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 B-Wavelength I-Wavelength O O O O B-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 B-Wavelength I-Wavelength O O O O O B-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 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-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 B-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 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-Wavelength I-Wavelength O O O O O 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 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
tokens: plot summarizing the relative marginal errors on parameters, , for all the parameters, the flux thresholds, the ELG samples and redshift bins, and the sky areas considered. In particular, each row refers to a specific parameter, namely from the top to bottom; each column refers to a specific flux threshold, i.e. from the left- to right-hand side; red, green, and blue lines, respectively, refers to refer to H α , O iii + H β , and O ii galaxies; and diamond, triangle, square, and circle markers refer to , respectively. Figure 7. Relative 1 σ marginal errors on redshift-dependent parameters from the clustering of galaxies detected through different line emission: H α in red, O iii + H β in green, and O ii in blue. Circles, squares, triangles, and diamonds refer to survey areas of 1, 5, 15, and 30 in , respectively, whereas the four columns illustrate the dependence of the constraints on the flux threshold, set to from the left- to right-hand side. The main conclusion one can draw from this plot is that – not counterintuitively – sensitivity is possibly more important than area for high-redshift observations. This is further demonstrated in Fig. 8 , where we focus on the extraction of RSDs in terms of constraints on the redshift-dependent quantity f σ 8 ( z ). We adopt the same colour code as before for the various ELG samples, and the two panels show forecast 1 σ marginal error bars on measurements of f σ 8 ( z i ) in each redshift bin, for a wide and shallow survey (left-hand panel) or a narrow and deep survey (right-hand panel). Clearly, measurements extracted from the original target, namely the H α -galaxy sample, are optimized for the former survey specifications, with error bars tighter than those obtained with the latter experimental configuration. It turns out that a large area and a relatively larger flux threshold is also better for RSD estimation from the O iii + H β sample, with error bars smaller than for a narrow and deep survey. On the other hand, when it comes to the extraction of cosmological information from redshift 3−5 O ii galaxies, it is better to observe as much as 30 times a smaller sky area, but with twice as deep a survey, which yields f σ 8 ( z ) measurements more constrained. Figure 8. Relative 1 σ marginal errors on f σ 8 ( z ) from the clustering of galaxies detected through different line emission: H α in red, O iii + Hβ in green, and O ii in blue, for two different surveys: on the left-hand side a lower sensitive but wide surveys (, ); on the right-hand side a narrow but more sensitive survey (, ). Finally, let us touch upon the importance of high-redshift oxygen-line galaxies to constrain cosmological parameters. Hitherto, we have focused on model-independent parameters related to the redshift evolution of the matter power spectrum, and on its modulation by BAOs, galaxy bias, and RSDs. The next stage will now be to translate constraints on those parameters to more fundamental cosmological parameters as, for