ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Tag O O O O O O B-Wavelength I-Wavelength O O B-Wavelength I-Wavelength O O O O O O O O O B-Wavelength I-Wavelength B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O B-Formula I-Formula I-Formula I-Formula I-Formula O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength I-Wavelength O B-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: modelled continuum. Star formation history was modelled by a short burst of star-forming galaxies with age less than 10 Myr, which represents the young stellar population in addition to continuous star formation responsible for older stars with ages t 1 and t 2 ( t 1 t 2 ) randomly varied in the range between 10 Myr and 15 Gyr. The derived age t 2 of the oldest stars is 10 Gyr in most of galaxies. The relation between [Mg/Ne] and stellar mass is shown in Fig. 4 . The linear regression to all Mg II galaxies is shown by a solid blue line and average values in bins of stellar masses by solid green lines. A slight slope is seen, meaning that more massive galaxies have higher magnesium depletion. In particular, [Mg/Ne] ≃ –0.15 for low-mass galaxies with M ⋆ ≃ 3 × 10 7 M ⊙ and ≃–0.35 for high-mass galaxies with M ⋆ ≃ 3 × 10 10 M ⊙ . A similar behaviour is seen for the magnesium depletion, which increases with metallicity (Figs. 1 c and d). Fig. 4. [Mg/Ne] – mass of stellar population log( M ⋆ / M ⊙ ) relation. Symbols are as in Fig. 1 . A linear regression to all Mg II galaxies is shown by the solid blue line, and the average values in bins of stellar masses are represented by solid green lines. 4.2. Dependence of [Mg/Ne] on O<sub>32</sub> O 32 = [O III ] λ 5007/[O II ] λ 3727 is an important parameter to search for galaxies with Lyman continuum (LyC) escaping radiation. The parameter O 32 is usually used for the selection of galaxy candidates able to ionise the intergalactic medium, which is interesting in connection with the problem of the reionisation of the Universe at redshifts z ∼ 5–10. The dependence of [Mg/Ne] on O 32 is shown in Fig. 5 . There is very large scatter of [Mg/Ne] for Mg II galaxies with O 32 ∼ 0–3 (Fig. 5 a). Nevertheless, in galaxies with O 32 below 3–4 [Mg/Ne] is constant, but at higher O 32 [Mg/Ne] increases with increasing O 32 . Linear regression to all the galaxies (purple line) and average values in bins of O 32 (blue lines) demonstrate an increase in [Mg/Ne] with increasing O 32 , which depends on the ionisation parameter. Moreover, the galaxies with O 32 > 5 are above the average value of [Mg/Ne] (long solid red and dashed black lines). We note that almost all galaxies with O 32 > 5 have low masses (log( M ⋆ / M ⊙ ) 9.0), low metallicities (12 + log O/H 8) and high EW(H β ) > 150 Å (dots inside green circles). In Fig. 5 b we only show galaxies with abundances derived by the direct T e method and accuracies better than 40% (more than 2.5 σ ) for the weak but important Mg II λ 2797Å and [O III ] λ 4363Å emission lines. Galaxies with flux ratios I [O III ] λ 4959/ I (H β ) less than 0.7 were also excluded to ensure that we use only high-excitation galaxies whose [O III ] λ 4363Å emission lines are reliably detected. The trend of increasing [Mg/Ne] with increasing O 32 becomes even more evident (purple line in Fig. 5 b). Fig. 5. Panel a : [Mg/Ne] – O 32 relations for all Mg II emitters depicted as in Fig. 1 . The dots