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Dust attenuation shapes the spectral energy distribution of galaxies. It isparticularly true for dusty galaxies in which stars experience a heavyattenuation. The combination of UV-to-IR photometry with the spectroscopicmeasurement of the H$\alpha$ recombination line helps to quantify dustattenuation of the whole stellar population and its wavelength dependence. Weselected an IR complete sample of galaxies in the COSMOS 3D-HST CANDELS fielddetected with the Herschel satellite with a signal to noise ratio larger thanfive. Optical to NIR photometry is available as well as NIR spectroscopy foreach source. We reduced the sample to the redshift range $0.6 < z < 1.6$ toinclude the H$\alpha$ line in the G141 grism spectra. We have used a newversion of the CIGALE code to fit simultaneously the continuum and H$\alpha$line emission of the 34 selected galaxies. Using flexible attenuation laws withfree parameters, we are able to measure the shape of the attenuation curve foreach galaxy as well as the amount of attenuation of each stellar population,the former being in general steeper than the starburst law in the UV-opticalwith a large variation of the slope among galaxies. The attenuation of youngstars or nebular continuum is found on average about twice the attenuationaffecting older stars, again with a large variation. Our model with power-laws,based on a modification of the Charlot and Fall recipe, gives results in betteragreement with the radiative transfer models than the global modification ofthe slope of the Calzetti law.

Dust attenuation and Halpha emission in a sample of galaxies observed with Herschel at $0.6 < z <1.6$