logT intervals (which
is how the ion fraction are specified). Thus this routine reads
in the DEM vs. logT information and then uses the IDL spline
function to tabulate the DEM over 0.1 logT intervals. The minimum
and maximum temperatures are those in the DEM file, rounded up to
the nearest 0.1. The new DEM function tabulated over 0.1 logT
intervals is contained in 'dem_int'.
For some of the dielectronic files, radiative decays that were in
the standard .wgfa file will also be present in the dielectronic
version of the .wgfa file. In these cases the line intensity
produced from the latter file needs to be ignored and so we have a
check in ch_synthetic to do this. An example is the 1-7 decay in
the ca_19.wgfa and ca_19d.wgfa files. In the latter case, the
model of the ion does not include electron excitation to level 7
and so the model for the 1-7 decay is incorrect, hence we ignore
it.
CATEGORY:
spectral synthesis.
CALLING SEQUENCE:
IDL> ch_synthetic,wmin,wmax, output=output, pressure=pressure,$
[MODEL_FILE=MODEL_FILE, err_msg=err_msg, msg=msg, $
density=density,all=all,sngl_ion=sngl_ion, $
photons=photons, masterlist=masterlist, $
save_file=save_file , verbose=verbose, $
logt_isothermal=logt_isothermal,$
logem_isothermal=logem_isothermal,$
goft=goft, ioneq_name=ioneq_name, dem_name=dem_name,$
noprot=noprot, rphot=rphot, radtemp=radtemp, progress=progress ]
INPUTS:
Wmin: minimum of desired wavelength range in Angstroms
Wmax: maximum of desired wavelength range in Angstroms
PRESSURE: pressure in emitting region (Pe, cm^-3 K).
Only a single value is accepted, and the calculation is
performed at constant pressure.
OPTIONAL INPUTS :
DENSITY: density in emitting region (Ne, cm^-3).
Only a single value is accepted, and the calculation is
performed at constant density, unless LOGT_ISOTHERMAL is
defined. In this case, DENSITY can be an array of values, but
has to have the same number of elements as LOGT_ISOTHERMAL.
MODEL_FILE Full path of the (Te,Ne) file if defined.
This file should have two columns, one with the Te (K)
values, and one with the Ne (cm^-3) values. If these
values are not sorted in ascending order of Te, the
routine does sort them.
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
IONEQ_NAME: Name of the ionization equilization name to use. If not
passed, then the user is prompted for it.
DEM_NAME: Name of the DEM file to used. If not passed, then the user
is prompted for it.
LOGT_ISOTHERMAL
Array of logarithmic temperatures.
If defined, the emissivities are calculated with an
isothermal approximation. The values are sorted in ascending
order.
LOGEM_ISOTHERMAL
Array of logarithmic emission measures.
If defined, the emissivities are calculated with an
isothermal approximation. The values are sorted in ascending
order. If LOGT_ISOTHERMAL is specified without
LOGEM_ISOTHERMAL then the emission measures are set to 1
(logem_isothermal=0).
RADTEMP The blackbody radiation field temperature (default 6000 K).
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
OUTPUTS:
OUTPUT: The name of the structure containing the line intensities and
details.
The tags of the structure are:
.lines A structure containing information about the lines.
Its size is the number of lines in the spectrum. The
tags are:
.iz The atomic number of the elements (e.g., 26=Fe)
.ion The ionisation stage (e.g., 13=XIII)
.snote The identification of the ion (e.g., 'Fe XXIV d')
.ident The identification of the transition, configuration
and terms in text form.
.ident_latex
The identification of the transition, configuration
and terms in latex form.
.lvl1 The lower level of the transition (see .elvlc
file for ion)
.lvl2 The upper level for transition.
.tmax The temperature of maximum emission of the line.
If the G(T) are output, tmax is the maximum of G(T).
If the isothermal approximation is used tmax=0.
If a DEM is used, tmax is the maximum of the
emissivity that includes the product of the ion
fraction and the DEM.
Rounded to nearest 0.1
.wvl Wavelength of the transition, in Angstroms.
.flag A flag, =-1 if the line has only theoretical energy
levels. Otherwise flag=0.
.int Intensity of line (erg/cm2/s/sr or phot/cm2/s/sr),
divided by the element abundance (exclusive with .goft).
.goft The G(T) of the line (optional /exclusive with .int).
.ioneq_name The ion balance file used (full path).
.ioneq_logt The Log10 T values associated.
.ioneq_ref The references.
.dem_name The differential emission measure file eventually used
(full path).
.dem The Log10 DEM values
.dem_logt The Log10 T values associated.
.dem_ref The references.
.model_name A string indicating the model used:
1- Constant density
2- Constant pressure
3- Function (Te,Ne)
.model_file Full path of the (Te,Ne) file if defined. Null string otherwise.
.model_ne the Ne value(s).
- a scalar if 'Constant density' is selected.
- an array if 'Function' is selected.
- 0. if constant pressure is selected.
.model_pe the Pe value.
- a scalar if constant pressure is selected.
- 0. if 'Constant density' is selected.
- an array=density*temperature if 'Function' is selected.
.model_te the Te values if 'Function' is selected. Otherwise 0.
.wvl_units The wavelength units.
.wvl_limits The wavelength limits specified by the user.
.int_units The intensity units.
1) If LOGT_ISOTHERMAL is defined, we have two cases:
a) LOGEM_ISOTHERMAL is not defined, and is therefore
assumed to be 0 (EM=1). In this case, units are
'photons cm+3 sr-1 s-1' or 'erg cm+3 sr-1 s-1'.
b) LOGEM_ISOTHERMAL is defined. In this case, units are
'photons cm-2 sr-1 s-1' or 'erg cm-2 sr-1 s-1'.
2) If LOGT_ISOTHERMAL is not defined, we have two cases:
a) intensities are calculated. In this case, units are
'photons cm-2 sr-1 s-1' or 'erg cm-2 sr-1 s-1'.
b) Contribution functions G(T) are calculated. In this
case, units are
'photons cm+3 sr-1 s-1' or 'erg cm+3 sr-1 s-1'.
.logt_isothermal
The Log10(T) values used.
.logem_isothermal
The Log10(EM) values used.
.date The date and time when the structure was created.
.version The version number of the CHIANTI database used.
.add_protons
A flag (0/1) to indicate whether proton data were used (1)
or not (0) to calculate the level population.
.photoexcitation
A flag (0/1) to indicate if photoexcitation was included (1)
or not (0).
.radtemp
The blackbody radiation field temperature used (if
photoexcitation was included).
.rphot
Distance from the centre of the star in stellar radius units
(if photoexcitation was included).
OPTIONAL OUTPUTS:
SAVE_FILE: If defined, then an IDL save file is created, with the output
structure.
GOFT: If set, the G(T) of the lines are calculated, and put in
the output structure, instead of the line intensities.
Units are 'photons cm+3 sr-1 s-1' or 'erg cm+3 sr-1 s-1'
KEYWORDS:
ALL: if set, then all lines are included. This means that lines for
which only an approximate wavelength is known,
denoted by a negative wavelength value in the .wgfa file, are
included. These are the lines for which there are no observed
energy levels.
PHOTONS: The output intensities will be in photons instead of
ergs.
VERBOSE: If set, the routine will list each ion it is looking at,
and how many lines from each ion it is including in the
spectrum.
GOFT: If set, the G(T) of the lines are calculated, and put in
the output structure, instead of the line intensities.
Units are 'photons cm+3 sr-1 s-1' or 'erg cm+3 sr-1 s-1'
NOPROT Switch off the inclusion of proton rates in the level
balance (default).
PROGRESS If set, a widget appears, showing the progress of the
calculation and allowing the user to halt the calculation.
NO_SUM_INT Prevents the summing of intensities over temperature.
Only works in conjunction with the LOGT_ISOTHERMAL
option, and is implemented in order to work the
ISOTHERMAL routine. The .INT tag in OUT.LINES becomes
an array with the same number of elements as
LOGT_ISOTHERMAL, corresponding to the intensities at
each temperature.
CALLS: CH_GET_FILE
many CHIANTI standard routines, including:
READ_IONEQ, READ_DEM, READ_MASTERLIST, ION2SPECTROSCOPIC,
ZION2FILENAME, READ_WGFA,READ_ELVLC,READ_SPLUPS,POP_SOLVER,
DESCALE_UPS, CONVERT_TERMS.
CONVERT_TERMS uses some standard SolarSoft routines:
REPSTR, STR_INDEX, DATATYPE,
VALID_NUM, DELVARX, INFO_PROGRESS, SAVEGEN
COMMON BLOCKS:
wgfa, wvl,gf,a_value
upsilon,splstr
elvlc,l1a,term,conf,ss,ll,jj,ecm,eryd,ecmth,erydth,eref
elements,abund,abund_ref,ioneq,ioneq_logt,ioneq_ref
radiative, radt, dilute
proton, pstr
ionrec,rec_rate,ci_rate,temp_ionrec,luprec,lupci,status
RESTRICTIONS:
SIDE EFFECTS:
CATEGORY:
spectral synthesis.
EXAMPLE:
This routine can be called in this way:
IDL> ch_synthetic,5.,10., output=structure, pressure=1.e+15
To make use of the output structure, use MAKE_CHIANTI_SPEC or CH_SS
PREV. HIST. :
Based on synthetic.pro, written by Ken Dere
WRITTEN :
Ver.1, 22-Jun-00, Peter Young (PRY) and Giulio Del Zanna (GDZ)
MODIFICATION HISTORY:
Ver.1, 22-Jun-00, Peter Young and Giulio Del Zanna
Ver.2, 25-Jul-00, PRY
Removed /all keyword; make_chianti_spec can be
used to filter out negative wavelengths.
Added flabel tag to output in order to pick out
dielectronic recombination lines.
Ver.3, 4-Oct-00, PRY
Replaced /all keyword.
Corrected bug when .wgfa files contain two A-values
for the same transition.
Ver.4, 5-Oct-00, PRY
Corrected bug that gave rise to lines from the same
transition when the dielectronic file existed.
V.5, 11-Oct-2000, GDZ
eliminate the abundance call; reinstate the /masterlist keyword;
added the tag ident_latex to have the identification in
late-style format; added a tag flag=-1 for the unobserved lines,
and =0 otherwise; reinstated all wavelengths > 0. ;
added the calculation of the G(T);
added a few other tags in the output, and various checks and
comments.
V.6 15-Oct-2000 ,GDZ
Replaced calls to solarsoft routines to standard IDL ones.
Corrected an error in the output creation, in relation to the
isothermal case. Added isothermal in the output. added checks to
the wavelengths. Default output name is TRANSITIONS. changed
const_net and added const_net_value + a few other things.
v.7, 27-Nov-2000, GDZ. Corrected an error in the calculation of the
G(T).
Version 8, 5-Dec-2000, GDZ, DAMTP. Fixed a bug when checking the
values in the .splups files.
V. 9, GDZ, 10-Apr-2001, corrected another error in the G(T) calc.
V. 10, GDZ, 30-Oct-2001 added CHIANTI Version number, changed isothermal
to logt_isothermal and added logem_isothermal to the output.
Removed the use of log T values, and the calculation.
Added err_msg, a text string with an error message.
Version 11, 8-Nov-01, GDZ
Changed the MASTERLIST keyword. Allowed double use, as a keyword
and as a string.
Version 12, 18-Nov-01, Peter Young
Added /NOPROT, RPHOT and RADTEMP keywords; changed upsilon
common block.
Version 13, 29-Apr-02, GDZ
Added no_protons, photoexcitation, rphot, radtemp
tags into the output structure.
Revised Header. Added the PROGRESS widget.
Added a check if the ion is present in the Ion. Frac. file.
Added informative MSG keyword.
Now uses savegen.pro to save the structure.
V. 14, 28-May-2002, GDZ:
generalize directory concatenation to work for Unix, Windows
and VMS.
modified tags:
limits -> wvl_limits
ioneq_t -> ioneq_logt
wvlunits -> wvl_units
intunits -> int_units
time --> date
no_protons -> add_protons
dem_t -> dem_logt
const_nte -> model_name
const_nte_value -> model_ne, model_pe, model_te
removed from the main STR: .ioneq ctemp
removed from the LINES STR: fwhm flabel
Added model_file input for model Ne(T). Had to considerably
modify the routine.
V. 15, 16-Jul-2002, Peter Young
Added keyword /NO_SUM_INT.
V. 16, 22-Jul-2002, Peter Young
Corrected a bug related to /NO_SUM_INT; logt_isothermal
can now be specified without logem_isothermal.
V. 17, 23-July-2002, GDZ
Modified a few checks on the input. Also, now it prints the
error message whenever the program aborts
V.18, 2-Aug-02, GDZ
Replaced all DBLARR and DOUBLE calls with floats.
Added a comment at the end of the routine when it finishes.
V.19, 8-Aug-02, GDZ
Added more error info. Changed the use of the DENSITY
keyword. It is possible to input an array of values if
LOGT_ISOTHERMAL is defined.
V. 20, 17-Sep-02, GDZ
Corrected a bug: the functional (T,N) form
is now only accepted if DENSITY is an array with at least two
values.
V. 21, 19-Sep-02, GDZ
Corrected the definition of the UNITS in case LOGT_ISOTHERMAL
is defined.
V. 22, 19-Aug-03, Peter Young
when logem_isothermal is input, the derived EM is now a
DOUBLE array rather than FLOAT, preventing infinities when
logem_isothermal values are large.
V. 23, 4-Oct-2003, GDZ
modified the input to POP_SOLVER, now it is dealt with an
input structure.
V.24, 10-Oct-2003, K.Dere
added modifications from K.Dere, regarding the satellite
lines.
V 25, 3-Nov-2003, GDZ
Added GROUP keyword, and modified so the progress widget can
be stopped within IDL Windows.
V 26, 17-Apr-2004, Enrico Landi (EL)
Added the recombination/ionization population processes.
V.27, 13-Apr-2005, EL
Replaced the main loop to calculate individual line intensities
with operations among arrays, to speed the whole program in case
of large numbers of lines.
VERSION : 27, 13-Apr-2004
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
SYNTHETIC
PURPOSE:
calculates a synthetic spectrum
PROCEDURE:
Calculations are done assuming either constant density or
constant pressure. See CH_SYNTHETIC for details.
CALLING SEQUENCE:
SYNTHETIC,Wmin, Wmax, Fwhm, Pressure= , Lambda, Spectrum ,List_wvl, List_ident
,[/all, density=, /cont, min_abund=]
INPUTS:
Wmin: lower limit of the wavelength/energy range of interest (Angstroms)
Wmax: upper limit of the wavelength/energy range of interest (Angstroms)
Pressure: pressure in emitting region (cm^-3 K), or
Density: density in emitting region (cm^-3).
Fwhm: gaussian full width at half maximum of the resolution of the output
spectrum, for example, to correspond to an observed spectrum
OPTIONAL INPUTS:
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
MIN_ABUND: If set, calculates the continuum only from those elements which
have an abundance greater than min_abund.
DEM_NAME: Name of the DEM file to used. If not passed, then the user
is prompted for it.
ABUND_NAME: Name of the abundance file to use. If not passed, then
the user is prompted for it.
IONEQ_NAME: Name of the ionization equilization name to use. If not
passed, then the user is prompted for it.
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
RADTEMP The blackbody radiation field temperature (default 6000 K).
OUTPUTS:
Lambda: wavelength array of calculated synthetic spectrum
Spectrum: intensity array (erg cm^-2 s^-1 str^-1 Ang^-1),
unless keyword photons is set then output is is
photons cm^-2 s^-1 str^-1 Ang^-1
List_wvl: a list of wavelengths for use with synthetic_plot.pro
List_ident: a list of line identifications for use with
synthetic_plot.pro
OPTIONAL OUTPUTS:
KEYWORD PARAMETERS:
ALL: if set, then all lines are included. This means that lines for which
only an approximate wavelength is known (only theoretical energy
levels are known) are included.
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
CONTINUUM: if set, then the continuum (free-free, free-bound and
two-photon) are included
MIN_ABUND: If set, calculates the continuum only from those elements which
have an abundance greater than min_abund. Can speed up the
calculations. For example, from Allen (1973):
abundance (H) = 1.
abundance (He) = 0.085
abundance (C) = 3.3e-4
abundance (O) = 6.6e-4
abundance (Si) = 3.3e-5
abundance (Fe) = 3.9e-5
PHOTONS: if set, intensities are in photons cm^-2 s^-1 sr^-1 Ang^-1
DEM_NAME: Name of the DEM file to used. If not passed, then the user
is prompted for it.
