Spectroscopic observation of stars and galaxies are intrinsically limited in number by current instrumentation at telescopes. In the last years, a strong science interest has developed to increase significantly the number of spectra of stars and galaxies to conduct statistical analysis. A number of international projects are thus in development. The table below give a summary of current facilities such as SDSS-V, AAOmega, PFS, DESI, 4MOST, MOONS, WEAVE and MSE, and the new instruments in development such as MUST, Spec-S5, WST, MOSAIC and BlueMUSE.
| First Light | Telescope | Project | Telescope Diameter | Number of optical fibers |
|---|---|---|---|---|
| 2006 | AAT | AAOmega | 3.9 m | 400 |
| 2008/2025 (2.0) | Subaru | PFS | 8.2 m | 2’400 |
| 2019 | Mayall | DESI | 4.0 m | 5’000 |
| 2020 | Apache Point/DuPont | SDSS-V | 2.5 m | 2 x 500 (one on each hemisphere) |
| 2022 | WHT | WEAVE | 4.2 m | 1’000 |
| 2023 | VISTA | 4MOST | 3.7 m | 2’400 |
| 2024 | VLT | MOONS | 8.2 m | 1’000 |
| 2029 | MUST Telescope | MUST | 6.5 m | 20’000 |
| 2030 | CFHT | MSE | 10 m | 3’200 |
| 2031 | VLT | BlueMUSE | 8.2 m | – |
| 2035 | ELT | MOSAIC | 39 m | 300 (optical-train positioners) |
| 2037 | Mayall/Blanco | Spec-S5 | 6 m | 2 x 14’000 (one on each hemisphere) |
| 2040 | WST Telescope | WST | 12 m | 20’000 |