A step by step user's guide to Cossam

Cossam_multi :	Codice per la sintesi spettrale nelle atmosfere magnetiche (con macchie)
	Codi per a la síntesi espectral en les atmosferes magnètiques (amb tacas)
	Code pour la synthèse spectrale dans les atmosphères magnétiques (avec taches)

Contents of the step by step user's guide to CossamMulti

Step 1 : Downloading and installing the compiler
Step 2 : Downloading the code
Step 3 : Splitting (chopping) the code
Step 4 : Compiling the code
Step 5 : Establishing the line data files
Step 6 : Calculating stellar Stokes spectra (co-rotating grid) with Cossam_multi
Step 7 : Understanding the output

A step by step user's guide to Cossam_multi and Lines (version 21-03-2022)

Step 1 : Downloading and installing the compiler

The latest free 32-bit or 64-bit GNAT compiler may preferably be obtained from the AdaCore site
or alternatively from any of the numerous Linux distributions.
Step 2 : Downloading the code
The following files are provided for the calculation of the Stokes spectrum of a spotted magnetic star similar to HD50773
- comulin_21_03_2022.ada
- lines.inp
- t8300_410_f.fil (atmospheric model)
- Stift_list_v1.list (atomic transition list)
- grev_sau.abund.FeNi (abundance file)
- cossam_multi_spot_iden.inp
- spots.abund_Ni_* (abundance files)
- Ni_5510.list (if you want to calculate spectra for a given interval about a list of wavelengths)
Step 3 : Splitting (chopping) the code

The file comulin_21_03_2022.ada contains many packages, procedure and functions. GNAT users have to split (gnatchop)
this file, because GNAT requires different compilation units to be in different files.

The following command will split the file: gnatchop -w comulin_21_03_2022.ada

Note: The -w option overwrites existing files.
Step 4 : Compiling the code

After splitting (gnat-chopping) comulin_21_03_2022.ada you have to create the executables lines and cossam_multi
by issuing the following 2 commands:

gnatmake -O3 -gnatfvp lines
gnatmake -O3 -gnatfvp cossam_multi

Note: In order to be able to execute lines or cossam_multi, make sure that your system provides unlimited stacksize.
With the tcsh shell for example set "limit stacksize unlimited"

Step 5 : Establishing the line data files

One has now to create the auxiliary files containing the atomic line data; this is done by invoking

./lines lines.inp

lines_run.7011962194	log file
sysom_ess.7011962194	essential model and abundance data
sysom_line.7011962194	data for all the selected lines
sysom_stream.7011962194	binary line data

would be line data and log files created by lines on 2017-01-19 17:16

What you have to specify in the input file lines.inp

Number of processors
Atmospheric model file
Atomic transition list file

Zeeman splitting option

'-'

Lande factors as given in the line file; set to unity if unknown (=99.00)

Hydrogen option

'h' or 'H'	Hydrogen line profiles according to the analytical formula of Hubeny
'-'	No hydrogen lines considered

Lower-upper level limit

'0.6667'

leave unchanged

Stark option

'a', 'A'	Stark broadening according to Gonzalez et al. 1995, A&A, 297, 223
'v', 'V'	Stark broadening as given in the atomic transition list file; zero if not listed
'n', 'N'	Stark broadening set zo zero and Unsoeld van der Waals broadening

Line strength option

'-'

Oscillator strengths log gf as given in the line file

Partition function preferences (4-character string)

'KCIB'

leave unchanged

Lower limit in lambda (in Angstroms)
Upper limit in lambda (in Angstroms)
Rel. line opacity contr. limit (typically 0.001 or 0.0005) :
a line is only considered if the ratio (central line opacity) / (cont. opacity)
exceeds this limit at any one optical depth
Microturbulence (in km/s)
Element file name (be careful to specify the highest elemental abundances to be used later in CossamMulti)
The input file has to end with FIN

Step 6 : Calculating Stokes spectra with CossamMulti

Step 6a : When there are n spots or rings, the code is invoked by

./cossam_multi input_file sysom_ess_ext_1 sysom_ess_ext_2 .... sysom_ess_ext_n

input_file	sysom_ess_ext_*
Any arbitrary name is permitted, e.g. cossam_multi_spot_iden.inp cossam_multi_spot_diff.inp cossam_multi_spot_mean.inp cossam_multi_ring.inp	the 10-digit extension of the line data files created with *lines*

Step 6b : What you have to specify in the input file

Number of processors (cores)
Sub-Interval size
Atmospheric model files
For each spot you have to specify the corresponding atmospheric file calculated with specific elemental abundances,
e.g. 12 atmospheric file names for 12 spots. The atmospheres can all be identical, but they can also feature different
temperatures, chemical compositions, micro-turbulence ... Only the number of depth points has to be the same for
all models.

