Gravitational and doppler redshifts of quasars interpreted as massive black holes ejected from galaxies

This is a first attempt to find a realistic explanation of the observed redshifts of quasars associated with galaxies, by considering, in addition to the inertial, also the gravitational time dilation in the strong field of quasars interpreted as huge black holes accreting matter from their surroundings. This interpretation allows us to understand the observed predominance of excess redshifts of quasars and construct possible semiquantitative models for the pair NGC 4319/Markarian 205. The proposed models do not contradict to the present astrophysical knowledge, but a selection of the most satisfactory one is still difficult because of the existing uncertainty in estimates of the sizes of radiating regions in matter accreted by a flying black hole.Essay received 2 March, 1979 by the Gravity Research Foundation (Gloucester, Mass., U.S.A.) and selected for Honorable Mention for 1979.     

Coherence between Seyfert galaxies and their surroundings

A sample of galaxy groups is investigated for the occurence of Seyfert objects within them. The velocity dispersion in groups with Seyfert galaxies is significantly larger than in groups without Seyfert galaxies. But there was not found any correlation between the galaxy density within the groups and the content of Seyfert galaxies.     

A comparison between the Hubble diagrams of type-I Seyfert galaxies and low-redshift,radio-weak quasars

We took 30 low-redshift, radio-weak quasars with 2 or more forbidden lines, and 16 Type-I Seyfert galaxies of the non-violent subtype, and compared their Hubble diagrams. We found that they each have a high correlation on the diagram, but they do not fall on a continuous line. This suggests that, contrary to the surmise by some people, they are not the same type of object. If quasars do evolve into Seyferts, then the transition must be very brief and rapid.     

An explanation of the discretization of redshifts of quasars

Published in Astrofizika, Vol. 38, No. 4, pp. 700–702, October–December, 1995.     

Narrow-line Seyfert 1 galaxies and the evolution of galaxies and active galaxies

Narrow Line Seyfert 1 galaxies (NLS1s) are intriguing owing to their continuum as well as emission-line properties. The observed peculiar properties of the NLS1s are believed to be as a result of an accretion rate close to the Eddington limit. As a consequence of this, for a given luminosity, NLS1s have smaller black hole (BH) masses compared with normal Seyfert galaxies. Here we argue that NLS1s might be Seyfert galaxies in their early stage of evolution and as such may be low-redshift, low-luminosity analogues of high-redshift quasars. We propose that NLS1s may reside in rejuvenated, gas-rich galaxies. We also argue in favour of collisional ionization for production of Fe  ii in active galactic nuclei.     

Clustering of galaxies at high redshifts

Recent observations show a large concentration of galaxies at high redshift. At first sight, strong clustering of galaxies at high redshifts seems to be in contradiction with the models of structure formation. In this paper we show that such structures are a manifestation of the strong clustering of rare peaks in the density field. We compute the frequency of occurrence of such large concentrations of galaxies in some models of structure formation.     

On an explanation of the discretization of the redshifts of quasars

We show that the relation ln(1+z)=0.206 proposed to describe the discretization of the spatial distribution of quasars is a consequence of observational selection and is predetermined by the choice of the photometric system (U, B, V, R), the ratios of the wavelengths of the emission lines of Mg II, C III, C IV, Ly and the absorption lines O VI (1035 å) of the quasars studied.Translated fromAstrofizika, Vol. 37, No. 4, 1994.In conclusion I express gratitude to L. V. Mirzoyan for constant interest and moral support in the course of the present work and to G. A. Arutyunyan for valuable advice.     

Report on discovery of new Seyfert galaxies

We report our discovery of new active galaxies in a small sample of 23 sources with 2.16 m telescope at Beijing Astronomical Observatory. After wavelength and flux calibration, they are classified by their degree of nuclear activities: one Seyfert 1, three Seyfert 2s, six Seyfert 3s, Seven HII galaxies and one possible Seyfert 3.     

