  The beamed emission by relativistic sources moving along the magnetic dipolar
field lines occur in the direction of tangents to the field lines. To receive
such a beamed radiation line-of-sight must align with the tangent within the
beaming angle 1/gamma, where gamma is the particle Lorentz factor. By solving
the viewing geometry, in an inclined and rotating dipole magnetic field, we
show that at any given pulse phase observer can receive the radiation only from
the specific altitudes. We find the outer conal emission is received from the
higher altitudes than the inner conal components including the core. At any
pulse phase, low frequency emission comes from the higher altitudes than the
high frequency emission. As an application of our model, we have applied it to
explain the emission heights of conal components in PSR B0329+54.