ABUND_NAME: Name of the abundance file to use. If not passed, then
the user is prompted for it.
IONEQ_NAME: Name of the ionization equilization name to use. If not
passed, then the user is prompted for it.
NOPROT If set, then proton rates are not included.
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
CALLS:
CH_SYNTHETIC, MAKE_CHIANTI_SPEC, READ_ABUND, STRPAD
COMMON BLOCKS: None
RESTRICTIONS:
SIDE EFFECTS:
EXAMPLE:
> synthetic,100.,200.,.1, pressure=1.e+16,lambda,spectrum,list_wvl,list_ident
CATEGORY:
spectral synthesis.
WRITTEN :
Version 1, 8-Nov-01, Giulio Del Zanna (GDZ).
Rewritten as a wrapper routine using the new procedures.
Compared to the previous SYNTHETIC, these are the main changes:
1-Now the PRESSURE value is a keyword as the DENSITY value
2-The keyword CONT is now renamed CONTINUUM
3-Added keywords PHOTONS, DEM_NAME, ABUND_NAME, IONEQ_NAME
4-MASTERLIST can now be used both as an input string or as a keyword.
5-The description of the line details now has the spectroscopic
designation at the end.
MODIFICATION HISTORY:
Version 2, 18-Nov-01, Peter Young
Added /noprot, rphot and radtemp keywords.
Version 3, 11-Dec-01, Peter Young
Changed call to ch_strpad to strpad.
Version 4, 28-Apr-02, GDZ, changed the call to make_chianti_spec and the
continuum keyword.
V. 5, 22-May-2002 GDZ. Removed const_net definitions.
V.6, 14-Feb-2003 GDZ.
Fixed a bug (keyword PHOTONS was not active).
VERSION : 6, 14-Feb-2003
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
synthetic_plot
PURPOSE:
to plot out synthetic spectra calculated with Synthetic
and interactively identify spectral lines
CATEGORY:
spectroscopy
CALLING SEQUENCE:
SYNTHETIC_PLOT,Wvl,Spectrum,List_wvl,List_ident,fwhm
INPUTS:
Wvl: wavelength array from synthetic
Spectrum: spectrum intensity array from synthetic
List_wvl: string array of spectral line wavelengths
List_ident: string array of spectral line identifications
Fwhm: when the cursor is clicked, spectral lines with fwhm
(Angstroms) of the cursor are printed out
KEYWORDS
xrange: similar to IDL keyword to determine wavelength range of plot
OUTPUTS:
None
PROCEDURE:
Click the left mouse button to select a wavelength
Click the right mouse button to exit
EXAMPLE:
> synthetic,100.,200.,.1,1.e+15,wvl,spectrum,list_wvl,list_ident
> synthetic_plot,wvl,spectrum,list_wvl,list_ident,0.1
note: it is not necessary for the two fwhm values to be the same
MODIFICATION HISTORY:
Written by: Ken Dere
May 1996: Version 2.0
Dec. 1998: revised by Ken Dere
V.4, 23 Oct 2000 GDZ, added the log keyword, and changed a few things
in the plot.
Ver.5, 12-Dec-2001, Peter Young
Changed style of printing, and made method of extracting the
intensity from list_ident compatible with the new version of
isothermal.pro.
VERSION 5 12 Dec 2001 Peter Young
NAME
ISOTHERMAL
PURPOSE:
Computes spectra from isothermal plasmas. A number of isothermal
plasmas can be included.
Note that this routine has a number of unique features that
distinguish it from the other CHIANTI synthetic spectra routines.
See the Programming Notes section.
INPUTS:
WMIN Minimum of desired wavelength range in Angstroms.
WMAX Maximum of desired wavelength range in Angstroms.
WAVESTEP Bin size of spectrum (in Angstroms)
TEMP Electron temperature (or array).
OPTIONAL INPUTS
PRESSURE Electron pressure in units of cm^-3 K.
EDENSITY Electron density in units of cm^-3.
EM Emission measure. The units of EM govern the intensity
units of the emission lines (i.e., column or volume
emission measure units). If EM is not specified, then the
emission measure is set to (N_e * N_H) where N_e is
derived from the user-specified PRESSURE or EDENSITY,
and N_H is derived from the routine PROTON_DENS.PRO.
SNGL_ION Rather than include the entire list of CHIANTI ions in
the calculation, this input can be used to select a
single ion, or a number of different ions. E.g.,
SNGL_ION='s_2' or SNGL_ION=['s_2','s_3','s_4'].
RADTEMP The blackbody radiation field temperature (default 6000 K).
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
MASTERLIST The list of ions that will be considered for the
spectrum is contained in the masterlist file in the
CHIANTI directories. The user can specify his own file
through this keyword. E.g.,
masterlist='/user/home/masterlist.ions'
ABUND_NAME: Name of the abundance file to use. If not passed, then
the user is prompted for it.
IONEQ_NAME: Name of the ionization equilization name to use. If not
passed, then the user is prompted for it.
KEYWORDS
NOPROT Switch off the inclusion of proton rates in the level
balance.
ERGS The units of the output spectrum are by default in photons.
Setting /ERGS switches to erg units.
CONT Adds continuum (free-free, free-bound, two-photon) to
spectrum.
OUTPUTS:
LAMBDA Wavelength array of calculated synthetic spectrum.
SPECTRUM Intensity array. The units depend on the user inputs to
ISOTHERMAL -- see note below.
LIST_WVL A list of wavelengths for use with synthetic_plot.pro
LIST_IDENT A list of line identifications for use with
synthetic_plot.pro
PROGRAMMING NOTES
Intensity Units
---------------
The units are of the form photons cm^3 s^-1 sr^-1 * (units of EM),
changing to ergs if the /ergs keyword is set.
The volume emission measure (N_e*N_H*V) has units cm^-3.
The column emission measure (N_e*N_H*h) has units cm^-5.
Unique features
---------------
The emission lines in the final spectrum have no width and thus
each occupies a single pixel of the spectrum. The size of the
pixels are set by WAVESTEP.
As stated above, the units of the output spectrum are
photons cm^3 s^-1 sr^-1, i.e., there is no "per angstrom" term.
This means that (i) the height of the emission lines in the
spectrum does not change with varying WAVESTEP, and (ii) the height
of continuum does change with WAVESTEP.
COMMON BLOCKS
ELEMENTS
CALLS
CH_SYNTHETIC, READ_ABUND, CH_GET_FILE, CONCAT_DIR, FREEFREE,
FREEBOUND, TWO_PHOTON
HISTORY
Ver.1, 8-Apr-02, Peter Young Rutherford Appleton Laboratory,
p.r.young@rl.ac.uk
Tries to replicate the behaviour of the original ISOTHERMAL which
was found in earlier versions of CHIANTI (v.3 and earlier).
MODIFICATION HISTORY
Ver. 2, Giulio Del Zanna (GDZ), 28-Apr-02
Added abund_name,ioneq_name keywords.
Also, added photons keyword in call to MAKE_CHIANTI_SPEC.
Ver. 3, Peter Young, 24-May-02
Modified to produce arrays of spectra when an array of
temperatures is given
V.4, GDZ, 28-May-02
Added a couple of checks on file existence and modified the call
to ch_synthetic and make_chianti_spec due to change of keyword
names.
V.5, Peter Young, 16-Jul-02
Restructured routine to avoid crashes when a large number of
temperatures is input.
V.6, 8-Aug-02 GDZ
Added one error checking
V.7, 18-Aug-03, Peter Young
Added EM= keyword.
VERSION :
Version 6, 8-Aug-02
PROJECT : CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME : MAKE_CHIANTI_SPEC
PURPOSE :
To create a CHIANTI synthetic spectrum
CALLING SEQUENCE:
IDL> make_chianti_spec, TRANSITIONS, LAMBDA, SPECTRUM,$
[BIN_SIZE= , ,INSTR_FWHM= , PIXEL=PIXEL, BINSIZE = BINSIZE, $
WRANGE= , ALL=ALL, continuum=continuum, $
ABUND_NAME= , MIN_ABUND=, photons=photons, effarea=effarea
PROCEDURE :
From information contained in the structure TRANSITIONS, constructs
a synthetic spectrum
By default, routine assumes thermal widths for lines.
PROGRAMMING NOTES
The line profile is constructed using the IDL gaussint routine.
For a wavelength pixel centred at l and with width dl, gaussint
is used to integrate the Gaussian up to l-dl/2 and up to l+dl/2.
The difference between the two is the intensity in this pixel.
INPUTS :
TRANSITIONS, the structure created by ch_synthetic.pro.
OPT. INPUTS :
LAMBDA Array of wavelengths (X-values). If not defined as input, it is
calculated on the basis of BIN_SIZE, and returned as an output.
If defined as input, the routine checks that there are at least
10 points in the wavelength range defined by WRANGE. If there
are, the corresponding subset of LAMBDA is returned, otherwise
the routine exits with an error.
BIN_SIZE Bin size in Angstroms of the spectrum to be created. A linear
spectrum is assumed. In case an effective area file is used, the
wavelenghts in the file (that might not be linear) are used to
create the spectrum, and this bin size looses any meaning.
WRANGE Allows a subset of the wavelength range to be turned into
a spectrum. When using syn_plot, this speeds up the routine
a lot if you've elected to zoom in on a region.
INSTR_FWHM Instrumental FWHM (Angstroms).
In case an effective area file is used, The line intensities
contributing to each bin are summed, and subsequently convolved
with a gaussian of full-width-half-maximum FWHM if FWHM is not
set = 0 . Please make sure that the FWHM value (if not set to
zero) is larger than the bin size.
ABUND_NAME A CHIANTI abundance file name can be set.
It allows the abundance file given in transitions.abund_name
(if present) to be over-ridden. Note that it also used for
the continuum calculation.
MIN_ABUND: If set, calculates line intensities only from those elements
which have an abundance greater than min_abund.
Can speed up the calculations. For example, from Allen
(1973):
abundance (H) = 1.
abundance (He) = 0.085
abundance (C) = 3.3e-4
abundance (O) = 6.6e-4
abundance (Si) = 3.3e-5
abundance (Fe) = 3.9e-5
FILE_EFFAREA
The Effective Area File (TWO COLUMNS - wavelengths in
Angstroms and cm^2 values) If defined, then the spectrum is
multiplied with these values. Any input LAMBDA value is
over-written by the wavelenghts in the file (that might not
be linear) and are used to create the spectrum.
Note that this option only works well if a sufficient number
of bins is given. The line intensities contributing to each
bin are summed, and subsequently convolved with a gaussian
of full-width-half-maximum FWHM, if FWHM is not set = 0.
Please note that the convolution might not work if a small
number of bins is defined.
OUTPUTS :
LAMBDA Array of wavelengths (X-values).
If not defined as input, it is
calculated on the basis of BIN_SIZE, and returned as an output.
If defined as input, the routine checks that there are at least
10 points in the wavelength range defined by WRANGE. If there
are, the corresponding subset of LAMBDA is returned, otherwise
the routine exits with an error.
SPECTRUM A structure containing all the information:
LAMBDA The array of X-values
SPECTRUM The array of Y-values
UNITS The units of LAMBDA, SPECTRUM
INSTR_FWHM The Instrumental FWHM
BIN_SIZE Width of the Bins (fixed) in angstroms
ABUND_NAME The CHIANTI abundance file name
ABUND The abundance values
MIN_ABUND The minimum abundance value used
ABUND_REF The references
CONTINUUM The values of the continuum (if calculated)
FILE_EFFAREA The Effective Area File used (optional)
EFFAREA The array of effective area values
(optional - same size of LAMBDA)
.LINES An array of structures, for all the lines used
to calculate the SPECTRUM.
The tags are the same as those created by
CH_SYNTHETIC, plus
.PEAK The peak intensity of the line in the spectrum
(approx. value)
OPT. OUTPUTS:
BINSIZE If BIN_SIZE is not specified, then the spectrum
bin-sizes are computed automatically, and the size of the
bin returned in BINSIZE.
KEYWORDS :
PIXEL The spectrum is given in /pixel units rather /ang
(DISABLED)
ALL Add lines that originally had negative wavelengths
PHOTONS If set=1, the output intensities will be in photons instead of
ergs.
CONTINUUM
If set, then the continuum is added to the
spectrum.
verbose
CALLS :
PRY: GET_ATOMIC_WEIGHTS
Chianti: FREEBOUND, FREEFREE
COMMON (with freefree freebound and two_photon):
elements,abund,abund_ref,ioneq,ioneq_logt,ioneq_ref
RESTRICTIONS: The input structure has to be of the type created by ch_synthetic.
The LAMBDA, EFFAREA values must be ordered in wavelength and the
LAMBDA values must be in Angstroms.
SIDE EFFECTS: None known yet.
EXAMPLES :
make_chianti_spec, output_struct, LAMBDA, SPECTRUM,$
bin_size=0.01, instr=0.1
CATEGORY :
spectral synthesis.
PREV. HIST. :
WRITTEN :
Peter Young , CfA, pyoung@cfa.harvard.edu 1-Sept-2000
MODIFICATION HISTORY:
Version 1, PRY 1-Sept-2000
Version 2, Giulio Del Zanna (GDZ) 10-Oct-2000
put ALL keyword, removed the FWHM obsolete and
confusing call. Reorganised various minor things.
Version 3, PRY 19-Oct-2000
Corrected the way continuum is treated for an isothermal
spectrum.
V. 4, 2-Nov-2001 GDZ. Now MIN_ABUND is effective not only in the
continuum calculation but also in the line spectrum.
Modified for the use of logt_isothermal
V.5, GDZ, added EFFAREA keyword: an ascii file with lambdas and
effective areas can be read
in. The line intensities are
calculated in a different way.
Also, changed the output.
V.6, GDZ, 28-Apr-02 redefined completely the OUTPUT structure.
Major revision (added two_photon verbose).
V.7, GDZ, 3-May-2002
fixed a bug, when negative angpix values occur.
V.8, GDZ, 22 May 2002, changed some tags of the output, and
added min_abund in the continuum call.
V.9, GDZ, 30-May-02 replaced fix() with round()
V. 10, 15-July-2002 , GDZ
changed the location of Effective area files.
V.11 14-Aug-02, GDZ
speeded up the routine, by changing the way the PEAK tag is
added to the structure. The drawback is that only the
'standard v.4 tags' are allowed, and future additions will
have to be dealt properly.
v.12 2-Dec-2002, GDZ.
Fixed a bug: Removed the plotting of the window with the effective areas.
v.13 26-Apr-2005, Enrico Landi (EL)
Fixed a minor bug: if the lines were more than 32768 (2^15), the main
loop crashed.
v.14 22-Jul-2005 GDZ
-fixed a bug. When the routine was run once without
defining the lambdas, and then with the lambdas
defined (the units were switched to photons)
-fixed a bug. When the effective areas were used,
all lines were used to create the spectrum.
-added hard-wired switch to photons when using
effective area files.
-added the keV option
-now can output a spectrum only with the continuum
(i.e. even if no emission lines are present).
15, 2-Aug-2005, GDZ
Added a check on the input structure. If it was
calculated with ch_synthetic and the keyword
/no_sum_int, it cannot be used here.
VERSION : 15, 2-Aug-2005
STILL TO DO:
-speed up the routine with the use of arrays.
-add the option to select only a list of ions, also in the
continuum procedures.
-Allow the use of user-defined line profiles.
-Enable PIXEL keyword
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
ASCII_WVL_DEM
PURPOSE:
create an ascii file of predicted spectral line intensities and
wavelengths corresponding to a selected abundance and differential
emission measure (DEM).
PROCEDURE:
Calculations are done assuming either constant density or
constant pressure. See CH_SYNTHETIC for details.
CALLING SEQUENCE:
ASCII_WVL_DEM, Wmin, Wmax, Pressure= , [density= ], $
[outfile= , mini= , sngl_ion=, /photons, /all, /masterlist], $
[/noprot, radtemp=, rphot=]
INPUTS:
Wmin: lower limit of the wavelength range of interest (Angstroms)
if kev keyword set, then wmin is in kev
Wmax: upper limit of the wavelength range of interest (Angstroms)
if kev keyword set, then wmax is in kev
Pressure: pressure in emitting region (cm^-3 K), or
Density: density in emitting region (cm^-3).
OPTIONAL INPUTS:
OUTFILE: the name of the output ascii file to be written.
MINI: Minimum intensity for a line to be included in the output.
