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Most of the Universe's populations of low energy cosmic ray electrons in theenergy range of 1-100 MeV still manage to elude from detection by ourinstruments, since their synchrotron emission is at too low frequencies. Weinvestigate a mechanism which can lead to observable emission of such electronpopulations: synchrotron-self Comptonization (SSC). The inverse Compton (IC)scattering can shift an otherwise unobservable low-frequency 10 kHz-10 MHzphotons into observable radio, infrared (IR) or even more energetic wave-bands.The resulting emission should be polarized. We also consider IC scattering ofthe cosmic microwave background (CMB) and the cosmic radio background (CRB).Electron spectral aging due to synchrotron, IC and adiabatic losses or gainsinfluences the resulting spectrum. The predicted radiation spectrum is a strongfunction of the history of the source, of the low energy spectrum ofrelativistic electrons, and of redshift. It has typically two maxima, and adecrement in between at CMB frequencies. Detection will give a sensitive probeof the environment of radio galaxies. We demonstrate that the fossil remnantsof powerful radio galaxies are promising detection candidates, especially whenthey are embedded in a dense intra-cluster medium (ICM). GHz peaked sources(GPS) have very low SSC luminosities, which may, however, extend into the X-rayor even the gamma ray regime. Clusters of galaxies with relativistic electronpopulations may be another detectable sources. Fossil radio plasma released byour own Galaxy could be revealed by its large angular scale SSC flux. Wediscuss the expected detectability of these sources with new and upcominginstruments as LOFAR, GMRT, EVLA, ATA, ALMA, PLANCK, and HERSCHEL.Comment: 17 pages, 14 figures, accepted by Astronomy & Astrophysics, some  changes due to referee's comments, new section about detectabilit

Synchrotron self-Comptonized emission of low energy cosmic ray electrons in the Universe