We compare the host galaxies of 902 supernovae, including Type Ia, II and Ibc, which are selected by cross-matching the Asiago Supernova Catalog with the SDSS DR7. We further selected 213 galaxies by requiring the light fraction of spectral observations > 15%, which could represent well the global properties of the galaxies. The diagrams related to Dn(4000), HδA, stellar masses, SFRs and specific SFRs for the SNe hosts show that almost all SNe II and most of SNe Ibc occur in SF galaxies. A significant fraction of SNe Ia occurs in AGNs and Absorp galaxies. These results are compared with those of the 689 comparison galaxies where the SDSS fiber captures < 15% of the total light. These comparison galaxies appear biased towards higher 12+log(O/H) (~0.1dex) at a given stellar mass, suggesting the aperture effect should be kept in mind when the properties of the hosts for different types of SNe are discussed.

We study and compare the stellar populations of host galaxies of different types of supernovae (SNe): SN Ia and core collapse SN (SN II and SN Ibc) at the same time. The 234 sample galaxies are selected by cross-matching the Asiago Supernova Catalogue (ASC) and the SDSS-DR7 main galaxy sample (MGS). The STARLIGHT software is used to analyze their stellar populations by fitting the continua and absorption lines of the hosts.

This paper presents the final discussion of the meeting, following introductory remarks by A. Ardeberg, B. Ellerbroek and C. Cunningham.

A cross-correlation between the IRAS PSC and the ROSAT All-Sky Survey has provided 242 sources detected in both surveys (Boiler et al. 1992). About half of these have redshifts in the literature and a spectral classification. An unexpected result was the discovery of many galaxies with X-ray luminosities up to a few 1043 ergs s−1, yet without Seyfert characteristics in their optical spectra (e.g., Boiler et al. 1993). To investigate this problem further and evaluate the frequency of occurrence of these peculiar objects, a spectroscopic follow-up has been undertaken to:

1. • Determine velocities and luminosities for all the unclassified objects.

2. • Reevaluate the classification of high X-ray luminosity objects previously not recognized as Seyferts. In particular, spectral resolution or coverage and variability are important parameters to consider if one wants to detect faint signs of Seyfert activity.

ROSAT All Sky Survey observations of IRAS galaxies have revealed up to now a number of (10) optically non-Seyfert galaxies with X-ray (0.1–2.4 keV) luminosities up to a few 1043erg · s−1 (Boller et al. 1992). The sources are brighter than previous detection limits of a few 1041erg · s−1 as found by Stocke et al. (1991) or Green, Anderson & Ward (1992) for Einstein sources. The optical classification is based on follow-up observations which indicate clearly the non-Seyfert (LINER and HII region-like galaxies) nature. Our investigations reveal that galaxies classified as non-Seyferts on the basis of optical spectroscopy may reach exceptionally high X-ray luminosities which are similar to that of Seyfert galaxies. On the basis of the present observational material we suppose a hidden low luminosity AGN in the centre of these objects as the source of energy production. The objects are of interest when evaluating starburst versus central activity.

The galactic Planetary Nebula G 258-15.7 is a large, bright nebula well suited for a detailed study. Known since Wray (1966), its morphology presents several blobs and ansae, generally associated with type I nebulae, and could be described as “late-butterfly” type according to the classification by Balick (1989). The central star has been classified as hydrogen-deficient by Mendez et al. (1985). Spectroscopy of the two main blobs shows a clear overabundance in He and N, with a marginally significant difference between the two sides. The most striking feature is the jet-like structure appearing on the [OIII]/Halpha picture (Fig. 1), the “jets” being located within the main blobs seen on the monochromatic images. A detailed appraisal of all the data will be presented in a subsequent paper.

We present the results from an HI survey of 160 IRAS galaxies with luminosities larger than 1010 L⊙. The observations were made with the Nanlay Radiotelescope and the overall detection rate is about 75%.

About 40 OH megamasers have been discovered up to now, occuring in luminous IR galaxies; their far-infrared (FIR) luminosities, however, span a rather large range, from a few 1010 to several times 1012 solar luminosities.

As part as of an extragalactic CH 9-cm ground-state emission survey of OH emitters (megamasers) and absorbers, we report the detections of the 3335 MHz main line in M82 and of the 3264 MHz satellite line in the luminous far infrared (FIR) galaxies NGC 3079 and NGC 5793, obtained with the Nançay radiotelescope.

The 18-cm and 21-cm surveys of luminous infrared galaxies achieved with the Nanlay radiotelescope led to the detection of OH and/or HI absorption lines in 7 bright IRAS galaxies. We show that a careful comparison of optical radial velocities and 1) HI absorption line radial velocities or 2) HI emission line radial velocities gives valuable indication on the radial motions of the circumnuclear gas in our sample of galaxies and in the IRAS galaxies studied by Mirabel and Sander (1988).

We present CaII and NaI spectra for a sample of stars in a 30'×30' field connecting 30 Dor with SN 1987A. Observations were taken with the CES spectrograph linked via fibres with the 3.6m ESO telescope at a resolution of ˜ 6 km s−1. The LMC gas shows a complex structure with both single and multiple components spanning 250 to 300 km s−1. Results can be interpreted using the multi-layer structure suggested by 21 cm observations. Comparing our optical absorptions with 21 cm emissions yields evidence that layers with increasing radial velocity are located one behind the other. The intermediate velocity components are numerous in CaII, but rare in NaI. Towards Sk-69 211, for which we have the highest S/N CaII spectrum, we have detected a number of components comparable to that found in SN 1987A. The 64 km s−1 cloud is detected in a well-confined region of the field, showing remarkable constancy in the radial velocity, which we interpret as evidence that this cloud is located close to the Galaxy.

