Messenger No. 52 (June 1988)

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1-3 (PDF)
H. van der Laan
Key programmes on La Silla: first round.

ADS BibCode:
van der Laan, H.
AA(Director General, ESO)
My request in the Messenger No. 51 for reactions has met an ampie response. Numerous letters, phone calls and visiting astronomers dropping by in my office supplemented some sixty preliminary proposals on the forms designed for that purpose. In this article I wish to report briefly about the composition and extent of this response.
3-4 (PDF)
H. van der Laan
Key programmes on La Silla: first round.

ADS BibCode:
van der Laan, H.
AA(Director General, ESO)
The following statement is a set of premisses and principles for a data-archiving policy which ESO will implement gradually in the next several years. It has been discussed in the Users Committee, in the Scientific-Technical Committee and in the Observing Programmes Committee. All three committees approve of this policy intent.
4-5 (PDF)
F. Merkle
2nd NOAO/ESO Conferenceon "High Angular Resolution by Interferometry"

ADS BibCode:
Merkle, F.
In 1985 the Director of the National Optical Astronomy Observatories (NOAO), J. Jefteries, and the Director General of ESO, L. Woltjer, stimulated the idea of having regular workshops jointly organized by the two institutions.
4-4 (PDF)
Staff Movements

ADS BibCode:
4-4 (PDF)
Diskettes for "Astronomy and Astrophysics" (First Announcement)

ADS BibCode:
5-7 (PDF)
F. Merkle
The VLT adaptive optics prototype system: status May 1988.

ADS BibCode:
Merkle, F.
In 1987 ESO decided to develop and construct an adaptive optics prototype system. This initial step into the field of adaptive optics at ESO has been taken in collaboration with the French three institutions ONERA, CGE-Laboratoires de Marcoussis, and the Observatoire de Paris-Meudon (DESPA). The system is dimensioned for F/8 focus of the ESO 3.6-m telescope and the 1.52-m telescope of the Observatoire de HauteProvence. It operates as a polychromatic adaptive system (see Fig. 1), i. e. it is equipped with an infrared camera for image detection in the 3 to 5 micron-meter range while its wavefront sensor works in the visible. It uses a deformable mirror with 19 actuators while the wavefront is sensed at 10 x 10 subapertures. It serves as a testbench for the various elements of an adaptive system and the modal control algorithms.
7-8 (PDF)
L. Zago
Latest studies lead to revised design of the VLT enclosure.

ADS BibCode:
Zago, L.
Like for many other systems of such an innovative project as the VLT, the design process of the enclosure is necessarily iterative. Those who have followed the evolution of the project from its beginning will remember the first concept which presented the arrangement of the four telescopes observing in the open air, behind a large wind shield and with mobile shelters for daytime and weather protection. Then inflatable domes were proposed: the resulting enclosure was certainly much lighter, more elegant and above all cheaper.
8-9 (PDF)
L. Zago
Inflatable VLT dome prototype erected at La Silla.

ADS BibCode:
Zago, L.
The 15-metre inflatable dome prototype has been erected at La Silla. First tests took place at the beginning of March and at the time these lines are written the dome is already sheltering a telescope, a new 40-cm seeing monitor which is being tested there previously to its installation at Cerro Vizcachas near La Silla.
9-9 (PDF)
SN 1987A (continued)

ADS BibCode:
9-9 (PDF)
M. Sarazin
Site evaluation for the VLT: seeing monitor No. 2 tested in Garching.

ADS BibCode:
Sarazin, M.
The ESO parking lot in Garching must be eliminated from the list of candidate sites for the VLT. During the night of April 19, the second seeing monitor (Fig. 1) underwent final full scale tests before being shipped to La Silla. It was an opportunity to verify that the seeing in Garehing is not of the quality that the VLT deserves. During the few minutes we had before the instruments were covered with condensed water, an average seeing of 3 arcsec was measured. (Not all that bad for Europe, though!)
10-11 (PDF)
M. Tarenghi, R. H. Wilson
With its optics complete, the NTT telescope homes in.

