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tokens: λλ1907, 1909, C iv 1548, 1551, and He ii λ1640. They find seven objects with [C iii ], C iii ] λλ1907, 1909 emission, some of them reaching extremely high equivalent width values (). Finally, they find that C iv 1548, 1551 and He ii λ1640 have equivalent widths below 2 Å and conclude that the detection of C iv 1548, 1551 atÅ may require extremely metal poor stars and gas. In SBS 0335−052E, which is more metal-poor that the previous sample, C iv 1548, 1551 shows a weak P-Cygni profile and nebular components. The EWs of the nebular [C iii ], C iii ] λλ1907, 1909 and C iv doublet emissions are 5 and 1.7 Å, respectively. The largest C iv 1548, 1551 EW which has been reported for a nearby starburst galaxy is Å. This is for galaxy J104457, which has 12+log(O/H) = 7.45 (Berg et al. 2019b ) and is at a very similar redshift (0.013) compared to SBS 0335−052E. Senchyna Stark ( 2019 ) present HST COS UV observations of six star-forming XMPs with 12+log(O/H) between 7.4 and 7.7, i.e. lower than in the work of Senchyna et al. ( 2017 ). They find stellar C iv 1548, 1551 in five of the galaxies and high [C iii ]+C iii ] equivalent widths (Å) in two objects. The highest EWs of C iv 1548, 1551 and He ii which they find are 4.4 and 1.7 Å, respectively. For SBS 0335−052E we find EWs of 1.7 Å for C iv 1548, 1551 and He ii λ1640. Although nebular C iv 1548, 1551 emission is present in some very high sSFR nearby systems, nearby systems do not reach the equivalent widths of C iv which are observed in individual lensed systems at z >6. Undisputed detections of nebular emission in He ii in predominantly star-forming systems at z >6 remain elusive (Senchyna Stark 2019 ). Objects located at z = 2-4 with high values of EWs(C iii ]), i.e. ≥10 Å, are analysed in Nakajima et al. ( 2018 ), who find that EWs(C iii ])>20 Å can only be modelled with a combination of photoionization by stars and an AGN. 6.2 C/O Berg et al. ( 2016 ) and Berg et al. ( 2019a ) studied the C/O ratio derived via UV collisionally excited emission lines of a sample of 12 low metallicity galaxies with significant detections of carbon and oxygen lines. At low metallicity, (12+log(O/H)8.0), they find that no clear trend is evident in C/O versus O/H. We find log(C/O) ∼ −0.45 via tests 2 and 3, and 12+log(O/H) = 7.48 / 7.42 via tests 4/5, respectively. This is very similar to what Berg et al. ( 2016 ) report for galaxy J120122, which is log(C/O) ∼ −0.45 and 12+log(O/H) = 7.45. 6.3 JWST observation As a simple exercise, we placed SBS 0335−052E at redshift z = 10, and used the COS G130M + G160M + G185M spectrum to simulate an observation of this galaxy with the near-infrared spectrograph (NIRSpec) onboard JWST . For this purpose, the spectrum’s flux was diluted using the luminosity distance for cosmological parameters H 0 = 69.6, Ω M = 0.286, and Ω vac = 0.714. In addition, we accounted for IGM absorption of UV photons using Madau ( 1995 ) attenuation. We degraded the spectrum to match NIRSpec’s prism