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- Matveenko, L. I., et al.
(author)
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The structure of the quasar 3C-345
- 1992
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In: Soviet Astronomy Letters. - Moscow : Rossijskaja akademija nauk / Russian Academy of Sciences. - 0320-0108. ; 18:6, s. 379-391
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Journal article (peer-reviewed)abstract
- We study the fine structure of the quasar 3C 345 at a wavelength of 49 cm. The apparent size of the core and low-frequency variability are due to the opacity of the surrounding ionized medium and the electron density distribution. We find the distance dependence of the size and brightness temperature of the components. Relativistic plasma is being ejected into a cone, with vertex angle approximately 40-degrees in position -110-degrees. The jet consists of narrow twisted filaments.
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| 2. |
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| 3. |
- Standke, K. J., et al.
(author)
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High Sensitivity VLBI at 86 GHz : First Fringes with the 100 m Radio Telescope at Effelsberg
- 1993
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In: VLBI Technology. - Tokyo : Terra Scientific. - 4887041128 ; , s. 75-85
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Book chapter (peer-reviewed)abstract
- Inclusion of large and sensitive antennas is of essential importance to further improve the imaging capabilities of VLBI at 3.5 mm wavelength. The combination of the 100 m radio telescope at Effelsberg (illuminated diameter ~60 m at lambda = 3.5 mm) with the 30 m radio telescope at Pico Veleta presently allows the detection of compact flux down to a level of 0.2 Jy (for τ=360 seconds integration time). Fringes have been found for 23 radio sources many of them not observed previously with VLBI at 86 GHz. On European baselines to Effelsberg the SNR typically was 10 to 30 (and ranged up to 107 for 3C279), facilitating model fitting for the brightest sources. Even in spite of chaning weather conditions during the observations (coherence times ranged between 10 to 100 seconds) and a still non-optimum pointing model for the 100 m antenna for observations at high frequencies, these results demonstrate that the 100 m radio telescope can be successfully incorporated in global VLBI experiments at 3.5 mm wavelength.
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