Morphology and Dynamics of the Milky Way

Start year
Organizational Unit

This project consists of two parts, each differentiated but both complementary: morphology and dynamics. Detailed study of the morphology of the Milky Way pretends to provide a data base for the stellar distribution in the most remote and heavily obscured regions of our Galaxy, through the development of semiempirical models based on the information in these catalogues. Kinematic and dynamical analysis, on the other hand, aims to aid our understanding of the origin of these observed features.

Our group has used a combination of its own data (which will include in the future spectroscopical observations with GRANTECAN/EMIR) and public-domain catalogues either in photometry (DENIS, 2MASS, UKIDSS, VISTA, SDSS) or spectroscopy (SDSS-APOGEE in near infrared, LAMOST). We have gathered detailed information on the stellar distribution of the dominant populations over a wide area of sky containing different structural components: the triaxial bulge, the long bar, the disc, the spiral arms, etc. The components of gas and dust are also a matter of study in infrared, or in microwave (analyses of Galactic contamination over the cosmic microwave background radiation, for instance with WMAP or PLANCK). Our research team has also become part of the Spanish node of Gaia with the idea of orientating part of our work towards the scientific exploitation of this mission, particularly with regard to the identification and study of large scale stellar populations in the Galaxy.

Principal investigator
Project staff
Nieves D. Castro Rodríguez
Antonio L. Cabrera Lavers
P.L. Hammersley
C. González Fernández
J. Molgó Sendra
F. Sylos-Labini
  1. Milky Way's disk much larger than previously thought. See press release of IAC:

Publications related

  • Fossil group origins. II. Unveiling the formation of the brightest group galaxies through their scaling relations

    Context. Fossil systems are galaxy associations dominated by a relatively isolated, bright elliptical galaxy, surrounded by a group of smaller galaxies lacking L∗ objects. Because of this extreme environment, fossil groups (FGs) are ideal laboratories for studying the mass assembly of brightest group galaxies (BGGs). Aims: We analyzed the near

    Méndez-Abreu, J. et al.

    Advertised on:

  • Ground-based Multisite Observations of Two Transits of HD 80606b

    We present ground-based optical observations of the 2009 September and 2010 January transits of HD 80606b. Based on three partial light curves of the 2009 September event, we derive a midtransit time of Tc [HJD] = 2455099.196 ± 0.026, which is about 1σ away from the previously predicted time. We observed the 2010 January event from nine different

    Shporer, A. et al.

    Advertised on:

  • Metallicity distribution of red giants in the Inner Galaxy from near infrared spectra

    Context: The existence in the Milky Way of either a long thin bar with a half length of 4.5 kpc and a position angle of around 45° with respect to the Sun-Galactic centre line or a bulge+bar complex, thicker and shorter, with a smaller tilt respect to the Sun-GC line, has been a matter of discussion in recent decades. Aims: In this paper, we

    González-Fernández, C. et al.

    Advertised on:


Talks related

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