Model of stellar population synthesis of the Galaxy

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The model of stellar population synthesis built by our team for three decades is used to elaborate a global view of the Galaxy including dynamical and evolutionary aspects. Scenarii for the formation and evolution produces theoretical distribution functions which are directly compared with survey observations of different types (photometry, kinematics, abundance distributions).

We link the kinematical and dynamical point of view to an evolution scheme through a key parameter: the stellar ages. The age distribution of stars in the solar neighbourhood is derived from a model of galactic evolution. The stellar populations of the galactic disc are selfconsistently constrained by the Boltzmann and Poisson equations through the potential of the mass model. Thus we directly derive observational predictions from an overall description of galactic structure and evolution.

A complete description of the model inputs can be found in Robin, Reylé, Derrière, Picaud (2003) A&A 409, 523.

However, important updates have been performed concerning different aspects of the model since this version. They concern :


The model is a powerful tool to constrain either evolutionary scenarii or galactic structure hypothesis through the comparison between model predictions and a large variety of observational constraints such as star counts, photometry or astrometry. Model simulations are produced in the form of:

A number of quantitative results has been obtained by comparing model predictions with suitable observations, like multidirectional photometric and astrometric star counts. Simulations may help for preparing observations, for evaluating the Galactic stellar contamination in extragalatic studies or in star cluster fields.

Simulated image of the Galaxy in BVR bands
Simulated image of the Galaxy in 3 visible colours, as seen from the sun. Colours are given by the integrated flux in bands BVR.
Simulated image of the Galaxy in JHK bands
Simulated image of the Galaxy in 3 infrared colours, as seen from the sun. Colours are given by the integrated flux in bands JHK.



Simulations are made at your own risks. The authors are not responsible for wrong applications of their model.

In case you would like complementary informations, you may contact the authors directly (modele[at]

Changes log

Here are summarized the model changes since the version released on November 25, 2003 (version described in A. C. Robin, C. Reylé, S. Derrière and S. Picaud. A synthetic view on structure and evolution of the Milky Way, 2003, Astron. Astrophys., 409:523 [ADS] and erratum: 2004, Astron. Astrophys., 416:157)