Messenger No. 47 (March 1987)
1-3 (PDF)
New meteorite finds at Imilac
ADS BibCode:
1987Msngr..47....1P
Author(s)/Affiliation(s):
Pedersen, H.; Garcia, F.
AA(European Southern Observatory, Garching, West Germany), AB(European Southern Observatory, Garching, West Germany)
Abstract:
The recent discovery of three meteorites at Imilac, totalling 59 kg, is reported. They have masses of 5, 9, and 35 kg, respectively, and were spotted at an altitude of 3,250 m. The find locations form an approximately equilateral triangle, with side lengths of 900 m. It is believed that all three are Pallasites. The asteroidal origin for Pallasites is discussed.
References:
Buchwald, V. F., 1975, Handbook of lron
Meteorites, University of California press,
Berkeley, vol. 1-3.
Cruikshank, D. P., and Hartmann, W. K.,
1984, Seienee 223,281.
Greenberg, R., and Chapman, C. R., 1984,
learus, 57, 267.
Nininger, H. H., 1952, Out of the Sky, Dover,
New York.
Peck, E., 1979, Sky and Teleseope, 58,
p.126.
Scott, E. R. D., Nature, 311, 708.
3-3 (PDF)
Tentative Time-table of Council Sessions and Commitee Meetings for First Half of 1987
4-7 (PDF)
Giant H II regions and the quest for the Hubble constant
ADS BibCode:
1987Msngr..47....4M
Author(s)/Affiliation(s):
Melnick, J.
AA(European Southern Observatory, Garching, West Germany)
Abstract:
The controversy over the exact value of the Hubble constant is discussed. A method is presented which uses the properties of giant H II regions as distance indicators. It relies on the correlation between H-beta luminosity, the emission line-profile widths, and the oxygen abundances of giant H II regions. The Hubble constant is estimated to be 85 + or - 10 km/sec/Mpc.
References:
(1) R. Kippenhahn: Light from the Depths of
Time (Springer) for the history of the Hubble
constant.
(2) A. Sandage: "The Dynamical parameters
of the Universe", in First ESO/CERN Symposium,
Large Seale Structure ofthe Universe,
Cosmology and Fundamental Physies,
p. 127, for a modern account of the
quest for the Hubble constant and the
defence of Ho = 50.
(3) M. Aaronson and co-workers in Astrophysical
Journal Vol. 302, p. 536
(1986) for a detailed discussion of the
Tully-Fisher method, the various radial
velocity corrections and a defence of the
Ho = 100 view.
(4) J. Melnick and co-workers in ESO preprint
number 440 (1986) for a discussion
of the use of giant H II regions as distance
indicators.
7-9 (PDF)
Visiting Astronomers (April 1-October 1, 1987)
9-9 (PDF)
First Announcement of an ESO/NOAO Conference on 'High-Resolution Imaging by Interferometry'
ADS BibCode:
1987Msngr..47S...9.
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
First Announcement of an ESO/NOAO Conference on 'High-Resolution Imaging by Interferometry'
9-9 (PDF)
List of ESO Preprints (December 1986-February 1987)
ADS BibCode:
1987Msngr..47R...9.
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
476. T.J.-L. Courvoisier et al.: The Radio to X-ray Continuum emission of the Quasar 3C 273 and its Temporal Variations. Astronomy and Astrophysics. December 1987.
9-9 (PDF)
Italian Delegation Visits ESO
10-13 (PDF)
Long-term photometric campaign at ESO and the new eclipsing P Cygni star R 81 in the LMC
ADS BibCode:
1987Msngr..47...10W
Author(s)/Affiliation(s):
Wolf, B.; Sterken, C.; Stahl, O.; Manfroid, J.
AA(Landessternwarte Koenigstuhl, Heidelberg, West Germany), AB(Vrije Universiteit, Brussels, Belgium), AC(European Southern Observatory, Garching, West Germany), AD(Liege, Universite de l'Etat, Belgium)
Abstract:
The Long-term Photometry of Variables project is described. All measurements were carried out in the Stromgren uvby system and preference was given to differential measurements with two comparison stars. Included in this photometry program was the study of R 81, the counterpart of P Cyg in the LMC. A variation period of 74.59 + or - 0.01 days was obtained for this eclipsing binary.
