11 Auxiliaries

Three plot programs, PROF1, and PLXY, are available on the computers at Tübingen. They are designed for the visualization of plot data files from the Tübingen NLTE Model-Atmosphere Package (TMAP). The program PLXY is able to plot any x-y table. The additional program WRPLOT is a plot program which is not exclusively based on the Tübingen NLTE Model-Atmosphere Package (TMAP). The two auxiliary programs RTFZ and PLADD are designed to interactively rectify and co-add spectra.

The programs are to be used interactively and allow an individual design of the plot. Interactive labeling etc. is possible. All interactively inserted label can be saved in files program.AUX and can be re-loaded if the program is invoked again later.

The plot files are created in PostScript format, EPSF is optional for a later inclusion in LATEX documents. The plot programs support color — PROF1 uses the “pen” number as follows:

1 black
2 red
3 blue
4 green
5 yellow
6 cyan
7 magenta

A more detailed description follows in the next sections.

At Tübingen, the programs are found at
/home/rauch/tools/pladd
/home/rauch/tools/plxy
/home/rauch/tools/prof1
/home/rauch/tools/rtfz

All programs are self-explaining ...

In the following sections some general comment on the programs are summarized. For details, especially for one-purpose derivates of the programs, please contact the authors.

11.1 PLADD

The program PLADD may be used to interactively co-add spectra with individual weights. Parts of the spectra which are obviously corrupted, e.g. by cosmics, can be eliminated. The program expects input spectra data file with the convention ¡name¿.ii, where ii is a two digit integer (default is 01). In the case of echelle spectra, ii is the order number:

Example file names to be co-added:

With PLADD, normalized as well as absolute flux spectra can be co-added. The absolute fluxes can be pre-normalized (with a constant value) for the processing. A Savitzky-Golay filter Savitzky & Golay (1964) may be invoked to clarify in case of heavy over-sampling.

11.2 PROF1

For the direct evaluation and visualization of line profile plot data files which are created by LINE1, or are available in WRPLOT format, the program PROF1 is available.

PROF1 can plot the data as well as process them in order to compare them to observations etc. A small “help” menu is available which can be invoked from the PROF1 main menu. Several submenus can be accessed from this main menu (input “L” at the right row ...). It is worthwhile to note that there is a plot box menu which can be accessed from the first row of the main menu.

For all further questions and assistance the authors are available via email.

In the following, the format of the line profile and spectra files is briefly summarized:

11.2.1 Line Profile Data Files

The line profile data files consist out of a LINE1 header and any number of plot data sets. The header has the following structure:

A5 program code of the line profile calculation, e,g. LINE1
A8 date of the line profile calculation
A8 time the line profile calculation
A5 program code of the model atmosphere calculation , e,g. PRO2
A8 date of the model atmosphere calculation
A8 time of the model atmosphere calculation
I5 number of the following plot data sets

Every plot data set is devided in three parts, i.e. a header, the plot data, and information about blends and the line broadening theories used for the calculation of the theoretical line profiles.

The header has the following format:

A80           comment (free)
A80           comment (free)
A80           comment (free)
A27,F11.3,A42 both strings (free) number field: central wavelength in Å         
A80           title
A80           abscissa label
A80           ordinate label
I5            number of following values in the data set

The central wavelength in the marked field is of special importance because PROF1 uses this value as origin of an internal coordinate system. The data of the line profiles is given relative to the line center. All following program steps refer to this wavelength.

It follows the number of x-y pairs as announced in the header. There is no special format necessary but the first four columns have to be blank.

At the end of every data set an information segment follows which is used by PROF1 to find the position of blends in the calculated line profile and to get informations about the line broadening theories which were used to calculate the line profiles. This segment has the following form:

I3         total number of lines (incl. blends) in this data set
A20,2F13.3 type of lines in TMAP Code (Sect. 2.1),
           distance (Å) relative to the central wavelength (see above),
           central depression of the line
...
I3         total number of lines
A20,A10    line broadening theory used to calculate the line (e.g. VCS 88)
..
.

11.2.2 Spectra

The basic format of all spectra files which are accepted by PROF1 is:

A20   name of spectrum
I6    number of x-y pairs
6X,*  x-y pairs
..
.

