Messenger No. 19 (December 1979)

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1-4 (PDF)
J. Lub
The Dutch telescope on La Silla.

ADS BibCode:
1979Msngr..19....1L
Author(s)/Affiliation(s):
Lub, J.
AA(ESO/Chile)
Abstract:
Welcome to La Silla! As the latest newcomer in the family of telescopes at ESO, the Dutch 90 cm "Lightcollector" has now been installed and, as expected, it performs very weil in its new environment. Dr. Jan Lub from ESO/Chile is in charge ofthis instrument and reports about its transfer from the African to the South American continent. His article also contains important information for all prospective users.
4-6 (PDF)
D. Baade
28 Canis Majoris - a short-period Be star.

ADS BibCode:
1979Msngr..19....4B
Author(s)/Affiliation(s):
Baade, D.
AA(the Astronomical Institute of the University of Münster, FRG)
Abstract:
Are Be stars nothing but ß Cephei stars? This farreaching possibility is supported by new observations of the Be star 28 CMa, which shows spectral variations with aperiod of 1.36 days. Dr. Dietrich Baade of the Astronomical Institute of the University of Münster, FRG, recently obtained spectra of this star with the large coude spectrograph at the ESO 1.52 m te/escope. Here is his report about this important discovery.
6-6 (PDF)
ESO
List of Preprints Published at ESO Scientific Group

ADS BibCode:
1979Msngr..19....6.
Author(s)/Affiliation(s):
ESO
AA(ESO)
7-10 (PDF)
B. E. Westerlund
Red stars in nearby galaxies.

ADS BibCode:
1979Msngr..19....7W
Author(s)/Affiliation(s):
Westerlund, B. E.
AA(the Uppsala Observatory in Sweden)
Abstract:
The study of the very cool stars in our Galaxy and in other galaxies is of great importanee for our understanding of galaxy evolution. The first step in such an investigation is to identify these stars among the numerous warmer ones. Various seareh teehniques are available and are here deseribed by Professor Bengt Westerlund from the Uppsala Observatory in Sweden and formerly ESO Direetor in Chile. In partieular, the new GRISMs at the prime foeus of the 3.6 m teleseope allow the deteetion of even very faint M, C and S stars. The extremely promising results of the initial observations are diseussed by the author.
10-12 (PDF)
T. Neckel
Photometric and polarimetric observations in NGC 6334, NGC 6357 and NGC 6302.

ADS BibCode:
1979Msngr..19...10N
Author(s)/Affiliation(s):
Neckel, T.
AA(the Max-Planek-Institut für Astronomie in Heidelberg,FRG,)
Abstract:
Polarization is observed in the light ot many stars and is normally attributed to interstellar dust partieles aligned in an interstellar magnetie fjeld. It is, however, quite possible that-at least in some eases-the polarization arises in dustyen velopes, surrounding stars during the earliest phases ot their Ide. Dr. Thorsten Neekel from the Max-Planek- Institut für Astronomie in Heidelberg, FRG, has reeently obtained observations ot such objeets trom La Silla. Combining photometrie and polarimetrie measurements, it has beeome possible to provide new, important evidenee tor the intrinsie, bipolar model.
References:
Alloin, D. and Tenorio-Tagle, G.: 1979, ESO Messenger No. 18.
Cohen, M. and Kuhi, V.: 1977, Astrophys. J., 213,79.
12-12 (PDF)
ESO
Tentative Time-table of Council Sessions and Committee Meetings in 1980

ADS BibCode:
1979Msngr..19...12.
Author(s)/Affiliation(s):
ESO
AA(ESO)
13-14 (PDF)
R. M. West
A Roof Over ESO Heads

