Research Lines

Birth and Internal Structure of the Stellar Clusters


Massive Stars in the Milky Way

  • Database. Create the largest possible spectral database for visually observable Galactic O stars using high-quality, high-S/N, uniform data.
  • Spectral Morphology. Reanalyze the fundamental spectral morphology for O stars.
  • Multiplicity. Analyze the multiplicity of massive stars.
  • Galactic Extinction. Obtain a new Galactic extinction law and analyze its relationship with the DIBs .
  • Spatial Distribution. Study of the spatial distribution of massive stars and dust within 3 kpc of the Sun.
  • Massive- star IMF. Derive the massive-star IMF in the solar neighborhood for both the field and some clusters.


PMS Stars in Clusters

  • Determination of the PMS population for a larger sample of young clusters in optical and NIR bands.
  • Mass Function and Age structure of the PMS sequences in the different clusters. Variations with Post-Main Sequence age and model dependencies.
  • Determination of a complete and precise IMF combining data for all our sample of clusters.
  • Derivation of Constraints to the Physical Inputs in PMS evolutionary models.


The Nuclear Star Cluster of the Milky Way

  • Improve current models for cluster with particular emphasis on size and mass of the cluster.
  • Search for young, massive stars in the cluster at projected distances between 0.5 and 5 pc from the central massive black hole, Sagittarius A*.
  • Accurately constrain the extinction law toward the NSC and create an extinction map with resolution of ~5 arcseconds.
  • Study the mid-infrared emission from stars and ISM in the NSC with VISIR/VLT and Canaricam/GTC.
  • Improve stellar proper motion measurements in the central parsec of the Galaxy and use these measurements to determine the mass and kinematic structure of the cluster.


Methodology and tools

  • Update CHORIZOS and implement the calculation of distances to individual stars and star clusters.
  • Development of tools to perform a systematic search of kinematic stellar systems as moving groups, open clusters, associations and tidal streams, using the database of the astrometric catalogue CdC-SF (Vicente et al. 2010), being the final aim the application to the GAIA catalogue.
  • Comparison of new algorithms for generating fractal clouds based on different physical principles.
  • Optical distortion of NACO S27. Determine the optical distortion solution for the S27 camera of NACO/VLT to submilliarcsecond precision.