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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
(See synt_spec/ch_line_list.pro)
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. V.13, 3-Oct-2005 GDZ Replaced FOR i=0, calls with FOR i=0L, calls, so the routine does not crash with a large number of lines. TO DO LIST: Control the range of Angstroms when clicking kev Allow plots in intensities instead of intensities A-1 VERSION : V.13, 3-Oct-2005
(See synt_spec/ch_ss.pro)
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. v.28, 31-Aug-2005, GDZ Fixed bug concerning the case when multiple temperatures (i.e. logt_isothermal) were defined as input. The program was, in some cases, returning null values. The problem was the use of nt, the number of good temperatures for each ion, for the definition of the arrays, instead of using the number of logt_isothermal values (and the t_index). v.29, 22-Aug-2008, Peter Young Changed list_goft_new and this_goft to be double precision, and changed str.goft to be double precision. v.30, 12-Jun-2009, Enrico Landi Changed the definition of the temperature array for ion fractions in the IONREC variable, now taken directly from the output of READ_IONEQ.PRO VERSION : 30, 12-Jun-2009
(See synt_spec/ch_synthetic.pro)
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. ALL Include all lines, i.e. also those for which wavelengths are only theoretical and not observed. 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. V.8, 14-Sept-2005 GDZ Added ALL keyword and modified header, error message. V.9, 3-Oct-2005, GDZ Now the FOR loop accepts more than 32000 lines. V.10, 7-Oct-2009, Peter Young The keyword EM_INT is now used in the call to the continuum routines. VERSION : Version 10, 7-Oct-2009
(See synt_spec/isothermal.pro)
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 If set, then print out information while the routine is running. KEV If set, then the output spectrum is in units erg cm^-2 s^-1 keV^-1. 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, 2002年5月22日, 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). v.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. v.16, 31-Aug-2005, GDZ Fixed a typo (keyowrd_set). v.17, 10-Mar-2006, Peter Young The /keV keyword is now passed to the continuum routines, rather than make_chianti_spec performing the conversion itself. v.18, 4-May-2006, Peter Young Changed LAMBDA to be a double array in order to correct a problem with line profiles for very small bin sizes. Problem pointed out by Matthew West (Imperial). v.19, 16-Nov-2007, Vincenzo Andretta, INAF/OACN (andretta@oacn.inaf.it) Fixed a problem with units when LOGT_ISOTHERMAL is set. v.20, 7-Oct-2009, Peter Young Modified call to continuum routines to use new EM_INT keyword (for isothermal plasmas). VERSION : 20, 7-Oct-2009, Vincenzo Andretta 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
(See synt_spec/make_chianti_spec.pro)
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
(See synt_spec/synthetic.pro)
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
(See synt_spec/synthetic_plot.pro)