ROMANO, PatriziaPatriziaROMANOLähteenmäki, A.A.LähteenmäkiVERCELLONE, StefanoStefanoVERCELLONEFOSCHINI, LUIGILUIGIFOSCHINIBerton, M.M.BertonRAITERI, Claudia MariaClaudia MariaRAITERIBraito, V.V.BraitoCiroi, S.S.CiroiJärvelä, E.E.JärveläBaitieri, S.S.BaitieriVarglund, I.I.VarglundTornikoski, M.M.TornikoskiSuutarinen, S.S.Suutarinen2025-01-132025-01-1320230004-6361http://hdl.handle.net/20.500.12386/35624We 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]STAMPAenArticle10.1051/0004-6361/2023459362-s2.0-85160748167http://arxiv.org/abs/2303.05534v1https://www.aanda.org/articles/aa/full_html/2023/05/aa45936-23/aa45936-23.htmlFIS/05 - ASTRONOMIA E ASTROFISICA