Messenger No. 38 (December 1984)

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1-2 (PDF)
D. Enard
Visit of STC to Possible Sites for the Very Large Telescope / VLT / in Northern Chile

ADS BibCode:
1984Msngr..38....1E
Author(s)/Affiliation(s):
Enard, D.
AA(ESO)
Abstract:
The STC (Seientifie Teehnieal Committee) met at La Silla the 8th and 9th of October. Following the meeting, a 3-day-long trip to northern Chile brought the STC members (Fig. 1) to and above a few sites whieh have been picked up as potentially interesting spots by A. Ardeberg during his exploratory survey of 1983/84.
2-6 (PDF)
N. Bergvall, K. Olofsson
Blue compact galaxies - Infants of the Universe?

ADS BibCode:
1984Msngr..38....2B
Author(s)/Affiliation(s):
Bergvall, N.; Olofsson, K.
AA(Astronomiska Observatoriet, Uppsala, Sweden), AB(Astronomiska Observatoriet, Uppsala, Sweden)
Abstract:
The blue light of blue compact galaxies (BCGs) is a consequence of their high proportion of young stars. Their compact appearance is due to relatively small dimensions and high surface brightness, which produce overexposed images on photographic survey plates. The IR image of the BCG ESO 338-IG04, however, exhibits regular isophotes reminiscent of an old galaxy, as well as a luminosity profile typical of old stellar systems. The assumption that these galaxies are indeed young is presently tested through a synthesis of their color evolution as a function of time, followed by a comparison of these results with observations. It is concluded that the possibility that a large portion of the mass of BCGs may take the form of old stars cannot be ruled out.
6-8 (PDF)
B. Marano et al.
A complete optical survey of candidate quasars down to B = 22.0 with the ESO 3.6 M telescope

ADS BibCode:
1984Msngr..38....6M
Author(s)/Affiliation(s):
Marano, B.; Zitelli, V.; Zamorani, G.
AA(Bologna, Universita, Bologna, Italy), AB(Bologna, Universita, Bologna, Italy), AC(CNR, Istituto di Radioastronomia, Bologna, Italy)
Abstract:
The first of the two primary methods that have been successfully applied to the optical selection of quasars, the 'ultraviolet excess' method, is based on the observational evidence that nearly all known quasars with redshift lower than 2.2 show U-B of less than 0.40. The second method involves the search for emission line objects and/or objects with blue continuum on deep 'grism' plates; nearly all radio-quiet quasars with redshift larger than 3 have been found by this technique. The characteristics of the two methods are such that they are most effective when simultaneously applied on the same field. Presently given is a still-preliminary account of the optical search for faint quasars that is being performed with the European Southern Observatory's 3.6-m telescope.
References:
Bonoli, F., Braccesi, A., Marano, B., Merighi, R. and Zitelli, V.: 1980,
Astronomy and Astrophysics, 90, L10.
Braccesi, A., Zitelli, V., Bonoli, F. and Formiggini, L.: 1980, Astronomy
and Astrophysics, 85,80.
Clowes, R. G.: 1981, M.N.RAS., 197, 731.
Cristiani, S.: 1984, The Messenger, 35, 13.
Koo, D. C.: 1983, Proceedings 24th Liege International Astrophysical
Symposium on "Quasars and Gravitational Lenses", p. 240.
Koo, D.C. and Kron, R. G.: 1982, Astronomy and Astrophysics, 105,
107.
Kron, R. G.: 1980, Astrophysical Journal Suppl., 43, 305.
Setti, G., and Woltjer, L.: 1982, "Astrophysical Cosmology", Proceedings
of the Vatican Study Week on Cosmology and Fundamental
Physics, HA Bruck, G. V. Coyne, and M. S. Longair (eds.), Pontificia
Academia Scientiarum, p. 315.
Tananbaum, H., Avni, Y., Branduardi, G., Elvis, M., Fabbiano, G.,
Feigelson, E., Giacconi, R., Henry, J. P., Pye, J. P., Soltan, A., and
Zamorani, G.: 1979, Astrophysical Journal Letters, 234, L9.
Veron, P.: 1983, Proceedings 24th Liege International Astrophysical
Symposium on "Quasars and Gravitational Lenses", p. 210.
Woltjer, L. and Selli, G.: 1982, "Astrophysical Cosmology", Proceedings
of the Vatican Study Week on Cosmology and Fundamental
Physics, HA Bruck, G. V. Coyne, and M. S. Longair (eds.), Pontificia
Academia Scientiarum, p. 293.
Zamorani, G.: 1982, "Progress in Cosmology", Proceedings of the
Oxford International Symposium, A. W. Wolfendale (ed.), p. 203.
Zamorani, G.: Henry, J. P., Maccacaro, T., Tananbaum, H., Soltan, A.,
Avni, Y., Lieber!, J., Stocke, J., Strittmatter, P.A., Weymann, R.J.,
Smith, M.G. and Condon, J.J.: 1981, Astrophysical Journal, 245,
357
9-13 (PDF)
B. Buzzoni et al.
The ESO Faint Object Spectrograph and Camera (EFOSC)

