First light Adaptive Optics system for large binocular telescope

被引：19

作者：

Esposito, S ^{[1
]}

Tozzi, A ^{[1
]}

Ferruzzi, D ^{[1
]}

Carbillet, M ^{[1
]}

Riccardi, A ^{[1
]}

Fini, L ^{[1
]}

Verinaud, C ^{[1
]}

Accardo, M ^{[1
]}

Brusa, G ^{[1
]}

Gallieni, D ^{[1
]}

Biasi, R ^{[1
]}

Baffa, C ^{[1
]}

Biliotti, V ^{[1
]}

Foppiani, I ^{[1
]}

Puglisi, A ^{[1
]}

Ragazzoni, R ^{[1
]}

Ranfagni, P ^{[1
]}

Stefanini, P ^{[1
]}

Salinari, P ^{[1
]}

Seifert, W ^{[1
]}

Storm, J ^{[1
]}

机构：

[1] Osserv Astrofis Arcetri, I-50125 Florence, Italy

来源：

ADAPTIVE OPTICAL SYSTEM TECHNOLOGIES II, PTS 1 AND 2 | 2003年 / 4839卷

关键词：

pyramid wavefront sensor; achromatic pyramid; first light LBT;

D O I：

10.1117/12.458866

中图分类号：

TH7 [仪器、仪表];

学科分类号：

0804 ; 080401 ; 081102 ;

摘要：

The paper describes the design of the single conjugate Adaptive Optics system to be installed on the LBT telescope. This system will be located in the Acquisition, Guiding and Wavefront sensor unit (AGW) mounted at the front bent Gregorian focus of LBT. Two innovative key features of this system are the Adaptive Secondary Mirror and the Pyramid Wavefront Sensor. The secondary provides 672 actuators wavefront correction available at the various foci of LBT. Due to the adaptive secondary mirror there is no need to optically conjugate the pupil on the deformable mirror. This allows having a very short sensor optical path made up using small dimension refractive optics. The overall AO system has a transmission of 70 % and fits in a rectangle of about 400x320mm. The pyramid sensor allows having different pupil sampling using on-chip binning of the detector. Main pupil samplings for the LBT system are 3000, 15x15 and 10x10. Reference star acquisition is obtained moving the wavefront sensor unit in a field of view of 3x2 arcmin. Computer simulations of the overall system performance show the good correction achievable in J, H, and K. In particular, in our configuration, the limiting magnitude of pyramid sensor results more than one magnitude fainter with respect to Shack-Hartmann sensor. This feature directly translates in an increased sky coverage that is, in K band, about doubled with respect to the same AO system using a Shack-Hartmann sensor.

引用

页码：164 / 173

页数：10

共 14 条

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Esposito, S
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[7] FOPPIANI I, IN PRESS SPIE C, V4837
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