Stellar Paths: Photographic Astrometry with Long-Focus by Peter Van De Kamp (auth.)

By Peter Van De Kamp (auth.)

This is the newest attempt in a series of shows all started in 1949 with a sequence of lectures on long-focus photographic astrometry given through the writer as Fulbright professor in Paris on the invitation by means of the overdue H. Mineur, at the moment Director of the Institut d' Astrophysique. those past lectures have been released as a sequence of evaluate articles in renowned Astronomy (1951) and seemed either as Contributions de l'Institut d'Astrophysique, Serie A, No. eighty one and as reprint No. seventy five of Sproul Observatory. A extra problematic presenta­ tion used to be given in 1963 in Stars and Stellar structures, which used to be by way of rules of Astrometry (1967, W. H. Freeman & Co.). through the moment 1/2 1974, back lower than Fulbright auspices, on the invitation of Pik Sin The, I lectured on the Astronomical Institute in Amster­ dam, by means of a quick path in May-June 1978 on the invitation of E. P. J. van den Heuvel. I gave a extra vast path on the Institut d' As­ trophysique on the invitation of J. C. Pecker of the school de France and of J. Audouze, Director of the LA.P. either in Amsterdam and in Paris I had offered occasional astrometric issues at a variety of occasions. the chance to lecture in France and in Holland has facilitated, inspired and more advantageous the association and contents of the displays with reference to long-focus photographic astrometry.

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The standard frame is simply an idealized or fictitious standard plate to whose origin, scale and orientation all other plates in the series are reduced. , [xsJ = [Ys] = O. 8) STELLAR PATHS 23 All measured positions can now be reduced to the scale, orientation, and origin of the reference frame (x$> Ys) through plate constants a, b, and c, which are given by the linear equations of condition for each reference star; a"xs + b"ys + c" = + byYs + cy = Xs - x', ayxs Ys - y'. 11 ) where Xo and Yo are adopted values of X and Y.

It is obvious that [D] = 1, and, because of the least-squares procedure, that [D2] is a minimum. In the plate-constant method, X and Yare implicit functions of (x') and (y'); the dependence method provides an explicit expression. 14) may be written as follows: X = [Dxs] + X' - [Dx'], Y = [Dys] + Y' - [Dy']. 16) The position [Dx s], [Dysl defines a point close to the central star, which is rigorously corrected for plate constants and is called the dependence center; [Dx'] , [Dy'] is the measured dependence background.

Clearly this error affects parallax determinations based on declination measures only, and generally would lead to a slight increase in the parallax values from declination observations made in the northern hemisphere. , a parameter of the central star appears involved. Whether this parameter is color atJdjor location in the sky, or something else, is not clear at the moment. However, for a large number of parallax determinations at the Sproul Observatory on the average the declination results for parallax are only O~0018 ± O~OOII larger than the right ascension results, perhaps a reason for some guarded satisfaction (Lippincott, 1971).

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