ADS BibCode:
1984Msngr..38....9B
Author(s)/Affiliation(s):
Buzzoni, B.; Delabre, B.; Dekker, H.; Dodorico, S.; Enard, D.; Focardi, P.; Gustafsson, B.; Nees, W.; Paureau, J.; Reiss, R.
AA(European Southern Observatory, Garching, West Germany), AB(European Southern Observatory, Garching, West Germany), AC(European Southern Observatory, Garching, West Germany), AD(European Southern Observatory, Garching, West Germany), AE(European Southern Observatory, Garching, West Germany), AF(European Southern Observatory, Garching, West Germany), AG(European Southern Observatory, Garching, West Germany), AH(European Southern Observatory, Garching, West Germany), AI(European Southern Observatory, Garching, West Germany), AJ(European Southern Observatory, Garching, West Germany)
Abstract:
The European Southern Observatory's Faint Object Spectrograph and Camera (EFOSC) has been available for general use in low dispersion spectroscopy and direct imaging modes since April 1985; this low dispersion spectrograph is mated with the ESO's 3.6 m telescope. The EFOSC configuration consists of a focal reducer which converts the F/8 telescope beam to F/2.5, entirely by means of lens combinations. Attention is given to the efficiency and wavelength coverage in the imaging and spectroscopic modes.
References:
(1) EFOSC Technical Report, in preparation.
(2) EFOSC Operating Manual, in preparation.
(3) D. Enard, B. Delabre, 1982, Two design approaches for high
efficiency, low resolution spectroscopy. Proceedings SPIE 445,
522.
(4) P. Biereichei, B. Gustafsson, G. Raffi, 1983, The New Data
Acquisition System for ESO Instrumentation, The Messenger 34,
35.
(5) H. Dekker and S. D'Odorico, 1984, First aso Spectra with EFOSC,
The Messenger 37, 7.
13-16 (PDF)
L. Binette
Abundances in LINERs

ADS BibCode:
1984Msngr..38...13B
Author(s)/Affiliation(s):
Binette, L.
AA(European Southern Observatory, Garching, West Germany)
Abstract:
Low Ionization Nuclear Emission Regions (LINERs) are noted to have an excitation mechanism whose nature has yet to be satisfactorily determined. A research program is underway for LINERs, and two types of results are already available: new diagrams of emission line ratios, which reveal tighter correlations when homogeneous data are used, and a new grid of photoionization calculations, which aim at analyzing the sensitivity to such input parameters as optical thickness, ionizing spectrum hardness, and gas distribution. It is concluded that abundances are more uniform, and solar, than previous work has suggested.
References:
(1) Keel, W. C.: 1983, Astrophys. J. Suppt. 52, 229.
(2) Stauffer, J.R.: 1982, Astrophys. J. Suppt. 50, 517.
(3) Phillips, M. M., Jenkins, C.J., Dapita, M.A., Sadler, E. M. and
Binette, L.: 1985, Astrophys. J. (submitted).
(4) Heckman, T., Balick, B. and Crane, P.: 1980, Astron. Astrophys.
Suppt. 40, 295.
(5) Heckman, T.: 1980, Astron. Astrophys. 87, 152.
(6) Ferland, G. J. and Netzer, H.: 1983, Astrophys. J. 264, 105.
(7) Halpern, J. P. and Steiner, J. E.: 1983, Astrophys. J. Lett. 269,
L37.
(8) Keel, W.C.: 1983, Astrophys. J. 269,466.
(9) Aldrovandi, S. M. V. and Cantini, M.: 1983, Astron. Astrophys.
127,15.
(10) Binette, L.: 1985, Astron. Astrophys. (ESO preprint 350).
(11) Stauffer, J.R.: 1982, Astrophys. J. 262, 66.
(12) Binette, L.: 1982, Ph. D. Thesis, Austraiian Nat. Univ., Canberra.
16-19 (PDF)
E. F. van Dishoeck, J. H. Black
Absorption lines of interstellar C2 and CN molecules

