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The {\it Gaia} satellite recently released parallax measurements for$\sim$260,000 high-confidence white dwarf candidates, allowing for precisemeasurements of their physical parameters. By combining these parallaxes withPan-STARRS and $u$-band photometry, we measured the effective temperature andstellar mass for all white dwarfs in the Northern Hemisphere within 100 parsecsof the Sun, and identified a sample of ZZ Ceti white dwarf candidates withinthe so-called instability strip. We acquired high-speed photometricobservations for 90 candidates using the PESTO camera attached to the 1.6-mtelescope at the Mont-M\'egantic Observatory. We report the discovery of 38 newZZ Ceti stars, including two very rare ultra-massive pulsators. We alsoidentified 5 possibly variable stars within the strip, in addition to 47objects that do not appear to show any photometric variability. However,several of those could be variable with an amplitude below our detectionthreshold, or could be located outside the instability strip due to errors intheir photometric parameters. In the light of our results, we explore thetrends of the dominant period and amplitude in the $M - T_{\rm eff}$ plane, andbriefly discuss the question of the purity of the ZZ Ceti instability strip(i.e. a region devoid of non-variable stars).

Searching for ZZ Ceti White Dwarfs in the Gaia Survey