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We investigate the properties of strong (H β + [O iii ]) emitters before and after the end of the “Epoch of Reionization” from z = 8 to z = 5.5. We make use of ultradeep JWST / NIRCam imaging in the parallel field (P2) of the MIRI Deep Imaging Survey (MIDIS) in the Hubble eXtreme Deep Field (H-XDF), in order to select prominent (H β + [O iii ]) emitters (with rest-frame equivalent width (EW _0 ) ≳ 100 Å) at z = 5.5–7, based on their flux density enhancement in the F356W band with respect to the spectral energy distribution continuum. We complement our selection with other (H β + [O iii ]) emitters from the literature at similar and higher ( z = 7−8) redshifts. We find (nonindependent) anticorrelations between EW _0 (H β + [O iii ]) and both galaxy stellar mass and age, in agreement with previous studies, and a positive correlation with specific star formation rate (sSFR). On the SFR– M ^⋆ plane, the (H β + [O iii ]) emitters populate both the star formation main sequence and the starburst region, which become indistinguishable at low stellar masses ( ${\mathrm{log}}_{10}({M}^{\star })\lt 7.5$ ). We find tentative evidence for a nonmonotonic relation between EW _0 (H β + [O iii ]) and SFR, such that both parameters correlate with each other at SFR ≳ 1 M _⊙ yr ^−1 , while the correlation flattens out at lower SFRs. This suggests that low metallicities producing high EW _0 (H β + [O iii ]) could be important at low SFR values. Interestingly, the properties of the strong emitters and other galaxies (33% and 67% of our z = 5.5–7 sample, respectively) are similar, including, in many cases, high sSFR. Therefore, it is crucial to consider both emitters and nonemitters to obtain a complete picture of the cosmic star formation activity around the Epoch of Reionization.