Multifrequency radio observations of 3C 28, 76.1, 186 and 319

MAGIC observations and multifrequency properties of the flat spectrum radio quasar 3C 279 in 2011

Aims. We study the multifrequency emission and spectral properties of the quasar 3C 279 aimed at identifying the radiation processes taking place in the source. Methods. We observed 3C 279 in very-high-energy (VHE, E > 100 GeV) γ-rays, with the MAGIC telescopes during 2011, for the first time in stereoscopic mode. We combined these measurements with observations at other energy bands: in high-e...

Multifrequency observations of the jets in the radio galaxy

We present images of the jets in the nearby radio galaxy NGC 315 made with the VLA at five frequencies between 1.365 and 5 GHz with resolutions between 1.5 and 45 arcsec FWHM. Within 15 arcsec of the nucleus, the spectral index of the jets is α = 0.61. Further from the nucleus, the spectrum is flatter, with significant transverse structure. Between 15 and 70 arcsec from the nucleus, the spectra...

HST, radio and infrared observations of 28 3CR radio galaxies at redshift z

HST , radio and infrared observations of 28 3 CR radio galaxies at redshift z ∼ 1 — I . The observations

Hubble Space Telescope images are presented of a sample of 28 3CR radio galaxies with redshifts in the range 0.6 < z < 1.8, together with maps at comparable angular resolution of their radio structure, taken using the Very Large Array. Infrared images of the fields, taken with the United Kingdom InfraRed Telescope, are also presented. The optical images display a spectacular range of structures...

Multifrequency Studies of Bright Radio Supernova Remnants . Iii . X - Ray and Radio Observations of 3 C 397

Radio-bright, presumably young supernova remnants offer the opportunity of studying strong-shock physics and the nature of the interaction of ejected material with the surrounding medium. The relation between radio and X-ray morphology varies considerably among supernova remnants , with important implications for the physics of the emission processes at different wavelengths. We use Very Large ...