References:
Appenzeller, 1.: 1972, Pub!. Astron. Soc. Japan
24, 483.
Cassatella, A, Beeckmans, F., Benvenuti, P.,
Clavel, J., Heck, A., Lamers, H.J. G. L. M.,
Macchetto, F., Penston, M., Selvelli, P. L.,
Stickland, D.: 1979, Astron. Astrophys. 79,
223.
Chiosi, C., Maeder, A.: 1986, in Ann. Rev.
Astron. Astrophys., 24, 329.
Humphreys, R. M.: 1986, in Luminous stars
and associations in ga!axies, lAU Symp.
No. 116, eds. de Loore, Willis, Laskarides,
p.45.
Lamers, H.J.G.L.M., de Groot, M.J.H.,
Cassatella, A.: 1983, Astron. Astrophys.
128,299.
Lamers, H. J. G. L. M., Korevaar, P., CassateIla,
A: 1985, Astron. Astrophys. 149,29.
Manfroid, J. Heck, A: 1983, Astron. Astrophys.
120,302.
Stahl, D., Wolf, B., de Groot, M.J.H., Leith.
erer, C.: 1985, Astron. Astrophys. Suppt.
61,237.
Stahl, D., Wolf, B., Zickgraf, F.-J.: 1987, Astron.
Astrophys., submitted.
Sterken, C.: 1983, The Messenger 33,10.
van Gent, R.H., Lamers, H.J.G.L.M.: 1986,
Astron. Astrophys. 158, 335.
Waters, L.B.F.M., Wesselius, P.P.: 1986,
Aslfon.Aslfophys. 155, 104.
Wolf, B., Campusano, L., Sterken, C.: 1974,
Astron. Astrophys. 36, 87.
Wolf, B., Stahl, D., de Groot, M. J. H., Sterken,
C.: 1981, Astron. Astrophys. 99, 351
13-14 (PDF)
Blue horizontal branch field stars in the outer Galactic halo
ADS BibCode:
1987Msngr..47...13S
Author(s)/Affiliation(s):
Sommer-Larsen, J.; Christensen, P. R.
AA(Copenhagen, Universitet, Denmark), AB(Copenhagen, Universitet, Denmark)
Abstract:
A sample of blue horizontal branch field stars (BHBF) in the outer Galactic halo is studied in an attempt to further understand the properties of distant halo objects. Observations were performed with the ESO 2.2-m telescope during 1984-1986. The system of BHBF stars in the Galactic halo is round with an axial ratio q of about 0.8. The density distribution out to the limit of the sample (r of about 40 kpc) is described by a power law with an index of about -3.
References:
Christensen, P.R. et al., 1984, The
Messenger 38, 38.
Lynden-Bell, D., Cannon, R.D., and Godwin,
P.J., 1983, Mon. Not. R. Astr. Soc., 204,
Short. Comm., p. 87.
Sommer-Larsen, J. and Christensen, P. R.,
1985, Mon. Not. R. Astr. Soc., 212,851.
Sommer-Larsen, J. and Christensen, P. R.,
1986, Mon. Not. R. Astr. Soc., 219, 537.
14-14 (PDF)
And then there were Three
15-17 (PDF)
Where peculiars turn normal - IR observations of CP stars
ADS BibCode:
1987Msngr..47...15K
Author(s)/Affiliation(s):
Kroll, R.
AA(Universitaets-Sternwarte, Goettingen, West Germany)
Abstract:
Infrared observations of CP stars are presented and a Rayleigh-Jeans diagnosis is performed. IRAS data reveal that all flux redistribution caused by the unusual chemistry of CP stars can end at IR wavelengths. IR light curves are obtained for HD 3980 and HD 29305.
References:
Bonsack, W.K., Dyck, H.M., 1983: Astron.
Astrophys. 125,29.
Groote, D., Kaufmann, J. P., 1983: Astron.
Astrophys. Suppl. Ser. 53, 91.
Koornneef, J., 1983: Astron. Astrophys.
Suppl. Ser. 51, 489.
Kroll, R., Schneider, H., Catalano, F.A., Voigt,
H. H., 1987: Astron. Astrophys. Suppl. Ser.
67, 195.
