Messenger No. 45 (September 1986)

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1-2 (PDF)
P. Crane
New interstellar molecule detected

ADS BibCode:
1986Msngr..45....1C
Author(s)/Affiliation(s):
Crane, P.
AA(European Southern Observatory, Garching, West Germany)
Abstract:
The molecule (C-13)N has been detected for the first time in the interstellar medium. A plot of a portion of the observed spectrum which contains the newly discovered line is shown. This new line is the R(0) line of the 0,0 band of the B 2 Sigma - X 2 Sigma electronic system of (C-13)N. Its equivalent width is 0.179 + or - 0.040 mA. The new feature allows a determination of the carbon isotope ratio in the interstellar cloud in the direction of Zeta Ophiuchi. The C-12/C-13 ratio determined from these measurements is 50(+13; -10). This can be compared to the terrestrial ratio of 89 and further substantiates theories of the enrichment of C-13 in the interstellar medium through evolution of the Galaxy since the formation of the solar system.
2-4 (PDF)
M. C. E. Huber, J. Breysacher
The work of the ESO Observing Programmes Committee.

ADS BibCode:
1986Msngr..45....2H
Author(s)/Affiliation(s):
Huber, M. C. E.; Breysacher, J.
AA(Institut für Astronomie, ETH Zürich, Chairman of the OPC) AB(ESO)
Abstract:
ESO astronomers devote considerable time to preparing, and put obvious care into writing Applications for Observing Time at La Silla. Many take justifiable pride in the presentation of their ideas. Yet, given the heavy oversubscription of telescope time, inevitably a selection of the proposed observing programmes must be made. And often this selection is drastic: in each Observing Period, the applied-for number of observing nights for the various telescopes exceeds the number of available nights by factors of two, at telescopes of intermediate size, to four, at the 2.2-m and 3.6-m telescopes!
3-3 (PDF)
ESO
Announcement of an 'International School on Astro-Particle Physics'

ADS BibCode:
1986Msngr..45R...3.
Author(s)/Affiliation(s):
ESO
AA(ESO)
3-3 (PDF)
ESO
Tentative Time-Table of Council Sessions and Committee Meetings in 1986

ADS BibCode:
1986Msngr..45Q...3.
Author(s)/Affiliation(s):
ESO
AA(ESO)
4-6 (PDF)
ESO
Visiting Astronomers (October 1, 1986-April 1, 1987)

ADS BibCode:
1986Msngr..45....4.
Author(s)/Affiliation(s):
ESO
AA(ESO)
5-5 (PDF)
ESO
Announcement of an ESO Workshop on 'Stellar Evolution and Dynamics in the Outer Halo of the Galaxy'

ADS BibCode:
1986Msngr..45....5.
Author(s)/Affiliation(s):
ESO
AA(ESO)
6-8 (PDF)
W. E. Celnik
Hunting Halley's comet.

ADS BibCode:
1986Msngr..45....6C
Author(s)/Affiliation(s):
Celnik, W. E.

Abstract:
Observers of bright comets have always been fascinated by the sight of these rare phenomena. However, it was as late as the 19th century that scientists started to make systematic observations of the appearance of comets and recorded them in the form of drawings and descriptions of comas and tails. Halley's comet in particular was observed intensively because the time of its return was weil known. The first photographic observations of the comet were made during its 1910 perihelion. A large number of photographs were taken using astronomical instruments of all dimensions showing structures within the extended ion tail and the bright coma. Pictures from that time are weil suited to be compared with recently obtained images of the 1986 appearance, although observing conditions were then much less favourable. Just when PI Halley was most active, at its brightest, and thus most interesting, namely during its perihelion passage, it was behind the Sun and unobservable. During the 2,000 years that observations of this comet have been recorded, there was only one appearance where the positions of Sun, Earth and comet were even worse for observations. In addition, the observing conditions in the northern hemisphere were extremely bad because at its best time the comet followed its path through the southern skies. Thus the only way to observe P/ Halley successfully after its perihelion passage was to got to the southern hemisphere. At a latitude of 30 degrees south the comet culminated near the zenith.
8-13 (PDF)
C. Arpigny et al.
Spectroscopy, photometry and direct filter imagery of Comet P/Halley

