Correction to: Characterizing X-ray, UV, and optical variability in NGC 6814 using high-cadence Swift observations from a 2022 monitoring campaign

We recently published the paper 'Characterizing X-ray, UV, and optical variability in NGC 6814 using high-cadence Swift observations from a 2022 monitoring campaign' in Monthly Notices of the Royal Astronomical Society 527 , 5569-5579 (2024).We have since disco v ered that an outdated Calibration Database (CALDB) version was erroneously used to process the Swift UV O T data in that work.We have reprocessed those data using the most recent CALDB version (20240201) and find that the original UV flux densities are significantly larger than those obtained with the new CALDB.Fortunately, the variability products (i.e.fractional variability, structure function, and interpolated cross-correlation function) of sections 3.1 -3.3 remain consistent within the uncertainties reported in the original work due to the normalization processes that are performed when computing each product.section 3.4 (i.e.flux-flux analysis), ho we ver, changes, as do the related Discussion points and Conclusions that are based on that result.We present the updated results and interpretations using the reprocessed data below.We performed the flux-flux analysis presented in section 3.4 of Gonzalez et al. ( 2024 ) following the exact same procedure, changing only the input light curves to the reprocessed ones.The updated results are shown in Fig. 1 and Table 1 , where it can be seen that the UV fit parameters for the average flux [ A ( λ)] and RMS [ R ( λ)], and consequently computed intrinsic AGN variability spectrum [ D ( λ)] and constant (i.e.host galaxy) component [ G ( λ)], are ∼1.6 times smaller on average than those in the original work.Now, the intrinsic AGN variability spectrum does not differ significantly from the expected F ν ∝ λ -1/3 of a standard accretion disc, except for in the U band.Fitting of the host galaxy component does not change due to the minimal effect of the updated CALDB version on the optical results, which dominate that fit.We jointly fit the updated intrinsic AGN variability spectrum and time-averaged X-ray spectrum from the original work using KYNSED (Dov čiak et al. 2022 ) in XSPEC (Arnaud 1996 ) following the exact same procedure outlined in the Discussion of Gonzalez et al. ( 2024 ).While we fixed the black hole mass to M BH = 1.85 × 10 7 M in the original work, here we left it free to vary when fitting in order to achieve realistic X-ray luminosities that did not exceed the total disc