White dwarfs (WDs) are generally intrinsically faint in the infrared (IR). Excess emission in the infrared results from low-mass companions or dusty material, potentially linked to the on-going accretion of planetary material. This work presents a new catalog of white dwarfs with (candidate) infrared excess. The final sample comes from a cross-match between the Gaia Early Data Release (EDR3) white dwarf candidates, and the CatWISE catalog, with candidate infrared excesses determined considering both magnitude and color excess. A magnitude excess is found to be more reliable than a color excess. The final catalog contains 554 infrared excess candidates (446 are presented for the first time here) from 41020 white-dwarf candidates with a Gaia magnitude of G<18.5mag. Our infrared excess candidate sample extends to a white-dwarf temperature range of 4500-98000K and a white-dwarf mass range of 0.1-1.2M_{sun}_. We caution that these objects should be treated as infrared excess candidates until confirmed with other methods. We present a three-fold increase in the sample of white dwarfs known to have infrared excesses. Among the sample applications is the study of the accretion of planetary material by white dwarfs and the identification of new white-dwarf-brown-dwarf pairs.

Cone search capability for table J/A+A/688/A168/table1 (Bright white dwarfs (G<=17mag) confirmed to have infrared excess)

Cone search capability for table J/A+A/688/A168/table3 (D, specifying those sources with infrared excesses (Sample F), as well as the contaminated sources (the ones excluded in the step from Sample E to Sample F))