DOI: 10.5281/zenodo.17183730
title: Simulated AGN lightcurves for the a small two-band UV-photometry mission

description: A small two-band UV-photometry mission QUVIK can be used to study accreting supermassive black holes. We focus on the following observational concept of dedicated monitoring of selected type-I Active Galactic Nuclei (AGN) in order to measure the time delay betweenthe far-UV, the near-UV, and other wavebands (X-ray and optical), Here we present artificial lightcurves corresponding to Figure 6 of the paper. The file without other extension represent the signal to nose (S/N) ratio 10, files with extension 100 represent the S/Nof 100.  Files were used to construct Figure 6 of Zajacek et al., Science with a Small Two-Band UV-Photometry Mission III: Active Galactic Nuclei and Nuclear Transients, 2024, Space Science Reviews, Volume 220, Issue 3, article id.29



response19.txt – light curve for infinite signal-to-noise ratio at wavelength 1500 Å

response19_noise.txt – same light curve with added noise

response49.txt – light curve for infinite signal-to-noise ratio at wavelength 3000 Å

response49_noise.txt – same light curve with added noise


a) tytuł zbioru danych;  Simulated AGN  lightcurves for the  a small two-band UV-photometry mission

b) autora(ów) i ich afiliacje; M. Zajaˇcek, B. Czerny, V. K. Jaiswal, M. ˇStolc, V.Karas, A. Pandey, D. R. Pasham, M. ´Sniegowska, V.Witzany, P. Sukov´a,  F. M¨unz, N. Werner, J. ˇR´ıpa, J.Merc4, M. Labaj, P. Kurf¨urst and J. Krtiˇcka

c) datę powstania danych i/lub daty gromadzenia; 2023/2024

d) opis metodologii badawczej i narzędzi użytych do pozyskania danych; To assess the possibility of performing UV continuum reverberation mapping by a UV small-satellite photometry mission, we performed simulations using the lamp-post model (Miniutti & Fabian 2004). In the model, the X-ray emitting corona source is positioned at the height H. Its variable emission is modelled using the Timmer-K¨onig method (Timmer & Koenig 1995) assuming the power spectral density modelled as a broken power-law function with two break frequencies. To mimic the observed light curves, we add noise to the signal, as it is demonstrated in Figure 6 for the light curves at 1500 and 3000 ˚A in the left and the right panels, respectively. The delays are calculated using two stan- dard methods; see Fig. 7 for an exemplary calculation using the ICCF and χ2 methods in the left and the right panels, respectively. In Tables 3 and 4, we list the results of the simulations. For the inferred time-delay values in Table 3, we used ten realizations of light curves to check the consistency of time delay, and the final delay is then expressed as the mean of all time delays with the corresponding standard deviation. To measure the time delay, we applied ICCF and χ2 methods (see e.g. Zajaˇcek et al. 2020). For reference, we also providethe expected time delay τψ calculated using the response function.

e) format i struktura danych; this is described above

f) warunki udostępniania i licencjonowania danych; Creative Commons Attribution License

g) adnotację o finansowaniu ze środków projektu i poprawny nr rejestracyjny projektu

(Narodowe Centrum Nauki, numer projektu).   V.K., B.C., V.K.J., and M.L. are grateful for the financial supportfrom the bilateral GA ˇCR-NCN collaboration project (ref. GF23-04053L –2021/43/I/ST9/01352/OPUS 22).