L_X−L_UV plane with our 1H 0707−495 observations in the high-(orange star) and low-(green star)-count-rate state. Results from an emcee (Foreman-Mackey et al. 2013) linear regression are shown for both broad-line AGNs (data points and regression as reported in Arcodia et al. 2019), (black circles; Liu et al. 2016) and NLS1s (data points from Gallo 2006, linear regression performed in this work). We computed the X-ray luminosity at 2 keV to compare with these literature measurements, while the UV proxy was computed at 3000, 2500, and 2910Å in XMM-XXL (Liu et al. 2016), NLS1 (Gallo 2006), and our OM-UVW1 data, respectively. The best-fit linear regressions emcee (Foreman-Mackey et al. 2013) are shown with a solid line, with corresponding 16th–84th percentile uncertainty intervals in a shaded area. The red dashed lines correspond to the fit intrinsic scatter of the NLS1 relation. The 2000 observation of 1H 0707−495 from Gallo (2006) is shown with a red star instead of a red square; the median flux level from the 2008 observations reported in Fabian et al. (2009) is shown with a light blue star. The 2 keV flux level during the eROSITA observation in the first all sky survey in April 2020 is shown with a grey dotted line.