A1 Refereed original research article in a scientific journal
Long-term radio variability of active galactic nuclei at 37 GHz
Authors: Kankkunen, Sofia; Tornikoski, Merja; Hovatta, Talvikki; Lähteenmäki, Anne
Publisher: EDP Sciences
Publishing place: LES ULIS CEDEX A
Publication year: 2025
Journal: Astronomy and Astrophysics
Journal name in source: Astronomy & Astrophysics
Journal acronym: ASTRON ASTROPHYS
Article number: A318
Volume: 693
Number of pages: 22
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202450561
Web address : https://doi.org/10.1051/0004-6361/202450561
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/485096683
Aims. We present the results of analysing the long-term radio variability of active galactic nuclei at 37 GHz using data of 123 sources observed in the Aalto University Metsahovi Radio Observatory. Our aim was to constrain the characteristic timescales of the studied sources and to analyse whether up to 42 years of monitoring was enough to describe their variability behaviour. Methods. We used a periodogram to estimate the power spectral density of each source. The power spectral density is used to analyse the power content of a time series in the frequency domain, and it is a powerful tool in describing the variability of active galactic nuclei. We were interested in finding a bend frequency in the power spectrum, that is, a frequency at which the slope beta of the spectrum changes from a non-zero value to zero. We fitted two models to the periodograms of each source, namely the bending power law and the simple power law. The bend frequency in the bending power law corresponds to a characteristic timescale. Results. We were able to constrain a timescale for 11 out of 123 sources, with an average characteristic timescale x(b) = 1300 days and an average power-law slope beta = 2.3. The results suggest that up to 42 years of observations may not always be enough for obtaining a characteristic timescale in the radio domain. This is likely caused by a combination of both slow variability as well as sampling-induced effects. We also compared the obtained timescales to 43 GHz very long baseline interferometry images. The maximum length of time a knot was visible was often close to the obtained characteristic timescale. This suggests a connection between the characteristic timescale and the jet structure.
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Funding information in the publication:
S.K. was supported by Jenny and Antti Wihuri Foundation, Väisälä Fund and Academy of Finland project 320085. T.H. was supported by Academy of Finland projects 317383, 320085, 322535, and 345899.