The number of x-y pairs is currently limited to 18 000.

11.2.3 PROF1 Auxiliary Files

The program PROF1 can create a variety of auxiliary files. These files are explained in the following. They can be recognized by their extension.

 .AEQ
This file is created if equivalent widths are measured with PROF1. It contains information about the measured interval, theoretical, and observed equivalent width (measure from the spectrum).

 .AUX
This file is created if labels are interactively inserted and saved! It can be easily edited and used for a following PROF1 session.

 .CMD
While a PROF1 session is active, all commands are recorded and can be saved at the end of the session. Thus, a batch job is created which can be run as a procedure and creates automatically plot files. If different plot data files are copied to the same path subsequently, this procedure can create “standard” plots of different plot files.

 .DAT_REN
This file is created if a spectrum is normalized by PROF1 and saved (basic format, see above).

 .LOAD
In this file all spectra a listed which shall be automatically loaded by PROF1 at the beginning of the session. It can be created from the “spectra menu” of PROF1.

 .MRK
In this file the base points for the rectification of spectra with natural splines can be saved.

 .REN
This file contains information about the normalization of a spectrum. Sometimes it appears necessary to correct the position of the local continuum. The following session can refer to this file, and thus, uses the same base points for normalization.

 .REN_DAT
This file contains a re-normalized spectrum.

 .SET
In the file information (defaults) about the size of the plot box etc. are saved. It is read by PROF1 at the beginning of the session.

11.3 PLXY

The program PLXY is an universal plot program for VMS and UNIX. The UNIX version is based on the PGPLOT graphics subroutine library which is provided by the California Institute of Technology (in the www, a documentation about this library is found under http://astro.caltech.edu/~tjp/pgplot/#documentation). It expects in the plot data file only a x-y table. Optional, commands can be given either by keywords (see below) in the plot data file or interactively.

11.3.1 Keywords for Commands in Plot Data Files

The program PLXY accepts some commands given in the plot data file which can be inserted at every position but flushed to the left. Valid are the last commands given before the end of a data set. Strings, e.g. for a comment, start directly after the “:” — without any “ |~| ”.



Table 2: Selection of plot symbols available for the use in PLXY


#symbol


840o
841[]
842 /_\
843 <>
844*
845+
846×
847*



11.3.2 Output devices

Three output devices can be requested:

11.4 RTFZ

RTFZ may be used to normalized spectra individually. RTFZ expects a xy table with the original spectrum. Continuum points can be set manually and a cubic spline fit will be performed for selected parts of the spectrum. In order to achieve more clarity, it is possible to smooth the spectra during the rectifying process by a Savitzky-Golay filter.

11.5 TEUV

The Tübingen EUV Absorption (TEUV ) tool was created to apply interstellar absorption to theoretical stellar spectra in the wavelength range c < 911 Å, where bound-free absorption by interstellar elements has a string influence on observed fluxes. This has to be considered when these observations are modeled. The hot and cool components of the interstellar medium are represented in the TEUV tool.

The program is intuitive to handle and controlled via a web interface ( http://astro.uni-_tuebingen.de/~TEUV) where all parameters of the interstellar components can be entered and the input model-flux table can be uploaded. For further assistance, the mouse can be hovered over the blue labels.

The following fields have to be selected or filled in:

After “Upload and Submit”, the theoretical model is corrected according to the given parameters. Additionally, models with a ten times larger and smaller H i and He i column densities are created. To be able to display these models, the maximum number of output wavelength points is reduced. It may take some seconds until these corrections are applied. Then, the uploaded model, observation, and corrected model are displayed. For an easier adjustment of the parameters, the user can choose to display the models with varied H i and/or He i column densities.

If the user wants to download the resulting model, the “Download your ISM_choice” button can be used. This triggers the calculation of the corrected model without normalization, for all entered wavelength points with the instrumental resolution applied. If the TEUV tool is used to determine results that are published later, the quote to cite in the acknowledgement is given at the website. The user can store the resulting file via the “Get your results file” button.

11.6 WRPLOT

WRPLOT is a program by Wolf-Rainer Hamann et al. which can be used to manipulate and visualize data. A manual for the use of this program is available at http://astro.uni-_tuebingen.de/~TMAP