By Alan H. Batten (auth.), D. S. Hayes, L. E. Pasinetti, A. G. Davis Philip (eds.)
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Additional resources for Calibration of Fundamental Stellar Quantities: Proceedings of the 111th Symposium of the International Astronomical Union held at Villa Olmo, Como, Italy, May 24–29, 1984
This fact circumscribed the choice of stars to be observed in this way. Whatever theoretical principles we may lay down, the stars we select as standards are to some extent dictated by what our instruments can do, and, even more strictly, by what we ourselves are prepared to do. Not many of us. are willing to take the time or the care to produce a high-resolution spectral atlas. Nevertheless, the selection of any kind of standard requires that kind of patient and not very glamorous work, if it is to be done properly.
That is a big advantage. ·At the DDO in Toronto, there is a complete grid of MK standards taken with each spectrograph, and for each dispersion, devel-, oper, slit width, and slit length combination. Then, for each observing run, the most important standards are re-observed and at least one standard is observed each night, just as a check on the stability of the equipment and processing techniques. Because of very careful attention to standardization of techniques, differences have only rarely been detected.
He made adjustments to the published errors in the parallaxes of each contributing observatory in order to more properly represent the true uncertainties in the data. Two independent methods were used for this purpose. In the first, the average difference without regard to sign was found from intercomparisons between the parallaxes of each observatory compared with every other observatory from which the external probable errors of each of the two series were estimated. The second method used differences between the trigonometric parallaxes of each observatory with spectroscopic parallaxes of the Mount Wilson Observatory.