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Recent data from CREAM seem to confirm early suggestions that primary cosmicray (CR) spectra at few TeV/nucleon are harder than in the 10-100 GeV range.Also, helium and heavier nuclei spectra appear systematically harder than theproton fluxes at corresponding energies. We note here that if the measurementsreflect intrinsic features in the interstellar fluxes (as opposed to localeffects) appreciable modifications are expected in the sub-TeV range for thesecondary yields, such as antiprotons and diffuse gamma-rays. Presently, theignorance on the origin of the features represents a systematic error in theextraction of astrophysical parameters as well as for background estimates forindirect dark matter searches. We find that the spectral modifications areappreciable above 100 GeV, and can be responsible for ~30% effects forantiprotons at energies close to 1 TeV or for gamma's at energies close to 300GeV, compared to currently considered predictions based on simple extrapolationof input fluxes from low energy data. Alternatively, if the feature originatesfrom local sources, uncorrelated spectral changes might show up in antiprotonand high-energy gamma-rays, with the latter ones likely dependent from theline-of-sight.

"Discrepant hardenings" in cosmic ray spectra: a first estimate of the effects on secondary antiproton and diffuse gamma-ray yields