a black box for the determination of stellar astrophysical parameters

 

 

Introduction

The TempLogG TNG program is designed to calculate fundamental astrophysical parameters from observed Strömgren, Geneva and Johnson colors. It is the successor to the templogg program written at the University of Vienna by Nathan Y. Rogers in 1985. Many new calibrations made it necessary to completely rewrite the old Fortran 77 code. All calibrations used in the old program are present in the new version.

 

 

Strömgren

Johnson

Geneva

 

 

 

Strömgren

 

Interactive Input

 

Figure 1: main program window

In the interactive input it is possible to calculate the fundamental parameters for one star. The program has to be provided with the input parameters and a desired calibration. An error estimation is possible if the errors of the input parameters are available.

 

File Bar

 

Figure 2: file bar

Trough the menu point Help - Manual, the manual for the program can be displayed in your web browser. The point About displays the current build version and the contact information to the author. The menu point Quit exits the program.

 

Calibration

 

Figure 3: calibration

The program is able to calculate the fundamental parameters with a set of different calibrations. Therefore it is necessary to select the desired one. The default calibration is selected after the program starts up. A description of the individual calibrations can be found in the respective papers. Templogg OLD stands for the calibration used in the old Templogg  written by Nathan Y. Rogers.

 

ADS Links:

Templogg OLD Moon 1985

uvbybeta Napiwotzki 1995

Balona 1994

Ribas 1997

Castelli 1997

 

Input Parameters

 

Figure 4: input values

The green fields on the tab Interactive Input the are for the input parameters. The dark green fields are required. It is possible to use the spectral type instead of the Hbeta value if no Hbeta is available. But one has always to keep in mind that a wrong spectral type will result in wrong fundamental parameters. The light green fields for the parallax and the vsini are optional and will help to improve the output values. The ash green fields are for the errors of the input values. If no errors are given no error estimation will be done.

The computation is started by clicking the Calculate button.

 

Message Box

 

Figure 5: message box

In the message box the program will display various comments or errors during the computation.

 

Output Parameters

 

Figure 6: output parameters

After the computation is finished the calculated values will be displayed. If the program was provided with input errors then for some values an error estimation for the output values will be given in the light blue fields. One has to keep in mind that the calculated errors are only internal errors due to the errors produced by the detector and not the errors witch are introduced by the different calibrations.

 

File Processing

 

Figure 7: file processing

In the File Processing Mode it is possible to calculate the fundamental parameters for a set of stars from an input file. An example for an input file is shown in the input.csv file located in the program directory. The files have to be *.csv (coma separated values) which can be done for instance in Excel.

 

File Selection

 

Figure 8: file selection

By clicking on the Input File button an input file can be selected. In the dialog only files with the extension csv will be shown for selection. In the Output File field the name and if necessary the path for the output file must be given. The output file has the same format as the input file, no matter what extension is given by the user in the Output File field.

 

Input File

 

Figure 9:input file

Figure 9 shows a typical input file. At least the identifier, the visual magnitude V, (b-y), m1, c1 and Hbeta have to be provided. The other parameters are optional. If an error estimation should be done, the errors of the input values have to be given. If the first character of a line is a # then the line is skipped.

 

Calibration

 

Figure 9: calibration

In the File Processing mode one or more different calibrations can be selected at once. If the input file contains error values for the input parameters then "Error Calculation" can be selected too.

 

Status

 

Figure 10: status

After clicking the Process button the program will calculate a wide rage of astrophysical parameters and store them in the specified output file. The number of the current processed star is displayed and the progress bar shows the overall progress. The message box gives additional information during the processing. The output file will be in coma separated format like the input file.

 

Calibration Settings

 

Figure 11: calibration settings

In the Calibration Settings section it is possible to select additional calibrations. These settings affect both the Interactive Input and the File Processing Mode.

 

Dereddening

 

Figure 12: dereddening

It is possible to select for specific types of stars different dereddening calibrations. This settings affect all the stars in the input file in the specified spectral range. Templogg OLD stands for the calibrations used in the old Templogg  written by Nathan Y. Rogers.

 

ADS Links:

Domingo 1999

Nissen 1989

 

Additional Settings

 

Figure 13: additional settings

For the dereddening it is possible to provide a spectral type for the star which will enhance the dereddening. One has always to keep in mind that a wrong spectral type will result in wrong fundamental parameters.

Further more it is possible to turn off the dereddening. This could be used if the intrinsic colours are known from a different source or if the star is known to have no reddening.