Kurucz, R. L., 1979: Astron. J. Suppl. Ser. 40,
1.
Michaud, G., 1980: Astron. J. 85, 589.
Preston, G.W., 1974: Ann. Rev. Astr. Astrophys.
12,257.
17-17 (PDF)
ESO Press Releases
18-19 (PDF)
BD +03 deg 740 - A new extreme metal-poor dwarf
ADS BibCode:
1987Msngr..47...18M
Author(s)/Affiliation(s):
Magain, P.
AA(European Southern Observatory, Garching, West Germany)
Abstract:
The results of a preliminary analysis of BD +03 deg 740 are presented. The analysis was based on the blue spectrum which was obtained with an exposure time of 40 min, giving a good S/N ratio for this 9.8-mag star. Graphs are presented which reveal the extreme weakness of the metal lines in the spectrum. The analysis of BD +03 deg 740, which is the most metal-poor dwarf in which s element abundances have been determined, confirms the presence of secondary elements in the atmospheres of the extreme halo dwarfs.
References:
Arpigny, C., Magain, P.: 1983, Astron. Astrophys.
127, L7.
Bessel, M. S., Norris, J.: 1981, lAU Coll. No.
68, p. 137.
Carney, B. W., Peterson, R. C.: 1981, Astrophys.
J. 245, 238.
Cayrel, R.: 1986, Astron. Astrophys. 168,81.
Fran90is, P.: 1986, Astron. Astrophys. 160,
264.
Jones, J. E.: 1985, Publ. Astron. Soc. Pacific
97,593.
Magain, P.: 1984, Astron. Astrophys. 134,
189.
Magain, P.: 1985, Astron. Astrophys. 146,95.
Magain, P.: 1987, Astron. Astrophys., in
press.
Spite, M., Spite, F.: 1978, Astron. Astrophys.
67,23.
19-23 (PDF)
BD Pavonis, a new double lined eclipsing cataclysmic binary.
ADS BibCode:
1987Msngr..47...19B
Author(s)/Affiliation(s):
Barwig, H.; Schoembs, R.
AA(Universitäts-Sternwarte München) AB(Universitäts-Sternwarte München)
Abstract:
Cataclysmic binaries are double stars consisting of a compact primary and a cool secondary component. They are so close that the surface of the secondary fills its so-called Rache limit and transfers matter towards the primary in a stream. Oue to the system's orbital motion, however, the stream does not impact on the primary but forms an accretion disk around it. Where the overflowing mass hits the rotating gas, a hot bright spot is produced. The momentum of the disk material has to be separated before it can be accreted onto the primary. Magnetic fields can influence the structure of the disk, in same cases no disk exists at all and matter is forced to flow along the magnetic field lines producing extremely hot X-ray emitting spots above the magnetic poles.
References:
Barwig, H., Schoembs, R.: 1981, Inf. Bull.
Var. Stars No. 2031.
Barwig, H., Schoembs, R.: 1983, Astron. Astrophys.
124,287.
Barwig, H., Schoembs, R., Buckenmayer, C.:
1987, Astron. Astrophys., Main Journal, in
press.
Boyd, C. D.: 1939, Harv. Ann. 90, 248.
Payne-Gaposchkin, C.: 1977, in: Novae and
related Stars, p. 3.
Schoembs, R., Dreier, H., Barwig, H.: 1987,
Astron. Astrophys., in press.
23-24 (PDF)
Strengthening Research Links between Astronomy/Astrophysics and Computing/Statistics
ADS BibCode:
1987Msngr..47...23M
Author(s)/Affiliation(s):
Murtagh, F.; Heck, A.; di Gesu, V.
AA(Space Telescope - European Coordinating Facility, European Southern Observatory) AB(Observatoire Astronomique, Strasbourg) AC(Dip. di Matematica ed Applicazioni, Univ. di Palermo, and IFCAI/CNR, Palermo)
Abstract:
In this article, a few current research directions are discussed, which relate to the common interfaces between astronomy/ astrophysics, computer science and statistics. They relate essentially to organizational matters (working groups, conferences). Within the next decade contact between researchers over computer networks will become increasingly trauble-free, but for the present, contact between widely scattered researchers (and especially among those who straddle traditional disciplines) is necessarily in hard-copy form, as for example in this journal!
