  Decayless kink oscillations of solar coronal loops (or decayless oscillations
for short) have attracted great attention since their discovery. Coronal bright
points (CBPs) are mini-active regions and consist of loops with a small size.
However, decayless oscillations in CBPs have not been widely reported. In this
study, we identified this kind of oscillations in some CBPs using 171 \AA\,
images taken by the Atmospheric Imaging Assembly (AIA) onboard the Solar
Dynamics Observatory (SDO). After using the motion magnification algorithm to
increase oscillation amplitudes, we made time-distance maps to identify the
oscillatory signals. We also estimated the loop lengths and velocity
amplitudes. We analysed 23 CBPs, and found 31 oscillation events in 16 of them.
The oscillation periods range from 1 to 8 minutes (on average about 5 minutes),
and the displacement amplitudes have an average value of 0.07 Mm. The average
loop length and velocity amplitude are 23 Mm and 1.57 \kms, respectively.
Relationships between different oscillation paraments are also examined.
Additionally, we performed a simple forward model to illustrate how these
sub-pixel oscillation amplitudes (less than 0.4 Mm) could be detected. Results
of the model confirm the reliability of our data processing methods. Our study
shows for the first time that decayless oscillations are common in small-scale
loops of CBPs. These oscillations allow for seismological diagnostics of the
Alfv\'{e}n speed and magnetic field strength in the corona.
