8.1 Input Files

The program LINE1 expects the following input files (only those which are marked with “^*” are necessary):

ABUNDi
It is possible to read occupation numbers for newly implemented levels from already existing models ( MODINi). i (from ABUNDi) is a number from 1 to 9. If the elemental abundances of the input model ( MODIN) and of the models MODINi differ, scaling factor can be given in the files ABUNDi which are applied to the occupation numbers of the models MODINi, respectively.
Example:
C2
N1.3

ADJUST
In practice NLTE model atmosphere calculations have shown that is is not possible in all cases to consider all line transitions simultaneously from the beginning. One method to overcome this problem is to reduce the oscillator strengths at the beginning with reduction factors which increase to unity in the course of the iteration.

The input file ADJUST contains the reduction factors and the factors with which the reduction factors are increased every iteration until the original oscillator strengths are reached.
Example:

C4    C4    1.0E-5 1
C422SC422P 0.01 1.05
C452SC452P 1.0E+5 1.0E+00

means:
the oscillator strengths of all C IV line transitions are reduced by a factor of 10^-5. This factor is constant over the whole calculation. Additionally, the C IV 2s-2p line is individually reduced by the factor of 0.01 ( total of 10^-7) but this factor (0.01) is increased by 5% every iteration. The C IV 5s-5p line is considered with its correct oscillator strength (10^{-5 .} 10⁺⁵ = 1). In the case that the temperature correction yields negative temperatures, the oscillator strengths are kept at their last value.

ATOMS^*
atomic data file (Sect. 2), like for the start model or extended ...

DATEN
input and output options (Sect. 5.4, 5.5, and 8.3)
this files has to be copied to stdin because LINE1 reads the options from there (e.g. /home/rauch/bimod/line1 < DATEN).

DISTA
The frequency grid for the detailed calculation of line profiles is created by LINE1 itself. The discretization of the frequency points within the line transitions can be split in intervals with different distances from point to point in order to represent the line centers or possible forbidden components (e.g. He I 4471Å) with a sufficient number of (narrowly spaced) frequency points. DISTA contains informations how many points at which distance ( in Å) shall symmetrically (to the line center) be inserted in these intervals.

Example:

5 0.1
10 0.3
15 0.5

results in points at ( in Å, only the “red” wing given):
0.0, 0.1, 0.2, 0.3, 0.4, 0.7, 1.0, 1.3, 1.6, 1.9, 2.4, 2.9, 3.4, 3.9, 4.4

In case on many lines and a high resolution, the parameter NRBBMAD (Sect. 1) may become very high. Due to compiler limitations in the size of arrays, no executable may be created then. To avoid this, the use of a respective F_BASE file (Sect. 3) and an adjusted DISTA is recommended.

Example:

F_BASE creates an equidistant frequency grid from 3000 Å to 7000 Å ( = 0.1 Å), then a DISTA

2 0.01
4 0.02
6 0.03
8 0.05
9 100.00
10 0.01

is sufficient (narrow points only until the F_BASE resolution is reached, then just an end point of the line and a CONT/(BLUE/RED) point (Sect. 3). In addition, a dynamical use of DISTA in LINE1_PROF is helpful and is described in Sect. 9.

FGRID^*
frequency grid (Sect. 3), not necessary in the case of line profile calculations (see above)

ION
contains the code for the selected ion (line profile calculations). It differs from theTMAP code (Sect. 2.1): the element is given in CHARACTER*2 format (flushed to the left) and the ionization stage is indicated in the third (and fourth) column.
Examples:
HE2
C2
CA10

SETF2 creates this file for a given atomic-data file (Sect. 3).

LINIEN this file contains information about the range which has to be considered in the calculation of the line profiles and the selected line to calculate:

BLENDRANGE40.0*
This card is of special importance and has to be the first record in LINIEN.
• LINE1 searches in the interval for line frequency points (Sect. 3) of other line transitions. All line transitions with points between CONT RED and CONT BLUE of the selected line (see below), are regarded as a blend and included in the calculation in detail. All other line transitions in the input file ATOMS (see above) are disregarded in the creation of the internal atomic data and frequency grid files by LINE1. This minimizes both, core memory and computational time requirements.
• LINE1 considers in the creation of the internal atomic data and frequency grid files only those radiative bound-free (RBF) transitions with an ionization energy smaller than c/(_o - _Blendrange) because RBF transitions with a higher ionization energy do not contribute to the opacity within the blendrange. This minimizes also the core memory and computational time requirements.

XXXXXXXXXXYYYYYYYYYY
TMAP code (Sect. 2.1) of selected lines for which theoretical line profiles shall be calculated

SETF2 creates this file for a given atomic-data file (Sect. 3).

MODIN*
start model (Sect. 4)

MODINi
see ABUNDI

OP_RBF_XXXX
bound-free cross-sections from the Opacity Project for levels of the ion XXXX

STARK_H1
VCS stark broadening tables for H I (Lemke M., 1997, A&AS 122, 285)

STARK_HE1
BCS and Griem tables for He I (Barnard A.J., Cooper J., Shamey L.J., 1969, A&A 1, 28; Griem H.R., 1974 Spectral line broadening by plasmas)

STARK_HE2
VCS tables for He II (Schöning T., Butler K., 1989, A&AS, 78, 51, Schöning T., Butler K., 1989, A&AS, 79, 153)

STARK_C4
tables for C IV (Schöning T., 1993, A&A, 267, 300 )

STARK_N5
tables for N V (Schöning T., 1995, A&AS, 113, 579 )

STARK_HEI
tables for He I (Dimitrijévic et al.)

STARK_CIV
tables for C IV (Dimitrijévic et al.)

STARK_CV
tables for C V (Dimitrijévic et al.)

STARK_NV
tables for N V (Dimitrijévic et al.)

STARK_OIV
tables for O IV (Dimitrijévic et al.)

STARK_OV
tables for O V (Dimitrijévic et al.)

STARK_OVI
tables for O VI (Dimitrijévic et al.)

STARK_SIIV
tables for Si IV (Dimitrijévic et al.)

STARK_SVI
tables for S VI (Dimitrijévic et al.)

Note: For H I, He I, He II, C IV (STARK_C4), and N V STARK_N5 the tables have only to be loaded. LINE1 uses these data files if they are available. For the other ions an option has to be given (see below) in DATEN to use the broadening tables for all lines of the ion, or for selected line transitions by requesting formula 5 (keyword RBB) in ATOMS (Sect. 2).