The object 3C390.3 is a well known broad-line radio galaxy (z=0.056), whose very broad emission lines are variable in time (see Veilleux and Zheng 1991, and Dietrich at al. 1998 for references). It is known as the prototypical source of broad double-peaked Hβ and Hα emission lines. In this paper we present the preliminary results of spectral observations of 3C390.3 in 1995–1998 on 6-m and 1-m telescopes of the Special Astrophysical Observatory of RAS.

The nucleus of NGC 3227 was classified as a Sy2 type before 1974, and a Sy1 type after 1974. The Seyfert type of the nucleus changed corresponding to its brightness: U brightness of the nucleus increased in 1974: ΔU ˜ 1m. Maximum brightness of the nucleus was observed in 1975 – 1977.

The beginnings of strong radio flares in six AGNs were detected and their evolution was studied using 1–22 GHz five epoch instantaneous spectral observations in 1997–1998. The phenomena started at the highest frequency and moved to the lower frequency in a regular fashion. Such behavior of the flares in AGNs can be explained by synchrotron emission from a compact relativistic jet implying different physical models which are discussed. For different types of AGNs the same behavior of flares is revealed, in favor of the same basic physical model for BL Lacs and quasars. A birth of new VLBI components in compact jets associated with these outbursts is predicted.

We present some results on the long term variability of the X-ray emission from optically catalogued galaxies, especially in view of their nuclear properties. For this investigation we use data from the ROSAT PSPC archive. Some future directions are also discussed.

It has become generally accepted that most or possibly all ellipticals and bulges of spirals harbor supermassive black holes in their center (see Ho 1998 for a recent review).

Observations indicate that ring galaxies are more active than spirals (e.g., Ghigo et al., 1983 Appleton and Struck-Marcell, 1987). However, Seyfert activity is noted in only a few ring galaxies, e.g. NGC 985 (de Vaucouleurs & de Vaucouleurs 1975), NGC 1144 = Arp 118 (Huchra et al. 1982), ring galaxy in Sextans-optical counterpart of the IRAS source 09595-0755 (Wakamatus & Nishida). This is indicative of the fact that this type of activity requires favorable circumstances. In this context a previous work on the stellar episode of ring formation, Chatterjee (1984), is extended, including gas and studying the evolution of the ring structure, due to rebounds of the compact elliptical about the plane of the disk.

The Hubble classification suggested for the spiral galaxies, Sa–Sb–Sc–Sm–Irr, was considered by many astronomers as an evolution succession. The version of transformation from early spirals to the late spirals and vice versa was considered. The existence of several parameters, monotonically increasing or decreasing along this succession, together with the parameters which do not depend on the structural type of the galaxies of this succession, is a confirmation of this succession to be a succession of stages of evolution. Let us consider in detail both types of parameters. About the full masses and luminosities of galaxies we can state, that except Irr and maybe Sm-galaxies there is not a clear expressed difference of mean values of these parameters for galaxies of different structural types. Irr galaxies are the systems with low masses and luminosities, but on the (M-L) diagram a part of them is obviously mixed with the late spirals. There is a strong change of the M/L ratio with changing of the structural type, though the early type galaxies on average apparently have the least values of that ratio. As monotonically changing parameters we can suggest the following three:

In Dravskikh & Dravskikh (1996) the results of a statistical analysis of quasar luminosity as a function of redshift, if it is assumed to be cosmological, are given (see Fig.1). Three quasar samples were analyzed separately:

1. • quasars with absorption lines;

2. • quasars associated with galaxies or association-quasars not having absorption lines (from Burbidge et al. 1996);

3. • other quasars not included in the first two groups.

