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The metallicity of the progenitor system producing a type Ia supernova (SNIa) could play a role in its maximum luminosity, as suggested by theoreticalpredictions. We present an observational study to investigate if such arelationship there exists. Using the 4.2m WHT we have obtainedintermediate-resolution spectroscopy data of a sample of 28 local galaxieshosting SNe Ia, for which distances have been derived using methods independentto those based on the own SN Ia parameters. From the emission lines observed intheir optical spectrum, we derived the gas-phase oxygen abundance in the regionwhere each SN Ia exploded. Our data show a trend, with a 80% of chance not tobe due to random fluctuation, between SNe Ia absolute magnitudes and the oxygenabundances of the host galaxies, in the sense that luminosities tend to behigher for galaxies with lower metallicities. This result seems like to be inagreement with both the theoretically expected behavior, and with otherobservational results. This dependence $M_{B}$-Z might induce to systematicerrors when is not considered in deriving SNe Ia luminosities and then usingthem to derive cosmological distances.

On the dependence of the type Ia SNe luminosities on the metallicity of their host galaxies