Messenger No. 53 (September 1988)
Active optics: the NTT and the future.
Wilson, R. N.; Franza, F.; Giordano, P.; Noethe, L.; Tarenghi, M.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO)
At a press conference on 13 July at Garl Zeiss, Oberkochen, jointly organized by ESO and Garl Zeiss, the final results of the manufacture (figuring) of the ND optics were announced. This included a functional test of the basic Active Optics correction of the telescope. The results were so good that they exceeded even the expectations Qf both Garl Zeiss and ESO in all respects. We consider this to be a milestone not only in the development of the ND and the history of ESO, but also in the evolution of the astronomical reflecting telescope in general.
 Wilson, R. N., Franza, F., Noethe, L., 1987,
"Active Opties I", ESO Preprint No. 484
and Journal of Modern Optics 34 (4),
 Noethe, L., Franza, F., Giordano, P., Wilson,
R. N., Citterio, 0., Conti, G., Mattaini,
E., 1987, "Active Opties 11", ESO Preprint
No. 560, accepted for publieation in Journal
of Modern Optics.
 Franza, F., Le Luyer, M., Wilson, R.N.,
1977, "3.6-m Telescope: The Adjustment
and Test on the Sky of the PF Optics with
the Gascoigne Plate Correctors", ESO
Technical Report No. 8.
 Wilson, R. N., Noethe, L., 1988, "Mirrors
and Supports", Proe. ESO Conf. on "Very
Large Telescopes and their Instrumentation",
Garching, March 1988, to appear
ESO Places Contract for World's Largest Mirror Blanks
The 3rd ESO/CERN Symposium.
Report on a symposium on 'Astronomy, cosmology and fundamental physics', held 16 - 20 May 1988 at Bologna, Italy.
List of ESO Preprints (June-August 1988)
592. P. Bouehet et al.: Infrared Photometry and Speetrophotometry of SN 1987A: March to Oetober 1987 Observations. Astronomy and Astrophysics.
Seeing measurements with a differential image motion monitor.
Pedersen, H.; Rigaut, F.; Sarazin, M.
AA(ESO) AB(ESO) AC(ESO)
Seeing is possibly the most important parameter describing a ground-based astronomical observatory. Under conditions of good seeing, an aberration-free telescope will produce sharp and bright images. The astronomer can then explore the universe to greater depths than otherwise possible. In recent years, a considerable amount of theoretical and experimental seeing studies have been conducted. The action of the earth's atmosphere on the quality of astronomical observations is now understood in quite some detail, and it has also become possible to measure the prevailing seeing, without the use of large and very expensive telescopes. This is obviously of great interest in the search for new observatory sites.
Visiting Astronomers (October 1988 - April 1989)
The first ESO-OHP school in astrophysical observations blessed by clear skies!
Chalabaev, A.; D'Odorico, S.
AA(Observatoire de Haute-Provence, C. N. R. 5., France) AB(ESO)
In the last decades. the search for better conditions for astronomical observations as weil as the need to cover the southern sky ted many countries to develop observatories at relatively remote sites. Among many positive consequences, this move also has a negative one. Because of the cost of travelling, the training of European students in astronomy is too often limited to data reduction or. if the students are sent overseas, they lack the guidance of a senior astronomer during their first observing run. As a consequence, sophisticated and expensive facilities are often not used in the most efficient way, since the gathering of accurate and reliable data in a minimum of telescope time while not an impossible art to learn quickly - greatly benefits from experience.
List of courses
20th General Assembly of the International Astronomical Union.
Following the earlier lAU General Assemblies in Montreal (1979), Patras (1982) and Oelhi (1985). the XXth IAU GA was held in Baltimore, Maryland, USA, from 2-11 August 1988. This was the first time in the United States since 1961. About 2,000 participants listened to more than 1,000 talks during more than 250 sessions, organized by 40 IAU Commissions. In addition, there were three Invited Oiscourses and seven oneday Joint Oiscussions. A full report will appear in the IAU Transactions and Highlights. In the meantime, and for the benefit of those Messenger readers who were not present, here is a small selection of items from the GA. They were mostly written by participating ESO astronomers at the editor's request and should only be regarded as personal reflections, culled from the enormous information flow. Others are adapted from the excellent daily newspaper, IAU Today and unsigned notes are by the editor.
Comparison of astronomical journals.
