All our observations were short direct exposures with CCD's. At
Lick Observatory we used a TI 500×500 chip
and a GEC 575×385, on the 1-m Nickel reflector. The only
filter available at Lick was red. At CTIO we used a GEC 575×385, with
B, V, and R filters, and an RCA 512×320, with #math163#U, B, V, R, and I
filters, on the 1.5-m reflector. In the CTIO observations we tried to
concentrate on the shortest practicable wavelengths; but faintness, reddening,
and poor short-wavelength sensitivity often kept us from observing in U or
even in B. All four cameras had scales of the order of 0.4 arcsec/pixel, and
our field sizes were around 3 arcmin.
The CCD images are unfortunately not always suitable, for very poor
clusters or for clusters with large cores. Since the latter are easily
studied by other means, we augmented our own CCD profiles by collecting
from the literature a number of star-count
profiles ([#kin68##1###,#pet76##1###,#har84##1###,#ort85##1###]),
as well as photoelectric profiles ([#kin66##1###]) and
electronographic profiles ([#kro84##1###]).
In a few cases we judged normality by eye estimates on one of the Sky
Surveys.