ADS BibCode:
1979Msngr..19...13W
Author(s)/Affiliation(s):
West, R. M.
AA(ESO)
Abstract:
On November 8th, 1979, another milestone in ESO history was passed. The new building for the future Headquarters in Garching, just north of Munich, was the scene of a happy celebration, on the occasion of the "setting up the roof", or "Richtfest" as it is called in Bavaria.
15-15 (PDF)
ESO
ESO Workshop on Two-dimentional Photometry

ADS BibCode:
1979Msngr..19Q..15.
Author(s)/Affiliation(s):
ESO
AA(ESO)
15-15 (PDF)
ESO
Heavyweight Technological on La Silla

ADS BibCode:
1979Msngr..19R..15.
Author(s)/Affiliation(s):
ESO
AA(ESO)
16-18 (PDF)
D. S. Brown
The prediction of on site telescope performance.

ADS BibCode:
1979Msngr..19...16B
Author(s)/Affiliation(s):
Brown, D. S.
AA(Newcastle upon Tyne)
Abstract:
The acceptance tests of an optical mirror are most often based on measurements of the slopes on its surface and the geometrical concentration of light. However, the result depends rather critically on the way of sampling and, furthermore, the final quality of the telescope is a combination (convolution) of many parameters: the optical quality, seeing, guiding, etc. Dr. D.S. Brown is responsible for the manufacturing and testing at Grubb Parson's workshop in Newcastle upon Tyne, which has recently polished the 1.5 m mirror for the new Danish telescope on La Silla and the optics for the 3.6 m CAT. Having spent most of his working life in the manufacture of astronomical optics, he has a keen interest in the prediction of actual telescope performance, based on tests in the optical shop. He explains -with a clear direction towards observing astronomers- that better test methods are now available which will let the future user know with good confidence how good (or bad) his new telescope will be, long before the first real observations are made.
18-21 (PDF)
E. J. Zuiderwijk
Neutron stars.

ADS BibCode:
1979Msngr..19...18Z
Author(s)/Affiliation(s):
Zuiderwijk, E. J.
AA(the ESO Seientifie Group in Geneva)
Abstract:
It is a common trick among astronomers who give popular lectures to shock the audience with large numbers. The statement that a matehbox of material from a white dwarf weighs as much as several large locomotives (or elephants if there are influential ecologists present) is always of great effect. But that is all antique by modern comparison. Now, one cubie millimetre of a neutron star (about the size of the head of a pin) weighs one million tons! Dr. Ed Zuiderwijk of the ESO Seientifie Group in Geneva is engaged in a theoretieal and observational study of these incredible objects. There is still much to be learned from them, both for physicists who look for the ultimate properties of matter and for astronomers who wonder how stars end their life.
21-25 (PDF)
T. Kreidl et al.
Image processing at the Astronomical Institute of the Ruhr-Universität Bochum.

ADS BibCode:
1979Msngr..19...21K
Author(s)/Affiliation(s):
Kreidl, T.; Buchholz, M.; Winkler, C.
AA(the Astronomical lnstitute of the Ruhr University in Bochum) AB(the Astronomical lnstitute of the Ruhr University in Bochum) AC(the Astronomical lnstitute of the Ruhr University in Bochum)
Abstract:
Image processing of astronomical photographs or, in general, one- and two-dimensional data, play a larger and larger role in the reduction of observations. Several institutes in Europe are acquiring their own hardware and, more recently, an effort to exchange the associated programmes, the software, has been initiated. At the Astronomical lnstitute of the Ruhr University in Bochum, image processing is already weil developed, as explain Drs. T. Kreidl and M. Buchholz together with graduate student Ch. Winkler in this review of the Bochum system.
References:
Albrecht, R., 1979: in "Proceedings of the International Workshop on Image Processing", Triest (in print).
Feitzinger, J. V., Schmidt-Kaler, Th., Schlosser, W., Winkler, Ch.,1979: Astron. & Astrophys. (in print).
Newell, S., 1979: in "Proceedings of the International Workshop on Image Processing", Triest (in print).
Schlosser, W., Schmidt-Kaler, Th., 1977: Vistas in Astronomy, 21,447.
de Vaucouleurs, G., 1973: Ap. J., 181,31.
25-26 (PDF)
West.R
When the Earth was Born