Pottasch, S. R.; Praderie, F.
AA(Editors of "Astronomy andAstrophysics") AB(Editors of "Astronomy andAstrophysics")
At the request of the Board of Oirectors of Astronomy and Astrophysics (AA), we have undertaken a comparison of the more important astronomical journals. The original reports covered the amount of material published, financial aspects, time delays in publication, aspects of refereeing and rejection of articles and the very difficult question of the overall scientific quality. Because of the general interest among astronomers in publishing and publications we have prepared this summary of the reports. Some of the information used has been supplied by Or. H. Abt, editor of the Astrophysical Journal (ApJ) and Prof. R.J. Tayler, editor of the Monthly Notices of the Royal Astron. Soc. (MNRAS). We have limited our comparison mainly to the three journals mentioned, plus the Astronomical Journal (AJ).
On the nature of the bars of SB0 galaxies - First results
Jarvis, B. J.; Dubath, P.; Martinet, L.; Bacon, R.
AA(Geneve, Observatoire, Sauverny, Switzerland), AB(Geneve, Observatoire, Sauverny, Switzerland), AC(Geneve, Observatoire, Sauverny, Switzerland), AD(Lyon, Observatoire, Saint-Genis-Laval, France)
Two-dimensional surface photometry in the Gunn-Thuan (1976) photometric system has been conducted for the five face-on southern SB0 galaxies NGC 1291, 1543, 1574, 4477, and 4754, together with the rotation velocity and velocity dispersion profiles along their principal axes. The complexity of the SB0 galaxies is considerable, as evidenced by the large variations noted in such observable parameters as their amounts of rotation, their asymmetry of rotation, and their velocity dispersion profile slope.
Betloni, D., Galletla, G.: Astron. Astrophys,
Botlema, R.: 1988, Astron. Astrophys. 197,
Gunn, J.E., Thuan, T.X.: 1976, Publ. Astron.
Soc. Pac. 88, 543.
Jarvis, B.J., Dubath, P.: 1988, Astron. Astrophys.
Let/. In press.
Jarvis, B.J., Dubath, P., Martinet, L., Bacon,
R.: 1988, Astron. Astrophys. Suppl. In
Kormendy, J., IIlingworth, G.: 1982, Astrophys.
J. 256, 460 (KI).
Kormendy, J.: 1983, Astrophys. J. 275, 529.
Longo, G., de Vaucouleurs, A.: 1983, A General
Catalogue of Photoelectric Magnitudes
and Colors in the U, B, V System of
3,578 Galaxies Brighter than the 16th magnitude
(1936-1982), University of Texas at
Longo, G., de Vaucouleurs, A.: 1985, Supplement
to the General Catalogue of Magnitudes
and Colors of Galaxies in the U, B,
V System, Dept. of Astronomy, University
of Texas at Austin.
Sargent, W. L. W., Schechter, P. L., Boksenberg,
A., Shortridge, K.: 1977, Ap. J. 212,
Tonry, J., Davis, M.: 1979, Astron. J. 84,
de Vaucouleurs, G.: 1975, Astrophys. J.
Suppl. Sero 29, 193.
Tentative Time-table of Council Sessions and Committee Meetings
The most massive LMC star Sk-66 deg 41 resolved
AA(European Southern Observatory, Garching, Federal Republic of Germany)
Sk-66 deg 41 is not a single star, but a compact cluster of at least six components with important implications for star formation theories and the distance scale in the universe. It is presently noted to constitute substantial evidence against the existence of stars possessing more than 100 solar masses, in view of recently obtained CCD images in B, V, and R. The possible multiplicity of sample stars in published catalogs will alter the shape of the upper part of the initial mass function.
Appenzeller, I.: 1970, Astron, Astrophys. 5,
Cassinelli, J. P., Mathis, J. S., Savage, B, D.:
1981, Science, 212, 1497.
Choisi, C., Nasi, E., Sreenivasan, S, R.: 1978,
Astron. Astrophys, 63, 103.
Clarke, J. N., Little, A. G., Mills, 8. Y.: 1976,
Australian J. Phys. Astrophys, Suppl, 40, 1.
