Top: Lomb-Scargle periodograms for V1716 Sco across Sectors 12, 39, and 93. The primary peak at ∼0.735 d⁻¹ corresponds to the orbital frequency (Ω), with the first harmonic (2Ω) also visible at ∼1.47 d⁻¹. The vertical dashed blue lines indicate potential instrumental artifacts related to the TESS orbital period (∼13.7 d) and its harmonics, which appear as sidebands to the main signal (Ω − 2Ω_TESS; Ω + 2Ω_TESS). The curved dashed black line represents the 99.99% significance threshold derived from an autoregressive [AR(p)] noise model. This frequency-dependent baseline accounts for the red-noise continuum (flickering) inherent in the system, which confirms that the orbital modulation remains statistically significant despite the increased noise power at low frequencies. Bottom left: Phase-folded light curve of Sectors 12, 39, and 93 at their detected orbital period, binned into 50 phase intervals to reduce point density and highlight the orbital modulation. Right: ASAS-SN g-band magnitude (blue points, left Y-axis) light curve of V1716 Sco before, during, and after the nova outburst recorded on MJD = 60055.178. The black points (right axis) show the raw TESS instrumental count rate. Note that the TESS Y-axis is independent and count rates are not scaled to the ASAS-SN g-band magnitude; sector-to-sector jumps in the TESS rate are due to varying background and crowding levels and do not affect the timing analysis.