V. Ambartsumian (1956) has shown that the observable quantity of double and multiple galaxies much exceeds that expected, based on the assumption about dissociative balance. He has concluded that the members of double and multiple systems, as well as the clusters, could not arise independently of each other, and only then to be united in systems, by mutual capture. They should arise in common. Moreover, when in a group are large luminous central galaxies, the origin of the weak members of the group should be caused by activity of a nucleus of the central galaxy (Ambartsumian 1962). On the other hand, recently, there was widespread the opinion that the properties of central galaxies of groups and clusters are caused by interactions with environmental galaxies.

It has been shown that the stage of activity of spiral galaxies depends on both the distance between them and their nearest neighbours and the structure of their central parts.

The nucleus of the Seyfert galaxy NGC 4151 is known to be variable in the optical on different timescales: from minutes to tens of years. A new cycle of activity of the nucleus is investigated from 1989.

In 1978 we have shown that Shakhbazian CGCG have an elongated form (Vardanian & Melik-Alaverdian 1978). Morever, they turned out to be of comet forms (1996), at the head of which basically are situated their bright members. This enables determination with high accuracy of the position angles θ of major axes of the elongated Shakhbazian CGCG. A closer examination of these angles shows that distribution of orientations of the major axes of groups is anisotropic and has two maximums (Vardanian 1996). (See Table, where θ is position angle, N is number of CGCG). These maximums are oriented in mutually perpendicular directions (θ = 45° and θ = 135°).

NGC 3077, an Irr II galaxy in the M81/M82 group of galaxies at 3.63 Mpc, suffered a tidal encounter with M81 about 400 Myr ago. Tidal structures of HI in this group of galaxies can best be seen in a VLA image by Yun et al. (1994).

A new sample of faint Gigahertz Peaked Spectrum (GPS) sources is presented here as an addition to our previous one (Ohanian, 1995). Comparison of the results of investigation of these samples with those of previously studied brighter samples (e.g. O'Dea et al. 1991) will delineate the properties of GPS sources over a wide range of luminosity, redshift and rest frame peak frequency. This will give noticeable information relevant to their cosmological evolution and relationship with other classes of extragalactic radio sources.

On the basis of new spectroscopic observations of the blue compact dwarf galaxy IZw18 in the narrow spectral range between 4000Å and 4500Å absorption components of Hγ and Hδ lines were discovered. Equivalent widths of Hγ and Hδ lines have been measured. From available data the OB population of IZw18 was analyzed.

A review is given of the principal successes in AGN research (black holes as the central engines, radiation mechanisms, population studies) and the most important open questions (creation of AGN, dynamics of the accretion flow, acceleration and collimation of relativistic jets). Some recent work that gives hope for progress towards answering these questions is also discussed.

This is a great honour for me to present a report on the influence of the outstanding scientist academician V.A. Ambartsumian. I was well familiar with V.A. Ambartsumian, but unfortunately, I did not manage to work with him in scientific research. When, in 1948, I arrived in the Leningrad State University (LSU) V.A. Ambartsumian already had left LSU and worked in Armenia. My teacher in LSU, academician V.V. Sobolev, was the best student of V.A. Ambartsumian. Therefore, to some degree, I can consider myself as a scientific grandson of V.A. Ambartsumian. However, I very frequently met V.A. Ambartsumian at scientific conferences, discussed with him scientific problems and problems of organization of scientific research. Contacts with this outstanding, strong and talented person have rendered large influence on my formation as a scientist.

From simply looking at pictures of galaxies Ambartsumian realized that new galaxies were formed in ejections from old galaxies. In the ensuing 40 years, observations have supported in increasing detail his original insight. We can now empirically outline the development of compact objects emerging from the nuclei of active galaxies into young star forming galaxies and finally into aggregates of old stars.

The observations actually require galaxies to continually originate in a low particle mass plasma which has remarkably similar properties to the “superfluid” which Ambartsumian foresaw. He had the courage to present these conclusions to influential astronomers who still today reject any origin of galaxies other than in the Big Bang. In this most important subject of science, the nature of our universe, Ambartsumian's revolutionary insights are now increasingly vindicated by observation.