ADS BibCode:
1984Msngr..38...16V
Author(s)/Affiliation(s):
van Dishoeck, E. F.; Black, J. H.
AA(Leiden, Rijksuniversiteit, Sterrewacht, Leiden, Netherlands), AB(Steward Observatory, Tucson, AZ)
Abstract:
The European Southern Observatory's Coude Echelle Spectrometer (CES) is one of the finest existing instruments for high resolution studies of the red part of the spectrum. The CES's use for molecule observations may yield valuable information on such physical conditions as temperature and density within interstellar clouds. C2 is an especially important molecule because, being a symmetric species with no permanent dipole moment, its excited rotational levels have long radiative lifetimes and may be highly populated in interstellar clouds by collisional and radiative processes. The CN molecule, which has a permanent dipole moment, would instead be in its ground rotational state.
19-19 (PDF)
ESO
ESO-IRAM - Onsala Workshop on (Sub)millimeter Astronomy

ADS BibCode:
1984Msngr..38...19.
Author(s)/Affiliation(s):
ESO
AA(ESO)
20-24 (PDF)
T. Korhonen et al.
Polarization measurements at La Silla

ADS BibCode:
1984Msngr..38...20K
Author(s)/Affiliation(s):
Korhonen, T.; Piirola, V.; Reiz, A.
AA(Turku University Observatory, Turku, Finland), AB(Helsinki University Observatory, Helsinki, Finland), AC(Universitetets Astronomiske Observatorium, Copenhagen, Denmark)
Abstract:
A multichannel double beam chopping polarimeter is being used in interstellar polarization measurements at the La Silla site of the European Southern Observatory. This polarimeter can be easily turned into a multichannel photometer. By means of a rotating chopper, two apertures in the focal plane diaphragm are alternately opened and closed at 25 Hz so that the photocathode is alternately illuminated by the sky and star apertures. When the instrument is used for polarization observations, a plane-parallel calcite plate is inserted in front of the focal plane. The polarizations measured in 1980 for all A and F Population II stars (for which reliable distances are available) are plotted in galactic coordinates.
References:
Appenzeller, 1.: 1957, Astron. Astrophys. 38,313.
Efimov, Y. S., Piirola, V., and Shakhovskoy, N. M.: 1984, Astron.
Astrophys. (in print).
Hsu, J.C. and Breger, M.: 1982, Astrophys. J. 262, 732.
Knude, J.: 1981, Astron. Astrophys. Suppl. 44, 225.
Markkanen, T.: 1979, Astron. Astrophys. 47, 201.
Mathewson, D. S., Ford, V. L.: 1970, Mem. Roy. Astron. Soc. 74, 139.
Piirola, v.: 1973, Astron. Astrophys. 27, 383.
Piirola, V.: 1975, Ann. Aead. Seien!. Fenn. Series A, VI. Phys. 418.
Piirola, V. and Vilhu, 0.: 1982, Astron. Astrophys. 110, 351.
Piirola, V., Vilhu, O. and Tuominen, 1.: 1983, in Cataelysmie Variables
and Related Objeets, M. Livio and G. Shaviv (eds.), Proe. lAU Coll.
No. 72, 101, p. 207.
Piirola, V.: 1983, ibid., p. 211.
Serkowski, K.: 1974, in Methods tor Experimental Physies, Vol. 12,
Astrophysies, Part A, Eds. M. L. Meeks and N. P. Carelton, p. 361,Aeademie Press, New York.
Serkowski, K., Mathewson, D. S., Ford, V. L.: 1975, Astrophys. J. 196,
262.
Tinbergen, J.: 1979, Astron. Astrophys. Suppt. 35, 325.
Tinbergen, J.: 1982, Astron. Astrophys. 105, 53.
Wilking, B.A., Lebovsky, M.J., Martin, P.G., Rieke, G.H. and Kemp,
J. C.: 1980, Astrophys. J. 235, 905.
Wilking, B.A., Lebovsky, M.J. and Rieke, G.H.: 1982, Astron. J. 87,
695.
24-28 (PDF)
J. Beckman et al.
Chromospheric modelling in late-type dwarfs: 1. Quiescent objects

