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http://hdl.handle.net/20.500.12386/35624
Title: | Long-term Swift and Metsähovi monitoring of SDSS J164100.10+345452.7 reveals multi-wavelength correlated variability | Authors: | ROMANO, Patrizia Lähteenmäki, A. VERCELLONE, Stefano FOSCHINI, LUIGI Berton, M. RAITERI, Claudia Maria Braito, V. Ciroi, S. Järvelä, E. Baitieri, S. Varglund, I. Tornikoski, M. Suutarinen, S. |
Issue Date: | 2023 | Journal: | ASTRONOMY & ASTROPHYSICS | Number: | 673 | First Page: | A85 | Abstract: | We report on the first multi-wavelength Swift monitoring campaign performed on SDSS J164100.10+345452.7, a nearby narrow-line Seyfert 1 galaxy formerly known as radio quiet which was recently detected both in the radio (at 37 GHz) and in the $\gamma$-rays, which hints at the presence of a relativistic jet. During our 20-month Swift campaign, while pursuing the primary goal of assessing the baseline optical/UV and X-ray properties of J1641, we caught two radio flaring episodes, one each year. Our strictly simultaneous multi-wavelength data closely match the radio flare and allow us to unambiguously link the jetted radio emission of J1641. Indeed, for the X-ray spectra preceding and following the radio flare a simple absorbed power-law model is not an adequate description, and an extra absorption component is required. The average spectrum of J1641 can be best described by an absorbed power law model with a photon index $\Gamma=1.93\pm0.12$, modified by a partially covering neutral absorber with a covering fraction $f=0.91_{-0.03}^{+0.02}$. On the contrary, the X-ray spectrum closest to the radio flare does not require such extra absorber and is much harder ($\Gamma_{\rm flare} \sim 0.7\pm0.4$), thus implying the emergence of a further, harder spectral component. We interpret this as the jet emission emerging from a gap in the absorber. The fractional variability we derive in the optical/UV and X-ray bands are found to be lower than the typical values reported in the literature, since our observations of J1641 are dominated by the source being in a low state. Under the assumption that the origin of the 37 GHz radio flare is the emergence of a jet from an obscuring screen also observed in the X-rays, the derived total jet power is $P^{\rm tot}_{\rm jet}=3.5\times10^{42}$ erg s$^{-1}$, comparable to the lowest measured in the literature. [Abridged] | URI: | http://hdl.handle.net/20.500.12386/35624 | URL: | http://arxiv.org/abs/2303.05534v1 https://www.aanda.org/articles/aa/full_html/2023/05/aa45936-23/aa45936-23.html |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/202345936 | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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aa45936-23.pdf | Pdf editoriale | 516.52 kB | Adobe PDF | View/Open |
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