Below, we derive the generalized 2D Fourier transform relation between the visibility and the source brightness distribution in the () system. The geometery for this derivation is shown in Fig 10.3.

Let the vector represent the direction of the phase center
and the vector
represent the location of all antennas
of an array with respect to a reference antenna. Then
. Note that
is phase by which the visibility should be rotated to stop the
fringe. For any source in direction
,
the output of an interferometer after fringe stopping will be

(10.2.8) |

If the array is such that all antennas are exactly located in the
() plane, is exactly zero and the above equation reduces to
an exact 2D Fourier transform relation between the source brightness
distribution and the visibility. This is true for a perfect east-west
array (like WSRT or ATCA). However to maximize the -coverage
arrays like GMRT or VLA are not perfectly east-west. As mentioned
earlier, the integrals in the above equation are finite for a small
portion of the sky (being limited by the primary beam patter of the
antennas). If the field of view being mapped is small (ie. for small
and )
and
can be neglected. Eq. 14.1.1 becomes

Since there are finite number of antennas in an aperture synthesis
array, the -coverage is not continuous. Let

(10.2.11) |

(10.2.12) |

Inverting the above equation and using the convolution theorem, we get
where is the Fourier transform of . is the
transfer function of the the telescope for imaging and is referred to
as the *Dirty Beam*. represents the raw image produced by
an earth rotation aperture synthesis telescope and is referred to as
the *Dirty Map*. Contribution of *Dirty Beam* to the map and
methods of removing these these effects will be discussed in greater
detail in later lectures.

In all the above discussion, we have assumed the observations are monochromatic with negligible frequency bandwidth and that the () measurements are instantaneous measurements. None of these assumptions are true in real life. Observations for continuum mapping are made with as large a frequency bandwidth as possible (to maximize the sensitivity) and the data is recorded after finite integration. Both result into degradation in the map plane and these effects will be discussed in the later chapters.

Neglecting the -term essentially implies that the source brightness distribution is approximated to be restricted to the tangent plane at the phase center in the sky rather than on the surface of the celestial sphere. At low frequencies, where the antenna primary beams are larger and the radio emission from sources is also on a larger scale, this assumption restricts the mappable part of the sky to a fraction of the primary beam. Methods to relax this assumption will also be discussed in a later lecture.