ADS BibCode:
1986Msngr..45....8A
Author(s)/Affiliation(s):
Arpigny, C.; Dossin, F.; Manfroid, J.; Danks, A. C.; Lambert, D. L.
AA(Liege, Universite, Belgium), AB(Liege, Universite, Belgium), AC(Liege, Universite, Belgium), AD(European Southern Observatory, Garching, West Germany), AE(Michigan State University, East Lansing)
Abstract:
Observational techniques and instrumentation applied in ground-based studies of the cometary coma during the post-perihelion phase of the recent passage of Comet Halley are summarized. Applications of a 1.5 m telescope equipped with a coude spectrograph for long slit investigations of spectral intensity distributions, a 1.4 m CAT, coude echelle spectrometer and reticon to evaluate the C-12/C-13 isotopic abundance ratio, and a 50 cm photometric telescope for narrow bandwidth spectroscopy are described. Finally, the 1.5 m Danish telescope, equipped with a CCD camera, collected high spatial resolution photographs of the various coma components when the comet was 0.42 AU from the sun.
References:
Arpigny, C.: 1976, Proc. IAU Coll. Nr.25,
"The Study of Comets", NASA SP-393
(Donn et al., eds.), 797-838.
Danks, A.C.: 1982, ESO Comet Halley Workshop,
Paris (Veron, ed.), 155-170.
Danks, A. C. and Arpigny, C.: 1973, Astron.
Astrophys. 29,347.
Danks, A. C., Lambert, D. L. and Arpigny, C.:
1974, Astrophys. J, 194,745.
Festou, M. C., Feldman, P. D. and Weaver,
H.A.: 1982, Astrophys. J 256, 331.
Johnson, J. R., Fink, U. and Larson, S. M.:
1984, /carus 60, 351.
Lambert, D. L. and Danks, A. C.: 1983, Astrophys.
J, 268, 428.
Spinrad, H.: 1982, Pub!. Astron. Soc. Pac. 94,
1008.
9-9 (PDF)
ESO
First Announcement of an ESO Conference on 'Very Large Telescopes and their Instrumentation'

ADS BibCode:
1986Msngr..45....9.
Author(s)/Affiliation(s):
ESO
AA(ESO)
13-17 (PDF)
J. E. Arlot et al.
The PHEMU 85 international campaign.

ADS BibCode:
1986Msngr..45...13A
Author(s)/Affiliation(s):
Arlot, J. E.; Bouchet, P.; Gouiffes, C.; Morando, B.; Schmider, F. X.; Thuillot, W.
AA(Bureau des Longitudes, Paris) AB(ESO, La Silla) AC(ESO, La Silla) AD(Bureau des Longitudes, Paris) AE(ESO, La Silla) AF(Bureau des Longitudes, Paris)
Abstract:
The mutual phenomena of the Galilean satellites of Jupiter take place every six years, when the Earth and the Sun cross the equatorial plane of Jupiter which coincides with the orbital planes of the satellites. At that time, mutual occultations and eclipses may occur. However, the only favourable situation for observing such phenomena is when the crossing of the equatorial plane occurs simultaneously with the opposition of Jupiter. These phenomena are often observable only once every twelve years. In 1985, during the latest opposition of Jupiter, its declination was between -19 and -15 degrees, which made La Silla one of the best places to observe them.
17-17 (PDF)
ESO
VLT Reports

ADS BibCode:
1986Msngr..45R..17.
Author(s)/Affiliation(s):
ESO
AA(ESO)
17-17 (PDF)
ESO
List of ESO Preprints (June-August 1986)

ADS BibCode:
1986Msngr..45Q..17.
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
445. B. Reipurth and G. Gee: Star Formation in Bok Globules and Low-Mass Clouds. III. Barnard 62. Astronomy and Astrophysics. June 1986.
18-20 (PDF)
G. Galletta
The unusual barred SO galaxy NGC 4546