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
OUTPUTS:
an ascii file: linelist.txt in the working directory by default
OPTIONAL OUTPUTS:
KEYWORD PARAMETERS:
MINI: Minimum intensity for a line to be included in the output
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
PHOTONS: units will be in photons rather than ergs
KEV: wavelengths will be given in kev rather than Angstroms
ALL: if set, then all lines are included. This means that lines
for which
only an approximate wavelength is known (only theoretical energy
levels are known) are included.
OUTFILE: the name of the output ascii file to be written. By
default a
file 'linelist.txt' in the user's working directory will be
created.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
CALLS:
CH_SYNTHETIC, CH_LINE_LIST
COMMON BLOCKS: None
RESTRICTIONS:
SIDE EFFECTS:
EXAMPLE:
IDL> ascii_wvl_dem,400.,800., out='linelist',$
pressure=1.e+15,mini=1.,sngl_ion='o_4'
CATEGORY:
spectral synthesis.
WRITTEN :
Version 1, 8-Nov-01, Giulio Del Zanna (GDZ).
Compared to the previous ASCII_WVL_DEM, these are the main changes:
1-Rewritten as a wrapper routine using the new procedures.
2-Now the PRESSURE value is a keyword.
3-The calculations can be done at constant DENSITY.
4-Energies (keV) can be output instead of wavelengths in Angstroms
5-MASTERLIST can now be used both as an input string or as a keyword.
MODIFICATION HISTORY:
18-Nov-01, Peter Young
Added /noprot, rphot and radtemp keywords
V. 2, 22-May-2002 GDZ. Removed const_net definitions.
VERSION : 2, 22-May-2002
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
LATEX_WVL_DEM
PURPOSE:
create a latex file of predicted spectral line intensities and
wavelengths corresponding to a selected abundance and differential
emission measure (DEM)
PROCEDURE:
Calculations are done assuming either constant density or
constant pressure. See CH_SYNTHETIC for details.
CALLING SEQUENCE:
LATEX_WVL_DEM, Wmin, Wmax, Pressure= , [density= ], $
[outfile= , mini= , sngl_ion=, /photons, /all, /masterlist]
INPUTS:
Wmin: lower limit of the wavelength/energy range of interest (Angstroms)
if kev keyword set, then wmin is in kev
Wmax: upper limit of the wavelength/energy range of interest (Angstroms)
if kev keyword set, then wmax is in kev
Pressure: pressure in emitting region (cm^-3 K), or
Density: density in emitting region (cm^-3).
OPTIONAL INPUTS:
OUTFILE: the name of the output latex file to be written.
MINI: Minimum intensity for a line to be included in the output.
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
RADTEMP The blackbody radiation field temperature (default 6000 K).
OUTPUTS:
a latex file: 'linelist.tex' in the working directory by default
OPTIONAL OUTPUTS:
KEYWORD PARAMETERS:
MINI: Minimum intensity for a line to be included in the output
SNGL_ION: specifies a single ion (e.g. SNGL_ION='Fe_10' to include
only Fe X lines) or an array (e.g. SNGL_ION=['Fe_10','Fe_11']
to include only Fe X and Fe XI lines) of ions to be used
instead of the complete set of ions specified in
!xuvtop/masterlist/masterlist.ions
MASTERLIST: string of a specific masterlist file (full path).
If defined as a keyword (i.e. MASTERLIST=1 or /MASTERLIST)
then a widget allows the user to select a user-defined
masterlist file. Shortcut for SNGL_ION.
PHOTONS: units will be in photons rather than ergs
KEV: wavelengths will be given in kev rather than Angstroms
ALL: if set, then all lines are included. This means that lines for which
only an approximate wavelength is known (only theoretical energy
levels are known) are included.
OUTFILE: the name of the output latex file to be written. By default a
file 'linelist.tex' in the user's working directory will be
created.
NOPROT If set, then proton rates are not included.
CALLS:
CH_SYNTHETIC, CH_LINE_LIST
COMMON BLOCKS: None
RESTRICTIONS:
SIDE EFFECTS:
EXAMPLE:
> latex_wvl_dem, 400.,800., mini=1, pressure=1.e+15,sngl_ion='o_4'
CATEGORY:
spectral synthesis.
WRITTEN :
Version 1, 8-Nov-01, Giulio Del Zanna (GDZ).
Compared to the previous LATEX_WVL_DEM, these are the main changes:
1-Rewritten as a wrapper routine using the new procedures.
2-Now the PRESSURE value is a keyword.
3-The calculations can be done at constant DENSITY.
4-MASTERLIST can now be used both as an input string or as a keyword.
MODIFICATION HISTORY:
Version 2, 18-Nov-01, Peter Young
Added /noprot, rphot and radtemp keywords.
V. 3, 22-May-2002 GDZ. Removed const_net definitions.
VERSION : Version 3, 22-May-2002
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
CH_LINE_LIST
PURPOSE:
Create a latex or an ascii file of predicted spectral line intensities and
wavelengths corresponding to selected parameters, as calculated by
CH_SYNTHETIC. Needs as input the line intensity structure calculated by
CH_SYNTHETIC (default) or the SPECTRUM structure output of
MAKE_CHIANTI_SPEC.
CALLING SEQUENCE:
IDL> ch_line_list, transitions, outname, latex=latex, ascii=ascii, $
abundfile=abundfile, min_abund=min_abund, $
wmin=wmin,wmax=wmax,$
SPECTRUM=SPECTRUM, minI=minI,photons=photons,kev=kev, $
all=all,no_sort=no_sort, sngl_ion=sngl_ion
PROCEDURE:
INPUTS:
The structure created by CH_SYNTHETIC
OPTIONAL INPUTS:
Wmin: lower limit of the wavelength/energy range of interest (Angstroms)
if kev keyword set, then wmin is in kev
Wmax: upper limit of the wavelength/energy range of interest (Angstroms)
if kev keyword set, then wmax is in kev
Mini: Minimum intensity for line to be included in output
SNGL_ION: specifies a single ion (or a list of ions) to be used instead
of the complete set of ions specified in the structure.
MIN_ABUND: If set, outputs only those elements which
have an abundance greater than min_abund.
For example, from Allen (1973):
abundance (H) = 1.
abundance (He) = 0.085
abundance (C) = 3.3e-4
abundance (O) = 6.6e-4
abundance (Si) = 3.3e-5
abundance (Fe) = 3.9e-5
KEYWORD PARAMETERS:
LATEX: Create a latex file (default, exclusive with /ASCII)
ASCII: Create an ascii file (exclusive with /LATEX)
MINI: Minimum intensity for line to be included in output
PHOTONS: units will be in photons rather than ergs
KEV: wavelengths will be given in kev rather than Angstroms
ALL: if set, then all lines are included. This means that lines for which
only an approximate wavelength is known, denoted by a negative
wavelength value in the .wgfa file, are included.
These lines are listed in the file with a * preceding the wavelength.
NO_SORT:
If set, then the lines are *not* sorted in wavelength (or energy).
SPECTRUM
If set, IT IS ASSUMED that the input structure is the SPECTRUM
structure output of MAKE_CHIANTI_SPEC, where the line
intensities have already been multiplied by the abundance factor!!
OUTPUTS:
A latex (default) or an ascii file with the line list
CALLS: Many SolarSoft routines.
COMMON BLOCKS:
none.
SIDE EFFECTS:
EXAMPLE:
> ch_line_list, trans,'linelist.tex',/latex, wmin=100.,wmax=200.,/all
CATEGORY:
spectral synthesis.
WRITTEN :
Version 1, Written by: Giulio Del Zanna (GDZ) Oct 31 2001.
MODIFICATION HISTORY:
V.2, 9-Nov-2001 GDZ.
Now correctly handles the case when no
abundances are passed to the routine.
v.3, 11-Dec-2001, PRY.
Removed calls to get_utc and anytim2cal. Replaced with
call to systime()
v.4, 29-Apr-02, GDZ
Fixed a few small bugs, some caused by a change in the
database file format for V4.
Added only_mini, file_effarea keywords to be able to use as
input the structure created by MAKE_CHIANTI_SPEC.
V.5, 22-May-2002, GDZ
generalized directory concatenation to work for
Unix, Windows and VMS. changed tags.
Changed and added various things, including flabel
V.6, 12-Aug-02, GDZ
Modified the output labeling, and fixed two bugs: 1) when /all was used
the keyword /mini was not working. 2) min_abund was not working
properly when /spectrum was used. Reduced size of latex output (was
12pt)
Changed output in isothermal case (no Tmax given). Better info printed (GDZ)
V.7, 3-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
v.8, 18-Jul-2005 GDZ
Modified the use of the /kev keyword. Also, now the
routine accepts input structure with the units in keV.
v.9, 4-Aug-2005 GDZ
Corrected a bug introduced in the previous version.
Also switched to \documentclass when making the latex file.
VERSION : 9, 4-Aug-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME: EMISS_CALC()
PURPOSE:
To compute the emissivities of all lines of a specified ion over
given ranges of temperature and density.
CATEGORY:
Scientific analysis
EXPLANATION:
This routine calculates:
hc
-- * N_j * A_ji
lamb
where hc = 1.986 * 10^-8 erg AA, lamb is in angstroms, N_j is the
fraction of ions in the upper emitting level j, and A_ji is the
radiative decay rate for the transition.
The emissivities are stored in a structure called EMISS that also
holds the wavelength of the transition, the level numbers i and j
and also a 'flag', which is set to -1 if the wavelength is negative.
The temperature and density ranges can be specified directly using
the TEMP and DENS keywords. Setting TMAX to the log T_max of the
ion, gives emissivities for 3 temperatures: log T_max +- 0.15.
If DENS is not set, then it is set to 8 to 12 in 0.5 dex intervals.
STDENS allows the start density (of 8) to be changed to some other
value; ND allows the number of densities to be varied (default 9);
DINT allows the density interval to be varied (default 0.5).
CALLING SEQUENCE:
EMISS=EMISS_CALC (IZ, ION, [ TEMP=TEMP, DENS=DENS, RADT=RADT, $
DIL=DIL, PATH=PATH, /NO_DE, /PROTON, $
QUIET, PRESSURE=PRESSURE)
EXAMPLES:
EMISS=EMISS_CALC(26,13)
EMISS=EMISS_CALC(26,13,temp=[6.2],dens=findgen(5)+8)
EMISS=EMISS_CALC(26,13,temp=findgen(11)/100.+5.5,press=10.^15)
INPUTS:
IZ The atomic number of the ion
ION The spectroscopic number of the ion (e.g., 12 = XII)
OPTIONAL INPUTS:
TEMP Direct specification of the temperature range (log T)
DENS Direct specification of the density range (log Ne)
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
PATH If specified, the routine will look for the atomic data in
the PATH directory, rather than in the CHIANTI database
PRESSURE If a temperature array is given, and PRESSURE set,
then the emissivities will be evaluated at the
specified temperatures, but for densities =
pressure/temperature. If DENS is set, then it will
be ignored. The pressure is assumed to be in units
K * cm^-3.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
SUM_MWL_COEFFS An array of coefficients of the same length as
the array of temperatures. Electron and proton rate
coefficients will be calculated at each temperature
and then a weighted sum of the coefficients is
performed using SUM_MWL_COEFFS. This allows
non-Maxwellian energy distributions to be
incorporated into the level balance equations.
This keyword is not compatible with the PRESSURE
keyword.
RADFUNC The name of a user-defined function that will generate
a radiation spectrum as a function of temperature.
This radiation field will replace the black-body that
is assumed when using the RADTEMP keyword in the call
to pop_solver.
KEYWORDS:
NO_DE Drops the hc/lambda factor in the computation of the
emissivities. Useful for emission measure analyses involving
photon fluxes
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
QUIET If set, don't list the temperatures and densities at which
the emissivities are caculated.
DIEL If the dielectronic recombination files exist for the ion,
then these are used to derive the emissivities.
NO_SETUP If emiss_calc is called from a routine where the ELEMENTS
common block has already been set up, then this keyword
stops emiss_calc loading up the common block
OUTPUT:
The structure that is output has the following tags:
.ion_name string; contains ion name, e.g., 'Fe XIII'
.lambda float; contains wavelength
.level1 integer; contains lower level of transition
.lvl1_desc string; gives config. and term of lower level
.level2 integer; contains upper level of transition
.lvl2_desc string; gives config. and term of upper level
.flag integer; a flag to mark particular transitions
.em fltarr(nt,nd); contains emissivities at particular
temperatures and densities.
PROGRAMMING NOTES:
Transitions where only theoretical energies are available for at
least one of the two levels are assigned negative wavelengths in
the .wgfa file. With emiss_calc, the wavelength is set to be
positive, but emiss.flag is set to -1 for that transition, so
that other routines can keep track of the theoretical wavelengths.
COMMON BLOCKS:
ELVLC, WGFA, UPSILON, RADIATIVE, PROTON, ELEMENTS, IONREC
CALLS:
SETUP_ION, POP_SOLVER
ZION2FILENAME, ZION2SPECTROSCOPIC
READ_PROT, PROTON_DENS
HISTORY:
Ver 1, PRY 28-Jun-97
Ver 2, PRY 26-Jul-97 - corrected problem with size of emiss
Ver 3, PRY 22-Sep-97 - allowed photo-excitation to be included
Ver 4, PRY 6-Jul-98 - added PATH
Ver 5, PRY 5-Sep-98 - added call to choose_ioneq
Ver 6, PRY 3-Dec-98 - dosen't crash if no params given
Ver 7, PRY 9-Jan-99 - allowed proton rates to be added through
/PROTON keyword.
Ver 8, PRY 10-Feb-99 - added /QUIET keyword
Ver 9, PRY 8-Oct-99 - for H-like ions, there's a 2-photon
transition with a non-zero A-value that is
assigned a zero wavelength (as it does not
produce an emission line). This caused
problems for dens_plotter, so emiss_calc
now removes this transition from the emiss
structure.
Ver 10, PRY 15-Dec-99 - added deu to the upsilon common block in
order to be consistent with the main Chianti
routines.
Ver 11, PRY 8-May-00 - added PRESSURE
Ver 12, PRY 17-Aug-00 - changed elvlc common block to match new
version of pop_solver
Ver 13, PRY 10-Oct-00 - now calls setup_ion to read ion data
Ver 14, PRY 1-Jun-00 - removed call to choose_ioneq; now makes use
of the !ioneq_file system variable.
Ver 15, PRY 25-Sep-01 - modified for 9-point splines and proton rates
Ver 16, PRY 9-Dec-01 - completed changes for v.4
V. 17, 29-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
Now we only call zion2filename, corrected the call to
zion2spectroscopic (dielectronic cases were not handled
correctly).
V.18, 6-Aug-2002, Peter Young
Theoretical wavelengths weren't being flagged so this
has now been corrected.
V.19, 7-Aug-2002, Peter Young
Stopped "lines" with zero wavelength being included in
the structure.
Changed the use of CHIANTI system variables.
V.20 14-Aug-2002, GDZ
Modified the use of Version, to make it compatible with the
other CHIANTI v.4 routines.
V.21 10-Sep-2002, Peter Young
Allowed a density of 1 cm-3 to be input.
V.22 7-Aug-2003, Peter Young
Added keyword /NO_SETUP
V.23 4-Oct-2003, GDZ
modified the input to POP_SOLVER, now it is dealt with an
input structure.
V.24 5-Mar-2004, Enrico Landi (EL)
included ionization and recombination as level population
processes
V.25 6-May-2005, EL
corrected a minor incompatibility with IDL 5.6
V.26 5-Jul-2005, Peter Young
added RADFUNC= and SUM_MWL_COEFFS= keywords
V.27 1-Aug-2005, Peter Young
re-ordered code for setup to prevent crash
V.28 3-Aug-2005,GDZ
fixed bug, only define ioneq_ionrec when files are
there (it was failing with neutrals)
VERSION : 28 3-Aug-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
GOFNT
PURPOSE:
calculate G(n,T) function (line intensity per unit emission measure)
PROCEDURE:
Must specify line to form numerator and denominator
Multiple lines can be selected and summed
This can now be done interactively or not.
CALLING SEQUENCE:
GOFNT,Ion,Wmin,Wmax,Temperature,G,Desc,density=
INPUTS:
Ion: the CHIANTI style name of the ion, i.e., 'c_5' for C V
Wmin: minimum of wavelength wavelength range of interest in Angstroms
Wmax: maximum of wavelength wavelength range of interest
OPTIONAL INPUTS:
Many - see the keywords below.
