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Trojan Search at ESO E Lf) provide an effective method (a) to dis­ Kron and A Renzini, (Dordrecht: Reidel), o criminate galaxy morphology, (b) to p.61. evaluate their intrinsic evolution and (c) Buzzoni, A: 1988, in preparation. Butcher, H. and Oemler, A.: 1984, Ap. J., 285, to estimate redshift with an accuracy of 426. 0.05. We emphasize that two main ± Coleman, G.D., Wu, C. C. and Weedman, ...--...0 requirements have to be fulfilled in order Q() D. W.: 1980, Ap. J. Supp., 43, 393. <\l to reach such a fair resolution in explor­ Couch, W.J. and Newell, E. B.: 1984, Ap. J., E ing the universe at large distances: 56,143. '-' <J Lf) (i) we need to observe clusters instead Couch, W.J., Ellis, R.S., Godwin, J. and Car­ o o of field galaxies to be able to recognize ter, 0.: 1983, MN.R.A.S., 205,1287. them with high statistical confidence; Ellis, R. S., Couch, W. J., Maclaren, I. and (ii) we need a combined comparison Koo, D.C.: 1985, MN.R.A.S., 217, 239. 2158+0351 Gunn, J. E., Hoessel, I. G. and Oke, J. B.: with evolutionary models, in order to 1986, Ap. J., 306, 30. properly account for the intrinsic photo­ Koo, D. C.: 1981, Ap. J. (Lett), 251, L 75. 0.4 0.5 metric properties as we use galaxies as Loh, E.D. and Spillar, E.J.: 1986, Ap. J., 303, REDSHI8 T standard candles in the cosmological 154. Figure 8: The photometrie determination of framework. Maclaren, 1., Ellis, R.S. and Couch, W.J.: the redshift of the cluster 2158 + 0351. Dis­ Such an approach is also preparatory 1988, MN. R. A. S., 230, 249. played is the merit funetion whieh minimizes to more detailed studies using the new Molinari, E.: 1988, Thesis dissertation, Uni­ the differenee between the eolours (g-r) and generation telescopes (VLT) and will be versity of Milan. (g-i) of the elliptieal galaxies deteeted and complemented by deep surveys on Rakos, K.D., Fiala, N., Schombert, J. M.: 1988, Ap. J. 328, 463. those predieted by the evolutionary model of selected fields possibly supported by Figure 7. Thuan, T.X. and Gunn, J.E.: 1976, P.A.S.P., spectrophotometric work. 88,543. Tinsley, B.M.: 1977, Ap. J. 211, 621. Wade, R.A, Hoessel, I. G., Elisas, J. M. and our diagram and of the luminosity func­ References Huchra, J.P.: 1979, P.A.S.P., 91, 35. tion of the clusters obtained via an Buzzoni, A.: 1987, in Towards understanding West, R. M., Kruszewski, A: 1981, Irish As­ accurate multicolour photometry may Galaxies at Large Redshifts, eds. R. G. tran. J., 15,25. Trojan Search at ESO E. W. ELST, Royal Observatory at Uccle, Belgium Doing minor planet research is some­ Lagrange (1736-1813), however, has motion of a Trojan is very complex, it will times considered a proof of bad taste shown that there is a solution in the not remain constantly at ~ or Ls; small among astronomers. It is a fact that special case that the three bodies (Sun, changes from the triangular configura­ asteroids, these rocky pieces between larger planet, asteroid) are moving in a tion will result in oscillations around the orbits of Mars and Jupiter, have lost fixed plane at equal distances from each these points. The theory of predicting much of their interest, now that most of other (triangular configuration). It is the larger ones have been catalogued: assumed that the mass of the third body their orbits are weil known, their chemi­ (the asteroid) is negligible (Fig. 1). cal structure has been studied and their The first object of this kind was found rotation properties investigated. Hence, in 1906 at the Observatory of Heidel­ chasing the smaller kilometer-sized berg. The discoverer was the famous members does not seem a useful occu­ Max Wolf, and for some reason, he pation. Indeed, why should they be dif­ called his newly discovered asteroid ferent from the larger ones? "Achilles", after the herD from the Trojan I got engaged in asteroidal work in war. May 1986 (first GPO mission at ESO). With the discovery of Achilles, a Since that time my interest in asteroids theoretical problem found an observa­ has grown rapidly. In March 1988 I tional confirmation. Since then, more ?