ADS BibCode:
Tarenghi, M.; Wilson, R. H.
On 11 May 1988 an important event took place for the development of telescope technology at ESO: the NTT optics was successfully tested at Carl Zeiss, FRG. This means that the three mirrors (primary, secondary and Nasmyth) are finished and within specification. The interferometric data currently available for the primary refer to this mirror on its manufacturing support (see Fig. 1). A further series of tests of the primary is scheduled for 1 July on the actual NTT support in its Gell. Final acceptance will take place in the finished, functioning telescope in La Silla at the beginning of March 1989.
11-13 (PDF)
G. Baier, J. Eckert et al.
Speckle masking observations of the central object in NGC 3603, Eta Carinae, and the Seyfert galaxies NGC 7469 and NGC 1068.

ADS BibCode:
Baier, G.; Eckert, J.; Hofmann, K.-H.; Mauder, W.; Schertl, D.; Weghorn, H.; Weigelt, G.
AA(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany) AB(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany) AC(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany) AD(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany) AE(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany) AF(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany) AG(Physikalisches Institut, Universität Erlangen-Nürnberg, F.R. Germany)
Speckle masking bispectrum processing yields diffraction-limited images in spite of image degradation by the atmosphere and by telescope aberrations. For example, with the ESO 3.6-m telescope a resolution of 0:'028 can be obtained at λ - 400 nm. The limiting magnitude is - 18^m.
Hofmann, K.-H., Weigelt, G., 1986, Astron.
Astrophys. 167, L 15.
Hofmann, K.-H., Weigelt, G., 1988, "Speckle
masking observation of Eta Carinae" (submitted
to Astron. Astrophys.).
Lohmann, A. W., Weigelt, G., Wirnitzer, S.,
1983, Appl. Opt. 22, 4028.
Weigelt, G., 1977, Opt. Commun. 21, 55.
Weigelt, G., Wirnitzer, S., 1983, Opt. Left. 8,
14-16 (PDF)
E. J. Wampler, A. Richichi
Observations of the antique wind of SN 1987 A

ADS BibCode:
Wampler, E. J.; Richichi, A.
AA(European Southern Observatory, Garching, Federal Republic of Germany), AB(European Southern Observatory, Garching, Federal Republic of Germany)
Green spectra obtained for SN 1987 A in the last days of 1987 show strong, narrow lines of forbidden O III. Arguments are presently adduced for the characterization of these observation results as indications of fluorescence radiation that is due to the ionization, by SN 1987 A's UV flash, of a shock front that had been generated in the progenitor wind during the star's progression from red to blue supergiant stage. The red supergiant wind is designated 'antique' to emphasize that it stopped blowing at about the time when human civilization began.
Fransson, C., Cassatella, A., Gilmozzi, R.,
Panagia, N., Wamsteker, W., Kirshner,
R. P. and Sonneborn. G. 1988, Astrophys.
J. (in press).
Vidal-Madjar, A., Andreani, P., Cristiani, S.,
Ferlet, R., Lang, 1. and Vladilo, G. 1987,
Astron. Astrophys. 177, L 17.
Woosley, S. E. 1988, Astrophys. J. (in press)
and private communication.
16-18 (PDF)
M. della Valle, E. Cappellaro et al.
Deep photometry of supernovae

ADS BibCode:
della Valle, M.; Cappellaro, E.; Ortolani, S.; Turatto, M.
AA(Padova, Universita, Padua, Italy), AB(Osservatorio Astronomico, Asiago, Italy), AC(Osservatorio Astronomico, Asiago, Italy), AD(Osservatorio Astronomico, Asiago, Italy)
Photometric observations of SNs have been initiated at intermediate and late stages, extending to much fainter limits the extensive SN survey of Rosino over the last 30 years. The correspondence between observed and estimated magnitudes via linear decline for the objects of the sample is judged to be good. Before ascertaining the intrinsic object properties, the reddening due to the galactic and internal absorption of the parent galaxy must be taken into account. Also noted are the features of SN 1986 g in NGC 5128.
Ardeberg, A.L., de Groot, M. 1974, Supernovae
and Supernova Remnants ed. C. B.
Cosmovici, Reidel, Dordrecht 45, 103.
Barbon, R., Cappellaro, E., Turatto, M., 1984,
Astron. Astrophys., 135, 27.
Phillips, M.M., et al. 1987, Pub.A.S.P., 99,
Schaeler, B., 1987a, Ap.J., 323, L51.
Schaefer, B., 1987B, Ap.J., 323, L47.
Sutherland, P. G., Wheeler, J. C. 1984, Ap. J.,
19-21 (PDF)
B. J. Jarvis, P. Dubath
A hole in the hat or evidence for a black hole in the Sombrero galaxy?