ADS BibCode:
1979Msngr..19...25W
Author(s)/Affiliation(s):
West.R
AA(ESO)
Abstract:
Astronomy offers the unique possibility of looking back in time. Contrary to other sciences, it allows us to see objects as they were a long time ago. This is of course due to the enormous distances in the Universe and the finite velocity of light: around 300,000 1/kms.
26-26 (PDF)
W. Richter
Instrumentation Schedule

ADS BibCode:
1979Msngr..19...26R
Author(s)/Affiliation(s):
Richter, W.
AA(ESO in Geneva)
Abstract:
This is an updated time schedule for the major instruments which are being developed at ESO in Geneva for use on the 3.6 m telescope. See also Messenger No. 15, p. 10. Target date is the date of "first light". Regular use starts about half a year later.
26-26 (PDF)
ESO
A New Bright Seyfert 1 Galaxy

ADS BibCode:
1979Msngr..19Q..26.
Author(s)/Affiliation(s):
ESO
AA(ESO)
26-26 (PDF)
ESO
La Silla in the Sky

ADS BibCode:
1979Msngr..19R..26.
Author(s)/Affiliation(s):
ESO
AA(ESO)
27-28 (PDF)
J. Bergeron, D. Kunth
Continuity of spectroscopic properties from nearby active galaxy nuclei to intermediate redshift quasars.

ADS BibCode:
1979Msngr..19...27B
Author(s)/Affiliation(s):
Bergeron, J.; Kunth, D.
AA(the ESO Scientific Group in Geneva) AB(the ESO Scientific Group in Geneva)
Abstract:
What are quasars? Astronomers have wondered ever since their discovery, more than 15 years ago, as a class of highly enigmatic astronomical objects. Now, however, a better understanding of the physical processes in their interiors is slowly emerging, thanks to improved observations, and it appears more or less confirmed that (most of the known) quasars are actually rather similar to the nuclei of nearby, active galaxies. Correlations between strengths of emission lines and absolute magnitude have been found. Drs. Jacqueline Bergeron and Daniel Kunth of the ESO Scientific Group in Geneva are presently studying the important question of radio-strong vs. radio-quiet quasars and report some extremely interesting observations with the 3.6 m telescope.
References:
Searle, L., and Sargent, W.L.W. 1968, Ap. J., 153, 1003.
Wampler, E.J., and Oke, J.B. 1967, Ap. J., 148,695.
Osterbrock, D. E. 1977, Ap. J., 215, 733.
Baldwin, JA 1977, M.N.R.A.S., 178,67 P.
Boksenberg, A., et al. 1978, Nature, 275,404.
Puelter, R.C., Smith, H.E., and Wiltner S.P. 1979, Ap. J., 227, L5.
Philipps, M.M. 1978, Ap.J. Suppl., 38, 187.
Osterbrock, D.E., Koski, A.T., and Philipps, M.M. 1976, Ap. J.,206,898.
Bergeron, J. 1979, Stars and Star Systems, ed. B.E. Westerlund,p.67.
Kunth, 0., and Sargent, W.L.W. 1978, Astron. Ap., 76, 50.
Baldwin, JA 1977, Ap.J., 214,679.
Veron, P. 1978, ESO preprint no. 45.
29-30 (PDF)
A. B. Muller
A supernova search with the ESO 1 m Schmidt telescope: greatly improved efficiency.

