  Superhumps are among the abundant variable phenomena observed in the light
curves of cataclysmic variables (CVs). They come in two flavours as positive
and negative superhumps, distinguished by periods slightly longer or shorter,
respectively, than the orbital periods of these interacting binary systems.
Positive superhumps are ubiquitous in superoutbursting short period dwarf novae
of the SU~UMa type but are less common in longer period systems with accretion
disks in a permanent bright state such as novalike variables and most old
novae. Negative superhumps do not seem not to have a preference for a
particular type of CV. Here, I take advantage of the long high cadence light
curves provided by TESS for huge number of stars, selecting all old novae and
novalike variables with past reported superhumps for which TESS light curves
are available and have not yet been analysed in previous publications in order
to study their superhump behaviour. In combination with information taken from
the literature the results enable to compile the most complete census of
superhumps in these stars so far. As a corollary, for the eclipsing systems in
the present sample of objects eclipse epochs derived from the TESS light curves
and in some cases from archival light curves are listed and used to update
orbital ephemeris and to discuss period changes.
