The radio-loud Active Galactic Nuclei (AGNi) having the radio emission arising from a core region rather than from lobes are often referred to as "blazars" and include Flat Spectrum Radio Quasars (FSRQ) and BL Lacertae (BL Lac) objects. We present results of long term observations of FSRQ: among them are known object 3c454.3 (z= 0.859), high-red shifted quasar 1739+522 (4c+51.37) (z= 1.375) and 4c+31.63 (z= 0.295), 4c+55.17 (z= 0.896) as well as BL Lac type object OJ 287 (z= 0.306) that was recently detected by SHALON Cherenkov telescopes. Also, the observation data on known BL Lac objects Mkn 421 (z= 0.031), Mkn 501 (z= 0.034), Mkn 180 (z= 0.046) and Radio galaxies NGC 1275 (z= 0.018), 3c 382 (z= 0.0578) are summarized in this paper. The observation results are presented with integral spectra, images and spectral energy distributions for each of sources at energies above 800 GeV. A number of variability periods in different wavelengths including VHE γ-rays were found.

The cluster of galaxies in Perseus have long been considered as possible candidates for the sources of high and very high energy γ-ray emission generated by various mechanisms. The Seyfert galaxy NGC 1275 is the central, dominant galaxy in the Perseus cluster of galaxies. NGC 1275 is known as a powerful source of radio and X-ray emission. The well-known extragalactic object NGC 1275 has been observed by the SHALON high-altitude mirror Cherenkov telescopes as a part of program of long-term studies of metagalactic gamma-ray sources. In 1996, the SHALON observations revealed a new metagalactic source of very high energy gamma-ray emission coincident in its coordinates with the galaxy NGC 1275. Having analyzed the SHALON data, we have determined such characteristics of NGC 1275 as the spectral energy distributions and images at energies > 800 GeV for the first time. The results obtained at very high energies by SHALON are indicate that a part of TeV γ-ray emission is generated by relativistic jets in the nucleus of NGC 1275 itself, but the presence of an extended structure around NGC 1275 is evidence of the interaction of cosmic rays and magnetic fields generated in the jets at the galactic center with the gas of the Perseus cluster. Also, we present the results of long-term observations of the Perseus Cluster which are revealed the γ-ray emission from the two of nearby object-GK Per of classical nova type, located at ∼ 3 • SW from NGC 1275 and the explosion of extragalactic supernova SN2006gy that is about 10 minutes away from NGC 1275. So, the explosion of extragalactic supernova was observed at TeV energies for the first time with SHALON Cherenkov telescope.

The investigation of VHE gamma-ray sources by any methods, including mirror Cherenkov telescopes, touches on the problem of the cosmic ray origin and, accordingly, the role of the Galaxy in their generation. The SHALON observations have yielded the results on Galactic supernova remnants (SNR) of different ages. Among them are: the shell-type SNRs Tycho's SNR (1572y), Cas A (1680y), IC 443 (age ∼ (3 ÷ 30) × 10 3 y), γ Cygni SNR (age ∼ (5 ÷ 7) × 10 3 y) and classical nova GK Per (Nova 1901). For each of SNRs the observation results are presented with spectral energy distribution by SHALON in comparison with other experiment data and images by SHALON together with data from X-ray by Chandra and radio-data by CGPS. The collected experimental data have confirmed the prediction of the theory about the hadronic generation mechanism of very high energy 800 GeV -100 TeV gamma-rays in Tycho's SNR, Cas A and IC443. Recently, unique data on GK Per TeV gamma-ray emission were obtained with SHALON experiment. The X-ray data shows that, the nova remnant of GK Per could be a younger remnant that will resemble older SNRs (like IC 443) which interact with molecular clouds. GK Per is supposed to be a candidate for TeV gamma-ray emission due to the accelerated particles in the reverse shock region. The analysis of SHALON observation data revealed the main TeV-emission region coinciding with the position of central source of GK Per and the weak emission of shell, that is also observed in X-ray by Chandra.

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The nineteen-year-long studies of the Cygnus Region at energies 800 GeV -100 TeV by SHALON telescope are presented in this paper. The long-term observations of the Cygnus region centered on Cyg X-3 with the SHALON telescope are revealed the γ-ray emission from the one of nearby object -γCygni SNR, placed at ∼ 2 o from Cyg X-3. The results of γCygni SNR observation since 1995y by SHALON are presented with spectral energy distribution, images and integral spectra at energies 800 GeV -50 TeV. The results of nineteen-year observations of the Cyg X-3 binary at energies 800 GeV -85 TeV, detected by SHALON in 1995y are presented with images and integral spectra. A number of high activity period of Cyg X-3 were detected at energies > 800 GeV during the all observation time. The correlation soft X-ray and TeV energy γ-ray fluxes is traced.