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The emission line survey within the Calar Alto Deep Imaging Survey (CADIS)detects emission line galaxies by a scan with an imaging Fabry-Perotinterferometer. It covers 5 fields of > 100 square arcmin each in threewavelengths windows centered on lambda ~ 700, 820, and 920nm, and reaches to atypical limiting line flux of 3 x 10^(-20) W m^(-2). This is the deepestemission line survey covering a field of several 100 square arcmin. Galaxiesbetween z = 0.25 and z = 1.4 are detected by prominent emission lines (fromHalpha to [OII]372.7) falling into the FP scans. Additional observations with adozen medium band filters allow to establish the line identification and thusthe redshift of the galaxies to better than sigma(z) =0.001. On the basis of atotal of more than 400 emission line galaxies detected in Halpha (92 galaxies),[OIII]500.7 (124 galaxies), or [OII]372.7 (222 galaxies) we measure theinstantaneous star formation rate (SFR) in the range 0.24 < z < 1.21. With thispurely emission line selected sample we are able to reach much fainter emissionline galaxies than previous, continuum-selected samples. Thus completenesscorrections are much less important. Our results substantiates the indicationsfrom previous studies (based on small galaxy samples) that the SFR decreases bya factor of ~20 between z = 1.2 and today. In fact, for a Omega(m) = 0.3,Omega(Lambda) = 0.7 cosmology, we find an exponential decline rho(SFR)proportional to exp(-lookback_time) / 2.6Gyr). The inferred SF density is inperfect agreement with that deduced from the FIR emission of optically selectedgalaxies which is explained by a large overlap between both populations. Weshow that self-consistent extinction corrections of both our emission lines andthe UV continua lead to consistent results for the SF density.Comment: accepted for publication in A&

Star forming rates between z = 0.25 and z = 1.2 from the CADIS emission line survey