Amorin, R.R.Amorin0000-0002-8900-0298Perez-Montero, E.E.Perez-Montero0000-0003-0898-2216Contini, T.T.Contini0000-0003-3278-4607Vilchez, J. M.J. M.Vilchez0000-0002-2282-5850BOLZONELLA, MICOLMICOLBOLZONELLA0000-0002-9336-7551Tasca, L. A. M.L. A. M.Tasca0000-0002-9087-2835Lamareille, F.F.Lamareille0000-0002-6986-0127Zamorani, I. G.I. G.Zamorani0000-0001-6958-0304Maier, C.C.Maier0000-0002-5845-8132Carollo, C. M.C. M.Carollo0000-0002-0101-6624Kneib, J. -P.J. -P.Kneib0000-0001-7455-8750Le Fevre, O.O.Le FevreLilly, S.S.LillyMainieri, V.V.MainieriRenzini, A.A.RenziniSCODEGGIO, MARCOMARCOSCODEGGIOBARDELLI, SandroSandroBARDELLIBONGIORNO, ANGELAANGELABONGIORNOCaputi, K.K.CaputiCUCCIATI, OlgaOlgaCUCCIATIde la Torre, S.S.de la Torrede Ravel, L.L.de RavelFRANZETTI, PAOLOPAOLOFRANZETTIGARILLI, BIANCA MARIA ROSABIANCA MARIA ROSAGARILLIIOVINO, AngelaAngelaIOVINOKampczyk, P.P.KampczykKnobel, C.C.KnobelKovac, K.K.KovacLe Borgne, J. -F.J. -F.Le BorgneLe Brun, V.V.Le BrunMignoli, M.M.MignoliPello, R.R.PelloPeng, Y.Y.PengPresotto, V.V.PresottoRicciardelli, E.E.RicciardelliSilverman, J. D.J. D.SilvermanTanaka, M.M.TanakaTresse, L.L.TresseVERGANI, DANIELADANIELAVERGANIZucca, E.E.ZuccaZcosmos Team2020-03-262020-03-262015http://hdl.handle.net/20.500.12386/23611Star formation rates have been computed from Hα or Hβ luminosity (IMF from Chabrier et al. (2003PASP..115..763C) and assuming a theoretical ratio Hα/Hβ=2.82) following Kennicutt (1998ApJ...498..541K). Uncertainties in SFR account for the propagation of errors in line fluxes and reddening. Gas-phase metallicity has been derived using four methods: (1) the direct method (Hagele et al., 2008MNRAS.383..209H); (2) the T<SUB>e</SUB>-Z correlation (This work); (3) the N2 calibration (Perez-Montero & Contini, 2009MNRAS.398..949P); and (4) the R23 calibration (McGaugh, 1991ApJ...380..140M) scaled to the direct method using the linear relation presented by Lamareille et al. (2006, Cat. J/A+A/448/893 and 2006A&A...448..907L, see also Perez-Montero et al., 2013A&A...549A..25P). In all cases, 1σ uncertainties in metallicity account for the propagated errors in line fluxes and reddening. (2 data files).enDatabase10.26093/cds/vizier.35780105http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/578/A1052015yCat..35780105AFIS/05 - ASTRONOMIA E ASTROFISICA