2. SYSTEMATICS
2.1. Ingredients
The morphological description of extended extragalactic radio sources
conventionally
identifies the following components (precise definitions are taken from
Bridle & Perley (1984)
and Bridle et al. (in preparation)):
Central component This is an unresolved component coinciding to
within the
observational errors with the nucleus of the associated galaxy or
quasar. Most, if
not all, central components appear to be the optically-thick bases of
jets (see
below and Marscher, these proceedings) and the definition is therefore
resolution and frequency-dependent.
Jet A jet is:
- at least 4 times longer than it is wide;
- separable at high resolution from any other extended structure;
- aligned with the nucleus of the parent object where it is closest to it.
The presumption is that a jet traces the path of a collimated flow or
"beam".
Hot-spot Powerful radio sources almost all have bright, compact
regions or
"hot-spots" close to the outer ends of their structures. The apparent
complexity of the
following definition results from an attempt to differentiate between
bright parts of
jets (knots) and features which represent the termination or major
disruption of a jet (hot-spots). A hot-spot must:
- be the brightest feature in the lobe
- have a surface brightness that is more than four times greater
than that of the surrounding emission and
- have a linear FWHM (after deconvolving the synthesized beam) that
is a small fraction (<2%, for example) of the largest diameter of the source.
If a jet is detected then we add the additional condition:
- that the hot-spot must be further from the nucleus than the end of
the jet, which is defined by:
- its disappearance
- an abrupt change of direction (i.e. by at least 30°
within a knot diameter) or
- decollimation by more than a factor of two (as indicated by the widths of
any ridge-like or knot-like features along the putative path of any continuing
flow).
Lobe The definitions of central component, jet and hot-spot refer
to the structure of
highest surface-brightness in a radio source. The remaining emission (if
any) on a
given side of the central component is termed a lobe. Lobes are commonly
divided into bridges and tails:
- Bridge A bridge is a lobe in which more than half of the emission
is between the
end of a jet (or hot-spot, if no jet is detected) and the nucleus of the
associated
galaxy. Synchrotron spectra of bridges show increased curvature towards the
nucleus and it is therefore likely that they are formed from electrons
left behind
at or flowing back from the region in which the jet interacts with the external
medium.
- Tail (or plume). A tail is a lobe whose emission is mostly
further from the nucleus
than the end of a jet or the position of a hot-spot. The synchrotron spectra of
tails show increasing curvature away from the nucleus, unlike those of bridges,
the inference being that they are flowing outwards.