Polarised formal solver option

'Z'	Zeeman Feautrier solver (default)
'z'	Zeeman Feautrier solver without magneto-optical terms

Hydrogen option (must agree with the values given in 'lines.inp')
Cossam checks for contradictions. You may only exchange 'h' for 'H' and vice versa

'h' or 'H'	Hydrogen line profiles according to the analytical formula of Hubeny
'-'	No hydrogen lines considered

Lower limit in lambda (in Angstroms)
Upper limit in lambda (in Angstroms)
Step size in lambda (in Angstroms) or in velocity (in km/s)
Interval delta_lambda around each line from line selection file over which the spectrum is synthesised (in Angstroms)
Element file names
For each spot you have to specify the corresponding element file with the appropriate abundances, e.g. 12 element
file names for 12 spots. The abundances need not correspond to the abundances used for the calculation of the
atmospheric models.

Line selection file name

'file_name'	The spectrum is synthesised only over intervals of delta_lambda (in Angstroms) centred on each line listed in this file, located between the lower and the upper limit in lambda.
'-'	no such selection, the spectrum is synthesised for the whole spectral region located between the lower and the upper limit in lambda.

Finally there are the keywords SPOTS (spots) or RING (ring) followed by the Oblique Rotator Model data
- for their definition see Stift, MNRAS 172, 133 (1975) - and the grid data

The inclination i    (in degrees)
The 3 Eulerian angles alpha, beta, gamma    (in degrees)
The decentring parameters x_2 and x_3   [-1 < x_2 < 1, -1 < x_3 < 1]

The dipole moment - half the polar field strength for a centred dipole (in Gauss)
The projected rotational velocity v sin i (in km/s)
The number of latitude rings defining the spatial resolution of the co-rotating grid; permitted values are :
6, 8, 9, 10, 12, 15, 18, 20, 24, 25, 30, 36, 40, 45, 50, 60, 72, 75, 90
The program automatically determines the nearest (lower) permitted value

No. of rings	No. of surface elements
8	80
15	284
24	732
40	2034
90	10310

Alternatively
A) The spot parameters
For each spot specified by an atmospheric and an element file name, there is 1 set of parameters.
In the example below the background is defined first, then 4 spots which are slightly offset and overlap.
When there is overlap, it is always the latest abundance that is taken. In this example, we thus define a
deformed Ni spot with 3 non-concentric abundance rings around the central part. The field factor
allows you to modify the absolute field strength inside the spot by a multiplicative factor.

Latitude	Longitude	Radius	Field factor	`Element`
0.0	100.0	180.0	1.00	`28`
+13.0	40.0	56.0	1.00	`28`
+15.0	35.0	43.0	1.00	`28`
+17.0	30.0	30.0	1.00	`28`
+19.0	25.0	17.0	1.00	`28`

B) The (warped) ring parameters
For each (warped) ring specified by an atmospheric and an element file name, there is 1 set of parameters.
In the example below the background is defined first, then 4 partially overlapping rings, defining a Fe ring
with different abundances at different distances from the "magnetic equator" (where the field lines are
90 degrees from the vertical).
Again, the background is defined first. The innermost rings extends between where the magnetic vector is
inclined from 85 to 95 degrees. The outermost rings goes from 70 to 75 and from 105 to 110 degrees.