OUTPUTS:
Temperature: an array of temperatures
G: Intensity per unit emission measure N_e*N_H*dh [cm^-5].
The resulting units are therefore erg cm^+3 s^-1 sr-1
C(T)= 1/(4*!pi)* A_ji*(N_j(X^+m)/N(X^+m))*(N(X^+m)/N(X))*(N(X)/N(H))/N_e
unless /NOABUND is set, in which case
C(T)= 1/(4*!pi)* A_ji*(N_j(X^+m)/N(X^+m))*(N(X^+m)/N(X))/N_e
G(T)=(hc/lambda_ij)*C(T)
G(T)= C(T) if /PHOTONS is set
Desc: a short string description of the selected line
OPTIONAL OUTPUTS:
Postscript file withthe plot of G(T).
Ascii file with the values of G(T).
VALUE The array of G(T) values corresponding to logt0.
KEYWORD PARAMETERS:
PRESSURE: specifies the pressure in units of NeT (cm^-3 K). G is then
calculated at that constant pressure
DENSITY: specifies the electron density in units of cm^-3. G is then
calculated at that value of the electron density. If neither the
density or pressure keywords are specified, a constant
density of 1.e+10 cm^-3 is assumed
PHOTONS: sets output in photons/s
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
RADTEMP The blackbody radiation field temperature (default 6000 K).
OUTFILE: the (optional) name of the output ascii file where a
listing of the line ratio intensity as a function of
temperature is saved.
PSFILE: the (optional) name of the output postscript file
where a plot of the chosen G(T) is saved.
NOABUND: If set, the G(T)'s are not multiplied by the abundance
factor.
NOPROT If set, then proton rates are not included.
ABUND_NAME: Name of the abundance file to use. If not passed, then
the user is prompted for it.
IONEQ_NAME: Name of the ionization equilization name to use. If not
passed, then the user is prompted for it.
ALL If set, all lines are calculated, including
the 'unobserved' ones.
LOWER_LEVELS
UPPER_LEVELS
Arrays with the indices of the lower and upper levels
pertaining to the transitions you want to get.
If more than one couple is given, the G(T) of the
lines are summed.
Obviously, the given indices must correspond to transitions
that are present in the database.
ARCSECS
If set, units are photons (ergs) cm^+3 s^-1 arcsecs^-2
VERBOSE
LOGT0 An array of log T values for which the G(T) are wanted.
VALUE The array of G(T) values corresponding to logt0.
If logt0 is defined, and within the limits of the
temperatures for which G(T) NE 0, the array VALUE
is returned with a simple spline interpolation.
CALLS:
CH_SYNTHETIC, CH_XMENU_SEL
COMMON BLOCKS: None
RESTRICTIONS:
SIDE EFFECTS:
EXAMPLE:
IDL> gofnt,'o_5',1000.,1500.,temp,goft,desc,density=1.e+16
CATEGORY:
spectral diagnostics
MODIFICATION HISTORY:
Written by: Ken Dere
October 4, 1996: Version 1
14-Jul-2000 Peter Young, now calls pop_solver
26-Oct-2000 GDZ, added keyword NOABUND to not multiply for the abundence
factor. Corrected header for a wrong description.
Version 4, 21-Dec-2000, William Thompson, GSFC
Modified for better cross-platform graphics capability
Version 5, 8-Nov-01, Giulio Del Zanna (GDZ).
Rewritten as a wrapper routine using the new procedures.
Corrected a few inconsistencies in the plots.
Version 6, 18-Nov-01, Peter Young
Added /noprot, rphot and radtemp keywords.
Version 7, 11-Dec-01, Peter Young
Changed call to ch_strpad to strpad.
V. 8, GDZ, 28-Apr-02 Added abund_name,ioneq_name keywords.
v. 9 21-May-2002, GDZ
generalized directory concatenation to work for
Unix, Windows and VMS.
V.10, 15-Aug-02, GDZ
Major revision:
-Removed the call to ch_xselect_s, that did not work for long lists.
-Added a '*' in the line lists, to identify 'unobserved' lines.
-Replaced the commands to create PS file, to make it
cross-platform compatible.
-Added a large number of cosmetics, mainly lables to the axes and
titles.
-Added keyword ALL. If set, all lines are calculated, including
the 'unobserved' ones.
-Added the CHIANTI version number in the outputs.
V. 11, 19-Sep-02, GDZ
Clarified output units.
V.12, 25-Jun-03, GDZ,
Added many new keywords. Now is possible to use the routine
with background jobs, in not-interactive mode.
Rounded the wavelengths.
V.13, 24-Sept-2003, GDZ
Corrected a bug when logt0 is not defined.
V.14, 3-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
VERSION : 14, 3-Nov-03
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME: G_OF_T()
PURPOSE:
To compute DE * F(T) * n_j * A_ji / N_e for selected emission lines.
Option to also multiply by abundance.
CATEGORY:
Atomic data analysis
EXPLANATION:
The G-of-T function has a number of different definitions in the
literature. In the most basic form it contains only the temperature
dependent parts (i.e., 0.83*n_j*A_ji*F(T)/N_e), but often a Delta-E
and Ab(X) are added as well. Here, the _default_ form is:
Delta-E * 0.83 * n_j * A_ji * F(T) / N_e
By using the NO_DE keyword, the Delta-E can be omitted, while the
ABUND keyword allows the abundance to be added.
The function that is output is tabulated over 4.0 <= logT <= 8.0
in 0.1 dex intervals. If you want the function tabulated over
smaller intervals, run the ION_INTERP routine afterwards.
CALLING SEQUENCE:
EXAMPLES:
RESULT=G_OF_T(26,13)
RESULT=G_OF_T(26,13,DENS=7)
RESULT=G_OF_T(26,13,GOFTFILE='my_gofts.dat')
RESULT=G_OF_T(26,13,/ABUND)
RESULT=G_OF_T(26,13,ABUND_FILE=ABUND_FILE, IONEQ_FILE=IONEQ_FILE)
INPUTS:
IZ: The atomic number of the ion (e.g., 26 = Fe)
ION: The spectroscopic number of the ion (e.g., 12 = XII)
OPTIONAL INPUTS:
DENS: The logarithm (to base 10) of the density at which the
emissivities are calculated (default=10.)
WRANGE: Wavelength range from which lines are required. If not
specified, then the 10 strongest lines are displayed.
PATH: If specified, the routine will look for the atomic data in
the PATH directory, rather than in the CHIANTI database
GOFTFILE: By specifying GOFTFILE as a filename, the G-of-T
function can be stored in this file. It is stored
in the form a structure (called goft_list) with the following
labels:
goft_list.label: user-specified string, e.g., 'Si XII 520.7'
goft_list.func: fltarr(41), the G-of-T function
If the same GOFTFILE is specified for another ion, then the
G-of-T function is added to the existing structure. The GOFTFILE
option only works when the ABUND keyword is set. The GOFTFILE is
meant to be read by another routine called GOFT_PLOTTER.
INDEX: Allows the direct specification of indices within the
emiss structure. This allows the g_of_t routine to be
run without the menu widget appearing. If the /quiet
keyword is also used, then the routine will run "silently".
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
IONEQ_FILE Directly specify the name of the ion balance file
(including directory path). If not set, then a widget will
pop up allowing you to select a file.
ABUND_FILE Directly specify the name of the abundance file
(including directory path). One can also use /ABUND_FILE
to include the abundances in the G(T) function, but allow
the abundance file to be picked through a widget.
KEYWORDS:
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
NO_DE: If set, then the output function will *not* contain the
Delta-E. Be careful using this if you are using blends
(as Delta-E is different for different wavelengths).
QUIET If set, then don't plot the G(T) function or print out
information to the screen.
CALLS:
EMISS_CALC, READ_IONEQ, READ_ABUND, EMISS_SELECT, CH_GET_FILE
RESTRICTIONS:
HISTORY:
Ver.1, PRY 28-Jul-97.
Ver.2, PRY 22-Jun-98, added CHOOSE keyword and removed RAY
Ver.3, PRY 4-Aug-98, cosmetic changes following comments of Giulio
Del Zanna
Ver.4, PRY 5-Sep-98, added call to choose_ioneq
Ver.5, PRY 23-Sep-98, added GOFTFILE input
Ver.6, PRY 3-Mar-99, now calls EMISS_SELECT
Ver.7, PRY 6-Nov-00, removed the /CHOOSE keyword; also changed
PICKFILE call to DIALOG_PICKFILE and removed call
to the CHIANTI routine ADD\_SUBDIR
Ver.8, PRY 18-Oct-01, adjusted for proton rates, and
photoexcitation.
Ver.9, PRY 9-Dec-01, completed modifications for v.4 of CHIANTI.
V. 10, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
Ver. 11, 9-Feb-2005, Peter Young
changed keyword_set(abund) to keyword_set(abund_file)
VERSION : 11, 9-Feb-2005
PROJECT
CHIANTI http://wwwsolar.nrl.navy.mil/chianti.html
CHIANTI is an atomic database package for the calculation of
continuum and emission line spectra from astrophysical plasmas. It is a
collaborative project involving the Naval Research Laboratory
(Washington DC, USA), the Arcetri Observatory (Firenze, Italy), and the
Cambridge University (United Kingdom).
NAME
dens_plotter
PURPOSE:
A widget-based routine to allow the analysis of density sensitive
ratios. **** See RATIO_PLOTTER for details. *****
CALLING SEQUENCE:
IDL> dens_plotter, name,$
EM, PATH=PATH, NOPROT=NOPROT, $
IONEQ_FILE=IONEQ_FILE, ABUND_FILE=ABUND_FILE
INPUTS:
The ion name (e.g. 'si_3' for Si III)
OPTIONAL INPUTS : none
OUTPUTS:
OPTIONAL OUTPUTS:
EM: Save the displayed emissivities to structure EM.
**** See RATIO_PLOTTER for details. *****
KEYWORDS:
PATH: Data in the CHIANTI format that is not in the CHIANTI
database can be read by specifying the directory in which
it lies through PATH.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
CALLS: CONVERTNAME RATIO_PLOTTER
COMMON BLOCKS: none
RESTRICTIONS:
SIDE EFFECTS:
CATEGORY:
spectral synthesis.
EXAMPLE:
IDL> dens_plotter, 'si_9'
WRITTEN :
Ver.1, 18-Apr-2002, Giulio Del Zanna (GDZ) written as a wrapper
routine to call RATIO_PLOTTER.
MODIFIED: V.2, 2-Aug-2005, GDZ
Now the routine handles the dielectronic case
VERSION : 2, 2-Aug-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
DENSITY_RATIOS
PURPOSE:
to calculate line intensity ratios as a function of electron density
CATEGORY:
scientific analysis
CALLING SEQUENCE:
DENSITY_RATIOS,Ion,Wmin,Wmax,Dmin,Dmax,Density,Ratio,Description
INPUTS:
Ion: the CHIANTI style name of the ion, i.e., 'c_5' for C V
wmin: minimum of the wavelength range of interest in Angstroms
wmax: maximum of the wavelength range of interest in Angstroms
dmin: log10 of the minimum desired density (8. = 10^8 cm^(-3) )
dmax: log10 of the maximum desired density range
INTERACTIVE INPUTS:
Must select the line for the numerator and denominator
It is possible to select multiple lines to be summed
KEYWORD PARAMETERS:
OUTFILE: the (optional) name of the output ascii file where a
listing of the line ratio intensity as a function of
density is saved. For example, outfile='den_rat.lis'
PSFILE: the (optional) name of the output postscript file
where a plot of the choses density sensitive line
ratio is saved. For example, psfile='den_rat.ps'
TEMP: to specify the temperature, otherwise the temperature at
the peak
of the ionization equilibrium is used. For example,
temp=1.e+6
/PHOTONS: if set, the ratio will be in photon units, as opposed
to ergs
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
VERBOSE To print out information about the lines.
OUTPUTS:
Density: an array of the density values for which the selected
intensity ratio calculated
Ratio: an array of line intensity ratios
Description: a string describing the transitions selected
Plots the intensity ratio of the selected line as a function of density
COMMON BLOCKS:
None.
CALLS
EMISS_CALC, ION2SPECTROSCOPIC, CONVERTNAME, READ_IONEQ,
CH_XMENU_SEL
EXAMPLE:
density_ratios,'o_5',1000.,1500.,8.,13.,den,rat,desc
choose the ratio of 1371.294 to 1218.393
MODIFICATION HISTORY:
Written by: Ken Dere
March 1996: Version 2.0
May 28, 1996: Ken Dere added psfile keyword/option
Sept 1996: modified to work with VMS
and added keyword TEMP, Ken Dere
Feb. 2000: Modified for Version 3, K. Dere
14-Jul-2000 Peter Young, now calls pop_solver
26-Sep-2001 Modified for 9-point splines and proton rates;
added radtemp and rphot keywords for photoexcitation.
20-Nov-2001 Routine now calls emiss_calc to get emissivities.
V.9, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
V.10, 1-Aug-02 GDZ
Changed all the formats.
V.11, 06-Aug-02 GDZ
Changed the use of CHIANTI system variables.
V.12, 15-Aug-02, GDZ
Major revision:
-Added the keyword VERBOSE, to avoid printing out long lists of lines.
-Removed the call to ch_xselect_s, that did not work for long lists.
-Added a '*' in the line lists, to identify 'unobserved' lines.
-Replaced the commands to create PS file, to make it
cross-platform compatible.
-Added a large number of cosmetics, mainly lables to the axes and
titles, that were missing.
-Removed plotting in windows already present.
-Added the CHIANTI version number in the outputs.
V.13, 3-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
VERSION : 13, 3-Nov-03
Project : SOHO - CDS
Name : CHIANTI_NE
Purpose : Calculate and plot CHIANTI density sensitive line ratios.
Explanation : CHIANTI_NE (density ratios)
calculates and plots density sensitive line ratios based on
the CHIANTI atomic database of Dere et. al.
Use : IDL> chianti_ne
Inputs : None
Opt. Inputs : None
Outputs : None
Opt. Outputs: None.
Keywords : None
Calls : CALC_DMM_DR, plot_dmm_dr_fig , make_ion_list
Common : dmm_dr_com dmm_lines(with plot_dmm_dr_fig),
Restrictions: None
Side effects: None
Category : Spectral
Prev. Hist. : Started life as 'density_ratios' by Ken Dere
Written : C D Pike, RAL, 13-Jan-96
Modified : Added selection of els/ions from master file. CDP, 21-Jan-96
Added hardcopy of line list, refs etc. CDP, 22-Jan-96
Include multiple lines in ratio. CDP, 27-Jan-96
General upgrade and added temp/unit selections. CDP, 6-Jun-97
Added intensity ratio selection. CDP, 17-Jul-97
Added wavelength ranges. CDP, 18-Jul-97
Fixed typos introduced in version 7. CDP, 22-Jul-97
Float the user-supplied Log Temperature. CDP, 1-Aug-97
Update for IDL v5.2. CDP, 20-Apr-99
v. 11 Update list of elements. CDP, 18-Jun-99
V.12. Added ratio plots and hardcopies in linear scale, added various
checks and minor things. Added a few tags to the
ratio output structure (temperature, units, comment).
Removed optional output structure.
Updated to be CHIANTI v.3-compatible.
Giulio Del Zanna, DAMTP, 7-Oct-2000
Version 13, 21-Dec-2000, William Thompson, GSFC
Modified for better cross-platform graphics capability
V. 14, 1-May-02, GDZ, commented out a few refs.
V. 15, 21-May-2002, GDZ, changed the way to deal with fonts.
V.16, 17-Sep-2002 (GDZ)
added !p.multi = 0 upon exit and added X-label.
Version : Version 16, 17-Sep-2002
Project : SOHO - CDS
Name : PLOT_CHIANTI_NE
Purpose : Plots a density sensitive ration saved from CHIANTI_NE
Explanation : The routine CHIANTI_NE allows the calculated ratio to be
saved in an IDL save file. This routine retrieves and
plots the ratio.
Use : IDL> plot_chianti_ne, file, data
Inputs : file - save file name (an extension of .CH_NE will have
been added, specifying this is optional)
Opt. Inputs : None
Outputs : None
Opt. Outputs: data - returns the retrieved ratio structure
Keywords : log. If set, a log-log plot is produced.
Calls : print2d_plot
Common : None
Restrictions: None
Side effects: None
Category : Synthetic spectra
Prev. Hist. : None
Written : C D Pike, RAL, 7-Oct-96
Modified : v.2 Added a few extra things, including possibility to create a
postscript file.
