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tokens: the limit in local color was slightly larger than the median value at U − V ~ 0.65 with a magnitude step significant at 7.4 σ . On the other hand, maximizing the mass step significance led to a mass limit of about , corresponding to a magnitude step of 7.2 σ significance.In this case, the separation does not lie close to the median value, since 31% of our sample is found below the new mass limit, and 69% above. This new limit is closer to the mass bin separation of , chosen in allprevious studies on host galaxies. In particular, Childress et al. (2013) found an apparent Hubble residual transition between 10 9.8 and . Choosing this mass separation yields comparably significant mass and color steps. The top and bottom panels of Fig. 19 show the evolution of step significance as a function of the cut position when local U − V colors and host stellar masses are used as a third standardization parameter. The sample median lies close to the maximum local color step significance, whereas the most significant mass step implies a bin separation at . Table 10 Summary of all tests performed throughout the paper with the corresponding number of SNIa in the sample, the local U − V color step, the host stellar mass step, and step values when corrected for one or the other effect. However, the correlations between the Hubble diagram residuals derived from a three-parameter standardization and our host variables yield additional information. When residuals are corrected for local U − V color, the remaining maximum mass step significance is of 3.8 σ (i.e., the maximum correlation between stellar mass and corrected Hubble diagram residuals using the most significant local step). Conversely, the remaining maximum local color step after mass correction as a third variable is of 5 σ (i.e., the maximum correlation between local U − V color and corrected Hubble diagram residuals using the most significant mass step). Hence, maximizing the significance still shows that scatter in the Hubble diagram is better accounted for when the supernova brightness is corrected for local environment. It is also worth noting that the local U − V color does not fully account for the remaining scatter either. A better proxy, or a combination of proxies, linked to properties of the local environment of SNIa, is yet to be found. 7 Summary and perspectives As elaborated in Sect. 1 , many studies in the literature have found compelling proof of a dependence of Type Ia supernovæ properties on their close or distant environment, concerning a few hundred events at most that exploded in the nearby Universe. In this work, we measured the photometry of the host galaxy and local fluxes in regions with a radius a 3 kpc for 882 supernovæ that are distributed in a wide redshift range, from z = 0.01 to z = 1.1. We consistently measured photometry from SNLS and SDSS images, and gathered additional photometry from the 2MASS catalog when needed, in order to complete our sample of host galaxy