Lower angle	Upper angle	`Element`
0.0	180.0	`26`
70.0	110.0	`26`
75.0	105.0	`26`
80.0	100.0	`26`
85.0	95.0	`26`

The number of rotational phases
The rotational phases [0 <= Phase_rot < 1]
(there can be only 10 phases per line; 25 phases for example have to be specified on 3 lines)

Step 7 : Understanding the output

The results of the calculations are written into the files cospot_pprof_[phase_number].[10-digits-extension].
For 10 phases you get the files cospot_pprof_r01.[ext] .... cospot_pprof_r10.[ext].
They contain 6 columns:

     wavelength (in Angstroms)
     Stokes I
     Stokes Q
     Stokes U
     Stokes V
     Continuum

cossam_multi_run.[10-digits-extension] is the corresponding log file when cossam_multi has been invoked with the commands

     ./cossam_multi input_file sysom_ess_ext_1 sysom_ess_ext_2 .... sysom_ess_ext_n

Contents of the file lines.inp

Contents of the file lines_run.7011962194

Data start at line 4, col 35    : !
=== Comment :
--------------------------------:
No. of processors               : 1
Atmospheric model               : t8300_410_f.fil
List of spectral lines          : Stift_list_v1.list
Zeeman splitting option         : -
Hydrogen option                 : -
lower-upper level limit         : 0.6666667
Stark option                    : A
Line strength option            : -
Partition function preferences : KCIB
Lower limit in lambda [A]       : 5503.000
Upper limit in lambda [A]       : 5517.000
Rel. line opacity contr. limit : 0.001
Microturbulence [km/s]          : 0.0
Element file                    : grev_sau.abund.FeNi
                                : FIN

Lines version                  : 18-01-2017
version produced by this run    : 7011962194
date                            : 19-01-2017 17:16:35

1 H   12.00    1.008 2   : -
2 He 10.93    4.00 3   : -
3 Li   1.10    6.94 4   : +
....
25 Mn   5.39   54.93 5   : +
26 Fe   7.50   55.85 5   : + 9.00
27 Co   4.92   58.94 5   : +
28 Ni   6.25   58.69 5   : + 7.00
29 Cu   4.21   63.54 3   : +
....
92 U    0.01 238.10 3   # -
------------------------------

Contents of the file sysom_ess.7011962194

ZS A KCIB
t8300_410_f.fil
Stift_list_v1.list
7011962194
8300.0 4.10 0.07833 0.00
192 1007 1038 283 1504 72 5503.000 5517.000
12.000 12.000 12.000 12.000 12.000 12.000 12.000 12.000 12.000 12.000 12.000 12.000 ....
....

Contents of the file sysom_line.7011962194

   Teff        Log g       He/H
8300.0       4.10       0.078
Microturb. = 0.00 (km/sec)
5504.515 C 1 8.520 -4.900 7.946 1.0 0.0 1.00 1.00 1.00   0.729   0.000 29.823 5.378E-03
5505.836 C 1 8.520 -2.770 8.848 1.0 2.0 1.50 1.50 1.50   0.729   0.000 28.117 1.095E-01
....
5509.597 Mg 1 7.580 -2.610 5.108 1.0 1.0 2.00 1.50 1.75   0.728   0.000 28.647 3.033E-01
5503.211 Si 1 7.550 -2.370 5.619 3.0 3.0 1.00 1.00 1.00   0.730   0.000 28.619 1.822E-01
5514.778 P 1 5.450 -2.000 7.404 1.5 2.5 1.00 1.00 1.00   0.727   0.000 29.602 6.397E-03
....
5513.522 Ti 2 5.020 -1.530 5.885 3.5 3.5 1.14 1.28 1.21   6.324 14.212 31.015 1.593E-01
5504.885 V 1 4.000 -0.882 1.711 1.5 0.5 1.20 2.21 0.95   0.298 15.000 31.082 5.064E-02
....
5513.425 Cr 2 5.670 -4.303 5.662 1.5 0.5 0.80 0.00 1.00   2.600 15.426 31.340 1.547E-02
5514.419 Cr 2 5.670 -2.904 6.484 3.5 3.5 0.89 1.00 0.95   3.327 15.411 31.503 6.684E-02
5504.218 Mn 1 5.390 -2.540 3.133 5.5 4.5 1.27 1.43 0.91   0.585 14.906 30.450 3.415E-02
5505.876 Mn 1 5.390 -2.230 2.178 1.5 2.5 1.87 1.89 1.90   3.999 14.739 30.965 5.378E-01
....
5512.054 Fe 1 9.000 -3.673 3.301 2.0 1.0 1.18 1.39 1.07   1.459 14.373 31.082 3.268E+00
5512.257 Fe 1 9.000 -1.420 4.371 4.0 4.0 1.10 1.28 1.19   1.820 12.398 29.550 6.086E+01
5512.397 Fe 1 9.000 -1.474 4.415 3.0 3.0 0.89 1.26 1.07   1.807 11.966 30.930 4.901E+01
....