ADS BibCode:
1986Msngr..45...18G
Author(s)/Affiliation(s):
Galletta, G.
AA(Padova, Universita, Padua, Italy)
Abstract:
The results of spectroscopic and photometric observations of NGC 4546 in May 1986 are reported. Details of the observational techniques and instrumentation employed for the scans in the 4900-5700 A interval are described. The spectral lines of the gas in the bar indicated that the gas rotates in a direction opposite to the stars in NGC 4546, which may be a visual artifact of the gas not being coplanar with the stars. Several hypotheses are presented for the source of the gas.
References:
Bieging, J. H., 1978, Astron. and Astrophys.
64,26.
Caldwell, N., Kirshner, R. P., Richstone, 0.,
1986, Astrophys. J., 305, 136.
Contopoulos, G. and Papayannopoulos, Th.,
1980, Astron. and Astrophys., 92, 33.
de Vaucouleurs, G., 1975, in Stars and Stellar
Systems, The University of Chicago Press,
Vol. IX, p. 584.
de Vaucouleurs, G., de Vaucouleurs, A. and
Corwin, H.G.Jr. 1976, RC2, Second Reference
Cat. of bright galaxies, Austin, Univers.
01 Texas Press.
de Zeeuw, T. and Merrit, D., 1983, Astrophys.
J., 267, 571.
Freeman, K.C., 1966, Mon. Not. of Royal
Astr. Soc., 134, 1.
Humason, M. L., MayalI, N. V. and Sandage,
A. R., 1956, Astron. J. 61, 101.
Kormendy, J., 1979, Astrophys.J., 227, 714.
Kormendy, J., 1983, Astrophys. J., 275, 529.
Oort, J. H., 1965, in Stars and Stellar Systems,
The University of Chicago Press,
Vol. V, p. 486.
Schweizer, F., 1983, IAU Symp. no.100,
p.319.
20-20 (PDF)
ESO
Applications for Observing Time at La Silla

ADS BibCode:
1986Msngr..45...20.
Author(s)/Affiliation(s):
ESO
AA(ESO)
21-22 (PDF)
T. J.-L. Courvoisier
Radio to X-ray observations of the quasar 3C 273

ADS BibCode:
1986Msngr..45...21C
Author(s)/Affiliation(s):
Courvoisier, T. J.-L.
AA(European Southern Observatory, Garching, West Germany)
Abstract:
A series of repeated multifrequency observations were made of 3C 273 at intervals from radio wavelengths to X-rays. The data were collected with the EXOSAT and IUE spacecraft and with telescopes at three ground-based sites. The measurements were repeated to offset uncertainties due to large short-term spectral variations. Variations observed at near-IR intervals demonstrated that near-IR radiation does not arise from the same source as observed far-IR radiation, i.e., synchrotron emissions. The X-ray emitting source was projected to be a light month across, while UV radiation originated from a source as large as that emitting visible light. Finally, the far-IR source was smaller than a few light months across.
References:
1. Courvoisier, T. J.-L., Turner, M., Robson,
E.I., Gear, W. K., Staubert, R., Blecha, A.,
Bouchet, P., Falomo, P., Valtonen, M. and
Teräsranta, H., 1986, in preparation.
2. Courvoisier, T.J.-L., 1984, TheMessenger
37, September 1984.
3. Robson, E.I., Gear, W.K., Brown, L.M.J.,
Courvoisier, T.J.-L., Smith, M.G., Griffin,
M.J. and Blecha, A., 1986, Nature, in
press.
4. Courvoisier, T. J.-L. and Ulrich, M. H.,
1985, Nature 316,554.
22-27 (PDF)
M. Rosa, D. Baade
Modelling space telescope observations

ADS BibCode:
1986Msngr..45...22R
Author(s)/Affiliation(s):
Rosa, M.; Baade, D.
AA(European Southern Observatory, Garching, West Germany), AB(European Southern Observatory, Garching, West Germany)
Abstract:
Features and the theoretical background for a software package devised for simulating observations which will be made with the Space Telescope (ST) are described. The package was developed to familiarize operators and experimenters with the use, capabilities, limitations and operational alternatives of the ST, which has six instruments and several hundred operational modes. Routines converted from the data analysis system MIDAS were combined with several specialized FORTRAN programs to obtain a package with target generation, optical path and detection capabilities. Simulated images of several typical celestial objects are provided.
27-29 (PDF)
M. Duchateau, M. Ziebell
The ESO TV autoguiders.

ADS BibCode:
1986Msngr..45...27D
Author(s)/Affiliation(s):
Duchateau, M.; Ziebell, M.
AA(ESO) AB(ESO)
Abstract:
In February 1985 four new autoguider systems have been installed at La Silla. The 3.6-m telescope, the CAT, the 2.2-m telescope and the Schmidt got equipped with a system. They have been used now successfully for one and a half year and we hope that they are not "job killers" but that in the meantime they have been accepted as an improvement of work conditions.
29-32 (PDF)
C. Perrier
ESO infrared specklegraph.

