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Supernova remnants (SNRs) are prime candidates for efficient particleacceleration up to the knee in the cosmic ray particle spectrum. In this workwe present a new method for a systematic search for new TeV-emitting SNR shellsin 2864 hours of H.E.S.S. phase I data used for the H.E.S.S. Galactic PlaneSurvey. This new method, which correctly identifies the known shellmorphologies of the TeV SNRs covered by the survey, HESS J1731-347, RX1713.7-3946, RCW 86, and Vela Junior, reveals also the existence of three newSNR candidates. All three candidates were extensively studied regarding theirmorphological, spectral, and multi-wavelength (MWL) properties. HESS J1534-571was associated with the radio SNR candidate G323.7-1.0, and thus is classifiedas an SNR. HESS J1912+101 and HESS J1614-518, on the other hand, do not haveradio or X-ray counterparts that would permit to identify them firmly as SNRs,and therefore they remain SNR candidates, discovered first at TeV energies assuch. Further MWL follow up observations are needed to confirm that these newlydiscovered SNR candidates are indeed SNRs.

Discovery of new TeV supernova remnant shells in the Galactic plane with H.E.S.S