Contents of the file cossam_multi_spot_iden.inp (identical atmospheric models)

                                :
Always start here               : !
--------------------------------:
No. of processors               : 5
Interval size in [A]            : 0.050
Atmospheric model 0             : t8300_410_f.fil
Atmospheric model 1             : t8300_410_f.fil
Atmospheric model 2             : t8300_410_f.fil
Atmospheric model 3             : t8300_410_f.fil
Atmospheric model 4             : t8300_410_f.fil
Atmospheric model 5             : t8300_410_f.fil
Atmospheric model 6             : t8300_410_f.fil
Atmospheric model 7             : t8300_410_f.fil
Atmospheric model 8             : t8300_410_f.fil
Atmospheric model 9             : t8300_410_f.fil
Atmospheric model 10            : t8300_410_f.fil
Atmospheric model 11            : t8300_410_f.fil
Atmospheric model 12            : t8300_410_f.fil
Formal solver option            : Z
Hydrogen option                 : -
Lower limit in lambda [A]       : 5508.750
Upper limit in lambda [A]       : 5511.250
Step size in lambda   [A]       : 0.050
Interval around line [A]       : 1.250
Element file 0                  : spots.abund_Ni_615
Element file 1                  : spots.abund_Ni_620
Element file 2                  : spots.abund_Ni_625
Element file 3                  : spots.abund_Ni_635
Element file 4                  : spots.abund_Ni_645
Element file 5                  : spots.abund_Ni_620
Element file 6                  : spots.abund_Ni_625
Element file 7                  : spots.abund_Ni_635
Element file 8                  : spots.abund_Ni_645
Element file 9                  : spots.abund_Ni_605
Element file 10                 : spots.abund_Ni_595
Element file 11                 : spots.abund_Ni_605
Element file 12                 : spots.abund_Ni_595
Line selection file             : Ni_5510.list
                                : SPOTS
Incl Alp Bet Gam y_2 y_3   : 40.0 -90.0 90.0 60.0 0.00 0.00
Dipole_moment Vrot Lat_step   : 1.0 46.0   75
Vp Phase_pul L_puls M_puls   : 0.0 0.00 0 0
Lat_0 Lon_0 Rad_0 Field_0    :   0.0 100.0 180.0 1.00 28
Lat_1 Lon_1 Rad_1 Field_1    : +12.0 126.0   41.0 1.00 28
Lat_2 Lon_2 Rad_1 Field_1    : +12.0 124.0   32.0 1.00 28
Lat_3 Lon_3 Rad_2 Field_2    : +11.0 122.0   18.0 1.00 28
Lat_4 Lon_4 Rad_2 Field_2    : +11.0 120.0   10.0 1.00 28
Lat_5 Lon_5 Rad_3 Field_3    : +24.0 303.0   41.0 1.00 28
Lat_6 Lon_6 Rad_3 Field_3    : +22.0 302.0   28.0 1.00 28
Lat_7 Lon_7 Rad_4 Field_4    : +20.0 301.0   20.0 1.00 28
Lat_8 Lon_8 Rad_4 Field_4    : +18.0 300.0   13.0 1.00 28
Lat_9 Lon_9 Rad_4 Field_4    : +5.0   30.0   42.0 1.00 28
Lat_10 Lon_10 Rad_4 Field_4    : +9.0   35.0   27.0 1.00 28
Lat_11 Lon_11 Rad_4 Field_4    : +20.0 210.0   32.0 1.00 28
Lat_12 Lon_12 Rad_4 Field_4    : +15.0 210.0   18.0 1.00 28
No. of rotational phases       : 5
Rotational phases [0<=phi<=1] : 0.00 0.20 0.40 0.60 0.80
                                : FIN