ADS BibCode:
1986Msngr..45...29P
Author(s)/Affiliation(s):
Perrier, C.
AA(Observatoire de Lyon, France)
Abstract:
An infrared specklegraph is available for Visiting Astronomers for use at the 3.6-m telescope F/35 focus. It has briefIy been described in the Announcement for Applications in periods 36 to 38. First tested in September 1984, it has since then achieved the expected performances during several runs. However, its theoretical limits have actually been reached only after a dome air-cooling system has been put into operation earIy this year. In this article we introduce the instrument assuming that the reader already has some knowledge of the short-exposure imaging principles.
32-32 (PDF)
P. Bouchet, F. Gutierrez
The Fast-Photometry Facilities at La Silla

ADS BibCode:
1986Msngr..45...32B
Author(s)/Affiliation(s):
Bouchet, P.; Gutierrez, F.
AA(ESO, La Silla) AB(ESO, La Silla)
Abstract:
We briefly present in this note the available programme (and its environment) to perform fast photometry at La Silla. This facility has become available on the mountain a lang time aga already but recent discussions with same Visiting Astronomers tend to show that potential users are not yet weil aware of it. Many programmes have already been carried out with this mode of observing, mainly in the infrared but also in the visible. Let us mention, for instance: - Occultations of stars by planets to discover and/or study rings as weil as to determinate the temperatures and variations of the atmospheres of the planets. (See for instance: Bauchet et al., The Messenger No. 26, Dec. 1981 and Haefner et al., The Messenger No. 42, Dec.1985)
33-33 (PDF)
ESO
ESO Image Processing Group: MIDAS Memo

ADS BibCode:
1986Msngr..45...33.
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
The ESO scientific computer facilities were moved into new rooms in the extension of the ESO Headquarters in Garching. The machines in the old computer room were disconnected and moved to the new location in the basement of the new wing on July 16. Since there is no large elevator down to the room, all big items like computer racks, disk drives and tape units had to be taken out of the building and lowered down by a crane as seen in Figure 1. The new computer room contains now most of the scientific computer equipment in ESO including the two VAX 8600 computers, the IHAP HP system, the database machine 10M 500, and the peripherals like disk drives, terminal multiplexer and DICOMED image recording unit (see Figure 2). The ESO archive will also be placed in this room which is fully air-conditioned and fire protected by a halon system. The magnetic tape drives are located in an adjacent room with general access. The user room is now also located in the new wing on the entrance level. All IHAP and MIDAS image processing workstations are placed there in additon to a number of public available terminals connected to the VAX's. Figure 3 shows the half of the user room which is dedicated to MIDAS stations. Furthermore, the main printing and plotting facilities are in a central section of the user room. The Image Processing Group has also moved to new offices just above the user room.
34-34 (PDF)
ESO
Extensions of ESO Headquarters Building Ready

ADS BibCode:
1986Msngr..45...34.
Author(s)/Affiliation(s):
ESO
AA(ESO)
35-35 (PDF)
ESO
Staff Movements

ADS BibCode:
1986Msngr..45R..35.
Author(s)/Affiliation(s):
ESO
AA(ESO)
35-35 (PDF)
ESO
Finalizadas las ampliaciones del edificio central de la ESO

ADS BibCode:
1986Msngr..45Q..35.
Author(s)/Affiliation(s):
ESO
AA(ESO)
36-36 (PDF)
M.C.E. Huber
Staff Movements

ADS BibCode:
1986Msngr..45...36H
Author(s)/Affiliation(s):
Huber, M.C.E.
Institut für Astronomie, ETH Zürich, Presidente del OPC J. Breysacher, ESO
Abstract:
Los astronomos de ESO dedican una considerable parte de su tiempo a la preparacion de solicitudes para tiempo de observacion en La Silla. Sin embargo, debido a la gran demanda par los telescopios, se debe hacer una seleccion, aveces drastica, de los programas de observacion presentados. EI Comite de Programas de Observacion (OPC) tiene como tarea evaluar el merito cientifico de las solicitudes presentadas. Basada en las recomendaciones dei OPC, ESO prepara una Lista de Tiempos de Observacion en la cual distribuye el tiempo disponible en los telescopios a los programas mejor evaluados.