The Star is in Histoire Céleste, p. 290, B. Transit at 17h.8m.32. To reduce these observations, it is necessary to allow for the differences of refraction in right ascension and declination, and also for the proper motion of the Comet. This proper motion was obtained, wherever it was possible, from the observations themselves where this could not be done, as in the case of single observations, I made use of Mr Stratford's Ephemeris. Having applied these differences to the places of the respective stars, as given in the accompanying Catalogue, I have obtained the apparent places of the Comet for the respective times of observation; and then applying the proper correction for parallax, I have got the geocentric places. In calculating the parallax, the Comet's distance from the Earth was deduced from Mr Stratford's Ephemeris. |