According to WolfR., Geschichte der Astronomie (Munich, 1877), 420–1, this is Petrus Theodori of Emden (Pieter Dircksz Keyser, d. 1596 near Java), who appears to have been responsible for forming some, if not all, of these constellations. A catalogue of the stars in the twelve southern constellations taken from Bayer's “last tables and manuscripts” by Jacob Bartsch is given by Kepler as the stars of the Third Class in the Rudolphine tables in Kepler, Gesammelte Werke, x, ed. by HammerF. (Munich, 1969), 138–41. Other new constellations, such as Columba, made up of previously unformed stars just south of Canis Major, and Crux, formed of four stars in Centaurus, appear on plates in the Uranometria, but are not distinguished in Kepler's catalogue. For a general description of constellations in early star atlases, see WarnerD. J., The sky explored: Celestial cartography 1500–1800 (New York, 1979).
2.
This is the only detailed analysis of the Uranometria.Wolf, Geschichte der Astronomie, 423–25, DelambreJ. B. J., Histoire de l'astronomie moderne (Paris, 1821), ii, 181–5, and Warner, The sky explored, 18–20, may also be consulted.
3.
The catalogue from the Progymnasmata is in Tychonis Brahe Dani Scripta astronomica, ed. by DreyerJ. L. E., ii (Copenhagen, 1915), 258–80, the catalogue of 1598 in ibid., iii (Copenhagen, 1916), 344–73, and the catalogue from the Rudolphine tables in Kepler, op. cit. (ref. 1), 105–29.
4.
This is the way the stars of the Second Class, the so-called Semi-Tychonic stars, were located in the catalogue in the Rudolphine tables in Kepler, ibid., 130–7. Here, of course, Argelander's conclusion is valid since it shows that, taken as a group, the non-Tychonic stars of Scorpio cannot be made to agree with the Tychonic stars by adding any constant of precession.
5.
Clavius, Opera mathematica, iii (Mainz, 1611), 76–97 with the explanation on p. 98, although Bayer of course used an earlier edition.
6.
Argelander found that the stars of Canis Major not taken from Tycho were 21;6° ahead of Ptolemy, and adding to this 6;40°, the longitude of γ Arietis in Ptolemy's catalogue, gives 27;46°, very close to the Copernican precession indeed. However, in our own measurements of the stars of Canis Major, to be taken up below, we did not find a systematic difference of 21;6° from Ptolemy's longitudes, which would give a difference of 0;11° from Schoener's.
7.
A single exception is the Southern Crown for which an addition of 0;30° seems likely, although there are differences, presumably errors, in the locations of γ and θ amqunting respectively to — 0;30° and +0;30° in longitude, and +1° and −2° in latitude.