Contents of the file cossam_multi_spot_diff.inp
(simple spot, different atmospheric models)

                                :
Always start here               : !
                                :
No. of processors               : 5
Interval size in [A]            : 0.100
Atmospheric model 0             : t12000_400_07.50.fil
Atmospheric model 1             : t12000_400_08.00.fil
Atmospheric model 2             : t12000_400_08.50.fil
Formal solver option            : Z
Hydrogen option                 : -
Lower limit in lambda [A]       : 4900.000
Upper limit in lambda [A]       : 5100.000
Step size in lambda   [A]       : 0.050
Interval around line [A]       : 0.700
Element file 0                  : spots.abund_0750
Element file 1                  : spots.abund_0800
Element file 2                  : spots.abund_0850
Line selection file             : Fe_alphaCanVen.list
                                : SPOTS
Incl Alp Bet Gam y_2 y_3   : 65.0 -80.0 0.0 0.0 0.00 0.00
Dipole_moment Vrot Lat_step   : 2000.0 18.0   75
Vp Phase_pul L_puls M_puls   : 0.0 0.00 0 0
Lat_0 Lon_0 Rad_0 Field_0    :   0.0 100.0 180.0 1.00 26
Lat_1 Lon_1 Rad_1 Field_1    : +10.0   40.0   40.0 1.00 26
Lat_2 Lon_2 Rad_2 Field_2    : +10.0   40.0   30.0 1.00 26
No. of rotational phases       : 5
Rotational phases [0<=phi<=1] : 0.00 0.20 0.40 0.60 0.80
                                : FIN

Contents of the file cossam_multi_spot_mean.inp
(simple spot, identical atmospheric models)

                                :
Always start here               : !
                                :
No. of processors               : 5
Interval size in [A]            : 0.100
Atmospheric model 0             : t12000_400_07.50.fil
Atmospheric model 1             : t12000_400_07.50.fil
Atmospheric model 2             : t12000_400_07.50.fil
Formal solver option            : Z
Hydrogen option                 : -
Lower limit in lambda [A]       : 4900.000
Upper limit in lambda [A]       : 5100.000
Step size in lambda   [A]       : 0.050
Interval around line [A]       : 0.700
Element file 0                  : spots.abund_0750
Element file 1                  : spots.abund_0800
Element file 2                  : spots.abund_0850
Line selection file             : Fe_alphaCanVen.list
                                : SPOTS
Incl Alp Bet Gam y_2 y_3   : 65.0 -80.0 0.0 0.0 0.00 0.00
Dipole_moment Vrot Lat_step   : 2000.0 18.0   75
Vp Phase_pul L_puls M_puls   : 0.0 0.00 0 0
Lat_0 Lon_0 Rad_0 Field_0    :   0.0 100.0 180.0 1.00 26
Lat_1 Lon_1 Rad_1 Field_1    : +10.0   40.0   40.0 1.00 26
Lat_2 Lon_2 Rad_2 Field_2    : +10.0   40.0   30.0 1.00 26
No. of rotational phases       : 5
Rotational phases [0<=phi<=1] : 0.00 0.20 0.40 0.60 0.80
                                : FIN

Contents of the file cossam_multi_ring.inp
(simple ring, identical atmospheric models)