References:
1. V. Di Gesü, L. Scarsi, P. Crane, J. H. Friedman
and S. Levialdi (eds.) (1984): Data
Analysis in Astronomy, Plenum Press, New
York.
2. V. Di Gesü, L. Scarsi, P. Crane, J. H. Friedman
and S. Levialdi (eds.) (1986): Data
Analysis in Astronomy 11, Plenum Press,
New York.
3. F. Murtagh and A. Heck (1986): An annotated
bibliographical catalogue of multivariate
statistical methods and of their
astronomical applications (magnetic tape).
Astronomy and Astrophysics Supplement
Series (in press); ESO Scientific Preprint
No. 465 (Sept. 1986).
4. F. Murtagh and A. Heck (1987): Multivariate
Data Analysis, D. Reidel, Dordrecht.
5. E.J. Rolfe (ed.) (1983): Statistical Methods
in Astronomy, European Space Agency
Special Publication 201 (270 pp.).
23-23 (PDF)
Announcement of a Summer School on 'Observing with Large Telescopes'
24-25 (PDF)
Crowded field photometry using EFOSC and ROMAFOT.
ADS BibCode:
1987Msngr..47...24M
Author(s)/Affiliation(s):
Mighell, K. J.
AA(Kapteyn Observatory, Roden, The Nether/ands)
Abstract:
The ESO Faint Object Spectrograph and Camera (EFOSC), instrument of the ESO 3.6-m telescope, can be used as a very efficient CCO camera for wideband photometry of crowded stellar fields. EFOSC was designed to match the RCA SIO 501 EX CCO (320 x 512 pixels, 30 x 30 microns pixel size). Each pixel corresponds to 0.675 arcsec and the total field of view is 3.6 x 4.7 arcminutes (1). Using the instrument in direct imaging mode, the limiting magnitude of a 15 minute exposure with seeing of FWHM = 1.3 arcseconds in the V band is about 25.5 for a signal-to-noise ratio of 3 (2).
References:
(1) D'Odorico, S., Oekker, H., "The Five Observing
Modes of EFOSC, the ESO Faint
Object Spectrograph and Camera Oesigned
Around a CCO Oetector".
(2) The Messenger 41, p. 26, 1985.
(3) Stetson, P. B., "OAOPHOT User's Manual",
Dominion Astrophysical Observatory,
Herzberg Institute of Astrophysics, 5071
West Saanich Road, Victoria, British Columbia
V8X 4M6, Canada.
(4) Buonanno, R., Corsi, C. E., Oe Baise,
G. A., Ferraro, 1., 1979, in Image Processing
in Astronomy, eds. G. Sedmak, M.
Capaccioli, and R.J. Allen, Trieste, Italy,
p.554.
24-24 (PDF)
Announcement of a ST-ECF Conference on 'Astronomy from Large Databases: Scientific Objectives and Methodological Approaches'
25-25 (PDF)
The Supernova in the LMC
25-25 (PDF)
Storm Petersen and Astronomy
26-27 (PDF)
The initial impact of the LMC supernova.
ADS BibCode:
1987Msngr..47Q..26W
Author(s)/Affiliation(s):
Wampler, J.
AA(ESO)
Abstract:
Between 2 o'clock and 7 o'clock universal time (UT) on Monday morning, February 23, 1987, a star in the Large Magellanic Cloud (LMC), at the position of the B3 I supergiant Sanduleak -69202, began to brighten rapidly. By 10 o'clock UT it had brightened by a factor of 200. And the next day it had increased in brightness by an additional factor of 10. As L. Woltjer notes above, this star is the first really bright supernova in the modern era. Because of its southern declination it can only be seen by southern observatories and space observatories.
27-27 (PDF)
Walraven photometry of supernova 1987A.
ADS BibCode:
1987Msngr..47...27M
Author(s)/Affiliation(s):
Monderen, P.; Schwarz, H. E.; Steeman, F.
AA(ESO) AB(ESO) AC(Leiden)
Abstract:
Walraven photometry of supernova 1987A.