ADS BibCode:
Jarvis, B. J.; Dubath, P.
AA(Observatoire de Geneve, Switzerland) AB(Observatoire de Geneve, Switzerland)
Studies of the nuclei of normal galaxies have received renewed interest in the past few years partially due to new detector technology, particularly CCD's, used in both direct imaging and spectroscopic modes. This has led to the understanding that the nuclei of some of these galaxies are dynamically complex systems exhibiting unusual kinematic and photometric behaviour compared to the surrounding bulge. The most notable examples are M87 (eg. Sargent et al., 1978), M31 (eg. Kormendy, 1988) and M32 (Dressler and Richstone, 1987). High spatial resolution kinematic data of the nuclei of these galaxies revealed the presence of large increases in velocity dispersion and large velocity gradients over the central few arcseconds. Both of these studies concluded that a central black hole most adequately explained the very large increase in central mass-to-light ratio.
Burkhead, M. S.: 1986, Astron. J 91, 777.
Dressler, A., Richstone, D.0.: 1987, Astrophys.
J 324, 701.
Jarvis, B.J., Dubath, P.: 1988, Astron. Astrophys.,
in press.
Kormendy, J.: 1988, Astrophys. J 325, 128.
Kormendy, J., lllingworth, G.: 1982, Astrophys.
J, 256, 460, KI.
Sargent, W. L. W., Young, P.J., Boksenberg,
A., Shortridge, K., Lynds, C. R., Hartwick,
D.A.: 1978, Astrophys. J 221, 731.
Schechter, P. L.: 1983, Astron. J Supp. 52,
Schweizer, F.: 1978, Astrophys. J 220, 98.
Whitmore, B. C., Kirshner, R. P., Schechter,
P. L.: 1979, Astrophys. J 234, 68.
Williams, T. B.: 1977, Astrophys. J. 214, 685.
21-23 (PDF)
C.-I. Lagerkvist, G. Hahn et al.
Physical studies of asteroids

ADS BibCode:
Lagerkvist, C.-I.; Hahn, G.; Lindgren, M.; Magnusson, P.
AA(Astronomiska Observatoriet, Uppsala, Sweden), AB(Astronomiska Observatoriet, Uppsala, Sweden), AC(Astronomiska Observatoriet, Uppsala, Sweden), AD(Astronomiska Observatoriet, Uppsala, Sweden)
An account is given of the variation in spin rate with mean distance from the sun that is exhibited by M-type asteroids whose diameters are smaller than 140 km. Comparisons are made with data for 36 C-type and 55 S-type asteroids. Attention is given to JHK broadband photometry, which yields color indices useful in the division of asteroids into different taxonomic classes, and IDS spectra of asteroids, which contribute to knowledge about the composition of asteroid surfaces and albedo variations.
(1) Lagerkvist, C.-I., Hahn, G., Magnusson,
P., Rickman, H.: 1987, "Physical studies
of asteroids XVI: photoelectric photometry
of 17 asteroids", Astron. Astrophys.
Suppl. Ser. 70, 21-32.
(2) Hahn, G., Lagerkvist, C.-I.: 1988, "Physical
studies of asteroids XVII: JHK photometry
of selected main-belt and nearEarth
asteroids", learus, in press.
(3) Lagerkvist, C.-I., Barucci, M.A., Capria,
M.T., Fulchignoni, M., Guerriero, L.,
Perozzi, E. and Zappala, V.: 1987, Asteroid
Photometrie Catalogue, Consiglio
Nazionale Delle Ricerche, Rome.
(4) Lagerkvist, C.-I., Magnusson, P.: 1988,
"An investigation of asteroid lightcurve
shapes", learus, in prep.
(5) Hahn, G., Lagerkvist, C.-I.: 1988,
"Ephemerides of asteroids of type M and
related types", Uppsala Astron. Obs.,
Rep. No. 46.
(6) Magnusson, P.: 1986, "Distribution of
spin axes of rotation for 20 large asteroids",
learus 68, 1.
(7) Lagerkvist, C.-I., Harris, A. W., Zappala,
V.: 1987. Asteorids II machine-readable
data base: March 1988 version, National
Space Seience Data Center, Greenbelt
(8) Hahn, G., Lagerkvist, G.-I., Magnusson,
P., Rickman, H.: 1986, "Physical Studies
of Asteroids XIII: IDS spectra of selected
asteroids", in Asteroids, Comets, Meteors
11. Eds. C.-I. Lagerkvist, B.A. Lindblad, H.
Lundstedt, H. Rickman, Uppsala University,
p. 93.
24-27 (PDF)
F. Bertola, M. Vietri et al.
Are bulges of disk galaxies triaxial? Evidence from the photometry and the gas dynamics.

