  Planetary nebulae (PNe) consist of an ionized envelope surrounding a hot
central star (CSPN) that emits mostly at ultraviolet (UV) wavelengths.
Ultraviolet observations, therefore, provide important information on both the
CSPN and the nebula. We have matched the PNe in The Hong Kong/AAO/Strasbourg
H$\alpha$ (HASH) catalog with the Galaxy Evolution Explorer (GALEX) UV sky
surveys, the Sloan Digital Sky Survey data release 16 (SDSS), and the Panoramic
Survey Telescope and Rapid Response System (Pan-STARRS) PS1 second release. A
total of 671 PNe were observed by GALEX with the far-UV (FUV; 1344-1786{\AA})
and/or the near-UV (NUV; 1771-2831{\AA}) detector on (GUVPNcat); 83 were
observed by SDSS (PNcatxSDSSDR16) and 1819 by Pan-STARRS (PNcatxPS1MDS). We
merged a distilled version of these matched catalogs into
GUVPNcatxSDSSDR16xPS1MDS, which contains a total of 375 PNe with both UV and
optical photometry over a total spectral coverage of $\sim$1540--9610{\AA}. We
analysed separately 170 PNe resolved in GALEX images and determined their UV
radius by applying a flux profile analysis. The CSPN flux could be extracted
separately from the PN emission for 8 and 50 objects with SDSS and Pan-STARRS
counterparts respectively. The multi-band photometry was used to distinguish
between compact and extended PNe and CSPNe (binary CSPNe) by color--color
diagram analysis. We found that compact PNe candidates could be identified by
using the $r-i < -0.4$ and $-$1$<$FUV$-$NUV$<$1 colors, whereas binary CSPNe
candidates in given $T_\mathrm{eff}$ ranges (all with color r$-$i$>-$0.4) can
be identified in the color region (FUV$-$NUV)$\leq$6(r$-$i)+1.3,
$-$0.8$<$FUV$-$NUV$<$0.4 and r$-$i$<$0.75.