27-28 (PDF)
Geneva seven colour photometry of supernova 1987A.
ADS BibCode:
1987Msngr..47...27B
Author(s)/Affiliation(s):
Babel, J.; Heynderickx, D.
AA(Lausanne/Geneve) AB(Leiden)
Abstract:
Geneva seven colour photometry of supernova 1987A.
27-27 (PDF)
A workshop will be held at the ESO Headquarters in Garching from July 6-8, 1987 on - "The Supernova in the LMC"
28-28 (PDF)
Strömgren photometry of supernova 1987A.
ADS BibCode:
1987Msngr..47...28H
Author(s)/Affiliation(s):
Helt, B. E.; Vaz, L. P. R.; Jørgensen, H. E.
AA(Copenhagen) AB(Säo Paulo) AC(Copenhagen)
Abstract:
Strömgren photometry of supernova 1987A.
29-29 (PDF)
Detection of the diffuse IS band at λ5780 Å in the Large Magellanic Cloud.
ADS BibCode:
1987Msngr..47...29V
Author(s)/Affiliation(s):
Vladilo, G.
AA(Trieste)
Abstract:
Detection of the diffuse IS band at λ5780 Å in the Large Magellanic Cloud.
29-29 (PDF)
The Temperature of 1987A
29-30 (PDF)
Fast photometry of 1987A.
ADS BibCode:
1987Msngr..47...29B
Author(s)/Affiliation(s):
Barwig, H.; Schoembs, R.; Cristiani, S.; Gouiffes, C.; Sauvageot, J. L.
AA(München) AB(München) AC(ESO) AD(ESO) AE(ESO)
Abstract:
Fast photometry of 1987A.
30-31 (PDF)
Chronology of a once-in-a-lifetime event.
ADS BibCode:
1987Msngr..47...30W
Author(s)/Affiliation(s):
West, R. M.
AA(ESO)
Abstract:
Only 48 hours separate the two photos above. but during this brief interval an event happened that excited an entire generation of astronomers. Reflecting the importance of this supernova, the Central Bureau for Astronomical Telegrams issued no less than 15 IAU Circulars in the course of 9 days only. breaking all records in the history of astronomy. At ESO, these circulars were read through a computer link to the Headquarters in Garching as soon as they were issued, and immediately sent on to the observers at La Silla by telefax. In this way, and also by numerous telex messages and phone calls, the scientists were kept informed about what was going on in other places.
32-33 (PDF)
The spectrum of supernova 1987A.
ADS BibCode:
1987Msngr..47...32F
Author(s)/Affiliation(s):
Fosbury, R.
AA(ST-ECF)
Abstract:
In the early phase of a supernova, the dense atmosphere of the progenitor star is blasted off with a high velocity. This surface radiates like a "black-body" and, as such emits a continuous spectrum which is essentially independent of the chemical composition and whose energy distribution is determined solely by its temperature: the light is radiated by charged particles as they scatter off one another.
33-35 (PDF)
High-resolution spectroscopy of 1987A.
ADS BibCode:
1987Msngr..47...33A
Author(s)/Affiliation(s):
Andreani, P.; Ferlet, R.; Vidal-Madjar, R.
AA(IAP, Paris) AB(IAP, Paris) AC(IAP, Paris)
Abstract:
High-resolution Spectroscopy of 1987A
36-38 (PDF)
CASPEC observations of sdO stars - Are some sdOs lazy remnants from the AGB?
ADS BibCode:
1987Msngr..47...36H
Author(s)/Affiliation(s):
Heber, U.; Hunger, K.
AA(Kiel, Sternwarte der Universitaet, West Germany), AB(Kiel, Sternwarte der Universitaet, West Germany)
Abstract:
Eight newly discovered subdwarf O stars which were observed in the blue spectral range (3900-4800 A) are analyzed. Strong lines of ionized helium are present in all eight stars whereas He I is very weak or even absent. This indicates very high effective temperatures (greater than 55,000 K). The NLTE analyses revealed the existence of a new group of sdO stars that were once CSPNs but were born again just before they reached the hot end of the cooling sequence of white stars; a last thermal pulse brought them back to life as a post-AGB star.
References:
Faulkner, D.J., Wood, P.R.: 1984, Proc. ASA
5,543.
