  Context. Solar active regions are known to have jets. These jets are
associated with heating and the release of particles into the solar wind.
  Aim. Our aim is to understand the spatial distribution of coronal jets within
active regions to understand if there is a preferential location for them to
occur.
  Methods. We analysed five active regions using Solar Dynamics Observatory
Atmospheric Imaging Assembly data over a period of 2-3.5 days when the active
regions were close to disk centre. Each active region had a different age,
magnetic field strength, and topology. We developed a methodology for
determining the position and length of the jets.
  Results. Jets are observed more frequently at the edges of the active regions
and are more densely located around a strong leading sunspot. The number of
coronal jets for our active regions is dependent on the age of the active
region. The older active regions produce more jets than younger ones. Jets were
observed dominantly at the edges of the active regions, and not as frequently
in the centre. The number of jets is independent of the average unsigned
magnetic field and total flux density in the whole active region. The jets are
located around the edges of the strong leading sunspot.
