منابع مشابه
Calibration of the MACHO Photometry Database
The MACHO Project is a microlensing survey that monitors the brightnesses of ∼60 million stars in the Large Magellanic Cloud (LMC), Small Magellanic Cloud, and Galactic bulge. Our database presently contains about 80 billion photometric measurements, a significant fraction of all astronomical photometry. We describe the calibration of MACHO two-color photometry and transformation to the standar...
متن کاملMacho Proper Motions From Optical/Infrared Photometry
Optical/infrared photometry can double the number of proper motion measurements of Massive Compact Objects (MACHOs) relative to single band photometry. The proper motion of a MACHO can be measured by nding the ratio q of the (known) radius of the source star to the Einstein radius of the MACHO, q = s= e. A classic method for doing this is to look for the e ect on the light curve of the nite siz...
متن کاملStellar Photometry and Astrometry with Discrete Point Spread Functions
The key features of the MATPHOT algorithm for precise and accurate stellar photometry and astrometry using discrete Point Spread Functions are described. A discrete Point Spread Function (PSF) is a sampled version of a continuous PSF which describes the two-dimensional probability distribution of photons from a point source (star) just above the detector. The shape information about the photon ...
متن کاملPSFs, Photometry, and Astrometry for the ACS/WFC
We develop and present effective PSFs for the F606W filter in the WFC, and then for five other filters. After briefly reviewing the concept of the effective PSF, we show that the WFC PSF varies with position in the detector. We represent the PSF by a 9×10 array of fiducial PSFs, between which a tailor-made PSF is to be interpolated for each star. Fitting these PSFs to star images gives photomet...
متن کاملAccurate Astrometry and Photometry of Saturated and Coronagraphic Point Spread Functions
Accurate astrometry and photometry of saturated and coronagraphic point spread functions (PSFs) are fundamental to both groundand space-based high contrast imaging projects. For ground-based adaptive optics imaging, differential atmospheric refraction and flexure introduce a small drift of the PSF with time, and seeing and sky transmission variations modify the PSF flux distribution. For space-...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1995
ISSN: 0074-1809
DOI: 10.1017/s0074180900228696