Giddings, J. R.: 1980, Ph. D. thesis, UCL,
London.
Groth, H. G., Kudritzki, R. P., Heber, U.: 1985,
Aslfon.Aslfophys. 152, 107.
Heber, U., Kudritzki, R. P.: 1986, Astron. Astrophys.
169,244.
Hunger, K., Gruschinske, J., Kudritzki, R. P.,
Simon, K. P.: 1981, Astron. Astrophys. 95,
244.
Husfeld, D.: 1986, Ph. D. thesis, München.
Husfeld, D., Heber, U., Drilling, J. S.: 1986,
Proc. IAU Coll. No. 87, p. 353.
Iben, I.Jr.: 1982, Astrophys. J. 260, 822.
Iben, I.Jr., Kaler, J. B., Truran, J. W., Renzini,
A.: 1983, Astrophys. J. 264,605.
Kudritzki, R. P., Simon, K. P.: 1978, Astron.
Astrophys. 70, 653.
Memdez, R. H., Kudritzki, R. P., Simon, K. P.:
1981, Astron. Astrophys. 101,323.
Schönberner, D.: 1979, Astron. Astrophys.
79, 108.
Schönberner, D.: 1983, Astrophys. J. 272,
708.
Simon, K.P.: 1980, Ph.D. thesis, Kiel.
39-41 (PDF)
P/Halley: characterization of the coma dust by polarimetry.
ADS BibCode:
1987Msngr..47...39D
Author(s)/Affiliation(s):
Dollfus, A.; Suchail, J.-L.
AA(Observatoire de Paris) AB(Observatoire de Paris)
Abstract:
The new photopolarimeter of Observatoire de Paris, at Meudon, was first used on Comet P/Hailey with the 1OO-em teleseope of Meudon Observatory from September to Deeember 1985. After full tests were seeured and eomet polarization measurements reeorded, the instrument was paeked and shipped to La Silla for an intensive polarization analysis of the eomet with the 1.52-m ESO speetroseopie teleseope. Nine nights were alloeated from 7 to 16 April, 1986. Of these, eight nights showed a perfeet sky with exquisit seeing! In addition, the teleseope, perfeetly weil adapted for the purpose, was aeeurately operated by Messrs. Miranda and Borguez, under the supervision of Mr. Le Saux.
References:
Dollfus, A., Suehail, J. -L., Crussaire, D.,
Killinger, R. (1987): Comet Halley: Dust
eharaeterization by photopolarimetry. To
be published in Proe. ESA Symposium Exploration
of Halley's Comet, Heidelberg,
FRG, 27-31 Oel. 1986
41-42 (PDF)
Multiple object redshift determinations in clusters of galaxies using OCTOPUS
ADS BibCode:
1987Msngr..47...41M
Author(s)/Affiliation(s):
Mazure, A.; Proust, D.; Sodre, L.; Lund, G.; Capelato, H.
AA(Meudon, Observatoire, France), AB(Meudon, Observatoire, France), AC(IAG, Sao Paulo, Brazil), AD(Nice, Universite, France) AE(Sao Jose dos Campos, Brasil)
Abstract:
The ESO multiobject facility, Octopus, was used to observe a sample of galaxy clusters such as SC2008-565 in an attempt to collect a large set of individual radial velocities. A dispersion of 114 A/mm was used, providing spectral coverage from 3800 to 5180 A. Octopus was found to be a well-adapted instrument for the rapid and simultaneous determination of redshifts in cataloged galaxy clusters.
References:
Carter, D.: 1980, Mon. Not. Roy. Astron.
Soc., 190, 307.
Mazure, A., Gerbal, D., Proust, D., Capelato,
H.V.: 1986, Astron. Astrophys. 157,159.
Mellier, Y., Mazure, A., Mathez, G., Chauvineau,
B., Proust, D.: 1987, preprint.
Visvanathan, N., Sandage, A.R.: 1977,Astrophys.
J., 216, 214.
41-41 (PDF)
Messenger Index
43-46 (PDF)
Coronography at La Silla - High resolution imaging of faint features near bright objects
ADS BibCode:
1987Msngr..47...43P
Author(s)/Affiliation(s):
Paresce, F.; Burrows, C.