A new strategy for estimating photometric redshifts of quasars

Based on the SDSS and SDSS-WISE quasar datasets, we put forward two schemes to estimate the photometric redshifts of quasars. Our schemes are based on the idea that the samples are firstly classified into subsamples by a classifier and then a photometric redshift estimation of different subsamples is performed by a regressor. Random Forest is adopted as the core algorithm of the classifiers, while Random Forest and k NN are applied as the key algorithms of regressors. The samples are divided into two subsamples and four subsamples, depending on the redshift distribution. The performances based on different samples, different algorithms and different schemes are compared. The experimental results indicate that the accuracy of photometric redshift estimation for the two schemes generally improves to some extent compared to the original scheme in terms of the percents in (|?z|)/(1+zi) 0.1 and (|?z|)/(1+zi) 0.2 and mean absolute error. Only given the running speed, k NN shows its superiority to Random Forest. The performance of Random Forest is a little better than or comparable to that of k NN with the two datasets. The accuracy based on the SDSS-WISE sample outperforms that based on the SDSS sample no matter by k NN or by Random Rorest. More information from more bands is considered and helpful to improve the accuracy of photometric redshift estimation. Evidently, it can be found that our strategy to estimate photometric redshift is applicable and may be applied to other datasets or other kinds of objects. Only talking about the percent in (|?z|)/(1+zi) 0.3, there is still large room for further improvement in the photometric redshift estimation.     

Statistical investigation of the space distribution of quasars and of their association with galaxies

Three distinct and representative sources of quasar data are used in this paper: 1) the Revised Optical Catalog of QSOs, 2) the quasars in the ?40° CTIO Curtis Schmidt Survey, and 3) the quasars in the Virgo Cluster region. Their redshift and magnitude distributions on various scales and their possible association with galaxies are analysed statistically.The preliminary conclusions are as follows. 1) The redshift and magnitude distributions on various scales are non-uniform. 2) The non-uniformity appears to be greater in the two local samples. 3) There is no evidence of a general association of quasars with field galaxies. 4) A general association of quasars with brighter cluster galaxies is statistically significant. 5) It seems likely that not all quasars have the same origin, some being local, some cosmological.     

ROSAT results on narrow-line Seyfert 1 galaxies

The excellent soft X-ray sensitivity of the PSPC detector onboard the ROSAT satellite provided the first chance to study precisely the spectral and timing properties of Narrow-Line Seyfert 1 galaxies. ROSAT observations of Narrow-Line Seyfert 1 galaxies have revealed (1) the existence of a giant soft X-ray excess, (2) a striking, clear correlation between the strength of the soft X-ray excess emission and the FWHM of the Hβ line, (3) the general absence of significant soft X-ray absorption by neutral hydrogen above the Galactic column, (4) short doubling time scales down to about 1000 s, (5) the existence of persistent giant (above a factor of 10), and rapid (less than 1 day) X-ray variability in extragalactic sources. The soft X-ray results on Narrow-Line Seyfert 1 galaxies indicate that their black hole regions are directly visible, further supporting the Seyfert 1 nature of these objects. The extreme X-ray properties of Narrow-Line Seyfert 1 galaxies make them ideal objects for understanding many of the problems raised generally by the Seyfert phenomenon.     

Seyfert galaxies and the radio–far-infrared correlation

We have observed a sample of 149 Seyfert galaxies and radio-quiet quasars at 13 cm with both a 275-km radio interferometer and the 6-km compact array of the Australia Telescope. The high-resolution observations searched for the presence of compact, high-brightness-temperature radio emission from the active nucleus. The low-resolution observations measured the total radio emission from the galaxy disc and Seyfert core and lobes. From these we draw the following conclusions. (i) Seyfert galaxies that lack compact radio cores display a correlation between radio and far-infrared (FIR) emission similar to the correlation displayed by normal spirals, albeit with greater scatter. The correlation is found to be intrinsic and is not an artefact of the richness effect. (ii) A very different radio–FIR correlation is displayed by those Seyferts that harbour compact radio cores. These tend to be more radio-loud than either normal spirals or the Seyferts that lack compact cores. The compact core emission thus seems to be responsible for the generally poor radio–FIR correlation displayed by Seyfert galaxies. (iii) The radio–FIR correlation is not significantly improved by subtracting off the 0.1-arcsec (20- to 200-pc) compact radio emission from the total radio emission. This suggests that the emission from the active galactic nucleus has significant structure on scales larger than 0.1 arcsec. Perhaps these structures are the 'linear' radio features that have been seen previously in Seyfert nuclei.