This list includes small flux ropes identified in the Solar Orbiter PDS list (https://doi.org/10.5281/zenodo.16038091). For each PDS event we derive the normalized reduced magnetic helicity, the normalized cross helicity, and the residual energy, following the methodology by Telloni et al. (2012) and Zhao et al. (2020). This methodology was applied to all the low-frequency (<1 mHz) PDS events in the list, where we searched for flux ropes by requiring the absolute normalized reduced magnetic helicity to be higher than 0.7, the absolute normalized cross-helicity to be lower than 0.4, and the normalized residual energy to be lower than -0.5. We further isolated the intervals for which: a) the central time of the small flux rope is within the PDS time limits, b) the flux rope had duration higher than the corresponding period and c) the mean frequency falls within the +-0.15 mHz range. The latter condition accounts for the uncertainty in the PDS frequency estimation using the MTM and wavelet methods. CK received support from the ESA Archival Research Visitor Programme. S.D. was also supported by NASA Grant 80NSSC21K0459.