The First Six Months of the LLNL-CfPA-MSSSO Search for Baryonic Dark Matter in the Galaxy's Halo via its Gravitational Microlensing Signature

Details The First Six Months of the LLNL-CfPA-MSSSO Search for Baryonic Dark Matter in the Galaxy's Halo via its Gravitational Microlensing Signature The First Six Months of the LLNL-CfPA-MSSSO Search for Baryonic Dark Matter in the Galaxy's Halo via its Gravitational Microlensing Signature

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.3808c&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #38.08; Bulletin of the American Astronomical Society, Vol. 24, p.1179

Astronomy and Astrophysics

Astronomy

4

Scientific paper

This collaboration, dubbed the MACHO Project (an acronym for MAssive Compact Halo Objects), has refurbished the 1.27-m, Great Melbourne Telescope at Mt. Stromlo and equipped it with a corrected {1°} FOV. The prime focus corrector yields a red and blue beam for simultaneous imaging in two passbands, 4500{ Angstroms}--6100{ Angstroms} and 6100{ Angstroms}--7900{ Angstroms}. Each beam is imaged by a 2x2 array of 2048x2048 pixel CCDs which are simultaneously read out from two amplifiers on each CCD. A 32 Megapixel dual-color image of 0.5 square degree is clocked directly into computer memory in less than 70 seconds. We are using this system to monitor more than 10(7) stars in the Magellanic Clouds for gravitational microlensing events and will soon monitor an additional 10(7) stars in the bulge of our galaxy. Image data goes directly into a reduction pipeline where photometry for stars in an image is determined and stored in a database. An early version of this pipeline has used a simple aperture photometry code and results from this will be presented. A more sophisticated PSF fitting photometry code is currently being installed in the pipeline and results should also be available at the meeting. The PSF fitting code has also been used to produce ~ 10(7) photometric measurements outside of the pipeline. This poster will present details of the instrumentation, data pipeline, observing conditions (weather and seeing), reductions and analyses for the first six months of dual-color observing. Eventually, we expect to be able to determine whether MACHOs are a significant component of the galactic halo in the mass range of \(10^{-6} M_{\sun} < M \ {lower .5exhbox {\: \buildrel < \over \sim ;}} \ 100 M_{\sun}\).

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