Galaxy Main Sequence at z ∼ 1

The influence of dust attenuation models on the relationship between star formation rate (SFR) and stellar mass ($M^*$) (so called "galaxy main sequence", MS) for star-forming galaxies was analyzed based on the sample of $\sim$ 24 000 galaxies from the VIMOS Public Extragalactic Redshift Survey (VIPERS {The VIPERS web site is http://www.vipers.inaf.it/ }), selected based on the NUVrK$_s$ color-color diagram. For this sample of galaxies, physical parameters based on the Spectral Energy Distribution (SED) fitting were derived. The procedure was repeated for two different attenuation models: \citet{2000ApJ...539..718C} (CF00) and \citet{2000ApJ...533..682C}. The significant difference between estimated values of $M^*$ for different attenuation models was found, with the \citet{2000ApJ...539..718C} attenuation model providing, in general, higher values of stellar mass ($M^*$) and larger scatter for obtained SFR as compared to the \citet{2000ApJ...533..682C} attenuation model. The MS obtained with these two attenuation models was also found to differ, with the MS$_{\rm CF00}$ having a higher slope (0.7) than MS$_{\rm Calzetti}$ (0.3).