Basic Interferometry

Basic Interferometry

Interferometry is the practice of using a two-or-more-element radio telescope array to observe astronomical sources. The array itself, along with the electronics used to synthesise the signals detected by the telescopes, are what we call the interferometer.

The Two-Element Interferometer

A two-element interferometer consists of two telescopes seperated by a vector ${\displaystyle \mathbf {b} }$, called the baseline. Both antennas receive electromagnetic radiation from an astronomical source in the sky, which is in the direction of the unit vector ${\displaystyle \mathbf {\hat {s}} }$. Because astronomical sources are far away, the radiation received by the antennas is in the form of plane waves. As the plane waves reach the antennas, one will actually receive the signal first and the second will not receive the signal until a certain amount of time has passed. The time that needs to pass is called the geometric delay, and is denoted by the variable ${\displaystyle \tau }$.

In order to find the value of ${\displaystyle \tau }$, we need to know the extra distance that the plane waves had to travel to reach the second telescope. This distance equal to the baseline vector ${\displaystyle \mathbf {b} }$ dotted with the unit vector ${\displaystyle \mathbf {\hat {s}} }$:

{\displaystyle {\begin{aligned}\mathbf {b} \cdot \mathbf {\hat {s}} \ .\end{aligned}}\,\!}

Since ${\displaystyle \mathbf {\hat {s}} }$ is a unit vector, this distance is actually the projection of the baseline vector, ${\displaystyle \mathbf {b} }$ onto the vector ${\displaystyle \mathbf {\hat {s}} }$ and is given by:

${\displaystyle \mathbf {b} \cdot \mathbf {\hat {s}} =\mid \mathbf {b} \mid \cos \theta ,\,\!}$

where ${\displaystyle \theta }$ is the angle between the baseline and direction vectors.

Knowing the distance, we just divide by the velocity of the plane waves, which is the speed of light, c:

$\displaystyle \tau ={\frac {\mathbf {b} \cdot \mathbf {\hat {s}} }{\emph {c}}}\ .\,\!$