 

Geneva

 

Figure 14: main program window

In the interactive input it is possible to calculate the fundamental parameters for one star. The program has to be provided with the input parameters and a estimation of the metalicity for stars hotter then 7500K. The program allows to determine the physical parameters for
C unreddned B to mid-G stars of the main sequence or just above it.

 

ADS Link:

Kunzli 1996

 

The green fields on the tab Interactive Input the are for the input parameters. The dark green fields are required. The light green fields for the E(B2-V1) is optional and will help to improve the output values.

The computation is started by clicking the Calculate button.

After the computation is finished the calculated values will be displayed. One has to keep in mind that the calculated errors which  are given in the light blue fields are only internal errors due to iterative process in the calculation and not the errors witch are introduced by the calibration.

 

File Processing

 

Figure 15: file processing

In the File Processing Mode it is possible to calculate the fundamental parameters for a set of stars from an input file. An example for an input file is shown in the input.csv file located in the program directory. The files have to be *.csv (coma separated values) which can be done for instance in Excel.

 

File Selection

 

Figure 16: file selection

By clicking on the Input File button an input file can be selected. In the dialog only files with the extension csv will be shown for selection. In the Output File field the name and if necessary the path for the output file must be given. The output file has the same format as the input file, no matter what extension is given by the user in the Output File field.

 

Input File

 

Figure 17:input file

Figure 17 shows a typical input file. At least the identifier, the visual magnitude V, (b-y), m1, c1 and Hbeta have to be provided. The other parameters are optional. If an error estimation should be done, the errors of the input values have to be given. If the first character of a line is a # then the line is skipped.

 

Status

 

Figure 18: status

After clicking the Process button the program will calculate a wide rage of astrophysical parameters and store them in the specified output file. The number of the current processed star is displayed and the progress bar shows the overall progress. The message box gives additional information during the processing. The output file will be in coma separated format like the input file.

 

Johnson

 

Figure 19: main program window

In the interactive input it is possible to calculate the fundamental parameters for one star. The program has to be provided with the input parameters and a estimation of the metalicity for stars hotter then 7500K. The program allows to determine the physical parameters for
C unreddned B to mid-G stars of the main sequence or just above it.

ADS Link:

Bessel 1998 for V-I and V-K calibration

Gray 1992 (Cambridge Astrophysics Series,  The observation and analysis of stellar photospheres, ISBN 0521403200) for B-V calibration

The green fields are for the input parameters. The computation is started by clicking the Calculate button. After the computation is finished the calculated values will be displayed.

 

Outlook

 

The next version will contain extended error calculation and a improved object structure for internal data handling and separate thread for the file processing mode.

 

Known Bugs

 

If the main window is covered by another window in file processing mode and then put back into the foreground, the window is no longer refreshed. After the file processing is finished the window is again being updated.

 

Version History

TempLogG TNG 1.4

Fixed a bug that prevented program to correctly read in negative colors in file processing mode.

TempLogG TNG 1.3

Fixed a bug that calculated the wrong metallicitys for K0-> stars from Strömgren photometry, added a link to the TempLogG homepage, added 2 new parameters for Geneva photometry.

TemplogG TNG 1.2

Added manual information on the Geneva and the Johnson system. Adopted some routines to run properly under Wine (Linux).

TemplogG TNG 1.1

Added calibration for the Geneva system and the Johnson system. CPU-process is now set to below normal class in file processing to avoid the system to freeze while calculating.

TemplogG TNG 1.0

Release Version.(=0.6 Beta)

0.6 Beta

Added the possibility to use comment lines (#), letters in the value-fields in the input file are now deleted, not available output values are now quoted as 'NA' instead of '999', no more 0 distance values, improved exception handling.

0.5 Beta

Added a switch to turn of dereddening, fixed a bug due to an error in the extrapolation routine, added first calibration for Johnson UBV, small GUI redesigns.

0.4 Beta

New grid without overshooting from Castelli included.

0.3 Beta

New tab based look, fixed 9504K bug in uvbybeta calibration. New input parameters: vsini, parallax and spectral type can now be used to improve output. Spectral type is derived according to calculated Teff. 

0.2 Beta

First official beta test version. Error estimation included. New calibrations for metallicity for Enrique Solana included. Object structure redesigned. New Logo. Only one temperature and logg result instead of empirical and grid.

0.1 Beta

First working version.

1 Alpha

First console based enviroment for basic subroutine developement