ADS BibCode:
Bertola, F.; Vietri, M.; Zeilinger, W. W.
AA(Dipartimento di Astronomia, Universita di Padova, Italy) AB(Osservatorio Astrofisico di Arcetri, Firenze, Italy) AC(Dipartimento di Astronomia, Universita di Padova, Italy)
It is now generally accepted that elliptical galaxies are triaxial in shape. There are at least two strong observational hints that this is indeed the case: the first one is the well-known fact that elliptical galaxies are, normally, slow rotators (Bertola 1972; Bertola and Capaccioli 1975; IIlingworth 1977) whose shape is not due to rotation and therefore must be due to the flattening of their velocity dispersion ellipsoids. This makes it likely that the dispersion velocity tensor is flattened also along the intermediate axis, so that the resulting galaxy's figure is triaxial, rather than oblate. Secondly, elliptical galaxies show radial variations in ellipticity and position angle of their apparent major axis (Bertola and Galletta 1979). a phenomenon that cannot occur if their shape is prolate or oblate. This observational evidence is supported by theory: we know now that several galaxy-formation scenarios (Aarseth and Binney 1978; see also Lake, and White 1987 for reviews) exist where collapse of the proto- c1oud in its three main directions occurs on different timescales, making a triaxial object the most likely end-product of the scenario. Also, we know that tri axial stellar-dynamical models exist, which are stationary (except for perhaps a slow figure rotation), and stable to at least the grossest instabilities (Schwarzschild 1979).
Aarseth, S. J. and Binney, J. J., 1978. Mon.
Not. Roy. Astr. Soc., 185, 227.
Bertola, F., 1972. in Proc. 15th Meeting ofthe
Ital. Astron. Soc.
Bertola, F. and Capaccioli, M., 1975. Astrophys.
J., 200, 439.
Bertola, F. and Galletta, G., 1979. Astron.
Astrophys., 77, 363.
Bertola, F., Bettoni, D., Danziger, J., Sadler,
E. M. and de Zeeuw, T., 1988, in preparation.
Beronson, T., 1981. Astroph. J. Suppl. Ser.,
Capaccioli, M. and Vietri, M., 1988. Mon. Not.
Roy. Astr. Soc., in press.
Davies, R.L., 1987. in Structure and Dynamics
of Elliptical Galaxies, I. A. U. Symp.
127, ed. T. de Zeeuw (Dordrecht:Reidel)
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J., 303, L45.
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Nachr., 304, 21.
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Roy. Astr. Soc., 223, 377.
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Reidel) p. 399.
Lllingworth, G., 1977. Astrophys. J., 204, 73.
Kormendy, J., 1982. Astrophys. J., 257, 75.
Lake, G., 1987, in Structure and Dynamics of
Elliptical Galaxies, I. A. U. Symp. 127, ed. T.
de Zeeuw (Reidel) p. 331.
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Zaritsky, D. and Lo, K. Y., 1986. Astrophys.
J., 303, 66.
27-32 (PDF)
T. J.-L. Courvoisier, A. Lauberts
Simulations of high redshift galaxies and observations with the Hubble Space Telescope

ADS BibCode:
Courvoisier, T. J.-L.; Lauberts, A.
AA(European Southern Observatory, Garching, Federal Republic of Germany), AB(European Southern Observatory, Garching, Federal Republic of Germany)
In order to evaluate the observational capabilities of the Hubble Space Telescope's Wide-Field Camera in the case of random fields, a simulation program was conducted on the basis of observations of a set of 14 nearby galaxies of all Hubble types using the ESO Schmidt telescope in B and R, which had been digitized and calibrated. The galaxies were shifted to different distances, scaling their angles as would be appropriate for the chosen Friedmann cosmology.
Rosa and Baade 1986, The Messenger 45.
Coleman, Wu and Weedman, 1980, Ap. J. Supp. 43, 393.
32-33 (PDF)
List of ESO Preprints

ADS BibCode:
33-35 (PDF)
J. Hesselbjerg Christensen
Large scale deviations from the Hubble flow.