+_-1- ---t'lJu pltor attended the "Asteroids 11" conference minor planets have been found at the in Tucson, Arizona. There I was really so-called libration point ~ and Ls and all impressed by the wealth of possibilities have been called after the heroes of in the field of minor planet research. Homer's lIias. My primary interest are the Trojan as­ It is interesting to note that we find teroids, these objects that are describ­ only "real" Trojans (Priamus, Aeneas, ing their orbits at a mean distance of 5.2 Anchises ...) at the libration point Ls A. U. from the Sun, i. e. at the 1 : 1 com­ (preceding point) and Greeks (Achilles, mensurability with Jupiter. Nestor, Agamemnon ...) at L4 (following It is known from celestial mechanics point). This is of course a consequence that the problem of three bodies does of the appropriate naming convention. not, in general, admit a finite solution in However, one Trojan (Hector) is at L4 terms of known functions. Joseph Louis and one Greek (Patroclus) at Ls. The Figure 1: Triangular eonfiguration. 53 JUPiTER 0.034 A. U.). It means that 1987 SB has I I I o 5 possibilities of close encounters to these planets, wh ich makes it rather , "dangerous" on long terms. The diame­ 40\... \ - ter is of the order of 2.5 km (/'As­ I tronomie, May 1988, p. 192). I could re­ o I cover the object on a plate taken by 30 r-----!_ _- C HUngarfao-- - Oscar Pizarro with the ESO-Schmidt in ~ PhO~~':-:- o November 1987. 0 0 I SUN nl 20 I- I "'.... - ... Other interesting objects (from the cl" I/ point of view of resonance studies) are U 0 I/ the Phocaea objects (1987 BO, dis­ c 10 r- 'I ­ covered at ESO; 1987 CR, discovered at I I Haute-Provence), and the Hungaria ob­ ~ r III jects (1988 BJ, discovered at Haute­ 2.0 2.5 3.0 3.5 Figure 2: Oscillation zones around the libra­ Provence, 1988 CR and 1988 CM , dis­ Semimajor Axis (AU) tion points. 3 covered at ESO; 1 prediscovery at the Figure 3: The Hungaria and Phocaea as­ Bulgarian National Observatory at teroids. the exact oscillation amplitudes and fre­ Rozhen: 1987 SJ 3) (Fig. 3). quencies is difficult, and much work has The positions of the Hungaria object the piano the suite "Asteroid 192". The still to be done (Fig. 2). Observation and 1987 SJ3 were sent too late to the Minor Trojan hero Odysseus, I have com­ discovery of new Trojans is therefore Planet Center and E. Shoemaker at memorated in the "Odysseus suite". The highly important. Mount Palomar got away with it (even first performance of the Nausikaa suite Since the mean distance from the Sun when he discovered it 4 days later), but took place in September 1986, at the is about 5.2 A. U., the mean motion of a that's part of the game. town of Plovdiv (Bulgaria), not far away Trojan is almost 1/3 of the mean motion from the Greek border, before a small of main belt asteroids. In order to detect audience of Bulgarian astronomers. The Music tor Asteroids their trails on the GPO plates, it is there­ Odysseus suite, I played for the first fore necessary to expose them much Nausikaa, the lovely person from the time at the home of Dr. R. Binzel, Tuc­ longer which is rather time consuming. Odyssey, inspired me to compose for son (Arizona), in March 1988. Another way to discover them is by tak­ ing two plates in succession. Blinking of the plates may then reveal the unknown objects. I must confess that I do not under­ stand why asteroidal research has such a bad quotation among astronomers. During the last two years since I got involved in this kind of work, this occu­ pation grew out to a real passion. The "infinite minor planet game" of Kohoutek became for me a most fas­ cinating reality (see below). From the point of view of observation­ al work I may mention the following: in 1986 I discovered the Trojan object 1986 VG, at the observatory of Haute­ Provence and in 1987 at ESO the Trojan objects 1987 ON, 1987 YT, and 1987 YU,. But there are more interesting ob­ jects. In September 1986, I observed the long lost planet Nolli (473) at the Bulga­ rian National Observatory. Since it was not recognized as such, it received from the Minor Planet Center in Massachu­ setts a new provisional designation (1986 PP4 ). In September 1987, I discovered the Apollo object 1987 SB in collaboration with the Bulgarian astronomers at Rozhen. The object was followed at var­ ious observatories up to the 15th of January 1988. This object (a = 2.20 A. U.) is characterized by a very high excentricity (e = 0.66) and a low inclina­ tion (i = 3°). It therefore can approach three planets to within less than 0.050 A. U.: Venus (0.023 A. U.), Earth (0.045 and 0.052 A. U.) and Mars (0.019 and Figure 4: The Phocaea asteroid 1987 BOI, discovered at ESO (January, 22, 1987). 54.
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