ANDES, the high-resolution spectrograph for the ELT: RIZ Spectrograph Preliminary Optical Design

被引:0
|
作者
Lanotte, Audrey A. [1 ]
Chazelas, Bruno [1 ]
Lovis, Christophe [1 ]
Weber, Michael [2 ]
Wosch, Manfred [2 ]
Oliva, Ernesto [3 ]
Delabre, Bernard [4 ]
Genolet, Ludovic [1 ]
Diaz, Pablo Santos [1 ]
Marconi, Alessandro [5 ,6 ]
Di Martantonio, Paolo [7 ]
Zanutta, Alessio [8 ]
Aliverti, Matteo [8 ]
Balestra, Andrea [9 ]
Cabona, Lorenzo [8 ]
Coretti, Igor [7 ]
Pariani, Giorgio [8 ]
Radaelli, Edoardo [8 ]
Scalera, Marcello [8 ]
Scaudo, Andrea [8 ]
机构
[1] Univ Geneva, Dept Astron, Chemin Pegasi 51, CH-1290 Versoix, Switzerland
[2] Astrophys Leibniz Inst Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany
[3] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy
[4] Ex ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany
[5] Univ Florence, Dept Phys & Astron, Florence, Italy
[6] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy
[7] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy
[8] INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Lc, Italy
[9] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy
基金
瑞士国家科学基金会;
关键词
astronomy instruments; spectrograph; optics;
D O I
10.1117/12.3017976
中图分类号
TH7 [仪器、仪表];
学科分类号
0804 ; 080401 ; 081102 ;
摘要
The first generation of ELT instruments includes an optical-infrared High Resolution Spectrograph, ANDES (ArmazoNes high Dispersion Echelle Spectrograph). The optical design and architecture of ANDES is primarily dictated by its high spectral resolving power (R=100'000), the area of the spectrograph slit projected onto the sky (> 1 arcsec(2)), its broad wavelength coverage and the large primary mirror of the ELT, and must foresee several huge fiber-fed spectrograph units. One of them is the RIZ spectrograph, covering wavelengths from 620 to 960 nm. It deals with a recomposed similar to 40-mm-long entrance slit and a pupil anamorphic magnification to overcome the limitation size of a mosaic 1.6-meter R4 Echelle grating. It requires two fast cameras with F/# close to the unity. This paper describes the preliminary optical design of the RIZ spectrograph instrument, its challenges, and its nominal and expected performances.
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页数:7
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