Cohen, R., Montani, J., Rubio, M.: 1984, in
Structure and Evolution of the Magellanic
Clouds, IAU Sympos. 108, eds. S. van den
Bergh, K. S. de Boer, p. 401.
de Vaucouleurs, G,: 1978, Astrophys. J. 224,
Feitzinger, J. V., Schlosser, W., Schmidt-Kaler,
Winkler, Ch.: 1980, Astron. Astrophys,
Henize, K.G.: 1956, Astrophys, J. Suppl.
Series 2, 315.
Heydari-Malayeri, M., Testor, G.: 1983, Astron.
Astrophys. 118, 116.
Heydari-Malayeri, M" Testor, G.: 1985, Astron.
Heydari-Malayeri, M" Niemela, V.S., Testor,
G.: 1987, Astron. Astrophys. 184, 300
Heydari-Malayeri, M., Magain, P., Remy, M.:
1988, Astron. Astrophys. Letters, in press
Hubble, E.: 1926, Astrophys, J. 64, 321,
Humphreys, R. M.: 1983, Astrophys. J. 269,
Humphreys, R. M., McElroy, D.B,: 1984, Asuophys,
J, 284, 565.
Kahn, F.D.: 1974, Astron. Astrophys. 37, 149.
Kahn, F.: 1975, in Atomic and Molecular Physics
and the Interstellar Matter, eds. R.
Salian, P. Encrenaz, J. Lequeux, North
Holland, Amsterdam, p. 533.
Kurucz, R. L.: 1979, Astrophys. J. Suppl.
Larson, R. S., Starrfield, S.: 1971, Astron. Astrophys.
Maeder, A.: 1980, Astron. Astrophys. 92, 101.
Maeder, A.: 1983, Astron. Astrophys. 120,
Maeder, A.: 1985, Astron. Astrophys. 147,
Magain, P.: 1988, in preparation.
Meinei, E. S.: 1986, SPIE, Instrumentation in
Astronomy 627, 715.
Melnick, J.: 1983, The Messenger, 32, 11.
Moffat, A.F.J., Seggewiss, W.: 1983, Astron.
Sandage, A.: 1986, in Luminous Stars and
Associations in Galaxies, lAU Sympos.
116, eds. C.W.H. de Loore et al., p. 31.
Sanduleak, N.: 1969, Cerro-Tololo-InterAmerican
Obs. Contr. 89.
Stift, M. J.: 1982, Astron. Astrophys. 112,
Vangioni-Flam, E., Lequeux, J., Maucherat-
Joubert, M., Rocca-Volmerange, S.: 1980,
Astron. Astrophys. 90, 73.
Walborn, N. R.: 1973, Astrophys. J. 179, 517.
Walborn, N. R.: 1984, in Structure and Evolution
of the Magellanic Clouds, lAU Sympos.
108, eds. S. van den Sergh, K. S. de
Soer, p. 243.
Weigelt, G., Saier, G., Ladebeck, R.: 1985,
The Messenger 40, 4.
Weigelt, G., Ebersberger, J.: 1986, Astron.
Astrophys. 163, L5.
Woolley, R. v. d. R.: 1963, Roy. Obs. Bull.
Age and star formation of the radio galaxy 0902+34 at redshift z=3.395 - Constraints for primeval galaxies
AA(CNRS, Institut d'Astrophysique, Paris; Paris XI, Universite, Orsay, France)
It is presently calculated that the best star formation rate yielded by evolutionary models for explaining the emission of the radio galaxy 0902+34 in the K band is an intense burst which began 3 Gyr earlier and persisted for 1 Gyr. An additional present (galaxy frame) burst of 0.1 Gyr explains the V, and partly accounts for the I emission. The dominant stellar component emitting in the K band is on the Asymptotic Giant Branch.
Bruzual, G., 1983, Aslrophys. J., 273, 105.
Cowie, L. L., preprint.
Djorgovski, S., Spinrad, H., Marr, J., 1984,
New Aspecis of Galaxy Pholomelry, Ed.
J. L. Nieto, Editions Springer-Verlag,
Dunlop, J., Longair, M., 1987, High Redshift
and Primeval Galaxies, Ed. J. Sergeron, D.
Kunth, S. Rocca-Volmerange, Tran Thanh
Van, Ed. Frontie2res, p. 93.
Guiderdoni, S., Rocca-Volmerange, S., 1987
(GRV), Aslron. Aslrophys., 186, 1.
