Top: GJ 3323 periodograms of RVs (black curve), (blue curve), Hα (red curve), and FWHM_CCF (green curve) for subsets satisfying BJD-2 450 000: 6500–6800, 6800–7200, and 7200–7500. The left column corresponds to raw RVs and the right column to the residues of subtracting the Keplerian adjusted to the 5.4-day signal. We note the temporal stability of the shorter RV periodicity and that the one at 40 days also shows power excess in the FWHM_CCF (first and second rows of right column). Bottom: periodogram for the V-band ASAS photometry with BJD between 2800–3200 and 3500–4000. Significant power excess arises at about 90 days.