Microlensing and pixel-lensing surveys play a fundamental role in the searches for galactic dark matter and in the study of the galactic structure. Recent observations suggest the presence of a population of old white dwarfs with high proper motion, probably in the galactic halo, with local mass density in the range 1.3×10-4-4.4×10-3 Msun pc-3, in addition to the standard galactic stellar disk and dark halo components. Investigation of the signatures on microlensing results towards the LMC of these different lens populations, with particular emphasis to white dwarfs, is the main purpose of the present paper. This is done by evaluating optical depth and microlensing rate of the various lens populations and then calculating through a Monte Carlo program, the probability that a lens which has caused a microlensing event of duration tE belongs to a certain galactic population. Data obtained by the MACHO Collaboration allow us to set an upper bound of 1.6×10-3 Msun pc-3 to the local mass density of white dwarfs distributed in spheroidal models, while for white dwarfs in disk models all values for the local mass density are in agreement with observational results.
Microlensing Signature of a White Dwarf Population in the Galactic Halo
DE PAOLIS, Francesco;INGROSSO, Gabriele;NUCITA, Achille
2004-01-01
Abstract
Microlensing and pixel-lensing surveys play a fundamental role in the searches for galactic dark matter and in the study of the galactic structure. Recent observations suggest the presence of a population of old white dwarfs with high proper motion, probably in the galactic halo, with local mass density in the range 1.3×10-4-4.4×10-3 Msun pc-3, in addition to the standard galactic stellar disk and dark halo components. Investigation of the signatures on microlensing results towards the LMC of these different lens populations, with particular emphasis to white dwarfs, is the main purpose of the present paper. This is done by evaluating optical depth and microlensing rate of the various lens populations and then calculating through a Monte Carlo program, the probability that a lens which has caused a microlensing event of duration tE belongs to a certain galactic population. Data obtained by the MACHO Collaboration allow us to set an upper bound of 1.6×10-3 Msun pc-3 to the local mass density of white dwarfs distributed in spheroidal models, while for white dwarfs in disk models all values for the local mass density are in agreement with observational results.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