                                :
Always start here               : !
                                :
No. of processors               : 5
Interval size in [A]            : 0.100
Atmospheric model 0             : t8300_410_f.fil
Atmospheric model 1             : t8300_410_f.fil
Atmospheric model 2             : t8300_410_f.fil
Atmospheric model 3             : t8300_410_f.fil
Atmospheric model 4             : t8300_410_f.fil
Formal solver option            : Z
Hydrogen option                 : -
Lower limit in lambda [A]       : 4900.000
Upper limit in lambda [A]       : 5100.000
Step size in lambda   [A]       : 0.050
Interval around line [A]       : 0.500
Element file 0                  : grev_sau.abund.Fe_0800
Element file 1                  : grev_sau.abund.Fe_0825
Element file 2                  : grev_sau.abund.Fe_0865
Element file 3                  : grev_sau.abund.Fe_0905
Element file 4                  : grev_sau.abund.Fe_0945
Line selection file             : Fe_alphaCanVen.list
                                : RING
Incl Alp Bet Gam y_2 y_3   : 60.0 15.0 25.0 -30.0 -0.11 0.15
Dipole_moment Vrot Lat_step   : 1250.0 25.0   60
Vp Phase_pul L_puls M_puls   :   0.0 0.00 0 0
ang_lo_0 ang_up_0              :   0.0 180.0 26
ang_lo_1 ang_up_1              : 70.0 110.0 26
ang_lo_2 ang_up_2              : 75.0 105.0 26
ang_lo_3 ang_up_3              : 80.0 100.0 26
ang_lo_4 ang_up_4              : 85.0   95.0 26
No. of rotational phases       : 5
Rotational phases [0<=phi<=1] : 0.00 0.20 0.40 0.60 0.80
                                : FIN

Sub-interval size

A good choice for the sub-interval size is <=1.000 Angstroms. The total interval size must be a multiple of the sub-interval size.

When synthesising a spectrum over a large interval, using a large number of processors, a sub-interval size of 1.000 Angstroms tends to ensure good load balance. Narrow intervals and many processors may require 0.500 Angstroms or less. In any case you have to make sure that every processor calculates at least 1 sub-interval.

The element file

The abundances in the element file are logarithmic with the abundance of hydrogen = 12.00).

1 H   12.00    1.008 2   : -
2 He 10.93    4.00 3   : -
3 Li   1.10    6.94 4   : -
4 Be   1.40    9.02 4   : -
5 B    2.55   10.82 4   : -
6 C    8.52   12.01 6   : - 7.50
7 N    7.92   14.01 6   : - 7.02
8 O    8.83   16.00 6   : - 8.02
9 F    4.56   19.00 6   : -
10 Ne   8.08   20.18 6   : -
11 Na   6.33   23.00 6   : -
12 Mg   7.58   24.32 6   : - Mg.koch
13 Al   6.47   26.97 6   : - 6.10
14 Si   7.55   28.06 6   : - 8.05
15 P    5.45   30.98 6   : -
16 S    7.33   32.07 6   : -
17 Cl   5.50   35.46 5   : -
18 Ar   6.40   39.94 5   : -
19 K    5.12   39.10 5   : -
20 Ca   6.36   40.08 5   : -
21 Sc   3.17   45.10 5   : -
22 Ti   5.02   47.90 5   : -
23 V    4.00   50.95 5   : -
24 Cr   5.67   52.01 5   : -
25 Mn   5.39   54.93 5   : -
26 Fe   7.50   55.85 5   : -
27 Co   4.92   58.94 5   : -
28 Ni   6.25   58.69 5   : + 6.15
29 Cu   4.21   63.54 3   : -
...

All elements are listed with:
atomic number, element symbol, solar abundance, atomic weight,
number of ionisation stages considered.

To specify a different constant abundance over optical depth,
enter the new value after the '-' (preceded by a blank).

To specify a different non-constant abundance over optical depth,
enter the name of a file after the '-' (preceded by a blank).
The file must contain an abundance value for each optical depth.

There must be no blanks following the '-' or the new abundances

The atmospheric model file

The minimum required data in the atmospheric input file for a Kurucz model with T_eff = 8300 K, log_g = 4.1, and 72 depth points look as follows

72
8300.0 4.10 0.07833
xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx
1.6716E-03 5.0194E-06 0.9289 -1.2167 1.3230 26.1994 ....
2.0560E-03 6.2506E-06 0.9208 -1.1133 1.4129 26.1449 ....
2.4786E-03 7.7604E-06 0.9156 -1.0345 1.4941 26.1039 ....
2.9490E-03 9.6182E-06 0.9098 -0.9544 1.5696 26.0581 ....
3.4700E-03 1.1907E-05 0.9041 -0.8768 1.6402 26.0113 ....
4.0461E-03 1.4730E-05 0.8982 -0.8008 1.7069 25.9631 ....
4.6819E-03 1.8215E-05 0.8924 -0.7265 1.7703 25.9142 ....
......

