Table 3.
Specs of the galaxy surveys considered in this work.
| Ng | λ/Δλ | Δzi | Catalog | z | |
|---|---|---|---|---|---|
| DESI | 𝒪(107) | 0.001 | 0.1 | BGS | [0.1, 0.4] |
| LRG | [0.4, 1.1] | ||||
| ELG | [1.1, 1.6] | ||||
| QSO | [1.6, 2] | ||||
| SDSS | 𝒪(105) | 0.002 | 0.1 | NYU MAIN | [0.1, 0.2] |
| BOSS LOWZ | [0.1, 0.4] | ||||
| BOSS CMASS | [0.4, 0.7] | ||||
| DR14 QSO | [0.7, 2] | ||||
Notes. We consider DESI (Adame et al. 2024) and SDSS, (Blanton et al. 2005; Reid et al. 2016). The forecasted sources in DESI are divided between bright galaxies (BGS), luminous red galaxies (LRG), emission line galaxies (ELG), and quasars (QSO). For SDSS, it contains results from the galaxy NYU value-added catalog, the luminous red galaxy samples in BOSS, and the quasars in the DR14 release. The total number Ng was obtained by integrating dNg/dzdΩ over the redshift and observed sky area. The term λ/Δλ defines the instrumental resolution, which sets the best possible spectroscopic resolution that one can reach, namely min(δzi) = λ/Δλ. Finally, Δzi describes the width of the redshift bins used in our forecast analysis (see Sect. 3.4).
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