Giulio Del Zanna (DAMTP), 10-Oct-2000
Version : Version 2, GDZ 10-Oct-2000
PROJECT
CHIANTI http://wwwsolar.nrl.navy.mil/chianti.html
CHIANTI is an atomic database package for the calculation of
continuum and emission line spectra from astrophysical plasmas. It is a
collaborative project involving the Naval Research Laboratory
(Washington DC, USA), the Arcetri Observatory (Firenze, Italy), and the
Cambridge University (United Kingdom).
NAME
temp_plotter
PURPOSE:
A widget-based routine to allow the analysis of temperature sensitive
ratios. **** See RATIO_PLOTTER for details. *****
CALLING SEQUENCE:
IDL> temp_plotter, name,$
EM, PATH=PATH, NOPROT=NOPROT, $
IONEQ_FILE=IONEQ_FILE, ABUND_FILE=ABUND_FILE
INPUTS:
The ion name (e.g. 'si_3' for Si III)
OPTIONAL INPUTS : none
OUTPUTS:
OPTIONAL OUTPUTS:
EM: Save the displayed emissivities to structure EM.
**** See RATIO_PLOTTER for details. *****
KEYWORDS:
PATH: Data in the CHIANTI format that is not in the CHIANTI
database can be read by specifying the directory in which
it lies through PATH.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
CALLS: CONVERTNAME RATIO_PLOTTER
COMMON BLOCKS: none
RESTRICTIONS:
SIDE EFFECTS:
CATEGORY:
spectral synthesis.
EXAMPLE:
IDL> temp_plotter, 'fe_13'
WRITTEN :
Ver.1, 18-Apr-2002, Giulio Del Zanna (GDZ) written as a wrapper
routine to call RATIO_PLOTTER (written by P. Young).
MODIFIED: V.2, 2-Aug-2005, GDZ
Now the routine handles the dielectronic case
VERSION : 2, 2-Aug-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
TEMPERATURE_RATIOS
PURPOSE:
calculate and display temperature sensitivity of line intensity ratios
CATEGORY:
spectral diagnostics
PROCEDURE :
The intensities (Population of the upper level * A) of the lines within
the selected ion are first calculated, either at constant pressure or
at constant density (however specified in the input). They are plotted
in window 0. The intensities relative to the brightest reference line
are then plotted in window 1. A widget allows the user to select a
number of lines (at least one!) for the numerator of the ratio, and a
number of lines for the denominator. In case of multiple selections, the
line intensities are summed. The ratio values are plotted in window 2, and
optionally also saved in a text file. A postscript file can also be
created. The ratio values, calculated at twice and half the prescribed
density are also calculated and overplotted, to show how the
temperature ratio also depends on the density.
CALLING SEQUENCE:
> temperature_ratios,ion,wmin,wmax,Log10(tempmin),Log10(tempmax),temperature,ratio,description,$
[pressure= ,density= , psfile= , outfile= ]
EXAMPLE:
> temperature_ratios,'c_4',100.,1600.,4.,6.,temp,ratio,desc,density=1.e+10,$
psfile='test.ps', outfile='test.txt'
then select the ratio of (384.17 + 384.19) to 1550.772
INPUTS:
Ion: the CHIANTI style name of the ion, i.e., 'c_5' for C V
Wmin: minimum wavelength limit in Angstroms
Wmax: maximum wavelength limit in Angstroms
Tempmin: log10 of lowest temperature of interest, i.e. 4 for 10.^4 K
Tempmax: log10 of highest temperature of interest
OPTIONAL INPUTS:
Must specify indices of lines which are to form the ratio
RADTEMP The blackbody radiation field temperature (default
6000 K).
RPHOT Distance from the centre of the star in stellar radius
units. I.e., RPHOT=1 corresponds to the star's surface.
(Default is infinity, i.e., no photoexcitation.)
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
OUTPUTS:
Temperature: an array of temperatures spanning Tempmin to Tempmax
Ratio: an array of the intensity ratio of the selected lines
Desc: a short string description of the selected line ratio
OPTIONAL OUTPUTS:
Ps and/or text file with the intensity ratio.
KEYWORD PARAMETERS:
DENSITY: calculates the intensity ratios for constant density.
If neither density or pressure are specified, a constant
density of 1.e+10 cm^-3 is assumed as default.
OUTFILE: the (optional) name of the output ascii file where a
listing of the line ratio intensities as a function of
temperature is saved.
PSFILE: the (optional) name of the output postscript file
where a plot of the chosen temperature sensitive line
ratio is saved.
NOPROT Switches off inclusion of proton rates.
VERBOSE prints out information
CALLS:
read_ioneq, convertname, ion2spectroscopic,ion2filename,
ch_xmenu_sel, emiss_calc
COMMON:
elvlc,l1a,term,conf,ss,ll,jj,ecm,eryd,ecmth,erydth,eref
wgfa, wvl,gf,a_value
upsilon,t_type,deu,c_ups,splups
proton, pstr, pe_ratio
radiative, radt, dilute
RESTRICTIONS:
SIDE EFFECTS: None known yet.
MODIFICATION HISTORY:
Written by: Ken Dere
May 1996: Version 2.0, Ken Dere
April 2000: V. 3 Ken Dere modified for V3
14-Jul-2000 V. 4 Peter Young, now calls pop_solver
2-Oct-2000 V. 5 Giulio Del Zanna, corrected an error in the
creation of the string list of the lines in the ratio.
Also corrected a few minor errors.
Removed the device,window_state call, and added a few
other 'cosmetic' adjustments.
Version 6, 21-Dec-2000, William Thompson
Modified for better cross-platform capability.
Ver.7, 6-Dec-2001, Peter Young
Revised to call emiss_calc for the emissivities.
V.8, 21-May-2002, GDZ
generalized directory concatenation to work for
Unix, Windows and VMS.
V.9, 1-Aug-02 GDZ
Fixed label mistake, and changed all the formats.
V.10, 06-Aug-02 GDZ
Changed the use of CHIANTI system variables.
V.11, 15-Aug-02, GDZ
Major revision:
-Added the keyword VERBOSE, to avoid printing out long lists of lines.
-Removed the call to ch_xselect_s, that did not work for long lists.
-Added a '*' in the line lists, to identify 'unobserved' lines.
-Replaced the commands to create PS file, to make it
cross-platform compatible.
-Added a large number of cosmetics, mainly lables to the axes and
titles, that were missing.
-Removed plotting in windows already present.
-Removed the pressure keyword.
-Added the CHIANTI version number in the outputs.
V.12, 3-Nov-03 GDZ
Modified format e8.2 to e9.2 for Windows compatibility.
VERSION : 12, 3-Nov-03
Project : SOHO - CDS
Name : CHIANTI_TE
Purpose : Calculate and plot CHIANTI temperature sensitive line ratios.
Explanation : CHIANTI_TE (temperature ratios)
calculates and plots temp. sensitive line ratios based on
the CHIANTI atomic database of Dere et. al.
Use : IDL> chianti_te
Inputs : None
Opt. Inputs : None
Outputs : None
Opt. Outputs: none.
Keywords : None
Calls : CALC_DMM_TR, make_ion_list
Common : dmm_tr_com
Restrictions: None
Side effects: None
Category : Spectral
Prev. Hist. : Started life as 'temperature_ratios' by Ken Dere
Written : H.E. Mason, 3 Oct 1996
Modified : Update for IDL v5.2. CDP, 20-Apr-99
V.3. Update list of elements. CDP, 18-Jun-99
V.4 , Giulio Del Zanna (DAMTP), 10 Oct-2000
Rewritten completely, adding possibility to select the density
at which the intensities are calculated, making this routine
compatible ith CHIANTI v.3, and with the same characteristics as
CHIANTI_TE. Added ratio plots and hardcopies in linear scale, added various
checks and minor things. Added a few tags to the
ratio output structure (density, units, comment).
Removed optional output structure.
Version 5, 21-Dec-2000, William Thompson, GSFC
Modified for better cross-platform graphics capability
V. 6, 1-May-02, GDZ, commented out a few refs.
V.7, 21-May-2002, GDZ, fixed a bug with the fonts.
V.8, 17-Sep-2002 (GDZ)
added !p.multi = 0 upon exit and added X-label
Version : Version 8, 17-Sep-2002
Project : SOHO - CDS
Name : PLOT_CHIANTI_TE
Purpose : Plots a temperature sensitive ratio saved from CHIANTI_TE
Explanation : The routine CHIANTI_TE allows the calculated ratio to be
saved in an IDL save file. This routine retrieves and
plots the ratio.
Use : IDL> plot_chianti_te, file, data
Inputs : file - save file name (an extension of .CH_TE will have
been added, specifying this is optional)
Opt. Inputs : None
Outputs : None
Opt. Outputs: data - returns the retrieved ratio structure
Keywords : log. If set, a log-log plot is produced.
Calls : None
Common : None
Restrictions: None
Side effects: None
Category : Synthetic spectra
Prev. Hist. : None
Written : C D Pike, RAL, 7-Oct-96
Modified : v.2 Added a few extra things, including possibility to create a
postscript file.
Giulio Del Zanna (DAMTP), 10-Oct-2000
Version : Version 2, GDZ 10-Oct-2000
PROJECT : CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME
FREEFREE
PURPOSE:
This routine computes the free-free continuum (bremsstrahlung)
using the fitting formulae of Itoh et al. (ApJS 128, 125, 2000)
and Sutherland (MNRAS 300, 321, 1998).
The Itoh et al. data are valid for smaller ranges for temperature
and wavelength than Sutherland and so for points outside of their
ranges we use the data of Sutherland.
INPUTS
TEMP Temperature (in K).
WVL Wavelengths in angstroms. Can be a scalar or vector.
OUTPUTS
INT Free-free continuum intensity in units of
10^-40 erg cm^3/s/sr/Angstrom
[ integral(N_H N_e dh) in cm^-5 ] if a DEM is not defined.
If DEM values are defined, it is assumed that they are given
as N_H N_e dh/dT. The units are 10^-40 erg/cm^2/s/sr/Angstrom.
If T is given as a 1-D array, then the output will be a 2-D array,
with one element for each temperature and wavelength
(but also see SUMT).
OPTIONAL INPUTS
DEM_INT An array of same length as TEMP which contains the
differential emission measure values at each temperature.
The emissivity at each temperature is multiplied by the
DEM value and the d(logT) value.
MIN_ABUND This keyword allows the specification of a minimum abundance,
such that any elements with an abundance (relative to
hydrogen) less than MIN_ABUND will not be included in the
calculation. E.g., MIN_ABUND=1e-5.
KEYWORDS
NO_SETUP By default the routine asks the user which ion balance
and abundance files to use via pop-up widgets. If
/no_setup is used then this data is taken from the common
block.
SUMT The default is to output the intensity array as an array
of size (nwvl x nT). Setting this keyword performs a sum
over the temperatures to yield a vector of same size as
the input wavelengths, thus producing the complete
free-free spectrum.
PHOTONS Gives output emissivity in photon units rather than ergs.
CALLS
SUTHERLAND, ITOH
COMMON BLOCKS
ELEMENTS
PROGRAMMING NOTES
The Itoh fitting formula is only valid for (6.0 LE logT LE 8.5).
For temperatures below this, we thus switch to the Sutherland
fitting formula. There is very little (<1%) between the two at
logT=6.
Itoh also has a constraint on the quantity u=hc/kTl (l=wavelength),
such that (-4 LE log u LE 1.0). The upper limit corresponds to the
continuum being cut-off prematurely at low wavelengths. E.g., for
T=10^6 the cutoff is at 14.39 angstroms. For these low wavelengths
we also use the Sutherland data to complete the continuum. Note that
the continuum at these wavelengths is very weak
MODIFICATION HISTORY
Ver.1, 5-Dec-2001, Peter Young
Completely revised to call the separate itoh.pro and
sutherland.pro routines.
V. 2, 21-May-2002, Giulio Del Zanna (GDZ),
Corrected the description of the units.
Added verbose keyword and a printout.
V. 3, 22-May-2002, Peter Young (PRY)
Added MIN_ABUND optional input.
Changed ioneq_t to ioneq_logt (GDZ).
V 4, 25-May-2005, GDZ
corrected routine header.
VERSION : 4, 25-May-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME
FREEBOUND
PURPOSE:
Calculates the free-bound (radiative recombination) continuum.
INPUTS
TEMP Temperature in K (can be an array).
WVL Wavelength in angstroms (can be an array).
OUTPUTS
INT Free-bound continuum intensity in units of
10^-40 erg cm^3/s/sr/Angstrom
( integral(N_H N_e dh) in cm^-5) if a DEM is not defined.
If DEM values are defined, it is assumed that they are given
as N_H N_e dh/dT. The units are 10^-40 erg/cm^2/s/srAngstrom
If T is given as a 1-D array, then the output will be a
2-D array, with one element for each temperature and
wavelength (but also see SUMT).
OPTIONAL INPUTS
DEM_INT The intensity array is multiplied by a DEM number for
each temperature. DEM_INT needs to be of the same size
as TEMPERATURE. It is needed for the synthetic spectrum
routines.
IZ Only calculate continuum for the element with atomic
number IZ
ION (To be used in conjunction with IZ.) Calculated continuum
for a single ion (IZ, ION).
KEYWORDS
NO_SETUP If the procedure setup_elements has already been called
then the keyword /nosetup should be set to avoid
repeating this step
MIN_ABUND If set, calculates the continuum only from those
elements which have an abundance greater than
min_abund. Can speed up the calculations. For
example:
abundance (H) = 1.
abundance (He) = 0.085
abundance (C) = 3.3e-4
abundance (Si) = 3.3e-5
abundance (Fe) = 3.9e-5
PHOTONS The output spectrum is given in photon units rather
than ergs.
SUMT When a set of temperatures is given to FREEBOUND, the
default is to output INTENSITY as an array of size
(nwvl x nT). With this keyword set, a summation over
the temperatures is performed.
VERBOSE Output information from FREEBOUND.
COMMON BLOCKS
ELEMENTS
CALLS
FREEBOUND_ION, SETUP_ELEMENTS, READ_KLGFB, GET_IEQ
HISTORY
Ver.1, 24-Jul-2002, Peter Young
Ver.2, 26-Jul-2002, Peter Young
revised call to freebound_ion; corrected ion fraction problem
V 3, 25-May-2005, GDZ
corrected routine header.
VERSION : 3, 25-May-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
TWO_PHOTON
PURPOSE:
Calculate the 2 photon continuum from a hot, low density plasma.
For the hydrogen isoelectronic sequence, A values
Parpia, F. A., and Johnson, W. R., 1982, Phys. Rev. A, 26, 1142.
and distribution function as a function of Z is taken from:
Goldman, S.P. and Drake, G.W.F., 1981, Phys Rev A, 24, 183
For the helium isoelectronic sequence, A values are from:
Drake, G.W.F., 1986, Phys. Rev. A, 34, 2871
and the distribution function as a function of Z is taken from:
Drake, G.W.F., Victor, G.A., Dalgarno, A., 1969, Phys.
Rev. A, 180, 25.
in this paper the distribution is only given up to Z=10 but
extrapolation to higher Z appears to be OK.
Note that, unlike the freefree and freebound routines, two_photon
requies the electron density to be specified. This is because there
is a call to pop_solver
CALLING SEQUENCE:
TWO_PHOTON,temperature, density, wavelength, intensity
INPUTS:
TEMPERATURE Temperature in degrees Kelvin, can be a 1D array
WAVELENGTH Wavelengths in Angstroms.
OPTIONAL INPUTS:
DENSITY Electron density in cm^-3, can also be a 1D array
of the same size as Temperature. If there are several
temperatures specified but only one density, then
density is assumed the same at all temperatures.
If not specified, then default densities of 10^10
electrons/cm^3 are assumed.
DEM_INT An array of same length as TEMP which contains the
differential emission measure values at each temperature.
The emissivity at each temperature is multiplied by the
DEM value and the d(logT) value.
KEYWORD PARAMETERS:
NO_SETUP: If the procedure setup_elements has already been called
then the keyword /no_setup should be set to avoid
repeating this step
MIN_ABUND: If set, calculates the continuum only from those
elements which have an abundance greater than min_abund.
Can speed up the
calculations. For example:
abundance (H) = 1.
abundance (He) = 0.085
abundance (C) = 3.3e-4
abundance (Si) = 3.3e-5
abundance (Fe) = 3.9e-5
SUMT If several temperatures have been specified, then /sumt
will sum the emissivities over the different
temperatures, giving an output INTENSITY that has the
same size as WAVELENGTH.