ADS BibCode:
Hesselbjerg Christensen, J.
AA(The Niels Bohr Institute, University of Copenhagen,Denmark)
All standard Big Bang cosmologies have one thing in common. The initial state from which the Universe has developed, was homogeneous and isotropic to a "very high degree". Indeed we now observe that the distribution of galaxies is very homogeneous and isotropic when smoothed over a suitable large area of the sky. Also we observe that galaxies recede from one another in a universal manner described by the Hubble law, and this law is considered as valid on sufficiently "Iarge scales". There is additional observational evidence in the "very high degree" of isotropy of the microwave background radition, neglecting the very weil understood dipole anisotropy for the moment.
Aaronson, M., Bothun, G.D., Mould, J. R.,
Huchra, J., and Schommer, R.A., 1986.
Ap. J. 302, 536.
Fixen, D.J., Cheng, E.S., and Wilkinson,
D.T.,1983, Phys. Rev. Lett. 50, 620.
Giraud, E., 1987. The Messenger No. 49, 20.
Lynden-Bell, D., Faber, S. M., Burstein, D.,
Davies, R. L., Dressler, A., Terlevich, R. T.,
and Wegner, G., 1988. Ap. J. 326, 19.
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and Roberts, M.S., 1976. Ast. J. 81, 719.
Wyse, R.F.G., 1982, M.N.R.A.S. 199, 1P.
35-39 (PDF)
A. Bragaglia, L. Greggio et al.
Searching for double degenerates.

ADS BibCode:
Bragaglia, A.; Greggio, L.; Renzini, A.; D'Odorico, S.
AA(Dipart. di Astronomia, Universita di Bologna, Italy) AB(Dipart. di Astronomia, Universita di Bologna, Italy) AC(Dipart. di Astronomia, Universita di Bologna, Italy) AD(ESO)
The majority of stars are members of binary systems; this is a frequently referred aphorism. The majority of stars also terminate their evolution as white dwarfs (WDs), as only few stars are born massive enough to experience a supernova explosion. We can easily conclude that the majority of binary systems must at some stage become a double WD binary, and that a good fraction of the stars listed in our catalogues as WDs may indeed be double.
Canizares, C. R., Fabbiano, G., Trinchieri, G.
1987, Ap. J., 312, 503.
Fabbiano, G. 1986, PASP, 98, 525.
Greenstein, J. L. 1986, Ap. J 92, 867.
Greggio, L., Renzini, A 1983, Astron. Astrophys.
118, 217.
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1979, Astron. Astrophys. 76, 262.
Liebert, J., Probst, R. G. 1987, Ann. Rev. Astron.
Ap. 25, 473.
39-41 (PDF)
R. Aniol, H. W. Duerbeck et al.
A search for flare stars with the GPO astrograph.

ADS BibCode:
Aniol, R.; Duerbeck, H. W.; Seitter, W. C.; Tsvetkov, M. K.
AA(Astronomisches Institut der Universität Münster, F. R. Germany) AB(Astronomisches Institut der Universität Münster, F. R. Germany) AC(Astronomisches Institut der Universität Münster, F. R. Germany) AD(Department ofAstronomy, Academy of Sciences, Sofia, Bulgaria)
The first systematic investigation of flare stars by the Mexican astronomer Guillermo Haro marks the beginning of long-term, multi-site studies of these objects in young stellar aggregates. His first series of observations with the Schmidt telescope of the Tonantzintla Observatory already showed the close relation between stars in the T Tauri stage and cool dwarf stars with enhaneed UV activity (= flare stars), both types of objects being still in their early stages of evolution.
41-44 (PDF)
M. P. Veron-Cetty, P. Veron
Dust in early-type galaxies

