Table 3.
Characteristics of instruments and exposures used for the simulations.
Inst. Tel. Obs. | l | D (m) | Field | texp (s) | r (″) | Mag. | ||
---|---|---|---|---|---|---|---|---|
Visible and near-IR Imagers | ||||||||
EFOSC NTT ESO (La Silla) | 3.6 | Vis | 4′ | 300 | 1 | 24.2 | Focal reducer (Buzzoni et al. 1984) | |
FORS VLT ESO (Paranal) | 8.2 | Vis | 6′ | 300 | 0.8 | 25.2 | Focal reducer (Appenzeller et al. 1998) | |
HAWKI VLT ESO (Paranal) | 8.2 | NIR | 60 | 0.6 | 21.4 | Near-IR imager (Kissler-Patig et al. 2008) | ||
MICADO ELT ESO (Armazones) | 39. | NIR | 50″ | 60 | 0.015 | 24.9 | Visible and near-IR imager with adaptive optics on the ELT (a) | |
OmegaCam VST ESO (Paranal) | 2.4 | Vis | 1.0° | 300 | 0.8 | 23.9 | Survey wide-field imager (Kuijken et al. 2002) | |
1.5 m Catalina U.AZ (Mt. Lemmon) | 1.52 | Vis | 2.2° | 30 | 1.5 | 21.4 | Survey wide-field imager (b) | |
LSST Cam. SST VRO (Pachon) | 8 | Vis | 3.0° | 15 | 0.8 | 24.6 | Survey wide-field imager (c) | |
0.7 m Catalina U.AZ (Mt. Bigelow) | 0.7 | Vis | 4.4° | 30 | 3 | 19.8 | Survey wide-field imager (b) | |
Photo | −30° | 0.07 | Vis | 75° ×55° | 60 | 60 | 10 | Photographic camera with a wide-angle lens from a good site. |
Visible and near-IR Spectrographs | ||||||||
FORS VLT ESO (Paranal) | 8.2 | Vis | 6′×1″ | 1200 | 0.8 | 22.0 | Long-slit low-resolution spectrograph (Appenzeller et al. 1998) | |
UVES VLT ESO (Paranal) | 8.2 | Vis | 10″ × 1″ | 1200 | 0.8 | 17.0 | High-resolution echelle spectrograph (Dekker et al. 2000) | |
4MOST-L VISTA ESO (Paranal) | 4 | Vis | 1200 | 0.8 | 20.5 | Multi fibre (1) spectrograph (low res.) (de Jong et al. 2016) | ||
4MOST-H VISTA ESO (Paranal) | 4 | Vis | 1200 | 0.8 | 18.6 | Multi-fibre (1) spectrograph (med res.) (de Jong et al. 2016) | ||
ESPRESSO VLT ESO (Paranal) | 8.2 | Vis | 1200 | 0.5 | 15.8 | High-resolution echelle (Pepe et al. 2021) | ||
Thermal IR | ||||||||
VISIR VLT | 8.2 | ThIR | 60″ | 10 | – | Imager (Lagage et al. 2004) | ||
METIS ELT | 39 | ThIR | 10″ | 10 | – | Adaptive Optics Imager on ELT (d),(2) |
Notes.
4MOST is a multi-object spectrograph equipped with 2436 fibres. Monte-Carlo simulations showed that, on average, a satellite crossing the field of view will affect 1.3 fibres.
Table key: l: latitude; D: diametre of the telescope; Field: field of view of the instrument; texp: exposure time [s]; r: resolution element [arcsec]; Mag: 5σ limiting magnitude for a point source for an exposure of duration texp.
References. (a)https://elt.eso.org/instrument/MICADO/, (b)https://catalina.lpl.arizona.edu/about/facilities/telescopes, (c)https://www.lsst.org/about, (d)https://elt.eso.org/instrument/METIS/.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.