PHOTONS If set the continuum emissivity is output in photon
units rather than erg units.
VERBOSE
OUTPUTS:
RAD 2 photon continuum intensity in units of
10^-40 erg cm^3/s/sr/Angstrom per unit emission measure
( integral(N_H N_e dh) in cm^-5) if a DEM is not defined.
If DEM values are defined, it is assumed that they are given
as N_H N_e dh/dT. The units are
10^-40 erg/cm^2/s/sr/Angstrom
If T is given as a 1-D array, then the output will be a 2-D array,
with one element for each temperature and wavelength
(but also see SUMT).
CALLS
POP_SOLVER, SETUP_ION, SETUP_ELEMENTS, READ_MASTERLIST,
CONVERTNAME
COMMON BLOCKS:
ELEMENTS, ELVLC, WGFA, UPSILON, PROTON
EXAMPLE:
> two_photon,1.e+6,3.e+10,wvl,int
> two_photon,1.e+6,3.e+10,wvl,int,min_abund=3.e-5
> two_photon,1.e+6,3.e+10,wvl,int,/no_setup
PROGRAMMING NOTES
For He 2-photon decays, the distribution function is from Table II
of Drake et al. (1969), except that the values have been divided by
the A-value from Drake (1986).
MODIFICATION HISTORY:
Written by: Ken Dere
February 2001: Version 1.0
Ver.2, 19-Dec-2001, Peter Young
Now allows an array of temperatures.
Added /SUMT keyword.
Added DEM_INT= optional input.
Switched to using spl_init & spl_interp for the spline fits.
Corrected a small bug.
Ver.3, 20-Dec-2001, Peter Young
Corrected a bug related to density indices.
Ver.4, 23-Apr-2002, Peter Young
Added /photons keyword.
Ver.5, 28-May-2002, Peter Young
Corrected way in which DEM_INT is handled.
V. 6, 28-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
Corrected the description of the units and various
inaccuracies in the header.
V.7, 14-Aug-02, GDZ
Added keyword VERBOSE
V.8, 4-Oct-2003, GDZ
modified the input to POP_SOLVER, now it is dealt with an
input structure.
V.9, 8-Jun-2004, EL
modified the input to POP_SOLVER, now it includes ion/rec
V.10, 5-Jul-2005
corrected problems with the input structure for pop_solver
v.11 29-Jul-2005, GDZ
fixed bug, only define ioneq_ionrec when files are
there (it was failing with neutrals)
VERSION : 11 29-Jul-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME: SHOW_POPS
PURPOSE:
To display populations of significant levels in a CHIANTI ion
model
CATEGORY:
Scientific analysis
EXPLANATION:
Displays percentage level populations and level IDs for all levels
in the specified ion with populations greater than 0.01%. If the
temperature is not specified, then it is taken to be where the
maximum of the ionisation fraction is.
CALLING SEQUENCE:
SHOW_POPS, IZ, ION [, POPSTR, DENS= , TEMP= , /NOPROT,
RADTEMP= , RPHOT= , /ALL, /DIEL, PATH=,
IONEQ_FILE= , ABUND_FILE= ]
EXAMPLES:
show_pops,26,13,popstr
show_pops,26,13,dens=7.5,temp=6.0,rphot=1.2
INPUTS:
IZ The atomic number of the ion
ION The spectroscopic number of the ion (e.g., 12 = XII)
OPTIONAL INPUTS:
DENS Logarithm of electron density
TEMP Logarithm of electron temperature. If not specified, then
T_max of the ion is used
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
PATH Directly specify the path where the ion data is contained,
e.g., path='/home/other_data/fe_13'
N_LEVELS The size of the ion model is automatically determined
from the information in the CHIANTI data files. Setting
this keyword allows the number of levels in the model to
be reduced. E.g., N_LEVELS=14 reduces the model to the
first 14 levels given in the .ELVLC file.
IONEQ_FILE To include proton rates in the level balance equations
requires the number of density of protons to be known,
and this requires an ion balance file and an abundance
file to be specified, which are done through the
IONEQ_FILE and ABUND_FILE keywords. If they are not set
then the default files specified by !ioneq_file and
!abund_file are used.
ABUND_FILE See IONEQ_FILE.
SUM_MWL_COEFFS An array of coefficients of the same length as
the array of temperatures. Electron and proton rate
coefficients will be calculated at each temperature
and then a weighted sum of the coefficients is
performed using SUM_MWL_COEFFS. This allows
non-Maxwellian energy distributions to be
incorporated into the level balance equations.
If this keyword is set for an ion that has ionization
and recombination included in the level balance, then
these processes will be switched off for the
calculation since their rates implicitly assume a
single Maxwellian to describe the ion fractions of
the neighbouring ions.
LEVEL Allows the control of which level populations are displayed
to the screen. If set to a positive scalar or array, then
only those levels are printed. If it is set to a negative
scalar (-n), then all level populations up to level n are
printed. E.g., LEVEL=20 (only level 20); LEVEL=[5,7,20]
(levels 5, 7 and 20); LEVEL=-20 (all levels up to level 20).
RADFUNC The name of a user-defined function that will generate
a radiation spectrum as a function of temperature.
This radiation field will replace the black-body that
is assumed when using the RADTEMP keyword in the call
to pop_solver.
; OPTIONAL OUTPUTS
POPSTR Send level population information to a structure. POPSTR has
the tags:
.dens Density (cm^-3)
.temp Temperature (K). Can be an array if SUM_MWL_COEFFS=
is used.
.radtemp RADTEMP. Set to -1 if RADTEMP not
set.
.rphot RPHOT value. Set to -1 if RPHOT not set.
.proton String set to 'yes' if proton rates included, 'no'
otherwise
.version CHIANTI version used to derive populations.
.date Date and time at which structure created.
.level Structure containing level information. Tags are:
.index CHIANTI level index
.term String containing level identifier.
.pop Population of level
.sumtst Set to 1 if the SUM_MWL_COEFFS keyword has been used.
Set to 0 otherwise.
.sum_mwl_coeffs Contains SUM_MWL_COEFFS. Set to -1 if sumtst=0.
KEYWORDS:
ALL Show populations for all levels.
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
DIEL Use the dielectronic recombination files. E.g., for Fe XXII,
the routine will read in the fe_22d.* files instead of the
fe_22.* files.
COMMON BLOCKS:
ELVLC, WGFA, UPSILON, RADIATIVE, PROTON, ELEMENTS
CALLS:
ZION2FILENAME, POP_SOLVER, SETUP_ION, READ_IONEQ,
READ_ABUND, PROTON_DENS, CONCAT_DIR
HISTORY:
Ver 1, PRY 22-Sep-97
Ver.2, PRY 5-Sep-98 - added call to choose_ioneq
Ver.3, PRY 23-Apr-99 - calls pop_solver now; added DENS keyword
Ver.4, PRY 18-Dec-99 - added deu to upsilon common block to be
consistent with main Chianti routines.
Ver.5, PRY 7-Aug-00 - added /DIEL keyword to allow populations of
the dielectronic recombination files to be studied.
Also changed elvlc common block to match new
version of pop_solver.
Ver 6, PRY 10-Oct-00 - now calls setup_ion to read ion data
Ver 7, PRY 12-Nov-01 - modified for proton rates, photoexcitation,
and 9 pt splines.
Ver 8, PRY 9-Dec-01 - completed modifications for v4 of CHIANTI.
V. 9, 25-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
Now we only call zion2filename
V. 10, 9-Aug-2002, Peter Young
corrected !ioneq_file problem
V. 11, 12-Aug-2002, Peter Young
added POPSTR output, and tidied up header.
V. 12, 4-Oct-2003, GDZ
modified the input to POP_SOLVER, now it is dealt with an
input structure.
V 13, 4-May-2005, Enrico Landi (EL)
Modified in order to include ionization and recombination
data in the input to POP_SOLVER
V.14, 26-May-2005, Peter Young (implemented by GDZ)
added SUM_MWL_COEFFS optional input for allowing
non-Maxwellian distributions to be considered.
added LEVEL= optional input to only print the populations of
a few levels.
V.15, 5-Jul-2005, Peter Young
added RADFUNC= and /QUIET keywords
VERSION : 15, 5-Jul-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
PLOT_POPULATIONS
PURPOSE:
plot the population of a number of the lowest levels as a function of
electron density for a specific temperature
CATEGORY:
science.
CALLING SEQUENCE:
PLOT_POPULATIONS,Ion,T,Nlevels
INPUTS:
Ion: CHIANTI style name for the ion, i.e., 'c_6' for C VI
T: electron temperature (K)
Nlevels: the number of levels for which populations are plotted
starts from level 1 (the ground level)
KEYWORD PARAMETERS:
OUTFILE: the (optional) name of the output file where the listing
is produced
PSFILE: the (optional) name of the output file where a postscript
plot produced
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
NOT_INTERACTIVE Avoid interactive use.
OUTPUTS:
COMMON BLOCKS:
common elvlc,l1a,term,conf,ss,ll,jj,ecm,eryd,ecmth,erydth,eref
common wgfa, wvl,gf,a_value
common upsilon,t_type,c_ups,splups
CALLS
POP_SOLVER, ION2SPECTROSCOPIC, ION2FILENAME, READ_IP,
CONVERTNAME, READ_ELVLC, READ_WGFA2, READ_SPLUPS
EXAMPLE:
to plot populations of the 5 ground configuration levels of Fe XIII
and store these values in a file 'Fe_XIII.lis' for a temperature of 1.5 MK
> plot_populations,'fe_13',1.5e+6,5,outfile='Fe_XIII.lis'
MODIFICATION HISTORY:
Written by: Ken Dere
March 1996: Version 2.0
November 1997: Ken Dere, added psfile keyword
September 1999: Ken Dere, for Version 3,
14-Jul-2000 Peter Young, now calls pop_solver
Version 6, 21-Dec-2000, William Thompson
Modified for better cross-platform capability.
V. 7, 21-May-2002, Giulio Del Zanna (GDZ), modified the plotting bit
generalized directory concatenation to work for
Unix, Windows and VMS.
V 8, 15-July-2002, GDZ
Added keyword not_interactive
V 9, 4-Oct-2003, GDZ
modified the input to POP_SOLVER, now it is dealt with an
input structure.
V 10, 4-May-2005, Enrico Landi (EL)
Modified in order to include ionization and recombination
data in the input to POP_SOLVER, now it allows choice of .ioneq
file needed to include ionization and recombination.
VERSION : 10, 4-May-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME: POP_PLOT
PURPOSE:
To compute n_j A_ji / N_e for a selected transition(s) and plot it
against N_e. If it is insensitive to N_e, then the line(s) is
suitable for emission measure analysis.
CATEGORY:
Atomic data analysis
EXPLANATION:
The routine calls EMISS_CALC to give values of DE*n_j*A_ji at the
temperature TEMP and densities from 10^8 to 10^12. You are then
asked to select which transition(s) you are interested in. (If
more than one line is selected, the lines are blended.)
DE*n_j*A_ji/N_e is then plotted against density.
If TEMP is not specified, then the temperature at which the
ionisation fraction has its maximum is calculated. For the iron
ions, the ion balance calcs of Arnaud & Raymond are used,
otherwise Arnaud & Rothenflug are used. If TEMP is specified,
and the value is less than 20, then it is assumed that the log
of the temperature has been specified.
In emission measure work it is important to isolate lines for
which DE*n_j*A_ji/N_e is insensitive to density. If only such lines
are used, then the derived emission measure curve is independent
of density.
CALLING SEQUENCE:
POP_PLOT, IZ, ION, WRANGE=WRANGE, [TEMP=TEMP, /QUICK, DATA=DATA, $
DENS_RANGE=DENS_RANGE, DILUTE=DILUTE]
EXAMPLES:
POP_PLOT, 26, 14, WRANGE=[330,360]
- 3 lines should appear in the widget. Selecting 334.17 should show
a curve that falls off with density. Choosing 353.83 shows a curve
that rises with density. By selecting a blend of the two lines,
the curve will be insensitive to density, telling us that only a
blend of 334.17 and 353.83 is suitable for emission measure work.
POP_PLOT, 8, 4, WRANGE=[550,560], TEMP=6.0, /QUICK, DENS_RANGE=[6,10]
- O IV is a member of the boron sequence, and so calculations take a
lot longer. Giving the QUICK keyword speeds things up. The
temperature is well away from the T_max of the ion
INPUTS:
IZ The atomic number of the ion
ION The spectroscopic number of the ion (e.g., 12 = XII)
OPTIONAL INPUTS:
DILUTE Used to set radiative dilution factor. (Default: 0.0)
TEMP The temperature at which calculations are required. Usually
this will be the Tmax of the ion.
DENS_RANGE The default density range is log Ne = 8 to 12. By
inputting two integers, a different range can be chosen.
WRANGE Wavelength range from which lines are required. If not
given, then the user is allowed to choose from the complete
set of lines for the ion.
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
RADTEMP The blackbody radiation field temperature (default
6000 K).
RPHOT Distance from the centre of the star in stellar radius
units. I.e., RPHOT=1 corresponds to the star's surface.
(Default is infinity, i.e., no photoexcitation.)
OPTIONAL OUTPUTS:
DATA: An array that contains the data that is plotted: data(*,0)
contains
the densities, while data(*,1) contains the Y-axis values.
KEYWORDS:
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
QUICK: The density range over which the calculations are done is
8 to 12 in 0.2 intervals. This keyword forces the
calculations to be done at 0.5 intervals.
CALLS:
EMISS_CALC, EMISS_SELECT, READ_IONEQ
HISTORY:
Ver.1, PRY 28-Jul-97.
Ver.2, PRY 23-Sep-97 - added DILUTE keyword for photo-excitation
Ver.3, PRY 30-May-98 - added DENS_RANGE
Ver.4, PRY 5-Sep-98 - added call to choose_ioneq
Ver.5, PRY 7-Apr-99 - tidied up, and introduced call to emiss_select
Ver.6, PRY 7-Dec-01 - modified for v.4 of CHIANTI
V. 7, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
V.8, 06-Aug-02 GDZ
added ABUND_FILE to the call to emiss_calc (was missing).
Changed the use of CHIANTI system variables.
VERSION : 8, 06-Aug-02
NAME
POP_PROCESSES
PROJECT
CHIANTI
PURPOSE:
Outputs to the screen the contributions of the different physical
processes to the population of the specified level within the ion.
E.g., for Fe XIII, level 4, the output is:
Population leaving level 4
rad. decay: 1.51e+01 39.17%
e de-exc: 3.56e-01 0.92%
e exc: 2.28e+01 59.12%
p de-exc: 2.63e-01 0.68%
p exc: 4.05e-02 0.11%
stim. emiss: 0.00e+00 0.00%
photoexc: 0.00e+00 0.00%
--------
TOTAL 3.85e+01
Population entering level 4
rad. decay: 3.59e+01 93.19%
e de-exc: 3.81e-02 0.10%
e exc: 1.46e+00 3.79%
p de-exc: 3.18e-03 0.01%
p exc: 1.12e+00 2.91%
stim. emiss: 0.00e+00 0.00%
photoexc: 0.00e+00 0.00%
--------
TOTAL 3.85e+01
which shows that the level population is dominated by electron
excitation and cascading into the level, and by radiative decay
out of the level.
Note that the rates for each physical process are multiplied by the
population of originating level (this results in the totals for
entering and leaving the level to balance).
For some ions, ionization and recombination are additional processes
included when working out the level balance. Because of the way these
processes are included (see the v.5 paper for details), the populations
entering and leaving some levels *will not balance*.
INPUTS
IZ The atomic number of the ion
ION The spectroscopic number of the ion (e.g., 12 = XII)
OPTIONAL INPUTS
LEVEL The ion level for which information is required.
DENS Electron density at which rates calculated (units: cm^-3).
If not specified, a value of 10^10 is assumed.
TEMP Temperature at which rates calculated (units: K). If not set,
then T_max of the ion is used
PATH If the ion data-files are not in the CHIANTI directories,
then PATH allows you to choose an alternative location.
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
RADTEMP Specify background radiation temperature (default: 6000 K)
N_LEVELS Restrict the ion model to this number of levels. E.g., if
the CHIANTI model contains 40 levels for the ion, then
setting N_LEVELS=12 reduces the model to 12 levels.
RADFUNC The name of a user-defined function that will generate
a radiation spectrum as a function of temperature.
