2D kinematics and physical properties of 1.0 less than or similar to z less than or similar to 1.5 star-forming galaxies

We combined two-dimensional kinematic and morphology information on the H alpha emission, obtained using near-infrared integral-field spectroscopy, with broad-band photometry to investigate the dynamical structure and the physical properties of a sample of 10 late-type galaxies at 1.0 less than or similar to z less than or similar to 1.5. Their star formation rate ranges from similar to 4 to similar to 400 M-circle dot yr(-1) with a mean value of similar to 80 M-circle dot yr(-1). We found that three of these objects are undergoing a strong burst of star formation. The sample displays a range of kinematical types which include one merger, one face-on galaxy and eight objects showing evidence of rotation. Among these eight objects, half are rotation-dominated galaxies, while the rest are dispersion-dominated. We found also that two galaxies out of the rotation-dominated galaxies are pure rotationally supported discs. They achieve a maximum velocity of similar to 180-290 km s(-1) within similar to 0.5-1 kpc, similar to local spirals with thin discs. Regarding the perturbed rotation and the dispersion-dominated galaxies, they display a plateau velocity range of 105-257 km s(-1), which is certainly underestimated due to beam smearing. However, their plateau radii (4.5-10.8 kpc) derived from our rotating disc model are significantly higher than those derived for pure rotating discs and local spiral galaxies. The galaxies of our sample have relatively young stellar populations (less than or similar to 1.5 Gyr) and possess a range of stellar mass of 0.6-5 x 10(10) M-circle dot. In addition, most of them have not yet converted the majority of their gas into stars (six galaxies have their gas fraction > 50 per cent). Therefore, those of them which already have a stable disc will probably have their final stellar mass similar to the present-day spirals, to which these rotating systems can be seen as precursors. We conclude our study by investigating the stellar mass Tully-Fisher relation at 1.2 less than or similar to z less than or similar to 1.5.