Optimizing the transmission of the GRAVITY/VLTI near-infrared wavefront sensor

Hippler, S.; Deen, C.; Böhm, A.; Brandner, W.; Henning, Thomas; Huber, Armin; Kendrew, Sarah; Lenzen, R.; Rohloff, Ralf-Rainer; Araujo-Hauck, Constanza; Pfuhl, O.; Clénet, Y.; Zhu, Jianqiang

doi:10.1117/12.925920

Cited by 5 publications

(1 citation statement)

References 9 publications

(11 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Further details of the optical design are presented by Yang et al 10 in these proceedings. Table 1 summarises the key requirements for detector performance for the WFS.…”

Section: Wavefront Sensor Optical Designmentioning

confidence: 99%

GRAVITY Coudé Infrared Adaptive Optics (CIAO) system for the VLT Interferometer

Kendrew¹,

Hippler²,

Brandner³

et al. 2012

SPIE Proceedings

View full text Add to dashboard Cite

GRAVITY is a second generation instrument for the VLT Interferometer, designed to enhance the near-infrared astrometric and spectro-imaging capabilities of VLTI. Combining beams from four telescopes, GRAVITY will provide an astrometric precision of order 10 micro-arcseconds, imaging resolution of 4 milli-arcseconds, and low and medium resolution spectro-interferometry, pushing its performance far beyond current infrared interferometric capabilities. To maximise the performance of GRAVITY, adaptive optics correction will be implemented at each of the VLT Unit Telescopes to correct for the effects of atmospheric turbulence. To achieve this, the GRAVITY project includes a development programme for four new wavefront sensors (WFS) and NIR-optimized real time control system. These devices will enable closed-loop adaptive correction at the four Unit Telescopes in the range 1.4-2.4 µm. This is crucially important for an efficient adaptive optics implementation in regions where optically bright references sources are scarce, such as the Galactic Centre. We present here the design of the GRAVITY wavefront sensors and give an overview of the expected adaptive optics performance under typical observing conditions. Benefiting from newly developed SELEX/ESO SAPHIRA electron avalanche photodiode (eAPD) detectors providing fast readout with low noise in the near-infrared, the AO systems are expected to achieve residual wavefront errors of ≤400 nm at an operating frequency of 500 Hz.

show abstract

“…Further details of the optical design are presented by Yang et al 10 in these proceedings. Table 1 summarises the key requirements for detector performance for the WFS.…”

Section: Wavefront Sensor Optical Designmentioning

confidence: 99%