Lobban, A.P.Zola, S.Pajdosz-Smierciak, U.Braito, V.Nardini, E.Bhatta, G.Markowitz, A.Bachev, R.Carosati, D.Caton, D.B.Damljanovic, G.Debski, B.Haislip, J.B.Hu, S.M.Kouprianov, V.Krzesinski, J.Porquet, D.Nuñez, F. PozoReeves, J.Reichart, D.E.2020-04-102020-04-102020-02-27Lobban, A.P.; Zola, S.; Pajdosz-Smierciak, U.; Braito, V.; Nardini, E.; Bhatta, G.; Markowitz, A.; Bachev, R.; Carosati, D.; Caton, D.B.; Damljanovic, G.; Debski, B.; Haislip, J.B.; Hu, S.M.; Kouprianov, V.; Krzesinski, J.; Porquet, D.; Nuñez, F. Pozo; Reeves, J.; Reichart, D.E.; X-ray, UV and optical time delays in the bright Seyfert galaxy Ark 120 with co-ordinated Swift and ground-based observations; High Energy Astrophysical Phenomena (2020); https://arxiv.org/abs/2002.12348http://hdl.handle.net/11603/17983We report on the results of a multiwavelength monitoring campaign of the bright, nearby Seyfert galaxy, Ark 120 using a ~50-day observing programme with Swift and a ~4-month co-ordinated ground-based observing campaign, predominantly using the Skynet Robotic Telescope Network. We find Ark 120 to be variable at all optical, UV, and X-ray wavelengths, with the variability observed to be well-correlated between wavelength bands on short timescales. We perform cross-correlation analysis across all available wavelength bands, detecting time delays between emission in the X-ray band and the Swift V, B and UVW1 bands. In each case, we find that the longer-wavelength emission is delayed with respect to the shorter-wavelength emission. Within our measurement uncertainties, the time delays are consistent with the \tau ~ \lambda^{4/3} relation, as predicted by a disc reprocessing scenario. The measured lag centroids are \tau_{cent} = 11.90 +/- 7.33, 10.80 +/- 4.08, and 10.60 +/- 2.87 days between the X-ray and V, B, and UVW1 bands, respectively. These time delays are longer than those expected from standard accretion theory and, as such, Ark 120 may be another example of an active galaxy whose accretion disc appears to exist on a larger scale than predicted by the standard thin-disc model. Additionally, we detect further inter-band time delays: most notably between the ground-based I and B bands (\tau_{cent} = 3.46 +/- 0.86 days), and between both the Swift XRT and UVW1 bands and the I band (\tau_{cent} = 12.34 +/- 4.83 and 2.69 +/- 2.05 days, respectively), highlighting the importance of co-ordinated ground-based optical observations.15 pagesen-USThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.Text