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The formation of protoplanetary disks is not well understood. To understandhow and when these disks are formed, it is crucial to characterize thekinematics of the youngest protostars at a high angular resolution. Here westudy a sample of 16 Class 0 protostars to measure their rotation profile atscales from 50 to 500~au and search for Keplerian rotation. We usedhigh-angular-resolution line observations obtained with the Plateau de BureInterferometer as part of the CALYPSO large program. From $\mathrm{^{13}CO}$($J=2-1$), $\mathrm{C^{18}O}$ ($J=2-1$) and SO ($N_{j}=5_{6}-4_{5}$) momentmaps, we find that seven sources show rotation about the jet axis at a fewhundred au scales: SerpS-MM18, L1448-C, L1448-NB, L1527, NGC1333- IRAS2A,NGC1333-IRAS4B, and SVS13-B. We analyzed the kinematics of these sources in the$uv$ plane to derive the rotation profiles down to 50~au scales. We findevidence for Keplerian rotation in only two sources, L1527 and L1448-C.Overall, this suggests that Keplerian disks larger than 50 au are uncommonaround Class 0 protostars. However, in some of the sources, the line emissioncould be optically thick and dominated by the envelope emission. Due to theoptical thickness of these envelopes, some of the disks could have remainedundetected in our observations.

Searching for kinematic evidence of Keplerian disks around Class 0 protostars with CALYPSO