Volume 500, Number 3, June IV 2009
|Page(s)||1027 - 1044|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||01 April 2009|
The EROS2 search for microlensing events towards the spiral arms: the complete seven season results *,**,***
Laboratoire de l'Accélérateur Linéaire, 23-, Université de Paris-Sud, BP 34, 91898 Orsay Cedex, France e-mail: firstname.lastname@example.org
2 , , , Centre d'Études de Saclay, 91191 Gif-sur-Yvette Cedex, France
3 The Niels Bohr Institute, Astronomy Group, Juliane Maries vej 30, 2100 Copenhagen, Denmark
4 Institut d'Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98 bis boulevard Arago, 75014 Paris, France
5 Observatoire Midi-Pyrénées, LATT, Université de Toulouse, CNRS, 14 Av. E. Belin, 31400 Toulouse, France
6 European Southern Observatory (ESO), Casilla 19001, Santiago 19, Chile
7 Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA
8 Observatoire de Marseille, , 2 place Le Verrier, 13248 Marseille Cedex 04, France
9 Dept. of Physics, Sharif University of Technology, Tehran, Iran
Accepted: 13 March 2009
Aims. The EROS-2 project has been designed to search for microlensing events towards any dense stellar field. The densest parts of the Galactic spiral arms have been monitored to maximize the microlensing signal expected from the stars of the Galactic disk and bulge.
Methods. 12.9 million stars have been monitored during 7 seasons towards 4 directions in the Galactic plane, away from the Galactic center.
Results. A total of 27 microlensing event candidates have been found. Estimates of the optical depths from the 22 best events are provided. A first order interpretation shows that simple Galactic models with a standard disk and an elongated bulge are in agreement with our observations. We find that the average microlensing optical depth towards the complete EROS-cataloged stars of the spiral arms is = 0.51±.1310-6, a number that is stable when the selection criteria are moderately varied. As the EROS catalog is almost complete up to IC = 18.5, the optical depth estimated for the sub-sample of bright target stars with ( = 0.39±.1110-6) is easier to interpret.
Conclusions. The set of microlensing events that we have observed is consistent with a simple Galactic model. A more precise interpretation would require either a better knowledge of the distance distribution of the target stars, or a simulation based on a Galactic model. For this purpose, we define and discuss the concept of optical depth for a given catalog or for a limiting magnitude.
Key words: cosmology: dark matter / Galaxy: disk / Galaxy: bulge / Galaxy: structure / Galaxy: kinematics and dynamics / Galaxy: microlensing
Color–magnitude tables of the EROS catalogs (Fig. 5) in ascii are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/500/1027
© ESO, 2009
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