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Mass loss of massive helium stars is not well understood even though it playsan essential role in determining their remnant neutron-star or black-holemasses as well as ejecta mass of Type Ibc supernovae. Radio emission from TypeIbc supernovae is strongly affected by circumstellar matter properties formedby mass loss of their massive helium star progenitors. In this study, weestimate the rise time and peak luminosity distributions of Type Ibc supernovaein radio based on a few massive helium star mass-loss prescriptions and comparethem with the observed distribution to constrain the uncertain massive heliumstar mass-loss rates. We find that massive helium stars in the luminosity rangeexpected for ordinary Type Ibc supernova progenitors (4.6 ~< log L/Lsun ~< 5.2)should generally have large mass-loss rates (> ~ 1e-6 Msun/yr) in order toaccount for the observed rise time and peak luminosity distribution. Therefore,mass-loss prescriptions that predict significantly low mass-loss rates forhelium stars in this luminosity range is inconsistent with the supernova radioobservations. It is also possible that massive helium stars shortly beforetheir explosion generally undergo mass-loss enhancement in a different way fromthe standard radiation-driven wind mechanism.

Mass loss of massive helium star supernova progenitors shortly before explosion constrained by supernova radio properties