This radiation field will replace the black-body that
is assumed when using the RADTEMP keyword in the call
to pop_solver.
KEYWORDS
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
CALLS
R2W, ZION2FILENAME, PROTON_DENS, POP_SOLVER, SETUP_ION
EXAMPLES
One can compare the effect of cascading on a level population by using
the N_LEVELS keyword. Consider the case of Fe XIV:
IDL> pop_processes,'fe_14',lev=5
IDL> pop_processes,'fe_14',lev=5,n_levels=12
With the first call there are two dominant terms to the population
entering level 5: approximately 47% for radiative decays (cascading)
and 53% for electron excitation. Setting n_levels=12, one finds that
the cascading contribution disappears as there are no longer any
high-lying levels that cascade into level 5. The cascading provides
a strong contribution to the population of this level.
HISTORY
Ver.1, 11-Sep-2002, Peter Young
Ver.2, 15-Jan-2004, Peter Young
modified call to pop_solver following recent revision to
pop_solver; changed input from IZ,ION to IONNAME to match other
CHIANTI routines
Ver.3, 26-May-2005, Peter Young
changed TEMP and DENS keywords
Ver.4, 10-Jun-2005, Peter Young
added common block for ionization/recombination data and modified
INPUT structure.
Ver.5, 14-Jun-2005, Peter Young
routine now prints the percentage contribution of each process;
added N_LEVELS= keyword
Ver.6, 1-Jul-2005, Peter Young
added warning for ions with ionization/recombination
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
RAD_LOSS
PURPOSE:
Calculates energy loss rate by free-free (ff), radiative
recombination (fb) and by line (bound-bound) radiation.
CATEGORY:
synthetic spectra
CALLING SEQUENCE:
RAD_LOSS,Temperature,Loss_rate
INPUTS:
None: The user will select an elemental abundance file and a
ionization equilibrium file through widgets.
KEYWORDS:
Pressure: pressure in emitting region (cm^-3 K)
density=pressure/temperature(K)
Density: density (cm^-3), constant for all temperatures
if neither density or pressure is set, then a default
constant density of 10^10 cm^-3 is used.
Psfile: to create a postscript plot of the radiative loss in
the file specified by the name assigned to 'Psfile'
Outfile: name of an ascii file where the radiative loss rate
as a function of temperature is output
RADTEMP Specify background radiation temperature (default: 6000 K)
RPHOT Distance from the centre of the star in stellar radius units.
I.e., RPHOT=1 corresponds to the star's surface. (Default is
infinity, i.e., no photoexcitation.)
NOPROT If set, then the default setting will be NOT to use
proton rates. This can be changed within the routine.
OUTPUTS:
Temperature: array of temperatures (K)
Loss_rate: energy loss rate in erg cm^3 s^-1
PROCEDURE:
if keyword pressure is set then calculations performed at constant pressure
if keyword density is set then calculations performed at constant density
otherwise, density is set to 1.e+10
pressure = density * temperature (cm^-3 K)
the user will be asked to select an abundance file and a
ionization balance file.
EXAMPLE:
> rad_loss,t,r
MODIFICATION HISTORY:
Written by: Ken Dere
January 1999: version 1, adopted from synthetic.pro
Version 2, 21-Dec-2000, William Thompson
Modified for better cross-platform capability.
Ver.3, 6-Dec-2001, Peter Young
Added /noprot, radtemp and dilute keywords.
Removed elvlc, wgfa and upsilon common blocks.
Removed calls to read_ip and read_masterlist (not needed).
Ver.4, 8-Jul-2003, Peter Young
Updated routine header (no changes to code).
V 5, 25-May-2005, GDZ
corrected routine header.
VERSION : 5, 25-May-2005, GDZ
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
Name : PLOT_IONEQ
Purpose : Plots the ionisation equilibrium values for an element.
Explanation :
Use : IDL> plot_ioneq, element [ ion=ion]
Inputs : element - the element name
Opt. Inputs : Ion (as keyword)
Outputs : None
Opt. Outputs: a postscript file.
Keywords : ION_RANGE - specify range of ions. E.g., ion_range=[5,8]
means V to VIII inclusive.
IONEQ_NAME: Name of the ionization equilization name to use.
If not passed, then the user is prompted for it.
NOT_INTERACTIVE Avoid interactive use.
Calls : Other CHIANTI routines
Common :
Restrictions: None
Side effects: None
Category : Spectral
Prev. Hist. : None
Written : C D Pike, RAL, 9-Jun-97
Modified : V.2. Update element list. modified definition of XUVTOP, and
allowed selection of ionization eq. file and creation of
postscript file.
Giulio Del Zanna (DAMTP) 10-Oct-2000
V.3, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
V 4, 15-July-2002, GDZ
Added keywords ioneq_name, not_interactive
V.5, 9-Feb-2005, Peter Young
Changed ion= keyword to ion_range=
VERSION : 5, 9-Feb-2005
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
Name : MAX_TEMP
Purpose : Calculates temperature at max ionisation ratio for an ion
Explanation :
Use : IDL> print,max_temp(ion)
Inputs : ion - the specific ion in the form eg 'Fe_XII' or 'Fe XII'
Opt. Inputs : None
Outputs : Function returns log of max temperature
Opt. Outputs: None
Keywords : ALL - if set produces a plot of all temperatures
Calls : Other CHIANTI routines
Common :
Restrictions: None
Side effects: None
Category : Spectral
Prev. Hist. : None
Written : C D Pike, RAL, 9-Jun-97
Modified : V.2 Update element list. CDP, 18-Jun-99
V.3 modified definition of XUVTOP, and allowed selection of
ionization eq. file. Giulio Del Zanna (DAMTP) 10-Oct-2000
V.4, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
VERSION : 4, 21-May-2002, GDZ
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
Name : CHIANTI_DEM
Purpose : Calculates the Differential Emission Measure DEM(T) using
the CHIANTI database, from a given set of observed lines.
Constant pressure or density can be used.
Category : diagnostic analysis
Explanation : This routine has several options, all in the form of keywords.
First, the input file with the observed fluxes is read.
THE FIRST TIME YOU USE THIS ROUTINE
you'll have to do the calculation of the contribution
functions G(T), so the routine GET_CONTRIBUTIONS will come
into play. You'll have to specify the value of the
pressure or density, and you'll be asked to select an
ionization equilibrium file and an abundance file.
GET_CONTRIBUTIONS searches the CHIANTI database (ion per ion)
for all the theoretical lines corresponding to the observed
lines, i.e. that lie in a OBS_WVL(i) +/- DELTA_LAMBDA_OBS(i)
interval centered on the observed wavelength OBS_WVL(i).
The routine calculates the C(T) values (G(T)=Ab(element)*C(T))
for the temperature interval log(T)= 4.0 - 8.0
with steps of log(T) = 0.1 .
You can either select a constant pressure OR a constant
density for all the lines; if you select a constant pressure,
for each ion the contribution function is calculated at an
electron density N_e equal to the ratio of the pressure
and the temperature of maximum ionization fraction:
C=C( T, N_e= P/T_ion )
The C(T) values are stored by GET_CONTRIBUTIONS in the output
file OUTPUT.CONTRIBUTIONS that can be used later to calculate
the DEM, changing various parameters,
without having to start again and read the CHIANTI database,
which can take long time.
In the case no theoretical lines corresponding to an observed
line are found, the routine writes the wavelength of the line
(to be excluded from the fit) in the array
EXCLU_OBS_WVL_NO_TEO. The lines with no theoretical
counterparts are then automatically excluded from the fit by
CHIANTI_DEM. You might consider the possibility to start again
incrementing the DELTA_LAMBDA_OBS, to see if there are
theoretical lines in the vicinity.
Note: if you want to exclude some of the observed lines from
the fit, you just have to use the keyword EXCLUDE_OBS_WVL,
BUT GET_CONTRIBUTIONS will store anyway the results (if any)
in the C(T) file.
After having excluded the lines in EXCLUDE_OBS_WVL,
any *.abund file present in the CHIANTI database or in
the working directory can be selected, and eventually edited,
if you like to change some abundances.
Then the $G(T)$ are calculated, multiplying each theoretical
line by the abundance factor. Then the
theoretical lines contributing to each blend are sorted by
intensity and then their G(T) can be plotted if the keyword
PLOT_GT is activated. It is recommended to do this the first
time, to check if there are some observed lines terribly
blended with lines of other elements, in which case it is
better to exclude them with a second run (if you are not
sure about the abundances).
Then the G(T) for each blend are summed and plotted.
Then the fit starts calling DEM_FIT.
A series of parameters can change the
result (DEM), especially the number and position of the mesh
points of the spline that represents the DEM. The keyword
MESH_POINTS serves for this purpose.
The other keywords that control the fit are N_ITER, DCHISQ_M.
At the end of the fit, the files OUTPUT.DEM and OUTPUT.GENERAL
are created.
Use : IDL>chianti_dem,output='serts89',file_input='serts89.obs',$
pressure=3.e15
Examples :
Assume you have a file input 'serts89.obs' like this:
243.031 491. 97. 0.1 He II
256.323 1580. 186. 0.1 He II b
315.024 253. 31. 0.1 Mg VIII
335.401 10400. 1650. 0.1 Fe XVI
319.839 113. 14. 0.1 Si VIII
356.027 218. 25. 0.1 Si X
IDL>chianti_dem,output='serts89',file_input='serts89.obs',$
pressure=3.e15,cut_gt=1e-30,/plot_gt
After having selected the ionization file,
the C(T) (with MAX(C(T)) gt 1e-30) are stored in the file
'serts89.contributions'. Then select one of the abundance
files.
Have a look at the plots of the G(T), and annotate
if there is a line you want to exclude, let's say the second.
Have a look at the DEM obtained ('serts89.dem') and at
the details contained in the file 'serts89.general'.
Maybe there is another line you want to exclude, let's say
the last one. Maybe you want to change the mesh points, too.
So run
IDL>chianti_dem,output='serts89_2',file_input='serts89.obs',$
file_gt='serts89.contributions',$
exclude_obs_wvl=[243.031,356.027 ],$
mesh_points= [4.5,5.,5.5,6.2,7.5]
The files 'serts89_2.dem' and 'serts89_2.general' will be
created. They have the essential information about what you
did.
Inputs : various, all in form of keywords. The required ones are
OUTPUT and FILE_GT (or PRESSURE/DENSITY)
Opt. Inputs : various... see the software note.
Outputs : OUTPUT.CONTRIBUTIONS
Created only if the keyword FILE_GT is NOT set.
Is the file where all the contribution functions G(T) are
stored. In the first two lines the ionization equilibrium
file name, and the constant value of pressure or density
adopted are reported. Then for each line you have reported
the observed wavelength, the theoretical one, the element and
ionization stage, then the C(T) values. At the end the
specification for each transition.
OUTPUT.DEM
Is the file where the log T and log DEM values are
written, with a format suitable
as input for the DMM_SS procedure,that calculates the
synthetic spectrum. At the end some info on how it was
calculated are printed.
OUTPUT.GENERAL
Is the file where general information is stored.
The abundance file, the ionization equilibrium file and the
constant value of pressure or density used are reported.
Then there is one line for each
observed line, with the provisional identification, the
observed wavelength, the observed flux, the theoretical one
(corresponding to the DEM), the error on the flux,
the square of the difference between the theoretical and the
observed fluxes divided by the error (this number should be
close to zero if the line is well reproduced), and finally
the ratio of the theoretical flux versus the observed one
(which should be close to 1).
After this line, there is one line per each theoretical line
contributing to the blend, with the identification, the
theoretical wavelength, the configuration and terms, and the
contribution to the total theoretical flux (in percentage)
of each line in the blend.
OUTPUT.OUT
This file , toghether with OUTPUT.DEM ,
can be used to reproduce the results using
user-written software. See the software notes.
The ouput has this format:
format='(a20,1x, 1f10.3,1x, 3e10.3, 1x, f4.2,1x,f6.3)'
Opt. Outputs:
An abundance file with the modifications inserted.
Postscript files of the G(T).
A postscript file with the DEM (OUTPUT.DEM.PS)
A postscript file with other plots too (OUTPUT_4PLOTS.PS)
Keywords :
ARCSEC:
optional. If set, it means that the intensities in the input
file are per arcsec-2 .
These intensities are then converted to
sterad-1 .
CUT_GT:
optional. If set, only the those theoretical lines that
have a MAX(C(T)) greater than the value set, are kept;
it is useful to set this value in order to reduce the number
of lines in the file where the C(T) are stored.;
if not set, a default value of 1e-30 is adopted.
DCHISQ_M:
optional. If not set, a default value of DCHISQ_MIN=1.e-5
is assumed. For each iteration, the CHISQ and it's variation
are calculated. As long as the iteration achieves an
improvement in CHISQ greater than DCHISQ_MIN , another
iteration will be performed.
DEM_FILE:
optional.If set (,/DEM_FILE) you have to choose a DEM file to
be used as a start, instead of the default constant value of
10.^22.
You can either choose one of the files in the CHIANTI database
or any you have in the working directory.
The values in the file are marked as crosses, the mesh points
are marked with triangles.
DENSITY :
the value of the density (Ne). Required if you do NOT have
already the contribution functions G(T).
EXCLUDE_OBS_WVL:
optional.
If set, you can exclude some of the observed lines from
the fit. Note that even if you set this keyword and run
GET_CONTRIBUTIONS all the theoretical lines found corresponding
to all the lines in the input file are written in the C(T)
file. It is only in the fit that the lines are excluded.
FILE_GT:
optional.
If NOT set, the routine GET_CONTRIBUTIONS is called.
If set, it has to specify the name of the file created by
GET_CONTRIBUTIONS, where all the contribution functions G(T)
are stored. In the first two lines the ionization equilibrium
file name, and the value of the pressure or density
adopted is reported. Then for each line you have reported
the observed wavelength, the theoretical one, the element and
ionization stage, then the C(T) values. At the end the
specification for each transition.
FILE_INPUT:
optional.
if set, you are not requested to select the observation file
using a widget-type search.
The input file must contain 5 columns, unformatted:
1)the observed wavelength (A)
2)the observed flux in erg cm-2 s-1 st-1
3)the corresponding error on the flux in erg cm-2 s-1 st-1
4)half the width (A) of the range (centered on the observed
wavelength) where you want to look for the corresponding
theoretical lines. A value of HWHM or more would do.
5)The identification, written as string (max 20 characters)
MESH_POINTS:
optional. It is a vector that specifies the mesh points for the
spline that represent the fitted DEM, in log(T).
If not set, the default values
[4.,4.5,5.,5.5,6.,6.5,7.,7.5,8.0] are assumed.
N_ITER:
optional.It is the number of iterations of the fitting routine.
If not set, a default value of 20 is assumed.
Changing this value alone might not affect the fit, since
also the value of DCHISQ_MIN is checked during the fit.
N_MATCHES:
optional.
In the unlikely event that more than 50 (default value for
N_MATCHES) theoretical lines corresponding to an observed
line are found, the routine stops; in this case, you have to
start again setting N_MATCHES equal to a greater number.
OUTPUT :
required.
It is the output name. Suffixes will be added when creating
the various outputs.
PHOT:
optional.
If set, it means that in the input file the intensities
are in photons instead of ergs.
PLOT_GT:
optional.
If set (,/PLOT_GT), plots of the G(T) for each
observed line not excluded are created.
PRESSURE:
the value of the pressure (Ne T). Required if you do NOT have
already the contribution functions G(T).
QUIET:
optional. Set to avoid various messages and the details of the
result.
Calls : GET_CONTRIBUTIONS
DEM_FIT
ZION2SPECTROSCOPIC
print2d_plot
Common : obs, obs_int,obs_sig,n_obs
obs_o, obs_wvl,obs_id,obs_delta_lambda
dem, d_dem_temp,dem_temp,log_dem_temp,log_t_mesh,log_dem_mesh
contr, ch_tot_contr
ab, abund_name,abund_info,xuvtop,ioneq_name
these are the commons with GET_CONTRIBUTIONS.PRO:
various, exclu_obs_wvl_no_teo,const_net,$
dem_temp_min,dem_temp_max,n_dem_temp,$
ch_wvl,ch_l1,ch_l2,ch_id,ch_z,ch_ion,ch_contr_wa,$
ch_pop,ch_contr_list, ch_term,ch_n_contr
Restrictions:
In the unlikely event that more than 50 (default value for
N_MATCHES) theoretical lines corresponding to an observed
line are found, the routine stops; in this case, you have to
start again setting N_MATCHES equal to a greater number.