ADS BibCode:
Veron-Cetty, M. P.; Veron, P.
AA(Haute-Provence, Observatoire, Saint-Michel-l'Observatoire, France), AB(Haute-Provence, Observatoire, Saint-Michel-l'Observatoire, France)
The present study finds no clear evidence that radio galaxies contain dust more frequently than radio-quiet galaxies. While the galaxies detected at 100 microns by IRAS exhibit clear evidence for dust on direct images, indicating that the IR emission must be due to the dust's thermal emission, galaxies with an active nucleus may have a detectable FIR flux; in such a case, the IR emission would be associated with the activity of the nucleus.
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44-47 (PDF)
S. van Amerongen, J. van Paradijs
Long-term Walraven photometry of cataclysmic variables

ADS BibCode:
van Amerongen, S.; van Paradijs, J.
AA(Amsterdam, Universiteit, Netherlands), AB(Amsterdam, Universiteit, Netherlands)
Observations of cataclysmic variables obtained over the last seven years with the Walraven photometer of the 90-cm Dutch telescope at La Silla yield, in the case of strongly variable blue sources, simultaneous detections in five bandpasses extending from the visible through the UV. The results thus obtained to date encompass measurements of changes in the rotation periods of accreting white dwarfs in these variables, very strong upper limits to secular changes in the optical brightness of dwarf novae between outbursts, and the recognition that accretion instabilities similar to dwarf novae outbursts also occur in systems which are not thus classifiable.
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B.J.M., Heise, J., Holberg, J.B., Polidan,
R. S., van Amerongen, S. F., van der
Woerd, H., van Paradijs, J., and Verbunt,
F., 1987. Mon. Not. R. Astr. SOc.,
van Amerangen, S., Damen, E., Graot, M.,
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Verbunt, F., Hassall, B.J. M., Marang, F.,
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[5] van Amerongen, S., Bovenschen, H., and
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[8] Schwarz, H. E., and Heemskerk, M. H. M.,
1987. IAU. Circular No. 4508.
Schwarz, H. E., van Amerangen, S. F.,
Heemskerk, H. M., and van Paradijs, J.,
1988. Astr. Astrophys., submitted.
47-48 (PDF)
P. Andreani, R. Ferlet et al.
IRAS molecular clouds in the hot local interstellar medium.

ADS BibCode:
Andreani, P.; Ferlet, R.; Lallement, R.; Vidal-Madjar, A.
AA(Institut d'Astrophysique, CNRS, Paris, France, ESA Fellow on leave trom Dipartimento di Fisica, Universita di Roma, La Sapienza, Roma, Italy) AB(Institut d'Astrophysique, CNRS, Paris, France) AC(Institut d'Astrophysique, CNRS, Paris, France,Service d'Aeronomie, CNRS, Verrieres le Buisson, France) AD(Institut d'Astrophysique, CNRS, Paris, France)
The picture of the nearby (d <= 100 pC) interstellar medium, as resulting from the observations in the wavelength range from X-ray to radio, consists of a very hot, low-density gas, forming a hot bubble, filled with many cloudlets of ionized and neutral material and located near to an interstellar condensation (see the "Local Interstellar Medium", NASA CP-2345, 1984; and Cox and Reynolds, 1987).
P. Andreani, R. Ferlet, A. Vidal-Madjar, in
D. P. Cox and R. J. Reynolds, Ann. Rev. Astran.
Astroph., 25, 303 (1987).
R. Ferlet, M. Dennefeld, Astran. Astraph.,
138, 303 (1984).
L. M. Hobbs, L. Blitz and L. Magnani, Ap. J.,
L 109, (1986).
I. A. U. Colloquium 81, NASA CP-2345 (1984).
"The Local Interstellar Medium", eds. Y.
Kondo, F. C. Bruhweiler and B. Savage.
IRAS Explanatory Supplement, 1984, edited
by C.A. Beichman, G. Neugebauer, H.J.
Habing, P.E. Clegg and T.J. Chester.
R.J. Laureijs, K. Mattila and G. Schnur, Astran.
Astraph., 184, 269 (1987).
L. Magnani, L. Blitz and L. Mundi, Ap. J., 295,
402 (1985).
A. Vidal-Madjar, R. Ferlet, C. Gry, R. Lallement,
Astran. Astroph., 155, 407 (1986).
J. L. Weiland, L. Blitz, E. Dwek, M. G. Hauser,
L. Magnani, L. J. Rickard, Ap. J., 306, L101
48-48 (PDF)
Letter to the Editor

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49-50 (PDF)
M. Friedjung, A. Bianchini et al.
Rapid spectral variations of old novae.

