  Context. Pulsars have a very stable rotation. However, sudden increases in
their rotation frequency known as glitches, perturb their evolution. While
large glitches are commonly detected, small glitches are harder to detect
because of the lack of daily-cadence observations over long periods of time.
  Aims. We aim to explore the timing behaviour of young pulsars at daily
timescales looking for small glitches and other irregularities. This will
further our comprehension of the distribution of glitch sizes, which has also
consequences for the theoretical modeling of the glitch mechanism.
  Methods. We observed six pulsars with up to daily cadence during 5 years with
the antennas of the Argentine Institute of Radio Astronomy (IAR). We used
standard pulsar timing tools to characterise the rotation of pulsars and
developed an algorithm to look for small timing events in the data and
calculate the changes in $\nu$ and $\dot\nu$ at those epochs.
  Results. We found that the rotation of pulsars in this dataset is affected by
small step changes in $\nu$ and $\dot\nu$. We found three glitches that had not
been reported before: two in PSR J1048-5832 with relative sizes $\Delta\nu /
\nu= 9.1(4) \times 10^{-10}$ and $\Delta\nu / \nu = 4.5(1) \times 10^{-10}$,
and one in the Vela pulsar with a size $\Delta\nu / \nu = 2.0(2) \times
10^{-10}$. We also report new decay terms on the 2021 Vela giant glitch, and on
the 2022 giant glitches in PSR J0742-2822 and PSR J1740-3015 respectively.
Besides, we found that the red noise contribution significantly diminished in
PSR J0742-2822 after its giant glitch in 2022.
  Conclusions. Our results highlight the importance of high-cadence monitoring
with an exhaustive analysis of the residuals to better characterize the
distribution of glitch sizes and to deepen our understanding of the mechanisms
behind glitches, red noise and timing irregularities.
