Volume 469, Number 3, July III 2007
|Page(s)||899 - 912|
|Published online||02 May 2007|
Statistical analyses of long-term variability of AGN at high radio frequencies*
Metsähovi Radio Observatory, Helsinki University of Technology, Metsähovintie 114, 02540 Kylmälä, Finland e-mail: firstname.lastname@example.org
2 Tuorla Observatory, University of Turku, Väisäläntie 20, 21500 Piikkiö, Finland
3 Department of Physics, University of Turku, 20100 Turku, Finland
4 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
Accepted: 23 April 2007
Aims.We present a study of variability time scales in a large sample of Active Galactic Nuclei at several frequencies between 4.8 and 230 GHz. We investigate the differences of various AGN types and frequencies and correlate the measured time scales with physical parameters such as the luminosity and the Lorentz factor. Our sample consists of both high and low polarization quasars, BL Lacertae objects and radio galaxies. The basis of this work is the 22 GHz, 37 GHz and 87 GHz monitoring data from the Metsähovi Radio Observatory spanning over 25 years. In addition, we used higher 90 GHz and 230 GHz frequency data obtained with the SEST-telescope between 1987 and 2003. Further lower frequency data at 4.8 GHz, 8 GHz and 14.5 GHz from the University of Michigan monitoring programme have been used.
Methods.We have applied three different statistical methods to study the time scales: the structure function, the discrete correlation function and the Lomb–Scargle periodogram. We discuss also the differences and relative merits of these three methods.
Results.Our study reveals that smaller flux density variations occur in these sources on short time scales of 1–2 years, but larger outbursts happen quite rarely, on the average only once in every 6 years. We do not find any significant differences in the time scales between the source classes. The time scales are also only weakly related to the luminosity suggesting that the shock formation is caused by jet instabilities rather than the central black hole.
Key words: galaxies: active / methods: statistical
© ESO, 2007
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