ADS BibCode:
Friedjung, M.; Bianchini, A.; Sabbadin, F.
AA(Institut d'Astrophysique, Paris, France) AB(Osservatorio Astronomico, Padova, Italy) AC(Osservatorio Astrofisica, Asiago, Italy)
Novae are a subclass of cataclysmic variables. The latter all appear to be binary with a white dwarf component and a companion usually near the main sequence. This companion seems to fill its Roche lobe and lose mass to the white dwarf via the inner Lagrangian point. Unless the magnetic fjeld of the white dwarf is very strong, the transferred mass is expected to spiral slowly to the white dwarf in an accretion disk, whose presence explains many observations. Different kinds of cataclysmic variable exist, such as different sorts of dwarf novae with outbursts generally having an amplitude of a few magnitudes at intervals of the order of weeks. The orbital periods determined up to April 1987 (Ritter 1987) lie between 2.00 days (the nova GK Per) and 0.052 days (the dwarf nova AF Cam), with a "period gap" between 0.118 and 0.086 days (only one known period inside the gap).
Bianchini, A., Friedjung, M., Sabbadin, F.
1985 a, IBVS No. 2650.
Bianchini, A., Friedjung, M., Sabbadin, F.
1985 b, in "Multifrequency Behaviour of
Galactic Accreting Sources". Ed. F.
Giovanelli, p. 82.
Bianchini, A., Friedjung, M., Sabbadin, F.
1985c, in "Recent Results on Cataclysmic
Variables", ESA-SP 236, p. 77.
Duerbeck, H. W., Seitter, W. C., Duemmler,
R., 1987, Mon. Not. R. Astron. Soc. 229,
Friedjung, M., 1987 a, Astron. Astropl7ys.
179, 164.
Friedjung, M., 1987 b, Astron. Astropl7ys.
Ritter, H., 1987, preprint.
Warner, B., 1985, Mon. Not. R. Astron. Soc.
217,1 p.
50-51 (PDF)
A. Moorwood
Status of the ESO Infrared Array Camera -IRAC.

ADS BibCode:
Moorwood, A.
IRAC is currently being tested in Garching in preparation for its installation and first test on the 2.2-m telescope at the end of June 1988. Assuming there are no unpleasant surprises, it is intended in July/August 1988 to issue a formal announcement of its availability for visiting astronomers in Period 43, i. e. as of April 1989. In the meantime, it is hoped that this article will serve as a useful introduction to this new instrument and its observational capabilities.
51-52 (PDF)
S. D'Odorico
Optical instrumentation for the NTT: EMMI and EFOSC2.

ADS BibCode:
D'Odorico, S.
With the New Technology Telescope a little more than six months from "first light", work is going on intensively at ESO on the instrumentation to be used at the two Nasmyth foci of the telescope.
52-53 (PDF)
MIDAS Memo:ESO Image Processing Group

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52-52 (PDF)
A Note on Equivalent Widths at the CES

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53-55 (PDF)
D. Ponz, M. Tapia
IRSPEC spectra reduced within MIDAS.

ADS BibCode:
Ponz, D.; Tapia, M.
The ESO 32-channel infrared (1 -5 micron-meter) grating spectrometer, IRSPEC, was put into operation and made available for Visiting Astronomers in October 1986. In this contribution we describe the reduction scheme implemented in MIDAS to process IRSPEC data taken in any of the two - discrete or Continuous - instrumental modes. The Ins~rument itself has already been descnbed in detail in another contribution to the Messenger
1. A. Moorwood, P. Biereichel, G. Finger, J.L.
Uzen, M. Meyer, W. Nees and J.
Paureau: 1986, The Messenger, No. 44,
2. A. Moorwood: 1986, IRSPEC Operating
3. P. Biereichel: 1986, IRSPEC Software
Operating Manual.
54-54 (PDF)
ES0 Book Soon Available in Spanish and French

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55-55 (PDF)
ESO Grid Processing Machine

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55-55 (PDF)
ESO at the IAU General Assembly

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56-56 (PDF)
Libro de la ESO en venta en espanol

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56-56 (PDF)
The ESO Milky Way Panorama

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