Russian 

About ASC
ASC Projects:
RadioAstron
Millimetron
Suffa (Uzbekistan)

ASC Divisions:
Moscow Branch
PRAO (Pushchino)
 
ASL for Windows

The software project Astro Space Locator для Windows 9x/NT/2000 is developed by the Laboratory for Mathematical Methods of the ASC to provide a free software package for VLBI data processing. We used the Microsoft Windows 2000 and MS Visual C++ 6.0 on IBM compatible PCs as the platform from which to make data processing and reconstruction of VLBI images. We believe this will make our software more easily available to a large number of astronomers who have access to PCs and notebooks. Our experience tells us that even though MS-Windows is considerably easy to use, it is not sufficiently robust, and it lacks some essential features for a more flexible implementation of computation-intensive algorithms.
The document (Russian) collection consists of user guides, on-line help files, etc., made available by the software developers.
Click here to get ASL documentation (zipped MS Word, PostScript and on-line files) written both in Russian and in English.
The ASL for Windows consists of four integrated parts. The parts are the following:
The ASL Editor is a part of the ASL for Windows software project intended for VLBI data editing and visualization.
With the ASL_Editor, you can:
  • view the observation data written in FITS format and its parameters;
  • edit the data (both time and spatial editing);
  • get statistical and other parameters of the data;
  • prepare the data for VLBI image synthesis.
  • ASL Editor includes FITS_UVX Viewer/Converter to view an input FITS file and then to convert it into UVX format (internal ASL format) for further processing.
  • ASL Editor also has a FITS Writer to convert a UVX file back into FITS file.
    Just GET IT and try it!
  • The ASL Fringe Fitting The ASL Fringe Fitting is a part of the ASL for Windows software project. The ASL Fringe Fitting procedure is the first stage of the data phase calibration.
    With the ASL Fringe Fitting you can:
  • fix phase errors on the correlator output;
  • compensate for baseline-movement.
    The procedure consists of the following steps:
  • deviding the observation time interval for each baseline into a few equal parts (solution intervals).
  • executing the "Fringe Search" procedure to find the initial approximation for four parameters (amplitude, delay,fringe rate, initial phase) for each solution interval.
  • correcting the data phase by means of non-linear Least Mean Square Method for each solution interval;
  • storing each corrected visibility function into an output UVX file.
    There are two possible options in the ASL Fringe Fitting possible:
  • single-band Fringe Fitting (separate for each Intermediate Frequency (IF) );
  • multi-band Fringe Fitting (for all available IF is).
    Just GET IT and try it!
  • The ASL Imager (Beta 2.0) is a part of the ASL for Windows software project intended for VLBI images synthises and its visualization.
    With the ASL_Imager, you can:
  • synthesise various kinds of the VLBI maps;
  • analyze the obtained images;
  • deconvolve images by means of CLEAN, Hybrid Mapping, and other deconvolution procedures;
    ASL Imager includes many various graphic features that allow you to obtain the best results in shortest time interval.
    Just GET IT and try it!
  • ASL Simulator is a part of the ASL for Windows software project intended for VLBI observation simulation. The software still under construction.
     
     
    ASL editor (часть 1)
    ASL editor (часть 2)
    ASL editor (часть 3)
    ASL самокалибровка (часть 1)
    ASL самокалибровка (часть 2)
    ASL редактор палитры
    Многочастотная
    обработка изображений
    UVX-формат
     
     
     
    Отчет о результатах обработки интерферометрических наблюдений на базе “Пущино - Радиоастрон” на волне 1.35 см
     
     
    РСДБ-наблюдения на однобазовом интерферометре “Пущино - Калязин”
     
     
    4-station ground based VLBI pre-launch test of "Radioastron" recording mode
     
     
    Comparision Ariadna and Caicif2 delay modeles