Table 1
Overview of existing and planned high-resolution spectrographs.
Spectrograph | Wavelength coverage (nm) | Resolution | Observatory | Mirror diameter (m) | References |
---|---|---|---|---|---|
HARPS | 383–693 | 120 000 | La Silla | 3.6 | 1 |
NIRPS | 950–1800 | 100 000 | La Silla | 3.6 | 25, (*) |
HARPS-N | 383–690 | 115 000 | TNG | 3.6 | 2 |
GIANO | 950–2450 | 50 000 | TNG | 8 | |
ESPRESSO | 380–788 | 70 000 | VLT | 8.2–16 | 3 |
140 000 | |||||
190 000 | |||||
CRIRES+ | 950–1120 | 100 000 | VLT | 8.2 | 4, 5 |
1116–1362 | |||||
1423–1769 | |||||
1972–2624 | |||||
2869–4188 | |||||
3583–5300 | |||||
UVES | 300–500 | 80 000 | VLT | 8.2 | 6 |
420–1100 | 110 000 | ||||
CARMENES | 520–960 | 94 600 | Calar Alto | 3.5 | 7 |
960–1710 | 80 400 | ||||
PEPSI | 384–913 | 50 000 | LBT | 2 × 8.4 | 9, 10 |
130 000 | |||||
250 000 | |||||
HIRES | 300–1100 | 67 000 | Keck | 10 | 11 |
NIRSPEC | 950–5500 | 25 000 | Keck | 10 | 12 |
MAROON-X | 500–920 | 80 000 | Gemini north | 8 | 13 |
GRACES | 400–1000 | 66 000 | Gemini north | 8.1 | 14 |
ESPaDonS | 370–1050 | 81 000 | CFHT | 3.6 | 15 |
SPIRou | 950–2500 | 71 000 | CFHT | 16 | |
IGRINS | 1450–2450 | 45 000 | Gemini south | 8 | 17 |
HDS | 300–1000 | 90 000 | Subaru | 8.2 | 18 |
160 000 | |||||
IRD | 970–1750 | 70 000 | Subaru | 8.2 | 19 |
FIES | 370–730 | 25 000 | NOT | 2.6 | 20 |
46 000 | |||||
67 000 | |||||
HARPS3 | 380–690 | 115 000 | INT | 2.5 | 21 |
Veloce | 580–930 | 75 000 | AAT | 3.9 | 22 |
EXPRES | 400–680 | 137 500 | LDT | 4.3 | 23 |
NEID | 380–930 | 60 000 | WIYN | 3.5 | 24 |
90 000 | |||||
HIRES | 550–1800 | 100 000 | ELT | 39 | 26, (*) |
References. (1) Mayor et al. (2003); (2) Cosentino et al. (2012); (3) Pepe et al. (2021); (4) Kaeufl et al. (2004); (5) Dorn et al. (2014); (6) Dekker et al. (2000); (7) Quirrenbach et al. (2016); (8) Oliva et al. (2012); (9) Strassmeier et al. (2018); (10) Strassmeier et al. (2015); (11) Vogt et al. (1994); (12) McLean et al. (1998); (13) Seifahrt et al. (2018); (14) Chene et al. (2014); (15) Donati et al. (2006); (16) Donati et al. (2020); (17) Park et al. (2014); (18) Noguchi et al. (2002); (19) Tamura et al. (2012); (20) Telting et al. (2014); (21) Thompson et al. (2016); (22) Gilbert et al. (2018); (23) Petersburg et al. (2020); (24) Schwab et al. (2016); (25) Wildi et al. (2017); (26) Marconi et al. (2021); (*) These instruments are still under development, and their characteristics are subject to change.
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