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Title:
The MACHO Project Large Magellanic Cloud Microlensing Results from the First Two Years and the Nature of the Galactic Dark Halo
Authors:
Alcock, C.; Allsman, R. A.; Alves, D.; Axelrod, T. S.; Becker, A. C.; Bennett, D. P.; Cook, K. H.; Freeman, K. C.; Griest, K.; Guern, J.; Lehner, M. J.; Marshall, S. L.; Peterson, B. A.; Pratt, M. R.; Quinn, P. J.; Rodgers, A. W.; Stubbs, C. W.; Sutherland, W.; Welch, D. L.; The MACHO Collaboration
Publication:
Astrophysical Journal v.486, p.697 (ApJ Homepage)
Publication Date:
09/1997
Origin:
APJ
ApJ Keywords:
COSMOLOGY: DARK MATTER, GALAXY: HALO, COSMOLOGY: GRAVITATIONAL LENSING, GALAXIES: MAGELLANIC CLOUDS, STARS: LOW-MASS, BROWN DWARFS, STARS: WHITE DWARFS
DOI:
10.1086/304535
Bibliographic Code:
1997ApJ...486..697A

Abstract

The MACHO Project is a search for dark matter in the form of massive compact halo objects (MACHOs). Photometric monitoring of millions of stars in the Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC), and Galactic bulge is used to search for gravitational microlensing events caused by these otherwise invisible objects. Analysis of the first 2.1 yr of photometry of 8.5 million stars in the LMC reveals eight candidate microlensing events. This is substantially more than the number expected (~1.1) from lensing by known stellar populations. The timescales (t) of the events range from 34 to 145 days. We estimate the total microlensing optical depth toward the LMC from events with 2<t hat <200 days to be tau 2002=2.9^{+1.4}_{-0.9}x10^{-7} based upon our eight event sample. This exceeds the optical depth, tau backgnd = 0.5 x 10-7, expected from known stars, and the difference is to be compared with the optical depth predicted for a "standard" halo composed entirely of MACHOs: tau halo = 4.7 x 10-7. To compare with Galactic halo models, we perform likelihood analyses on the full eight-event sample and a six-event subsample (which allows for two events to be caused by a non-halo "background"). This gives a fairly model-independent estimate of the halo mass in MACHOs within 50 kpc of 2.0^{+1.2}_{-0.7}x1011 Mȯ, which is about half of the "standard halo" value. We also find a most probable MACHO mass of 0.5^{+0.3}_{-0.2} Mȯ, although this value is strongly model dependent. In addition, the absence of short duration events places stringent upper limits on the contribution of low-mass MACHOs: objects from 10-4 Mȯ to 0.03 Mȯ contribute <~20% of the "standard" dark halo.
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