Guiderdoni, S., Rocca-Volmerange, B.,
1988a, Aslron. Aslrophys. Suppl. Series,
Guiderdoni, S., Rocca-Volmerange, S., Proceedings
of The Epoch of ihe Galaxy Formation,
Durham, July 1988.
Gunn, J., Stryker, L., 1983, Aslrophys. J.
Suppl. Series, 52, 121.
Larson, R., Slarburst Galaxies, Ed. 1. Montmerle
and T. X. Thuan, Tran Thanh Van,
Editions Frontieres, p. 467.
Lilly, S., 1988, preprint.
Lilly, S., Longair, M., 1984, M.N.R.A.S., 211,
Rocca-Volmerange, B., 1988, M.N.R.A.S., in
Rocca-Volmerange, B., Guiderdoni, S.,
1988a, High Redshift and Primeval Galaxies,
Ed. J. Bergeron, D. Kunth, B. RoccaVolmerange,
Tran Thanh Van, Ed. Frontieres,
Rocca-Volmerange, S., Guiderdoni, B. (RVG),
1988b, Aslron. Astrophys., Suppl. Series,
Rocca-Volmerange, S., Guiderdoni, B.,
1988c, Proceedings of The Epoch of lhe
Galaxy Formation, Durham, July 1988.
Rocca-Volmerange, B., Lequeux, J.,
Maucherat-Joubert, M., 1981, Astron. Astrophys.,
Scalo, J. M., 1986, Fundamental of Cosmic
Physics, 11, 1.
Spinrad, H., 1988, Proceedings of The Epoch
of lhe Galaxy Formation, Durham, July
Spinrad, H., Fillipenko, A. V., Wyckoff, S.,
Stocke, J.T., Wagner, R. M., Lawrie, D. G.,
1985, Astrophys. J., 299,17.
Stasinska, G., 1984, Astron. Astrophys.
Suppl. Series, 55, 15.
Tyson, A., 1988, preprint.
Comet Halley is Still Active
CCD photometry of globular clusters
AA(Instituto Isaac Newton, Santiago, Chile)
A CCD with 512 x 320 pixels was used to obtain BVRI frames lasting from a few sec to several min for several globular clusters in order to cover the full range of magnitudes without image saturation. The reductions of these images were accomplished with the MIDAS/INVENTORY software, which uses point-spread function techniques. Precise color equations are established for the CCD telescope system, on the basis of 140 BVRI frames and a total of 40 standard stars with a wide color range.
Search for faint nearby stars
Ruiz, M. T.; Maza, J.; Mendez, R.; Wischnjewsky, M.
AA(Universidad de Chile, Santiago), AB(Universidad de Chile, Santiago), AC(Universidad de Chile, Santiago), AD(Universidad de Chile, Santiago)
The possibility that the 'missing mass' in the solar neighborhood may be accounted for by the existence in sufficiently great numbers of such very low mass stars as brown dwarfs, as well as very old dead stars now observable as cold, low-luminosity degenerates, is presently addressed observationally with a search through ESO R Survey plates using a stereocomparator. Attention is given to ESO area 439, where four low-luminosity degenerates have been discovered by the present study.
D'Antona, F. and Mazzitelli, I., 1986, Astron.
Astrophys., 162, 80.
Eggen, 0.,1984, A.J., 89,1350.
Elmegreen, B.G., 1983, "IAU Coll. N° 76", ed.
A. G. D. Philip and A. R. Upgren, p. 235.
Liebert, J., Dahn, C. C. and Monet, D. G.,
1988, Ap. J. (Sept. 1 issue).
Luyten, W.J., 1979, "LHS Catalogue", University
A search for magnetic fields in blue stragglers of M 67
AA(Geneve, Observatoire, Sauverny, Switzerland)
An observational program has been conducted for the blue straggler stars of the galactic cluster M 67, in order to test the hypothesis that they are quasi-homogeneously evolved stars. Abundances have been determined for C, N, and O to ascertain whether they have standard main sequence values or values typical of CN-equilibrium; attention is given to evidence for the presence of two agents that may be responsible for a mixing of the stellar interior, namely rapid rotation and magnetic field. It is concluded that large scale-organized magnetic fields do not appear to be responsible for the blue straggler phenomenon in old open clusters.