AA(Space Telescope Science Institute, Baltimore, MD), AB(ESA, Space Science Dept., Paris, France)
Abstract:
Techniques devised for high resolution imaging of faint features near bright objects are described. A simple coronograph mated to the 2.2-m Cassegrain telescope at La Silla was used. Images of Alpha and Beta Pictoris and R Aquarii are presented.
References:
1. Burrows, C., F. Paresce, and A. Evzerov.
Instrumentation and Data Reduction
Techniques for the Detection of Circumstellar
Material, B.A.A.S., 18, 1027, 1986.
2. Paresce, F. and C. Burrows, Wide Band
Imaging of the Beta Pictoris Circumstellar
Disk, BAA.S., 18, 1027, 1986.
3. Gillett, F.C., "IRAS Observations of Cool
Excess around Main Sequence Stars", in
Light on Dark Matter, ed. F. T. Israel, D.
Reidel, 61,1986.
4. Solf. J., and H. Ulrich. "The structure of
the R Aquarii Nebula", Astron. Astrophys.,
148,274,1985.
46-49 (PDF)
Search for supernovae in distant clusters of galaxies
ADS BibCode:
1987Msngr..47...46H
Author(s)/Affiliation(s):
Hansen, L.; Jorgensen, H. E.; Norgaard-Nielsen, H. U.
AA(Universitetets Astronomiske Observatorium, Copenhagen, Denmark), AB(Universitetets Astronomiske Observatorium, Copenhagen, Denmark), AC(Dansk Raumforskninginstitut, Lyngby, Denmark)
Abstract:
A project initiated in September 1986 to find SNe I in elliptical galaxies is described. The results of five runs on the Danish 1.5-m telescope are discussed. Particular attention was given to clusters with z in the range of 0.2-0.4.
References:
(1) Tammann, G. A.: 1979, in Astronomical
Uses of the Space Telescope, proceedings
from the ESNESO workshop, ed.
Macchetto et al.
(2) Stobie, R. S., Sagar, R., and Gilmore, G.:
1985, Astron. Astrophys. Suppl. 60, 503.
(3) Koo, D. C., Kron, R.G., and Cudworth,
K. M.: 1986, Publ. Astron. Soc. Pacific 98,
285.
49-50 (PDF)
On the rates of radiation events in ESO CCDs.
ADS BibCode:
1987Msngr..47...49D
Author(s)/Affiliation(s):
D'Odorico, S.; Deiries, S.
AA(ESO) AB(ESO)
Abstract:
Radiation events (cosmic rays and local radiation) stand out in exposures taken with thinned CCD devices as spikes covering 1-4 pixels. Their intensities vary from about one hundredth electrons (the lower detection limit) above the background to a few thousand for the most energetic events. In front-illuminated, thick CCOs energetic particles can produce a short track of electrons as they cut diagonally through the silicon layer.
50-51 (PDF)
New Technology Telescope taking shape.
ADS BibCode:
1987Msngr..47...50T
Author(s)/Affiliation(s):
Tarenghi, M.
AA(ESO)
Abstract:
As an intermediate step towards a very large telescope (VLT), ESO decided to design and build a New Technology Telescope (NTT) with a mirror measuring 3.5 m in diameter. This telescope will help reduce demand on the 3.6 m telescope and will offer an opportunity for practical testing of new ideas for telescope design.
51-52 (PDF)
NTT control/acquisition software.
ADS BibCode:
1987Msngr..47...51R
Author(s)/Affiliation(s):
Raffi, G.
AA(ESO)
Abstract:
In these months, while the main mechanical and optical components are being prepared for the NTT, the control software has also to meet its first deadlines. In a few months, members of the Electronics Group will be testing the main telescope movements at INNSE in Brescia.
53-54 (PDF)
New CCD control camera and first test of a TEK 512 CCD at La Silla.
ADS BibCode:
1987Msngr..47...53D
Author(s)/Affiliation(s):
D'Odorico, S.
