The angular dimensions of extragalactic radio sources

The angular dimensions of compact components of extragalactic radio sources are calculated theoretically on three hypotheses: (a) magnetic field and relativistic particles energy equipartition; (b) equilibrium between synchrotron and Compton losses; (c) radiative lifetime of the same order as the source's light-travel time. Using angular measurements of 73 radio components, divided into two groups (multicomponent and single-component sources), a correcting formulae is derived to reduce the theoretical values to the observed values.This work was partially supported by the Brasilian research agency CNPq.     

Surveys of compact extragalactic radio sources

Several recent global and Space VLBI surveys of quasars, Active Galactic Nuclei of other types and star-burst galaxies provide a wealth of material on milli- and sub-milliarcsecond radio structures in hundreds of sources. Results of these projects are presented with an emphasis on the statistics of redshift- and angular-scale-dependent properties of the milli- and sub-milliarcsecond radio structures. These studies make possible disentanglement of intrinsic (possibly, evolutionary) phenomena of parsec-scale radio structures and the imprints of the cosmological model. The studies indicate a very promising potential of high-resolution applications of the Square Kilometer Array. Based on our pilot projects we estimate that a sample containing of the order of 10⁴ faint radio sources in the luminosity range 10²²–10²⁶ W/Hz can be surveyed by a high-resolution SKA with the milliarcsecond resolution at cm wavelengths. Such the high resolution radio survey, including those conducted jointly by SKA and Space VLBI missions, in conjunction with data from other domains, will provide a new ground for extragalactic studies.     

Origin of the central radio gaps in extragalactic radio sources

We propose an explanation of the origin of the central radio gaps which are usually observed in extragalactic radio sources that exhibit jet structures.An estimate was made of neutron Lorentz factors of neutrons responsible for energy transport from the central engine of active galactic nuclei (AGNs) to the jet turn-on point of typical AGNs.The probable explanations of the existence of different belts in the radio gap morphology was attempted.     

The ATCA intraday variability survey of extragalactic radio sources

We present the results of an Australia Telescope Compact Array (ATCA) survey for intraday variability (IDV) of the total and polarized flux densities of 118 compact, flat-spectrum, extragalactic radio sources from the Parkes 2.7-GHz Survey. A total of 22 total flux density IDV sources were discovered and 15 sources were found to show IDV of their polarized flux density. We discuss the statistical properties of the IDV sources, including the distribution of source modulation indices, and the dependence of the variability amplitude on source spectral index and on Galactic position. We suggest interstellar scintillation (ISS) in the Galactic interstellar medium as the most likely mechanism for IDV. Even so, the inferred high brightness temperatures cannot be easily explained.     

Interstellar scintillation of compact extragalactic radio sources

The recent discovery of radio variability of a quasar on short time-scales (hours) prompts us to examine what is expected in respect of the interstellar scintillation of very compact, extragalactic radio sources. We find that large-amplitude, rapid, variability is predicted at commonly observed radio frequencies (1–20 GHz) over the vast majority of the extragalactic sky. As a guide to assist observers in understanding their data, we demonstrate simple techniques for predicting the effects of interstellar scintillation on any extragalactic source.     

The radio luminosity function and the luminosity diameter function of extragalactic radio sources

On the basis of a radio index-surface brightness diagram recently published, the luminosity function and the luminosity diameter function are obtained. The uncertainties due to the incompleteness of the sample are of the same order as the statistical uncertainties. The luminosity function differs considerably from a simple power law and supports the distinction of two populations. The density of the weak population (P<10³⁵ W Hz⁻¹ ster⁻¹ at 1400 MHz) follows nearly a power law in P and increases towards small diameters at least down to I kpc. The density of the strong population (the high luminosity and small diameter part of which is occupied by the quasars) has a maximum between 10²⁵ and 10²⁸ W Hz⁻¹ ster⁻¹ and around 100 kpc. A strong evolution effect is clearly present and is in a good agreement with the models obtained from the log N-log S counts.     

Evaluation of catalogues of extragalactic radio sources

A combined catalogue is constructed from the observations of extragalactic radio sources compiled in independent catalogues providing precise positions determined by radio interferometric techniques. Positions and catalogue differences are derived and discussed. The average precision of the combined catalogue is at the level of 0.7 mas in right ascension and 1.3 mas in declination. For the more recent catalogues the systematic differences amount to a fraction of a millisecond of arc.     

Search for groups of extragalactic radio sources

We explore the possibility of searching for groups of radio sources from the FIRST catalog on angular scales 1′–5′. We developed an efficient method of searching for such groups that takes into account the need for combining the components of extended sources represented in the catalog by separate objects. We found 31 groups of radio sources with angular sizes <5′ that contain no fewer than five sources with flux densities ≥3 mJy. This number is at least triple the expected number of such groups for a random Poisson distribution of radio sources in the sky. The prospects for using groups of radio sources to detect and study distant systems of galaxies are discussed.     

A relation between the properties of extragalactic radio sources

An empirical relation between the observable properties radio surface brightness and radio index on the one hand, and the intrinsic properties linear diameter of the radio source, radio luminosity, and optical luminosity on the other hand is found and shown in a diagram. The relation is strong enough to yield useful distance estimates. In this manner, distances of 8 quasars and 17 unidentified radio sources are obtained.     

