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\paperID{P10-1}
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\title{New Simulation Software for VLBI Observations}
\titlemark{Simulation Software for VLBI Observations}

\author{I.\ Guirin, S.\ Likhachev, and A.\ Chuprikov}

\affil{Astro Space Center of P.\ N.\ Lebedev Physical Institute of
Russian Academy of Sciences,Profsoyuznaya 84/32, 117997,
Moscow, Russia, Email: achupr@asc.rssi.ru}

\contact{Andrey Chuprikov}
\email{achupr@asc.rssi.ru}

\paindex{Guirin, I.}
\aindex{Likhachev, S.}
\aindex{Chuprikov, A.}

\authormark{Guirin, Likhachev, \& Chuprikov}

\keywords{radio astronomy: VLBI data simulation}

\begin{abstract}          % Leave intact
This is a report on simulation software for VLBI observations. The software
is part of the {\tt ASL for Windows} project. It implements a new class of
mathematical algorithms that allow a user to completely simulate any VLBI
observation on the MS Windows platform. In particular, these are simulations
of the interferometer structure, simulations of a radio source structure, and
simulations of the noises. The possibility to introduce any new radio telescopes
including space radio telescopes is also explored and presented in this software.
The software is extremely user friendly.
\end{abstract}


\section{Introduction}

Investigation of astronomical radio sources with VLBI method often requires to create
the simulated VLBI-data. At least three problems could be solved with VLBI-data simulator:
\begin{enumerate}
\item The creation of schedule for any future VLBI observation
\item The evaluation of results of future VLBI observation in advance
\item The evaluation of Space VLBI data processing results.
\end{enumerate}

\noindent %% FO
Thus, it is necessary to create some algorithms of VLBI data synthesis. The initial data of
these algorithms are the geocentrical coordinates of antennae, and also {\tt Right Ascension} and
{\tt Declination} of sources observed. If the source structure is known in advance, it is not a
problem to estimate the values of visibility function for any time, any frequency, and any
baseline. The main principle of such calculation is that any interferometer is, in fact, a
3-dimensional Fourier transformer.

Hence, the {\tt Astro Space Locator} (Chuprikov\ 2002) VLBI-data simulator consists of 3 parts:
\begin{enumerate}
\item The simulation of (u, v)-plane (VLBI Configuration Modeling)
\item The simulation of structure of the source to be observed (Source Modeling)
\item The simulation of visibility amplitude and phase noises (Error Modeling).
\end{enumerate}


\section{The simulation of the (u, v)-plane}

As mentioned above, we use some a priori data to simulate the baseline motion. The VSOP
continuum source list (Fomalont et al.\ 2000) has been included into our simulator.
Moreover, the user could simply insert the source coordinates manually if necessary.

We use the extended NRAO list of antennae with their coordinates, effective area values
and noise parameters. The user could insert any new ground as well as new space antenna
into this listing manually if necessary. List of antennae contains
data for 126 scopes for today.

There is a possibiltty to install manually any {\tt time structure} and {\tt frequency structure},
and any {\tt polarization type} of data simulated. The current version of {\tt ASL Simulator}
is able to synthesize the VLBI data for any of 12 radio astronomical frequency ranges
({\tt 3 mm, 7 mm, 1.35 cm, 2 cm, 2.4 cm, 4 cm, 6 cm, 13 cm, 18 cm, 21 cm, 50 cm, 92 cm}), and
for any of 12 polarizations ({\tt RR, RL, LL, LR, XX, XY, YY, YX, I, Q, U, V})

%                                                One column figure
%----------------------------------------------------------- S_vib
\begin{figure}
\vspace{180pt}
\special{psfile=P10-1fig1.eps hscale=58 vscale=58 angle = 270 hoffset=-80 voffset=270}
 \caption{Model of Source (left) and model of (u, v)-plane coverage (right).}
     \label{P10.1-fig-1}
\end{figure}
%__________________________________________________________________
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\section{The simulation of the astronomical radio source}

The radio structure of source simulated is determined by user. The user has to choose
the number of components and properties for each of them. These properties are :
the {\tt Flux Density} value (in {\tt Jy}), the {\tt Large Axis} value (in {\tt Arcsecond}),
the {\tt Axes ratio} value, the component {\tt Inclination} value (in {\tt Degrees}).
Location of component in the image plan depends on the {\tt Position Angle} (in {\tt Degrees}),
and the {\tt Distance} from the centrum (in {\tt Arcsecond}).
Another important parameter is a type of component.
There are the following component types :

\begin{enumerate}
\item Gaussian
\item Disk
\item Thin Ring
\item Thin Sphere
\item Rectangle
\end{enumerate}