AA(ESO)
Abstract:
At the beginning of February 1987 a new CCD control camera has been successfully installed at the 3.6-m telescope by R. Reiß and P. Sinclaire. It will be used with all of the CCD-based instruments like CASPEC, EFOSC and the B & C spectrograph. The camera is a so-called generation V system from Princeton Scientific Instrument. It has been interfaced to the standard ESO computer in Garching in such a way that the observers will not detect any difference in the contral programme of the instruments. Notable advantages with respect to the previous system come from the use of electranic components of improved quality, such as the on-chip amplifiers and high speed 16-bit converters, shorter read-out time and a simplified pracedure in the set-up of different CCO types.
53-53 (PDF)
ESO Image Processing Group: MIDAS Memo
ADS BibCode:
1987Msngr..47...53.
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
The plotting facilities have been upgraded with many new features such as negative increments on axes and overplot of error bars. The INTAPEIFITS command was updated so that it now reads blocked FITS tapes according to the agreement of the FITS committees i. e. a physical blocking factor of up to 10 is allowed. The Dicomed commands have been upgraded to allow for spooling of the output files. That means the BI Wand colour mode can be used simultaneously at ESO/Garching.
54-54 (PDF)
New Staff Association Committee in Garching
54-54 (PDF)
Staff Movements
55-59 (PDF)
Multiobject spectroscopy with EFOSC: observation of the cluster A 370.
ADS BibCode:
1987Msngr..47...55D
Author(s)/Affiliation(s):
Dupin, J. P.; Fort, B.; Mellier, Y.; Picat, J. P.; Soucail, G.; Dekker, H.; D'Odorico, S.
AA(Observatoire de Toulouse, France) AB(Observatoire de Toulouse, France) AC(Observatoire de Toulouse, France) AD(Observatoire de Toulouse, France) AE(Observatoire de Toulouse, France) AF(ESO) AG(ESO)
Abstract:
Since the first experiment with Multiple Object Spectroscopy (MOS - see The Messenger 41, September 1985) made on EFOSC, the announced new facility called PUMA 2 has been implemented. This is a smalI, computercontrolled punching machine with which the observer (on the site and during his own run) can make the aperture masks he or she needs.
References:
Bruzual, A. G., 1981, PhO Thesis.
Butcher, H., Oemler, A. and Wells, O. C.,
1983, Ap. J. Suppl. 52, 183.
D'Odorico, S., Dekker, H., 1986, Proceedings
of the ESO-OHP Workshop on the Optimization of
the Use of CCD Oetectors in
Astronomy, J. P. Baluteau and S.
D'Odorico eds., published by ESO, 315.
Fort, B., Mellier, Y., Picat, J. P., Rio, Y. and
Lelievre, G., 1986, Proc. SPIE Instrumentation
in Astronomy VI, Vol. 627, 321.
Guiderdoni, B., 1986, PhO Thesis.
Guiderdoni, B., and Rocca-Volmerange, B.,
1987, in preparation.
Hornes, K., 1986, Publ. Astr. Soc. Pac., 98,
609.
Mellier, Y., Fort, B., Mathez, G., and Soucail,
G., 1987, in preparation.
Soucail, G., Mellier, Y., Fort, B., Picat, J. P.
and Cailloux, M., 1987, submitted to Astron.
Astrophys.
59-60 (PDF)
Spanish Summary (Nuevos meteoritos encountrados en lmilac)
ADS BibCode:
1987Msngr..47Q..59.
Author(s)/Affiliation(s):
ESO
AA(ESO)
Abstract:
Desde tiempos prehistoricos han sido coleccionadas piedras que caen dei cielo. Hasta hace poco eran la unica fuente para hacer estudios de laboratorio de la materia extragal, ktica, e incluso en nuestra era espacial, siguen siendo una valiosa fuente de investigacion de la temprana historia dei sistema solar. Se estima que como termine medio cada kilometro cuadrado de la superficie terrestre es golpeada cada millon de aiios por un meteorito con un pese superior a 500 gramos. La mayoria se pierden en los oceanos 0 caen en regiones con escasa poblacion. Como resultado, los museos en el munda reciben anualmente tan solo alrededor de 6 meteoritos cuya caida fuera atestiguada. Otros llegan por hallazgos casuales que en la mayoria de los casos son meteoritos que han cardo en tiempos prehistoricos.
59-59 (PDF)
Note Added in Proof