Estimates of proton energies in extragalactic radio sources

It is shown that inelastic proton collisions in extragalactic radio sources can account for their radio and -ray emissions. The proton Lorentz-factor _p responsible for -ray emission is estimated to lie between 1.4 and 86. But for the radio emission (with _e ~ 10³-10⁴) the estimated _p values lie between 7 to 300. The estimates of total particle and magnetic energy for a typical radio source is in agreement with equipartition theory.     

Phaseless VLBI mapping of compact extragalactic radio sources

The problem of phaseless aperture synthesis is of current interest in phase-unstable VLBI with a small number of elements when either the use of closure phases is not possible (a two-element interferometer) or their quality and number are not enough for acceptable image reconstruction by standard adaptive calibration methods. Therefore, we discuss the problem of unique image reconstruction only from the spectrum magnitude of a source. We suggest an efficient method for phaseless VLBI mapping of compact extragalactic radio sources. This method is based on the reconstruction of the spectrum magnitude for a source on the entire UV plane from the measured visibility magnitude on a limited set of points and the reconstruction of the sought-for image of the source by Fienup's method from the spectrum magnitude reconstructed at the first stage. We present the results of our mapping of the extragalactic radio source 2200+420 using astrometric and geodetic observations on a global VLBI array. Particular attention is given to studying the capabilities of a two-element interferometer in connection with the putting into operation of a Russian-made radio interferometer based on Quasar RT-32 radio telescopes.     

A preferred orientation of extragalactic double radio sources

The distribution of the main axes of double radio sources is used to test isotropy of that part of the universe which is accessible to radio investigations. Data for 274 double and/or extended sources have been taken from the literature to compute the fit to several simple models of global orientation by means of a ²-test. The best fit has been found on a 3%-significance level for the preferred orientation along a right-handed helix with pitch angle 82° in the direction =95°, =–38° (165°,b=20°). This preferential alignment of radio sources is assumed to be caused by a largescale magnetic field.     

Observations of extragalactic radio sources at 36 GHz

The observations of 34 extragalactic radio sources with the 22-m Crimean Astrophysical Observatory radio telescope at 36 GHz in 1985–1994 are presented. Intensity variations were detected in 27 objects, which may result from the appearance of new components in their cores.     

Circular polarization and the structure of compact extragalactic radio sources

The origin of the circularly polarized (CP) component of the synchrotron radiation in compact extragalactic radio sources is investigated. A convenient quantity, the CP excess, is defined as the ratio of the observed to the expected degree of CP in a source, with the latter calculated from synchrotron theory for transparent sources, using magnetic field strengths from VLBI measurements, and the degree of inhomogeneity estimated from the observed degree of linear polarization. For almost all sources, the CP excess is much larger than unity, and in addition appears to depend on the absolute luminosity of the source for both the radio galaxy and the quasar populations. Explanations for the amount and the luminosity dependence of the CP excess are considered, and the origin of the excess is suggested to lie in a special magnetic field geometry of the compact sources. A simple model with helical magnetic field and relativistic beaming, consistent with the quasar data, is presented. The importance of considering the CP component of radiation in the context of different physical source models is emphasized.     

The X-ray nuclei of intermediate-redshift radio sources

We re-assess the question of a systematic time delay between the formation of the progenitor and its explosion in a Type Ia supernova (SN Ia) using the Hubble Higher- z Supernova Search sample. While a previous analysis indicated a significant time delay, with a most likely value of 3.4 Gyr, effectively ruling out all previously proposed progenitor models, our analysis shows that the time-delay estimate is dominated by systematic errors, in particular due to uncertainties in the star formation history (SFH). We find that none of the popular progenitor models under consideration can be ruled out with any significant degree of confidence. The inferred time delay is mainly determined by the peak in the assumed SFH. We show that, even with a much larger supernova sample, the time-delay distribution cannot be reliably reconstructed without better constraints on the SFH.     

The core dominance parameter and Fermi detection of extragalactic radio sources

By cross-correlating an archive sample of 542 extragalactic radio sources with the Fermi-LAT Third Source Catalog(3FGL), we have compiled a sample of 80 γ-ray sources and 462 non-Fermi sources with available core dominance parameter(RCD), and core and extended radio luminosity; all the parameters are directly measured or derived from available data in the literature. We found that RCD has significant correlations with radio core luminosity, γ-ray luminosity and γ-ray flux; the Fermi sources have on average higher RCD than non-Fermi sources. These results indicate that the Fermi sources should be more compact,and the beaming effect should play a crucial role in the detection of γ-ray emission. Moreover, our results also show Fermi sources have systematically larger radio flux than non-Fermi sources at fixed RCD, indicating larger intrinsic radio flux in Fermi sources. These results show a strong connection between radio andγ-ray flux for the present sample and indicate that the non-Fermi sources are likely due to the low beaming effect, and/or the low intrinsic γ-ray flux. This supports a scenario that has been published in the literature:a co-spatial origin of the activity for the radio and γ-ray emission, suggesting that the origin of the seed photons for the high-energy γ-ray emission is within the jet.