The infrared excess shown by white dwarfs can be an indicator of a low-mass substellar companion, like a brown dwarf or even an exoplanet. In this work, we describe the methodology followed to identify white dwarfs with infrared excess within 100 pc and we show the preliminary results. Our initial sample is an almost complete volume-limited white dwarf sample within 100pc. We use the available infrared photometry at the Virtual Observatory (VO) and the J-PAS synthetic photometry obtained from the Gaia DR3 spectra. This work may also be considered as the starting point of a spectroscopic study to unveil the nature of peculiar white dwarf systems.