We present results for IUE, optical and IR observations of Nova Muscae 1983, from early outburst to January 1986 obtained by the European IUE Target of Opportunity Team. A detailed description of the data will appear elsewhere (Hassall et al., 1989), but here we summarise the most important results.

The outburst lightcurve initially indicated a fast speed class for this nova, but was later characterised by a rather slow optical decline with two or more secondary outbursts with sudden doubling of the bolometric flux. In Figure 1, we show the contributions of X-ray, UV, optical and IR to the total luminosity for 1200 days following outburst, assuming a distance of 4.3kpc and an interstellar extinction E(B-V)=0.5. In the absence of dust formation, first the UV and later the X-ray flux (Ögelman et al, 1984) dominate the radiative energy late into the nebular phase. There was a plateau stage lasting about 500 days, with a bolometric luminosity of ~ 1038ergs s−1 near the Eddington limit. The secondary outbursts were thus super-Eddington. We estimate a total outburst energy (including kinetic and gravitational potential energy of the ejecta) of ~ 5·l046 ergs, corresponding to a mass of ~ 4·10−6Mº of hydrogen burnt in the thermonuclear runaway.

The detailed analysis of high resolution, high signal-to-noise spectra of four G and K dwarfs lying within 10 pc of the Sun is presented. This analysis is part of a project aiming at building up a homogeneous set of reliable atmospheric parameters for all F, G and K stars nearer than 10 pc according to the Gliese catalogue.

The powerful OH megamasers detected in IC4553 (Baan et al. 1982), NGC3690, Mrk231 (Baan, 1985; Kazès and Dickey, 1985) and Mrk273 (Bottinelli et al. 1985a) show several common properties; in particular, they are strong IR emitters. We have thus undertaken a study of the strongest far IR (100 μm) uncatalogued IRAS sources and we report here on the discovery of a new strong extragalactic maser in the IR source IRAS 17208 −0014 (Bottinelli et al., 1985b)

Two studies of OH maser emission in envelopes of late type stars -miras (3) and OH/IR objects- have been performed with the Nancay radio-telescope. Mainly, the OH miras are found with thicker dust envelopes than the non OH ones. A sample of unidentified IRAS point sources selected on their colors has been observed. We have detected 46 new OH sources. The OH detection rate is a function of the galactic longitude and of the IRAS spectral classification.

The spectral range redwards of about 7300 Angströms has up to now been rarely explored for any kind of object because of lack of adequate detectors. This situation is changing with the availability of silicon detectors whose response extends up to 1.1μ with reasonable quantum efficiency. We have used the ESO Reticon System behind the Boller and Chivens Spectrograph at the Cassegrain focus of the ESO 3.6m telescope to obtain spectra of several Supernova Remnants in the range 6000–10500 Å. The spectral resolution was 8 å and the dual array allowed a clear sky-subtraction, indispensable because of the presence of numerous atmospheric OH bands in this region. Data reduction was done with standard techniques using wavelength calibration, flat-field correction, response curve determination through observations of standard stars and extinction correction. We present below results based on the first spectra obtained for the Galactic remnants RCW 86, RCW 103 and Kepler SNR and the Magellanic Cloud ones N 49 and N 63A. The Crab Nebula will be discussed separately at the end.

The observations reported here have been obtained with the ESO Reticon system attached to the Boller and Chivens spectrograph at the 3.6 m telescope. The reciprocal dispersion was 228 A mm−1 with a useful spectral range extending from 5800 A to 11000 A. The slit was 200 µm wide which corresponds to 1.4 arcsec on the sky and to about 33.5 µm(∼ 7.6 A) in the plane of the detector. Sky substraction was performed by means of observations at 93 arcsec. East and West of the object. The correction for atmospheric extinction was based on a mean extinction curve of La Silla (Tug, 1977). As a consequence the strongest atmospheric bands are still present on the final spectra. The data were also corrected for the instrument sensitivity response by using calibrated stars selected from Breger's catalog (1976). As these reference data are from filter photometry, they are not well suited to the resolution of our spectra, at least in some regions. This problem can be significant, as clearly illustrated by Johnson (1980).

November 27, 1980, we had the opportunity to make near infrared observations of a few WR stars of the Magellanic Clouds with the ESO reticon system attached to the Boller and Chivens spectrograph at the 3.6 m telescope. The observing conditions as well as the reduction procedure have been described in another paper of this symposium (Vreux et al., 1982). We will immediately show how the near infra-red can be useful to improve our knowledge of some WR stars.

Among the 0 stars, Conti and Leep (1974) define the Oe class as those stars showing emission in the hydrogen lines but without emission in N III or 4686 He II.

In the blue-red region, aside from the presence of Lambda 4542 in absorption, the overall appearance is similar to Be stars. So far no Oe star has been observed until 1.1 μ: the aim of this paper is to fill this gap. We present observations of Oe stars in the near infra-red region as well as new observations of Hα profiles.