Interpretation of the Paper Tape Output of the Worley Filar Micrometer

An investigation of the output of the Worley Filar Micrometer is presented.
This will insure that the ``paper trail'' of the data can be followed in the future.

Four observations of ADS 8119 (= HR 4374/4375 = STF 1523 = Xi Ursae Majoris) from Worley (1978) were selected. Observations from a single night are found on a single paper tape output. The last line of these dates is a six-digit number in a format yymmdd which gives the date of the observation. This is converted to the Besselian year, usually on the tape, and these correspond to a single entry.

Four observations were made of ADS 8119 in the Spring, 1974 observing season. Scans of these four outputs is provided in Figures 1-4 below.

Scans of the papertape outputs of (from left to right) : April 30, 1974 (1974.327), May 8, 1974 (1974.348), May 15, 1974 (1974.368) and May 22, 1974 (1974.387).

The output of an observation consists of at least twelve lines. Outputs for the twelve lines will be explained below:

Each four of these reduced measures is transferred to an index card (at right). for each target per season. These lines correspond almost exactly to the output seen in Worley (1978). Note that, in the case of the 1974.348 observation (which corresponds to Figure 2), the position angle (which was measured five times) is given a ``:'' indicating a measure of lesser quality. However, it does not seem to be weighted less in the determination of the mean. It is possible that were it significantly different from the other values that it may have been given lesser or zero weight. Finally, the mean is determined, and residuals are calculated from a published orbit [in this case, Heintz 1966 (actually 1967)]. The mean (which is actually comes from twelve measures) is the final value which is used in orbit determinations and is placed in the WDS.