ADS BibCode:
1979Msngr..19...29M
Author(s)/Affiliation(s):
Muller, A. B.
AA(ESO)
Abstract:
Supernovae are astrophysically extremely interesting objects. It is presently believed that most, if not all, heavy elements are created when stars explode as supernovae. About ten supernovae are presently discovered each year and much thought has been given to the problem of discovering new supernovae as early as possible after the rise in luminosity, in order to study the physics of such objects in their initial phases. Dr. Andre Muller from ESO has conceived many ingenious technical solutions to a wide variety of problems. In this article, he describes a new device for the quick and efficient detection of supernovae with the ESO 1 m Schmidt telescope. The results of the first practical tests of this method will soon be available.
30-30 (PDF)
ESO
In the Mail

ADS BibCode:
1979Msngr..19...30.
Author(s)/Affiliation(s):
ESO
AA(ESO)
31-33 (PDF)
P. Crane
Data reduction facilities available at ESO in Geneva.

ADS BibCode:
1979Msngr..19...31C
Author(s)/Affiliation(s):
Crane, P.
AA(ESO/Geneva)
Abstract:
Nowadays, the astronomer is likely to spend more time at a computer terminal than at the telescope. To assure efficient reduction of the photographic plates from ESO and other telescopes, fast measuring machines have been provided at ESO/Geneva, together with advanced computer programmes for handling the large masses of data that result from these machines and other instruments. Dr. Philip Grane, who is in charge of the system, describes the present configuration and explains how visitors can request time.
33-34 (PDF)
K. Klim
The 4 cm McMullan camera for the 3.6 m telescope.

ADS BibCode:
1979Msngr..19...33K
Author(s)/Affiliation(s):
Klim, K.
AA(ESO-Geneva)
Abstract:
The testi ng in Geneva of the 4 cm McMullan Camera for the 3.6 m telescope was completed by the end of September 1979 and it is planned to ship the camera to Chile in November where tests on the telescope wi II be performed
34-34 (PDF)
ESO
Personnel Movements

ADS BibCode:
1979Msngr..19...34.
Author(s)/Affiliation(s):
ESO
AA(ESO)
35-36 (PDF)
ESO
Brave New World?

ADS BibCode:
1979Msngr..19...35.
Author(s)/Affiliation(s):
ESO
AA(ESO)
35-35 (PDF)
M. Tarenghi, M. Ziebell
3.6 m triplet adapter: tests on the telescope.

ADS BibCode:
1979Msngr..19...35T
Author(s)/Affiliation(s):
Tarenghi, M.; Ziebell, M.
AA(ESO-Geneva) AB(ESO-Geneva)
Abstract:
The first test installation of the triplet adapter on the 3.6 m telescope took place on La Silla in September 1979
37-39 (PDF)
J. V. Feitzinger, T. Schmidt-Kaler
R 136 - source of excitation of the Tarantula Nebula.

ADS BibCode:
1979Msngr..19...37F
Author(s)/Affiliation(s):
Feitzinger, J. V.; Schmidt-Kaler, T.
AA(the Astronomical Institute of the Ruhr University in Bochum, FRG) AB(the Astronomical Institute of the Ruhr University in Bochum, FRG)
Abstract:
Among the few extragalactic objects that can be seen with the naked eye, the LMC and its Tarantula Nebula (30 Doradus) are perhaps the most impressive. This nebula, a giant region of ionized hydrogen, has long attracted astronomers and has been extensively studied with a large variety of telescopes. Drs. Johannes Feitzinger and Theodor Schmidt-Kaler from the Astronomical Institute of the Ruhr University in Bochum, FRG, have recently obtained extremely interesting observations ofthe central stars in the Tarantula Nebula. It would appear that one of these objects, R136, could be the most massive single "star" that has yet been discovered.
39-40 (PDF)
ESO
Algunos Resumenes

ADS BibCode:
1979Msngr..19R..39.
Author(s)/Affiliation(s):
ESO
AA(ESO)
39-39 (PDF)
ESO
ASTEL - a FORTRAN Programme to Decipher IAU Telegrams

ADS BibCode:
1979Msngr..19Q..39.
Author(s)/Affiliation(s):
ESO
AA(ESO)