Distance and extinction to the Milky Way spiral arms along the Galactic centre line of sight

Context. The position of the Sun inside the disc of the Milky Way significantly hampers the study of the spiral arm structure given the high amount of dust and gas along the line of sight, and the overall structure of this disc has therefore not yet been fully characterised. <BR /> Aims: We aim to analyse the spiral arms in the line of sight towards the Galactic centre (GC) in order to determine their distance, extinction, and stellar population. <BR /> Methods: We use the GALACTICNUCLEUS survey, a JHK<SUB>s</SUB> high-angular-resolution photometric catalogue (0.2″) for the innermost regions of the Galaxy. We fitted simple synthetic colour-magnitude models to our data via χ<SUP>2</SUP> minimisation. We computed the distance and extinction to the detected spiral arms. We also analysed the extinction curve and the relative extinction between the detected features. Finally, we studied extinction-corrected K<SUB>s</SUB> luminosity functions (KLFs) to study the stellar populations present in the second and third spiral arm features. <BR /> Results: We determined the mean distances to the spiral arms: d<SUB>1</SUB> = 1.6 ± 0.2 kpc, d<SUB>2</SUB> = 2.6 ± 0.2 kpc, d<SUB>3</SUB> = 3.9 ± 0.3 kpc, and d<SUB>4</SUB> = 4.5 ± 0.2 kpc, and the mean extinctions: A<SUB>H1</SUB> = 0.35 ± 0.08 mag, A<SUB>H2</SUB> = 0.77 ± 0.08 mag, A<SUB>H3</SUB> = 1.68 ± 0.08 mag, and A<SUB>H4</SUB> = 2.30 ± 0.08 mag. We analysed the extinction curve in the near-infrared for the stars in the spiral arms and find mean values of A<SUB>J</SUB>/A<SUB>H</SUB> = 1.89 ± 0.11 and A<SUB>H</SUB>/A<SUB>K<SUB>s</SUB></SUB> = 1.86 ± 0.11, in agreement with the results obtained for the GC. This implies that the shape of the extinction curve does not depend on distance or absolute extinction. We also built extinction maps for each spiral arm and find them to be homogeneous and that they might correspond to independent extinction layers. Finally, analysing the KLFs from the second and third spiral arms, we find that they have similar stellar populations. We obtain two main episodes of star formation: &gt; 6 Gyr (∼60 − 70% of the stellar mass), and 1.5 − 4 Gyr (∼20 − 30% of the stellar mass), compatible with previous work. We also detect recent star formation at a lower level (∼10%) for the third spiral arm.