1997/08/11 by D. Markovic, Markovic, D.
Earth and Planetary Sciences · Physics and Astronomy · #Adaptive optics and wavefront sensing #Astrophysics (astro-ph) #FOS: Physical sciences #Geophysics and Gravity Measurements #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9708100
MNRAS LaTeX style, 14 pages, 13 multi-part figures embeded. Also available from http://www.tac.dk/~draza/papers/macho1.ps.Z
arxiv created 1997/08/11 · openalex publication_date 1997/08/11 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We study the use of parallax microlensing to separate the effects of the mass function of dark massive halo objects (MHOs or `machos') on the one hand and their spatial distribution and kinematics on the other. This disentanglement is supposed to allow a much better determination of the two than could be achieved entirely on the basis of the durations of events. We restrict our treatment to the same class of power-law spherical models for the halo of MHOs studied in a previous paper (astro-ph/9609187). Whereas the duration-based error in the average MHO mass, μexceeds (at N=100 events) μby a factor of 2 or more, parallax microlensing remarkably brings it down to 15-20% of μ, regardless of the shape of the mass function. In addition, the slope αof the mass function, dn/dμ∝μα, can be inferred relatively accurately (σα < 0.4) for a broader range, -3