  This paper continues our study of radio pulsar emission-beam configurations
with the primary intent of extending study to the lowest possible frequencies.
Here we focus on a group of 133 more recently discovered pulsars, most of which
were included in the (100-200 MHz) LOFAR High Band Survey, observed with
Arecibo at 1.4 GHz and 327 MHz, and some observed at decameter wavelengths. Our
analysis framework is the core/double-cone beam model, and we took opportunity
to apply it as widely as possible, both conceptually and quantitatively, while
highlighting situations where modeling is difficult, or where its premises may
be violated. In the great majority of pulsars, beam forms consistent with the
core/double-cone model were identified. Moreover, we found that each pulsar's
beam structure remained largely constant over the frequency range available;
where profile variations were observed, they were attributable to different
component spectra and in some instances to varying conal beam sizes. As an
Arecibo population, many or most of the objects tend to fall in the Galactic
anticenter region and/or at high Galactic latitudes, so overall it includes a
number of nearer, older pulsars. We found a number of interesting or unusual
characteristics in some of the pulsars that would benefit from additional
study. The scattering levels encountered for this group are low to moderate,
apart from a few pulsars lying in directions more toward the inner Galaxy.