M_dep
T_eff, log_g, He

rho_x, tau, theta,
log_pe, log_pg,
log_k

M_dep

T_eff
log_g
He
rho_x
tau
theta
log_pe
log_pg
log_k

Number of depth points
M_dep must be negative if there are no columns with H and He number densities
M_dep must be positive if there are these columns
effective temperature
logarithm of gravity
He abundance (by number)
column mass
optical depth at 5000 A
reciprocal temperature 5040 / T
logarithm of electron pressure
logarithm of gas pressure
scaled logarithm of continuous opacity at 5000 A

The atomic transition list file

The atomic transitions are taken from the VALD database (or from the Kurucz CD). The atomic transition list file must have the following format

4015.000 26.00 -0.610   1.557 3.0   4.652 2.0 1.09 0.69 1.48 8.009 -6.213 -7.620    a3F       y3F B+    MFW       3   3
4025.000 26.00 -1.252   2.223 1.0   5.314 2.0 2.50 1.82 1.48 7.572 -6.220 -7.819    a5P       x5P 0.037 BWL       3   3
4035.000 26.00 -0.587   3.047 4.0   6.134 3.0 1.00 1.00 99.00 0.000 0.000 0.000    a1G   Fsp3 1F 0.045 BWL       3   3
4045.000 26.00 -0.200   3.573 5.0   6.661 5.0 1.00 1.03 1.01 7.500 -4.535 -7.768 (2H)4s a1H(3G)sp y1H             1   5
4055.000 26.00 -0.729   2.758 3.0   5.840 4.0 0.76 0.88 1.07 7.470 -6.262 -7.755    a3G       z3H 0.029 BWL       3   3
4065.000 26.01 -2.439   4.495 2.5   7.575 2.5 1.18 1.01 1.09 8.489 -6.653 -7.943       2|3D4)2D       1|3P4)2D    1   2
4075.000 26.01 -2.572   4.495 2.5   7.568 2.5 1.18 0.80 0.99 8.576 -6.664 -7.943       2|3D4)2D       1|3H4)4G    1   2
....
5510.003 28.00 -0.900   3.847 3.0   6.097 4.0 1.05 1.05 1.05 8.215 -5.230 -7.810 2D)4p z1F (2D)4d e3G 0.025 WLa   5   5
....

Alam0 Isym Algf Chi_low J_low Chi_up J_up g_low g_up g_eff Rad Alc4 Alc6 Dummy_string

  Alam0  

                  Isym  

                  Algf  

                  Chi_low  

                  J_low  

                  Chi_up  

                  J_up  

                  g_low  

                  g_up  

                  g_eff  

                  Rad  

                  Alc4  

                  Alc6  

                  Dummy_string

 
                wavelength  

                  element symbol  

                  oscillator strength log_gf  

                  excitation potential of lower level  

                  J value of lower level  

                  excitation potential of upper level  

                  J value of upper level  

                  Lande factor of lower
                level          
                (99.00 means unknown) 

                  Lande factor of upper
                level          
                (99.00 means unknown) 

                  "effective" Lande
                factor        
                     (99.00 means unknown) 

                  radiation damping constant   
                        (0.000
                  means unknown) 

                  constant for Stark effect   
                         (0.000 means
                  unknown) 

                  constant for van der Waals broadening (0.000
                  means unknown) 

                  extra information on transition 

              

Line selection file

It is recommended to use part of the output contained in sysom_line.[10-digit-extension] for line selection, e.g. (first 3 lines), but any list containing at least the wavelengths of the lines to be synthesised will do it (last line).

4015.000 Fe 1 10.000 -0.610 1.557 3.0 2.0 1.09 0.69 1.49   1.021 14.801 30.563 1.593E+05
4025.000 Fe 1 10.000 -1.252 2.223 1.0 2.0 2.50 1.82 1.48   0.373 14.811 31.060 1.053E+04
4035.000 Fe 1 10.000 -0.587 3.047 4.0 3.0 1.00 1.00 1.00   1.357   0.000 30.268 1.064E+04
....
5510.003 28.00 -0.900   3.847 3.0   6.097 4.0 1.05 1.05 1.05 8.215 -5.230 -7.810 2D)4p z1F (2D)4d e3G 0.025 WLa   5   5

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