Astronomy and Astrophysics
Aims: We derive the density distributions of the average (old) whole population and the supergiants (representative of a young population), and we use them to constrain their warp and flare. By comparing the results, we study how the properties of these phenomena depend on the studied population.
Methods: We used Lucy's deconvolution method to recover corrected star counts as a function of distance, from which we derive the density distribution.
Results: We find that supergiants have an asymmetric warp, reaching a maximum amplitude of zw = 0.658 kpc and minimum amplitude of zw = −0.717 kpc at a distance of R = [19.5, 20] kpc, which is almost twice as high as the amplitude of the whole population of the disc. We find a significant flare of the whole population, especially in the thick disc. The scale height increases from hz,thick ≈ 0.7 kpc and hz, thin ≈ 0.3 kpc in the solar neighbourhood, to hz, thick ≈ 2.6 kpc and hz, thin ≈ 0.6 kpc in the remote regions of the Milky Way (R ≈ 18 kpc). The supergiants' population has only a small flare.

El objetivo general del Proyecto es el estudio de la estructura, historia evolutiva y proceso de formación de galaxias a través de sus poblaciones estelares resueltas, tanto a partir de fotometría como espectroscopia. El proyecto puede dividirse en cuatro líneas principales: I. Historia de formación estelar en el Grupo Local. El objetivo de esta