Expectations for time-delay measurements in active galactic nuclei with the Vera Rubin Observatory

Open Access

Fig. 9.

Sensitivity of the simulations to the assumed parameter for the first year of DDF data, faint quasars log L₃₀₀₀ = 44.7. Top panel: alternative values of the line EWs. Second panel: assuming a larger photometric error. Third panel: at shorter timescales for the frequency breaks of the power spectrum. Lowest panel: at lower variability amplitude (see Sect. 3.4 for details).

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