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Multi-Parametric Iris-Photometry

Published online by Cambridge University Press:  26 July 2016

T.B. Georgiev
T.B. Georgiev*
Affiliation:
Rozhen National Astronomical Observatory, P.O. Box 136, BG-4700 Smolyan, Bulgaria

Extract

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Usually, the reduction of iris-measurements d of stellar photographic images to magnitudes m is performed with one-dimensional regression m = f(d), obtained using standard stars (Burkhead & Seeds 1971). The derivation of accurate magnitudes is difficult due to many factors (Butler 1972). Considering that the star image shape contains information on the sensitivity of the plate and the color of the star, Vladimirov (1978) recommended multi-parametric determination of the magnitudes, using a system of isodense bounded areas of the stellar images. Here this approach is implemented using software that performs a general multi-parametric method (MPM) of iris-photometry.

Type
Part Six: Calibration: Astrometric and Photometric
Information
Symposium - International Astronomical Union , Volume 161: Astronomy from Wide-Field Imaging , 1994 , pp. 311
Copyright
Copyright © Kluwer 1994 

References

Burkhead, M. and Seeds, M., 1971. AAS Photo Bull., 1, 15.Google Scholar
Butler, C.J., 1972. The Irish AJ., 10, 251.Google Scholar
Garcia-Pelayo, J.M. and Alfaro, E.J., 1982. Rev. Mexicana Astron. Astrophys., 5, 167.Google Scholar
Vladimirov, S.B., 1978. Astron. Tzirc., 980, 4.Google Scholar