Also, if the starting DEM values are not proper, or you
don't have enough constraints at lower and higher temperatures,
you might get "strange" results, and should consider using
different starting values.
Of course you need to have the enviroment variable CDS_SS_DERE
pointing to the CHIANTI database top directory.
Side effects: None known yet.
Category : spectrum
Prev. Hist. :
Written by Ken Dere (NRL) as part of the CHIANTI package
in collaboration with Brunella Monsignori Fossi, Enrico Landi
(Arcetri Observatory, Florence), Helen Mason and Peter Young
(DAMTP, Cambridge Univ.). Incorporated into the CDS software.
Written :
V. 1.0 5 November 1997 Giulio Del Zanna (GDZ),
UCLAN (University of Central Lancashire, UK)
Modified : Removed the print2d_plot subroutine. Increased the default value
of N_MATCHES from 20 to 50. Changed way to deal with xuvtop.
GDZ, 31-Oct-2000
Version : 2.0 GDZ, DAMTP, 31-Oct-2000
V.3, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
VERSION : 3, 21-May-2002, GDZ
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
PLOT_DEM
PURPOSE:
To plot differential emission measure (DEM) values
CATEGORY:
Widgets.
CALLING SEQUENCE:
PLOT_DEM,filename
INPUTS:
filename: the name of the DEM file to be plotted. The file must b
in the standard CHIANTI format for DEM files. If filename
is a blank string ('') then an interactive window will come
up to allow the user to select a DEM file from the CHIANTI
DEM directory or some other directory.
KEYWORD PARAMETERS:
PSFILE: If set, the a postscript plot will be place in the
file 'psfile' specified by the user
OUTPUTS:
None, other than a plot
EXAMPLE:
> plot_dem,'ademfile.dem'
or
> plot_dem,''
MODIFICATION HISTORY:
Written by: Ken Dere
June 1998: Version 1.0
Version 2, 21-Dec-2000, William Thompson, GSFC
Modified for better cross-platform graphics capability
V. 3, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
VERSION : 3, 21-May-2002
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME: INTEGRAL_CALC
PURPOSE:
To compute the atomic data integral for use in column or volume
emission measure work.
CATEGORY:
Scientific analysis
EXPLANATION:
Defining
G(T) = 0.83 * Fr(T) * N_j * A_ji / N_e
where Fr(T) is the ionisation fraction (e.g., from Arnaud &
Rothenflug), N_j the relative population of level j, A_ji the
A-value for the j->i transition and N_e the electron density. The
0.83 is the ratio of hydrogen to free electrons, which is constant
above around 10^4 K. This function is sharply-peaked at a
temperature T_mem (the temperature of maximum emission, which can
be different from the temperature of maximum ionisation, T_max)
and so an oft-used approximation is to take G(T) constant in the
range log T_mem - 0.15 to log T_mem + 0.15 and zero outside. The
value of the constant, which we call C_lambda here, is then given
by
C_lambda = integral { G(T) dT }
--------------------
T_mem * (10^0.15 - 10^-0.15)
If EM(s) is the column emission measure, F the flux (erg cm-2 s-1)
in a line lambda, Ab the abundance of the element and DE (erg) the
energy for the transition, then:
F = DE * Ab * C_lambda * EM(s)
If we are dealing with intensities I (erg cm-2 s-1 sr-1) then:
4pi * I = DE * Ab * C_lambda * EM(s)
This program extracts the ionisation balance and emissivities from
the CHIANTI database and calculates C_lambda for all lines in the
specified wavelength interval WRANGE by integrating over
0.02 dex temperature intervals, using the IDL INT_TABULATED function.
The C_lambda functions for all the lines in the selected wavelength
range WRANGE are displayed as well as the temperature of maximum
emission (T_mem), DE*C_lambda and 4pi/(DE*C_lambda). These latter
two quantities are useful for the emission measure analysis.
Any combination of the displayed lines can then be blended and the
corresponding quantities for the blend will be displayed.
The function Fr(T) * N_j * A_ji can also be plotted at this stage.
CALLING SEQUENCE:
INTEGRAL_CALC, IZ, ION, [WRANGE=WRANGE, /CHOOSE, DENS=DENS]
EXAMPLES:
INTEGRAL_CALC, 26, 13, WRANGE=[200,205], /CHOOSE
INTEGRAL_CALC, 14, 10, WRANGE=[250,270], DENS=10.
INPUTS:
IZ: The atomic number of the ion
ION: The spectroscopic number of the ion (e.g., 12 = XII)
OPTIONAL INPUTS:
DENS: The density at which the emissivities are calculated
(default=10.)
WRANGE: Wavelength range for which C_lambda functions are
calculated. If not given, then the 10 strongest lines
are printed.
INDEX: Particular elements in the emissivity structure can be
selected with INDEX. This allows integral_calc to be run
'silently'. The output is contained in the OUTSTR structure.
If index is given as, e.g., [7,8], then the C_lambda
functions for these two lines are summed and output.
PATH: Directly specify the directory path where the Chianti data
for the ion is found
ABUND_FILE The name of a CHIANTI abundance file. This is used for
calculating the proton to electron ratio. Default is
!abund_file.
IONEQ_FILE The name of a CHIANTI ion balance file. This is used for
calculating the proton to electron ratio and evaluating
the T_max of the ion. Default is !ioneq_file.
RADTEMP The blackbody radiation field temperature (default
6000 K).
RPHOT Distance from the centre of the star in stellar radius
units. I.e., RPHOT=1 corresponds to the star's surface.
(Default is infinity, i.e., no photoexcitation.)
KEYWORDS:
CHOOSE: Allow ion balance calculations to be selected manually
(see choose_ioneq.pro routine).
OPTIONAL OUTPUTS:
OUTSTR: A structure with the following tags
.tmem - the T_mem for the line(s)
.dec - total( de * c_lambda )
.pidec - 4 * pi / total( de * c_lambda )
Only output when INDEX is specified.
COMMON BLOCKS:
None.
CALLS:
EMISS_CALC, CH_GET_FILE, READ_IONEQ
HISTORY:
Ver.1: PRY, 28-JUN-97.
Ver.2: PRY, 7-OCT-97. Added TEMPI and GOFT, for plotting.
Ver.3: PRY, 31-JUL-98. Added PATH.
Ver.4: PRY, 6-APR-99. Added INDEX, OUTSTR. Removed TEMPI and GOFT
(these can be got from the g_of_t routine).
Ver.5: PRY, 9-Dec-01. Modified for v.4 of CHIANTI.
V.6, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
V.7, 06-Aug-02 GDZ
Changed the use of CHIANTI system variables.
VERSION : 7, 06-Aug-02
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
READ_ABUND
PURPOSE:
to read CHIANTI abundance files
CATEGORY:
science.
CALLING SEQUENCE:
READ_ABUND,File,Abundance,Reference
INPUTS:
File: the name (string) of the file containing the abundance values
(relative to hydrogen) usually of the form
'!xuvtop/abundance/*.abund'
OUTPUTS:
Abundance: an array of abuncance values
Reference: a string containing the reference to the chosen set
of abundances in the scientific literature
PROCEDURE:
You can describe the foobar superfloatation method being used here.
EXAMPLE:
> read_abund,'allen.abund',abundance,ref
abundance(26) = abundance of iron relative to hydrogen
quoted by C.W. Allen in Astrophysical Quantities
MODIFICATION HISTORY:
Written by: Ken Dere
March 1996: Version 2.0
V. 3, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
VERSION : 3, 21-May-2002
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
READ_DEM
PURPOSE:
to read values the differential emission measure as a function
of temperature
CATEGORY:
science.
CALLING SEQUENCE:
READ_DEM, File, T, Dem, Ref
INPUTS:
File: the name of the file containing the DEM values, usually in
!xuvtop/dem/*.dem
OUTPUTS:
T: Log10 values of temperature (K)
Dem: Log10 values of the differential emission measure
Ref: the reference to the DEM values in the scientific literature
OPTIONAL OUTPUTS:
Describe optional outputs here. If the routine doesn't have any,
just delete this section.
EXAMPLE:
> read_dem,!xuvtop+'/dem/active_region.dem',t,dem,ref
MODIFICATION HISTORY:
Written by: Ken Dere
March 1996: Version 2.0
V. 3, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
Ver.4, 20-Nov-2002, Peter Young
DEM values of -1 caused errors, so this has been corrected.
VERSION : 4, 20-Nov-2002
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
READ_IONEQ
PURPOSE:
to read files containing the ionization equilibrium values
CATEGORY:
science.
CALLING SEQUENCE:
READ_IONEQ, File, T, Ioneq, Ref
INPUTS:
File: for example, !xuvtop+'/ioneq/arnaud_rothenflug.ioneq'
OPTIONAL INPUTS:
None:
OUTPUTS:
T: array of log10 temperatures
Ioneq: 3-d array (T,element,ion)
of the fractional abundance of the ion in
ionization equilibrium.
Ref: reference in the scientific literature
EXAMPLE:
> read_ioneq,!xuvtop+'/ioneq/arnaud_rothenflug.ioneq'
> help,t,ioneq
> T FLOAT = Array(41)
> IONEQ FLOAT = Array(41, 28, 29)
> print, minmax(t)
> 4.00000 8.00000
> print,t(20)
> 6.0000
> print,ioneq(20,25,9)
> 0.269 = fractional abundance of Fe X in
ionization equilibrium
MODIFICATION HISTORY:
Written by: Ken Dere (KPD)
March 1996: Version 2.0
March 1999: KPD to read both number of temperature and number
of elements
25-Oct-2000 V. 4, Giulio Del Zanna (GDZ).
Corrected to interpret the '-1' as a reference only
if within the first 3 columns
V. 5, 21-May-2002, Giulio Del Zanna (GDZ)
generalized directory concatenation to work for
Unix, Windows and VMS.
v.6, 25-Oct-2004, Peter Young
modified format statement so that it will read any number of
temperatures.
V 7, 25-May-2005, GDZ
corrected routine header.
VERSION : 7, 25-May-2005
PROJECT: CHIANTI
http://wwwsolar.nrl.navy.mil/chianti.html
CHIANTI is an atomic database package for the calculation of
continuum and emission line spectra from astrophysical plasmas. It is a
collaborative project involving the Naval Research Laboratory
(Washington DC, USA), the Arcetri Observatory (Firenze, Italy), and the
Cambridge University (United Kingdom).
NAME:
CH_READ_FITS
PURPOSE:
Read standard CHIANTI FITS binary table data containing the output from
CH_SYNTHETIC and output a TRANSITIONS structure.
CALLING SEQUENCE:
CH_READ_FITS, Filename, TRANSITIONS
INPUTS:
Filename = String containing the name of the CHIANTI FITS file written
by CH_WRITE_FITS.
OUTPUTS:
TRANSITIONS = Structure to be written.
OPTIONAL INPUTS: none
KEYWORDS: none
NOTES:
CALLS:
MRDFITS, ADD_TAG
COMMON BLOCKS: none.
RESTRICTIONS:
(3) The input FITS file must have been written by CH_WRITE_FITS
PREV. HIST. :
EXAMPLE:
ch_read_fits, 'file.fits', transitions
WRITTEN :
Ver.1, 8-Apr-02 Giulio Del Zanna (GDZ)
V.2 GDZ 31 May 2002 added more checks.
MODIfICATION HISTORY:
VERSION : 2, 31 May 2002
PROJECT: CHIANTI
CHIANTI is an Atomic Database Package for Spectroscopic Diagnostics of
Astrophysical Plasmas. It is a collaborative project involving the Naval
Research Laboratory (USA), the University of Florence (Italy), the
University of Cambridge and the Rutherford Appleton Laboratory (UK).
NAME:
CH_WRITE_FITS
PURPOSE:
Write standard FITS binary table data from CHIANTI input structure.
CALLING SEQUENCE:
CH_WRITE_FITS, Input, Filename
INPUTS:
Input = Structure to be written to FITS file.
OUTPUTS:
Filename = String containing the name of the file to be written.
CH_WRITE_FITS creates two binary table extension in a single
FITS file. The second one is appended as a new extension.
OPTIONAL INPUTS: Header COMMENTS.
KEYWORDS:
head1, head2
Additional COMMENTS to be added at the bottom of the two binary tables.
NOTES:
Any existing FITS file can be over-written or not.
Use CH_READ_FITS to convert the FITS file back into a structure.
CALLS:
FXPAR(), FXADDPAR, IS_IEEE_BIG(), HOST_TO_IEEE, DIALOG_MESSAGE
COMMON BLOCKS: none.
RESTRICTIONS:
(1) Limited to 127 columns in tables by IDL structure limits.
(2) String columns with all columns of zero length crash the
program
(3) The input structure has to be of the type TRANSITIONS.
PREV. HIST. :
The subroutines in this procedure are extracted without modifications from
the MWRFITS.PRO routine, written by T. McGlynn Version 0.95 2000-11-06
and present in the ASTRON library (in SolarSoft under /gen/idl_libs/astron/).
EXAMPLE:
ch_write_fits, transitions , 'test.fits'
WRITTEN :
Ver.1, 22-May-02 Giulio Del Zanna (GDZ)
MODIfICATION HISTORY:
VERSION : 1, 22-May-02, GDZ
NAME
WHICH_LINE
PROJECT
CHIANTI
PURPOSE:
Upon given an ion name and wavelength, this routine prints out a list
of possible line IDs for the wavelength. Wavelengths within 1% of the
input wavelength are searched for.
INPUTS
IONNAME Name of an ion in the CHIANTI format. E.g., 'fe_13' for Fe XIII.
WVL A wavelength in angstroms.
OUTPUTS (to screen)
Prints a list of atomic transitions and wavelengths for lines close to
the input wavelength. A '*' is placed next to the closest wavelength
match.
KEYWORDS
NARROW Narrows the search range to 0.02% of the specified wavelength.
EXAMPLE
IDL> which_line,'o_6',1032
Wavelength i j Lower level Upper level A-value
1037.615 1 2 1s2.2s 2S1/2 - 1s2.2p 2P1/2 4.21e+008
1031.914 1 3 1s2.2s 2S1/2 - 1s2.2p 2P3/2 4.28e+008
CALLS
CONVERTNAME, ZION2FILENAME, READ_WGFA2, READ_ELVLC
HISTORY
Ver.1, 22-Jun-2004, Peter Young
Project : CHIANTI
CHIANTI is an atomic database package for the calculation of
continuum and emission line spectra from astrophysical plasmas. It is a
collaborative project involving the Naval Research Laboratory
(Washington DC, USA), the Arcetri Observatory (Firenze, Italy), and the
Cambridge University (United Kingdom).
Name : USE_CHIANTI
Purpose : Sets up system variables for use of CHIANTI routines
Explanation : The CHIANTI software uses system variables
that have to be defined. This routine is called by the
CHIANTI routines if these system variables are not defined.
** If one is using the solar-soft package, these should
already be defined*****.
** If the CHIANTI package is used as stand-alone, then
this routine can be used for the setup with e.g.:
use_chianti,'/home/data/chianti/'
if /home/data/chianti/ points to the actual place where
the CHIANTI top directory is.
Use : IDL> use_chianti, '/home/data/chianti/', $
[ioneq= , abund=]
Inputs : None
Opt. Inputs : The full pathname of the CHIANTI top directory.
Outputs : None
Opt. Outputs: None
Keywords : IONEQ - to define the default ionization eq. file to be used.
ABUND - to define the default abundance file to be used.
Calls : None
Common : None
Restrictions: None
Side effects: None
Category :
Prev. Hist. : Based on use_dere_chianti, written by C D Pike, RAL
Written : Giulio Del Zanna (GDZ) DAMTP (University of Cambridge, UK)
Modified : Version 1, GDZ 10-Oct-2000
Version 2, GDZ 10-Jan-2001
added the definition of the !abund_file
V. 3, GDZ, 2-May-2002 Modified substantially, adding a new
system variable.
V.4, 10-July-2002 GDZ
Removed the definition of !chianti_top, upon request.
V.5, 25-July-2002, GDZ
Fixed a problem with IDL versions earlier than 5.3 (the routine
would not compile). ALso, introduced the use of concat_dir for
cross-platform compatibility.
V.6, 06-Aug-02 GDZ
Changed the use of CHIANTI system variables. Added comments on
the which CHIANTI version is used.
V.7 12-Aug-02 GDZ Changed default abundance file. Removed '***'
V.8, GDZ 13-Feb-2003
Changed default ioneq file, to include ALL the elements.
Version : V.8, 13-Feb-2003