\noindent %% FO
We use the stadard Fourier transformation equations to make all necessary
estimations for each type pointed above. The source structure could be directly laid on the :

\begin{enumerate}
\item (u, v)-plane has already been simulated (see {\tt paragraph 2})
\item (u, v)-plane has been read from {\tt any available UVX-file}
\end{enumerate}

The transformation between {\tt FITS} and {\tt UVX} format is very quick and easy.
Thus, our software allows the user to lay any created source structure on any real
(u, v)-plane. The comparison of real visibility with synthesized one should be very useful.

\section{The simulation of the noise}

The user has to install :

\begin{enumerate}
\item the {\tt Input UVX-file} containing the visibility has already been simulated
\item the {\tt Output UVX-file} will contain the same visibility with noises
\item the level of {\tt Phase Noises} in {\tt Degrees} for each antenna
\item the level of {\tt Amplitude Noises} in {\tt dB} for each antenna
\end{enumerate}

\noindent %% FO
This simulation allows to evaluate the influence of noise and to develop some  methods to decrease it. 

\section{An example of VLBI data simulation}

%                                                One column figure
%----------------------------------------------------------- S_vib
\begin{figure}
\vspace{180pt}
\special{psfile=P10-1fig2.eps hscale=57 vscale=57 angle = 270 hoffset=-90 voffset=276}
\caption{The visibility simulated amplitude (left) and phase (right).}
\label{P10.1-fig-2}
\end{figure}
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%                                                One column figure
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\begin{figure}
  \vspace{180pt}
 \special{psfile=P10-1fig3.eps hscale=53 vscale=53 angle = 0 hoffset=-40 voffset=-131}
   \caption{The reconstructed source image {\tt (CLEAN MAP)}.}
   \label{P10.1-fig-3}
\end{figure}
%__________________________________________________________________
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Figure~\ref{P10.1-fig-1} shows the simulated radio source consisting of two Gaussian
functions. This is a good model for the "core-jet" source. The (u, v)-plane for the
{\tt "Radioastron"} Space VLBI observation is shown in the right picture. We supposed to
use 5 VLBA antennae (HN, MK, OV, PT, SC) in this experiment.
Wavelength range is 1.35 cm.
Source is close to the perpendicular to the current orbit plane direction. Coordinates
of source are :

Right Ascension  10 h 37 m 06 s

Declination  +85:12:46

The orbit has high apogee (approximately 360000 km). Perigee is about 19000 km, and the orbit
period is about 11 days.

VLBI observation is between 3-d and 8-th day after perigee and the Integration Time value is
supposed to be equal to 1 hour.


Figure~\ref{P10.1-fig-2} shows the simulated amplitude and phase of visibility.
Figure~\ref{P10.1-fig-3} shows the reconstructed image of source simulated.

\section{Conclusions}

The VLBI-data simulator presented above is a part of the software titled 
{\tt Astro Space Locator (ASL for Windows)}. Our main goal is to give another
possibility for any VLBI-data processing to astronomers who prefer to deal with
PC-computers. The ASL software is free and could be easily installed. 
It is availabe in the Internet
(see {\tt http://platon.asc.rssi.ru/DPD/ASL/asl.html}).

Development of the {\tt Astro Space Locator} software is continuing.

\acknowledgments
We are grateful to Dr. Edward B. Fomalont (National Radio Astronomy Observatory, USA)
for valuable comments and discussion


\begin{references}
\reference Chuprikov, A.\ A., In: Ros, E.\, Porcas, R.\ W., Lobanov, A.\ P.,
\& Zensus, J.\ A. (Eds.), Proceedings of the 6th European VLBI Network Symposium,
Bonn, Germany, June 25-28, 2002, 27.
\reference Fomalont, E.\ B., Frey, S.\, Paragi, Z.\, Gurvitz, L.\ I.,
    Scott, W.\ K., Taylor, A.\ R., Edwards, P.\ G., \&
    Hirabayashi, H.\  2000, \apjs, 131, 95
\end{references}

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