Microlensing constraints on the Galactic Bulge Initial Mass Function

Details Microlensing constraints on the Galactic Bulge Initial Mass Function Microlensing constraints on the Galactic Bulge Initial Mass Function

2007-11-23

arxiv.org/abs/0711.3758v2

Astron.Astrophys.480:723-733,2008

Astronomy and Astrophysics

Astrophysics

A&A in press - Minor changes to match the published version

Scientific paper

10.1051/0004-6361:20078439

Aims. We seek to probe the Galactic bulge IMF starting from microlensing observations. Methods. We analyse the recent results of the microlensing campaigns carried out towards the Galactic bulge presented by the EROS, MACHO and OGLE collaborations. In particular, we study the duration distribution of the events. We assume a power law initial mass function, $\xi(\mu)\propto \mu^{-\alpha}$, and we study the slope $\alpha$ both in the brown dwarf and in the main sequence ranges. Moreover, we compare the observed and expected optical depth profiles. Results. The values of the mass function slopes are strongly driven by the observed timescales of the microlensing events. The analysis of the MACHO data set gives, for the main sequence stars, $\alpha=1.7 \pm 0.5$, compatible with the result we obtain with the EROS and OGLE data sets, and a similar, though less constrained slope for brown dwarfs. The lack of short duration events in both EROS and OGLE data sets, on the other hand, only allows the determination of an \emph{upper} limit in this range of masses, making the overall result less robust. The optical depth analysis gives a very good agreement between the observed and the expected values, and we show that the available data do not allow one to discriminate between different bulge models.

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