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 ten late-type galaxies at 1.0 \stackrel { < } { \scriptstyle \sim } z \stackrel { < } { \scriptstyle \sim } 1.5 .
Their star formation rate ranges from \sim 4 to \sim 400 M _ { \odot } yr ^ { -1 } with a mean value of \sim 80 M _ { \odot } 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 disks .
They achieve a maximum velocity of \sim 180-290 km s ^ { -1 } within \sim 0.5-1 kpc , similar to local spirals with thin disks .
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 disk model are significantly higher than those derived for pure rotating disks and local spiral galaxies .
The galaxies of our sample have relatively young stellar populations ( \stackrel { < } { \scriptstyle \sim } 1.5 Gyr ) and possess a range of stellar mass of 0.6-5 \times 10 ^ { 10 } M _ { \odot } .
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 disk 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 \stackrel { < } { \scriptstyle \sim } z \stackrel { < } { \scriptstyle \sim } 1.5 .