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We construct from Gaia DR2 an extensive and very pure ($\lesssim 0.2\%$contamination) catalog of wide binaries containing main-sequence (MS) and whitedwarf (WD) components within 200 pc of the Sun. The public catalog contains,after removal of clusters and resolved higher-order multiples, $>$50,000 MS/MS,$>$3,000 WD/MS, and nearly 400 WD/WD binaries with projected separations of $50\lesssim s/{\rm AU} < 50,000$. Accounting for incompleteness and selectioneffects, we model the separation distribution of each class of binaries as abroken power-law, revealing marked differences between the three populations.The separation distribution of MS/MS systems is nearly consistent with a singlepower-law of slope $-1.6$ over at least $500 < s/{\rm AU} < 50,000$, withmarginal steepening at $s > 10,000$ AU. In contrast, the separationdistributions of WD/MS and WD/WD binaries show distinct breaks at $\sim$ 3,000AU and $\sim$1,500 AU, respectively: they are flatter than the MS/MSdistribution at small separations and steeper at large separations. Usingbinary population synthesis models, we show that these breaks are unlikely tobe caused by external factors but can be explained if the WDs incur a kick of$\sim$ 0.75 km s$^{-1}$ during their formation, presumably due to asymmetricmass loss. The data rule out typical kick velocities above 2km s$^{-1}$. Ourresults imply that most wide binaries with separations exceeding a few thousandAU become unbound during post-MS evolution.

Imprints of white dwarf recoil in the separation distribution of Gaia wide binaries