Abt, H.A.: 1985, Astrophys. J. Letters 294,
Babcock, H.W.: 1960, in Stellar Atmospheres,
J. L. Greenstein (Ed.), University
01 Chicago Press, Chicago, p. 282.
Duran, C.M., Graziati, L.S.: 1986, in New
Insights in Astrophysics, ESA SP-263,
Maeder, A.: 1987, Astron. Astrophys. 178,
Mathys, G., Stenflo, J.O.: 1986, Astron. Astrophys.
Mathys, G., Stenflo, J.O.: 1988, in The Impact
of Vel)l High SIN Spectroscopy on
Stellar Physics, lAU Symp. No. 132, G.
Cayrel de Strobel and M. Spite (Eds.),
Kluwer, Dordrecht, p. 317.
Pendl, E.S., Seggewiss, W.: 1976, in Physics
of Ap Stars, lAU Coll. No. 32, W. W. Weiss,
H. Jenkner and H. J. Wood (Eds.), University
of Vienna, p. 357.
First Announcement: A Workshop organized by ESO on Low Mass Star Formation and Pre-main Sequence Objects
Molecular probes of the cosmic background radiation.
In the late 1930's observers at the Mount Wilson observatory using the 100-inch telescope and the Coude Spectrograph discovered absorption lines of the interstellar molecules CH, CH', and CN. In the case of CN, an absorption line from an excited rotational state in addition to the ground rotational state was also seen. In fact, an excitation temperature of about 2.3 K was deduced, but the connection to cosmology and the cosmic background radiation was not realized. The full significance of these observations only became obvious in 1964 when the cosmic background radiation (CBR) was finally discovered using radiometers, and found to have a temperature of about 3.1 K.
Blades, J.C., 1978, M.N.R.A.S. 185, 451.
Crane, P., Hegyi, D.J., Mandolesi, N., and
Danks, A.C. 1986, Ap. J. 309, 1.
Crane, P., and Hegyi, D.J., 1988, Ap. J. (Letters),
Matsumoto, T., Hayakawa, S., Matsuo, H.,
Murakami, H., Sato, S., Lange, A.E., and
Richards, P.L., 1988, Ap. J. 329, 567.
Smoot, G.F., Bensadoun, M., Bersanelli, M.,
Oe Amici, G., Kogut, A., Levin, S., and
Witebsky, C., 1987, Ap. J. (Letters),3137,
Thaddeus, P. 1972 Ann. Rev. Astron. and
Astrophys., 10, 305.
The abundance of manganese in halo stars.
Gratton, R. G.
AA(Osservatorio Astronomico di Roma, Italy)
The chemical composition of halo stars provides primary data about the nucleosynthesis processes that built up the metals present in young stars and in the interstellar medium. Theoretical information about the basic mechanisms of metal production are rather scarce. We know that only a tiny amount of metals was produced during the Big Bang; and we think that most of the heavy elements presently observed were manufactured in massive stars, or in intermediate-mass binaries, exploding as supernovae. However, the relative role of type I und type I1 (and/or type II b) supernovae is quite unknown. Furthermore, we do not know precisely the composition of the ejecta of such supernovae. Therefore, empirical data are still at the basis of an interpretation of the chemical evolution of our Galaxy.
Barbuy, B.: 1988. Astron. Astrophys. 191,
Beynon, T.G. R.: 1978. Astron. Astrophys. 64,
Booth, A.J., Shallis, M.J., Wells, M.: 1983.
Monthly Not. Roy. Astron. Soc. 205, 191.
Booth, A.J., Blackwell, D.E., Petford, A.D.,
Shallis, M.J.: 1984. Monthly Not. Roy. Astran.
Soc. 208, 147.
Francois, P.: 1988. Astron. Astrophys. 195,
Gratton, R. G.: 1988. In Stellar Evolution and
Dynamics of the Galactic Halo, M.
Azzopardi and F. Matteucci eds., ESO,
Gustafsson, B.: 1988. In Stellar Evolution and
Dynamics of the Galactic Halo, M.
Azzopardi and F. Matteucci eds., ESO,
Helfer, H. L., Wallerstein, G., Greenstein, J. L.:
1959. Astrophys. J. 129, 700.
Lambert, D.: 1987. J. Astrophys. Astron. 2,
Magain, P.: 1987. Astron. Astrophys. 179,
Matteucci, F.: 1988. In Stellar Evolution and
Dynamics of the Galactic Halo, M.
