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Astron. Astrophys. 320, 428-439 (1997)


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The evolution of the Milky Way disc

I. Vertical structure and local constraints

M. Haywood 1, A.C. Robin 2, 3 and M. Crézé 3

1 DASGAL, URA CNRS 335, Section d'Astrophysique, Observatoire de Paris, F-92195 Meudon Cedex, France, (Misha.Haywood@obspm.fr)
2 Observatoire de Besançon, 41 bis, Av. de l'Observatoire, BP 1615, F-25010 Besançon Cedex, France, (Robin@obs-besancon.fr)
3 Observatoire de Strasbourg, CNRS URA 1280, 11 rue de l'Université, F-67000 Strasbourg, France, (Michel.Creze@iu-vannes.fr)

Received 5 April 1996 / Accepted 9 May 1996

Abstract

Deriving the Initial Mass Function and the Star Formation Rate (hereafter IMF and SFR) history of disc stars from local data implies assumptions concerning the vertical structure of the disc. Conversely, an accurate description of the vertical density of the stellar disc would require a precise knowledge of the stellar formation history. In this paper, the constraints available from local data on these two aspects are reviewed, and the interdependence between the SFR, the secular heating of the disc stars, and the shape of the density profile in the z direction is quantified.

As a consequence, the validity of exponential density models to represent the vertical structure of the disc is questioned and the uncertainties that affect the IMF derivation from the local LF are reevaluated. We show that under realistic assumptions on the SFR history, the observed local luminosity function gives little support for a bimodal IMF. Comparison of the observed local LF with synthetic LF brings tighter contraints on acceptable SFR and their corresponding IMF between 1 and 3 solar masses. These include decreasing SFR with IMF index [FORMULA] 1.5, constant SFR with IMF index [FORMULA] 2.0, or increasing SFR with IMF index [FORMULA] 2.5.

Key words: stars: luminosity function, mass function – Galaxy: evolution – Galaxy: solar neighbourhood – Galaxy: stellar content – Galaxy: structure

Send offprint requests to: M. Haywood

© European Southern Observatory (ESO) 1997

Online publication: June 30, 1998

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