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A minimum in stellar velocity dispersion is often observed in the centralregions of disc galaxies. To investigate the origin of this feature, known as a{\sigma}-drop, we analyse the stellar kinematics of a high-resolution N-body +smooth particle hydrodynamical simulation, which models the secular evolutionof an unbarred disc galaxy. We compared the intrinsic mass-weighted kinematicsto the recovered luminosity-weighted ones. The latter were obtained byanalysing synthetic spectra produced by a new code, SYNTRA, that generatessynthetic spectra by assigning a stellar population synthesis model to eachstar particle based on its age and metallicity. The kinematics were derivedfrom the synthetic spectra as in real spectra to mimic the kinematic analysisof real galaxies. We found that the recovered luminosity-weighted kinematics inthe centre of the simulated galaxy are biased to higher rotation velocities andlower velocity dispersions due to the presence of young stars in a thin andkinematically cool disc, and are ultimately responsible for the {\sigma}-drop.

The kinematics of {\sigma}-drop bulges from spectral synthesis modelling of a hydrodynamical simulation