Azzopardi and F. Matteucci eds., ESO,
Sneden, C.: 1985. In Production and Distribution
of C, N and 0 Elements, J. Danziger,
F. Matteucci and K. Kjär eds., ESO, Garching,
Spite, M., Spite, F.: 1985. Ann. Rev. Astron.
Astrophys. 23, 225.
Zinn, R., West, M.J.: 1984. Astrophys. J.
Suppl. 55, 45.
Chemistry at high galactic latitudes - CH, CH(+) and CN absorption lines
van Dishoeck, E. F.; de Vries, C. P.
AA(California Institute of Technology, Pasadena), AB(Leiden, Rijksuniversiteit, Netherlands)
High latitude clouds have low visual extinctions similar to those of diffuse clouds, but their strong CO mm-emission is more typical of that found in dark clouds. An effort is presently made to ascertain whether the abundances of other simple molecules are enhanced in high latitude clouds, by searching for CH, CH(+), and CN molecular absorption lines in southern high latitude clouds. Attention is given to the comparative species concentrations of HD 210121, Zeta Oph, HD 169454, and HD 147889.
Andreani, P., Ferlet, R., lallement, R., and
Vidal-Madjar, A. 1988, The Messenger, 52,
Blitz, L. 1988, in "Structure 01 Galaxies",
Proc. 10th European Regional Meeting 01
the lAU, ed. J. Palous (Czech Academy 01
Sciences, Prague), p. 204.
Danks, A. C., Federman, S. R. and Lambert,
D. L. 1984, Astron. Astrophys. 130, 62.
Desert, F.X., Bazell, 0., and Boulanger, F.
de Vries, C. P. and Le Poole, R. 1985, Astron.
Astrophys., 145, L7.
de Vries, C.P. and van Dishoeck, E.F. 1988,
Astron. Astrophys., in press; and in preparation.
Hobbs, L. M., Blitz, L., and Magnani, L. 1986,
Astrophys. J (Letters), 306, L109.
Knapp, G. R., Drdla, K., and van Dishoeck,
E. F. 1988, in preparation.
Magnani, L., Blitz, L., and Mundy, L. 1985,
Astrophys. J, 295, 402.
Magnani, L., Blitz, L., and Wouterloot, J.G.A.
1988, Astrophys. J, 326, 909.
Mattila, K. 1986, Astron. Astrophys., 160,
van Dishoeck, E.F. and Black, J.H. 1988a,
Astrophys. J., submitted.
van Dishoeck, E. F. and Black, J. H. 1988 b, in
Rate Goefficients in Astrochemistry, eds.
T.J. Miliar and D.A. Williams (Kluwer, Dordrecht),
Evolutionary features in distant clusters of galaxies
Buzzoni, A.; Molinari, E.; Manousoyannaki, I.; Chincarini, G.
AA(Osservatorio Astronomico di Brera, Milan, Italy), AB(Osservatorio Astronomico di Brera, Milan, Italy), AC(CNR, Istituto di Fisica Cosmica, Milan, Italy), AD(Osservatorio Astronomico di Brera; Milano, Universita, Milan, Italy)
Observational results obtainable for high-redshift clusters of galaxies are found to contribute a quantity of meaningful constraints on the evolutionary status of the different hierarchical structures populating the universe in the present and in the past. It is found that the statistical analysis of the color-color diagram and of the luminosity function of clusters obtained via accurate multicolor photometry may furnish an effective method for (1) the discrimination of galaxy morphology, (2) the evaluation of intrinsic evolutions, and (3) the estimation of redshifts.
Buzzoni, A.: 1987, in Towards understanding
Galaxies at Large Redshifts, eds. R. G. Kron and A Renzini, (Dordrecht: Reidel), p.61.
Buzzoni, A: 1988, in preparation.
Butcher, H. and Oemler, A.: 1984, Ap. J., 285,
Coleman, G.D., Wu, C. C. and Weedman,
D. W.: 1980, Ap. J. Supp., 43, 393.
Couch, W.J. and Newell, E. B.: 1984, Ap. J.,
Couch, W.J., Ellis, R.S., Godwin, J. and Carter,
0.: 1983, MN.R.A.S., 205,1287.
Ellis, R. S., Couch, W. J., Maclaren, I. and
Koo, D.C.: 1985, MN.R.A.S., 217, 239.
