  This study investigates and compares brightness and area of coronal bright
points (CBPs) inside and outside of coronal holes (CHs) using the single-dish
Band 6 observations by the Atacama Large Millimeter/submillimeter Array (ALMA),
combined with extreme-ultraviolet (EUV) 193 $\overset{\circ}{\mathrm{A}}$
filtergrams obtained by the Atmospheric Imaging Assembly (AIA) and magnetograms
obtained by the Helioseismic and Magnetic Imager (HMI), both on board Solar
Dynamics Observatory (SDO). The CH boundaries were extracted from the SDO/AIA
images using the Collection of Analysis Tools for Coronal Holes (CATCH) and
CBPs were identified in the SDO/AIA, SDO/HMI, and ALMA data. Measurements of
brightness and areas in both ALMA and SDO/AIA images were conducted for CBPs
within CHs and quiet Sun regions outside CHs. A statistical analysis of the
measured physical properties resulted in a lower average CBP brightness in both
ALMA and SDO/AIA data for CBPs within the CHs. Depending on the CBP sample
size, the difference in intensity for the SDO/AIA data, and brightness
temperature for the ALMA data, between the CBPs inside and outside CHs ranged
from between 2$\sigma$ and 4.5$\sigma$, showing a statistically significant
difference between those two CBP groups. For CBP areas, CBPs within the CH
boundaries showed smaller areas on average, with the observed difference
between the two CBP groups between 1$\sigma$ and 2$\sigma$ for the SDO/AIA
data, and up to 3.5$\sigma$ for the ALMA data, indicating that CBP areas are
also significantly different. Given the measured properties, we conclude that
the CBPs inside CHs tend to be less bright on average, but also smaller in
comparison to those outside of CHs. This conclusion might point to the specific
physical conditions and properties of the local CH region around a CBP limiting
the maximum achievable intensity (temperature) and size of a CBP.