ADS BibCode:
1984Msngr..38...24B
Author(s)/Affiliation(s):
Beckman, J.; Crivellari, L.; Foing, B.
AA(Consejo Superior de Investigaciones Cientificas, Instituto de Astrofisica de Canarias, La Laguna, Spain), AB(Trieste, Osservatorio Astronomico, Trieste, Italy), AC(Meudon, Observatoire, Meudon, Hauts-de-Seine, France; European Southern Observatory, Garching, West Germany)
Abstract:
Attention is given to problems which arise when an attempt is made to use observational material to clarify the mechanisms responsible for the heating of the chromosphere in a late-type star, in order to derive a clearer physical view of the nature of a chromosphere, its relation to the underlying photosphere, and the overlying corona. Problems arise in the prediction of line shapes by means of simple models, in chromospheric inhomogeneities, in two-stream modeling, and in the coexistence of two temperature structures. It is deemed necessary to take the dominant role played by inhomogeneities into account, and to ensure that any interstellar effects in the line profile data are well and truly eliminated.
28-31 (PDF)
I. Appenzeller et al.
CASPEC and IUE : A perfect match

ADS BibCode:
1984Msngr..38...28A
Author(s)/Affiliation(s):
Appenzeller, I.; Klare, G.; Stahl, O.; Wolf, B.; Zickgraf, F.-J.
AA(Koenigstuhl, Landessternwarte, Heidelberg, West Germany), AB(Koenigstuhl, Landessternwarte, Heidelberg, West Germany), AC(Koenigstuhl, Landessternwarte, Heidelberg, West Germany), AD(Koenigstuhl, Landessternwarte, Heidelberg, West Germany), AE(Koenigstuhl, Landessternwarte, Heidelberg, West Germany)
Abstract:
The Cassegrain Echelle Spectrograph, or 'CASPEC' of the European Southern Observatory, developed as an auxiliary instrument for the 3.6-m telescope at La Silla, can operate in the 3500-9500 A range. The IUE spacecraft's spectrograph is devoted to UV wavelengths in the 1100-3200 A range, in which ground-based observations are rendered impossible by strong atmospheric absorption. Attention is presently given to cases of successful combination of IUE and CASPEC data to obtain the greatest possible physical information. These include the Henry Draper Extension star catalog object HDE 269599 and two variable stars R127 and S Doradus.
31-32 (PDF)
M. Azzopardi et al.
Catching Carbon Stars in the Baade's Windows

ADS BibCode:
1984Msngr..38...31A
Author(s)/Affiliation(s):
Azzopardi, M.; Lequeux, J.; Rebeirot, E.
AA(ESO) AB(Observatoire de Marseille) AC(Observatoire de Marseille)
Abstract:
Near-infrared objective prism surveys at low dispersion (1 700 to 3400 Amm-1) using Schmidt telescopes have been extensively used to detect M-, S- and C-type stars in the galactic equatorial zone, and in other strategically selected regions of the Milky Way. The detection techniques have been perfected by Nassau and his associates (Nassau and Velghe, 1964, Astrophysical Journal 139, 190) during their survey, at Cleveland, of the northern part of the Milky Way. These techniques are based on the identification of a number of typical molecular bands (TiO, CN, LaO, Va) that fall in the 6800-8800 Aspectral range, and which are used to classify M-, S- and C-type stars (Mavridis, 1967, Coll. on Late Type Stars, p. 420). Using the same method, partial or entire nearinfrared surveys of the southern Milky Way have been carried out by Blanco and Münch (1955, Bol. Obs. Tonantzintla y Tacubaya 12, 273) at Tonantzintla, Smith and Smith (1956, Astronomical Journal 61, 273) at Bloemfontein, and later by Westerlund (1971, Astronomy and Astrophysics Suppl. 4, 51 ; 1978, ibid. 32, 401) with the Uppsala Schmidt telescope at Mount Stromlo Observatory.
33-38 (PDF)
B. Edvardsson et al.
Light element abundances in F stars and the chemical evolution of the galactic disk

