We calculate the optical depth and the number of events due to gravitational microlensing towards the Galactic bulge, the spiral arm directions gamma Scutum, beta Scutum, gamma Normae, vartheta Muscae and some dwarf galaxies in the halo of the Galaxy. Using the events found by the MACHO collaboration during their first year of observation towards Baade's Window we estimate the mass functions for the bulge and disk populations following the mass moment method. We find that the mass function can be described by a decreasing power-law with slope alpha =~ 2.0 in both cases and a minimal mass of ~ 0.01 Msun for the bulge and ~ 0.02 Msun for the disk, respectively. Assuming that the obtained mass function for the disk is also valid in the spiral arms, we find that the expected number of events towards the spiral arms is in reasonable agreement with the observations. However, the small number of observed events does not yet constrain much the different parameters entering in the computation of the mass function. To study the influence of the Magellanic Clouds on the shape and the velocity dispersion in the halo we perform a N-body simulation. We find that their presence induces a slight flattening of the halo (qH =~ 0.8). As a result the expected number of microlensing events towards some targets in the halo, such as the LMC or the SMC, decreases by about 20%, whereas due to the modification induced on the velocity dispersion the event duration increases.

Microlensing towards different Galactic targets

DE PAOLIS, Francesco
1999

Abstract

We calculate the optical depth and the number of events due to gravitational microlensing towards the Galactic bulge, the spiral arm directions gamma Scutum, beta Scutum, gamma Normae, vartheta Muscae and some dwarf galaxies in the halo of the Galaxy. Using the events found by the MACHO collaboration during their first year of observation towards Baade's Window we estimate the mass functions for the bulge and disk populations following the mass moment method. We find that the mass function can be described by a decreasing power-law with slope alpha =~ 2.0 in both cases and a minimal mass of ~ 0.01 Msun for the bulge and ~ 0.02 Msun for the disk, respectively. Assuming that the obtained mass function for the disk is also valid in the spiral arms, we find that the expected number of events towards the spiral arms is in reasonable agreement with the observations. However, the small number of observed events does not yet constrain much the different parameters entering in the computation of the mass function. To study the influence of the Magellanic Clouds on the shape and the velocity dispersion in the halo we perform a N-body simulation. We find that their presence induces a slight flattening of the halo (qH =~ 0.8). As a result the expected number of microlensing events towards some targets in the halo, such as the LMC or the SMC, decreases by about 20%, whereas due to the modification induced on the velocity dispersion the event duration increases.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11587/104529
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