Gunn, J. E., Hoessel, I. G. and Oke, J. B.:
1986, Ap. J., 306, 30.
Koo, D. C.: 1981, Ap. J. (Lett), 251, L 75.
Loh, E.D. and Spillar, E.J.: 1986, Ap. J., 303,
Maclaren, I., Ellis, R.S. and Couch, W.J.:
1988, MN. R. A. S., 230, 249.
Molinari, E.: 1988, Thesis dissertation, University
Rakos, K.D., Fiala, N., Schombert, J. M.:
1988, Ap. J. 328, 463.
Thuan, T.X. and Gunn, J.E.: 1976, P.A.S.P.,
Tinsley, B.M.: 1977, Ap. J. 211, 621.
Wade, R.A, Hoessel, I. G., Elisas, J. M. and
Huchra, J.P.: 1979, P.A.S.P., 91, 35.
West, R. M., Kruszewski, A: 1981, Irish Astran.
Trojan search at ESO.
Elst, E. W.
AA(Royal Observatory at Uccle, Belgium)
Doing minor planet research is sometimes considered a proof of bad taste among astronomers. It is a fact that asteroids, these rocky pieces between the orbits of Mars and Jupiter, have lost much of their interest, now that most of the larger ones have been catalogued: their orbits are weil known, their chemical structure has been studied and their rotation properties investigated. Hence, chasing the smaller kilometer-sized members does not seem a useful occupation. Indeed, why should they be different from the larger ones?
3.3-μm spectroscopy with IRSPEC.
Le Bertre, T.
IRSPEC is a cooled grating spectrometer in service at ESO since October 1986. It is equipped with a linear array of 32 InSb detectors and with two back-to-back-mounted gratings; in its present stage, it permits spectroscopy in the 1-5 um region at a spectral resolution (R = x/delta x) of 1,000 to 2,000, depending on grating, order and wavelength. A description of it and a report on its performances can be found in Moorwood et al. (1986).
Cohen, M., Tielens, A. G. G. M., Allamandola,
L.J.: 1985, Astrophys. J. 299, L 93.
Leger, A., Puget, J.-L.: 1984, Astron. Astrophys.
Martin, W.: 1987, Astron. Astrophys. 182,
Moorwood, A., Biereichei, P., Finger, G., Uzon,
J.-L., Meyer, M., Nees, W., Paureau,
J.: 1986, The Messenger, 44,19.
de Muizon, M., Geballe, T. R., d'Hendecourt,
L.B., Baas, F.: 1986, Astrophys. J. 306,
EMMI Grating Unit under Test
The photograph shows a grating unit of EMMI (ESO Multi-Mode Instrument, the optical-range spectrograph for one of the Nasmyth foci of the NTT) that is currently being tested in ESO's integration laboratory in Garching. The mechanical parts for this unit have been manufactured by Enraf-Nonius in the Netherlands using designs made by the ESO mechanics group. The concept and design had been successfully tested on a prototype in the fall of 1987. Two gratings are mounted back to back in the grating holder of which the angular position is servo-controlled. Selection of the central wavelength will be remotely controlled as weil as flipping the grating holder 180 degrees to select the other grating.
ESO Image Processing Group: MIDAS Memo
The table file system is being enhanced with a number of astrometric functions which will make it possible to perform full astrometric reductions in MIDAS. They include transformations between different coordinate systems, correction for epoch and equinox differences, and general astrometric reduction programmes. Reduction procedures for data from the Infrared Array Camera (IRAG) are being developed in collaboration with A. Moneti. Besides extensive use of the existing CCD package, some new programmes were made to optimize the extraction of data utilizing the special characteristics of IR array detectors.
'Remote' Control of the 1.52-m Telescope!
'Remote' Control of the 1.52-m Telescope!
My Visit to La Silla
The Director General of ESO, Harry van der Laan, invited me to La Silla as consultant during the realuminization and the optical trimming of the ESO Schmidt telescope. I was very happy with this invitation because it gave me an opportunity not only to spend some time at the Schmidt, but also to meet with many friends in Chile. At La Silla I had the good luck to meet Richard West who suggested to me to write a short contribution for the Messenger about my stay in Chile which I have done with pleasure.
Latest News: SEST Observes SN 1987A!
A supernova in AC 118 (Z = 0.31).
New ESO Publications