ADS BibCode:
1984Msngr..38...33E
Author(s)/Affiliation(s):
Edvardsson, B.; Gustafsson, B.; Nissen, P. E.
AA(Uppsala Astronomiska Observatoriet, Uppsala, Sweden), AB(Stockholms Observatorium, Saltsjobaden, Sweden), AC(Aarhus, Universitet, Aarhus, Denmark)
Abstract:
A project for investigation of the evolution of the chemical elements in the galactic disk, and in particular of the elements in the third and fourth period of the periodic table, is presented. Chemical abundances of F dwarfs of different ages and of different overall metal abundance are used for this purpose. Preliminary results for 15 stars are reported; they indicate abundance ratios of O, Mg, Si, Ca and Ti relative to iron that are systematically greater than the solar ratio for stars with Fe/H lower than -0.5, and with the excess increasing with decreasing Fe/H and decreasing atomic number. An odd-even effect for the sequence Na, Mg, Al, Si is found for the metal-poor disk stars.
References:
Ardeberg, A., Lindgren, H. and Nissen, P. E. 1983. Astron. Astrophys.
128,194.
Arnett, W. D. 1971, Astrophys. J. 166, 153.
Arnett, W. D. 1978, Astrophys. J. 219, 1008.
Clegg, R. E.S., Lambert, D. L. and Tomkin, J. 1981. Astrophys. J. 250,
262.
Gustafsson, B., Bell, R.A., Eriksson, K. and Nordlund, Ä. 1975, Astron.
Astrophys. 42,407.
Hejlesen, P.M. 1980, Astron. Astrophys. Suppl. 39,347.
Luck, R. E. and Bond, H. E. 1984, Astrophys. J., submitted.
Mihalas, D. 1978, Stellar atmospheres, W. A. Freeman & Co., p. 286.
Nissen, P. E. 1981, Astron. Astrophys. 97, 145.
Nissen, P. E. and Gustafsson, B. 1978, Astronomical papers dedicated
to Bengt Str
37-37 (PDF)
ESO
ESO Workshop on the Production and Distribution of Carbon Nitrogen and Oxygen in Stellar Systems

ADS BibCode:
1984Msngr..38...37.
Author(s)/Affiliation(s):
ESO
AA(ESO)
38-41 (PDF)
P. R. Christensen et al.
The RPCS Detector

ADS BibCode:
1984Msngr..38...38C
Author(s)/Affiliation(s):
Christensen, P. R.; Hviid, E.; Thomsen, G.; Ulfbeck, O.
AA(Niels Bohr Institute, University ofCopenhagen) AB(Niels Bohr Institute, University ofCopenhagen) AC(Niels Bohr Institute, University ofCopenhagen) AD(Niels Bohr Institute, University ofCopenhagen)
Abstract:
A one-dimensional dual array linear photon counting device for optical spectroseopy of faint astronomical objects has been developed and tested.
References:
(1) S. A. Shectman and W. A. Hiltner, P.A.S.P. 88 (1976), 960.
(2) P. Young and W. L. W. Sargent, Astrophysical Journal Suppl.
Series 48 (1982). 455.
(3) J. B. Oke, Astrophysical Journal Suppl. Series 27 (1974) 21.
42-42 (PDF)
R. M. West
ESO Photographer Finds New Celestial Object / Zodet's Planetary = ESO:135-PN4 = 15H05M -61.5DEG

ADS BibCode:
1984Msngr..38...42W
Author(s)/Affiliation(s):
West, R. M.
AA(ESO)
Abstract:
The production of eopies for the ESO/SRC Atlas of the Southern Sky is proceeding at the ESO Sky Atlas Laboratory in Garching. For this atlas 606 blue sensitive plates have been exposed at the UK Schmidt telescopes in Coonabarabran, Australia, and corresponding red sensitive plates are being made with the ESO Sehmidt telescope at La Silla, Chile.
42-42 (PDF)
M.-P. Veron-Cetty, P. Veron
Nova Sagittarii 1984

ADS BibCode:
1984Msngr..38...42V
Author(s)/Affiliation(s):
Veron-Cetty, M.-P.; Veron, P.
AA(ESO) AB(ESO)
42-43 (PDF)
ESO
List of Preprints Published at ESO Scientific Group (September - November 1984)

ADS BibCode:
1984Msngr..38...42.
Author(s)/Affiliation(s):
ESO
AA(ESO)
43-44 (PDF)
ESO
Algunos Resumenes

ADS BibCode:
1984Msngr..38S..43.
Author(s)/Affiliation(s):
ESO
AA(ESO)
43-43 (PDF)
ESO
Personnel Movements (September-November 1984)

ADS BibCode:
1984Msngr..38R..43.
Author(s)/Affiliation(s):
ESO
AA(ESO)
43-43 (PDF)
ESO
Departure of Dr. Inge Meinen

ADS BibCode:
1984Msngr..38Q..43.
Author(s)/Affiliation(s):
ESO
AA(ESO)