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.
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.
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.
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:
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.
Figure 5: message box
In the message box the program will display various comments or errors during the computation.
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.
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.
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.
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.
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.
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.
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.
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:
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.
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:
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.
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.
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.
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.
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.
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.
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.
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.
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