tokens: larger intensity variations in the range and a patchy distribution peaked at the location of recent star formation events. The patchy ionization structure yields an escape fraction of , a value consistent with observations of lower redshift galaxies with similar brightness (e.g. Bouwens et al. 2016 ; Grazian et al. 2017 ), and averaged values of simulated galaxies with similar mass (Xu et al. 2016 ). We note, however, that large fluctuations are expected between different evolutionary stages (Trebitsch et al. 2017 ). The [C ii ] line luminosity of Freesia is . The emission extends on a few kpc scales, with peaks around Freesia-A, Freesia-B, and dense non-star-forming clumps found near the galaxy. The emission mostly comes from gas with and illuminated by an ISRF intensity . Instead, [O iii ] emission is concentrated around Freesia-A, the star-bursting component of the system, and its emission is dominated by gas with a wider range of properties, i.e. and U ≃ (6 ± 2) × 10 −3 . At the Freesia-A location, the oxygen line is very bright, . However, the smaller extent of the [O iii ] emitting region implies a lower galaxy-integrated emission, i.e. . With respect to [C ii ], the [O iii ] show both a spatial offset () and a spectral shift of (), reminiscent of similar evidence found in some systems at high z (Carniani et al. 2017 ). Freesia lies below the local [C ii ]–SFR relation (De Looze et al. 2014 , within ≃ 2σ), as it is in a starburst phase; that is, it sits above the KS relation (Schmidt 1959 ; Kennicutt 1998 , within ≃ 2σ). Spatial analysis reveals that patches of the galaxy that are above the resolved local – De Looze et al. ( 2014 ) relation are located below KS, and vice versa. In particular, due to the recent starburst, the dense centre () of Freesia lies above the KS () relation. At such high star formation surface densities the increases with less rapidly than expected from the local relation De Looze et al. ( 2014 ), which however only covers the low end of the range. Thus, the observed [C ii ]–SFR deficit can be primarily ascribed to negative stellar feedback during starburst phases, disrupting MCs around star formation sites. This interpretation was originally proposed in Vallini et al. ( 2015 ); our results fully endorse it. Metallicity effects have a weaker impact on the origin of [C ii ]–SFR deviations. Gas with extremely low ( Z ≲ 10 −2 Z ⊙ ) metallicities fails below both the local – and the KS relations, because of lack of C + ions and inefficient H 2 formation, respectively. However, gas with Z ≲ 10 −2 Z ⊙ is scarce in Freesia and its combined contribution is sub-dominant when galaxy integrated relations are considered. This situation is common to most of the galaxies in our sample. A metallicity effect might be relevant for galaxies that cannot retain their metal production (Xu et al. 2016 ; Jeon Bromm 2019 ), which are expected to be smaller ( M ⋆ ≲ 5 × 10 6 M ⊙ ), and with a lower star formation (), for which however
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