Pre-shipment test of the ARGOS laser guide star wavefront sensor

Bonaglia, Marco; Busoni, Lorenzo; Mazzoni, Tommaso; Puglisi, Alfio; Antichi, J.; Esposito, Simone; Xivry, Gilles Orban de; Rabien, S.

doi:10.1117/12.2056596

Cited by 5 publications

(5 citation statements)

References 4 publications

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“…Both ARGOS LGS wavefront sensors are based on a Shack Hartmann (SH) scheme to detect the laser guide stars Figure 3 shows a drawing and the SH pattern on the detector. Details are described in [9]. Being located in the plane of the 12km focus, a field stop with ~4.5arcsec diameter forms the entrance to the WFS optics.…”

Section: Wavefront Sensingmentioning

confidence: 99%

“…The optics is adjusted such that the three SH patterns are nicely distributed over the CCD, each sub-aperture owns 8x8 pixels and the split frame transfer does not cross subapertures. More information on the wavefront sensor performance is given in [9]. The CCD itself is based on a deep-depletion technology, offers 264x264 pixels and a low readout noise at a kHz frame rate.…”

Section: Wavefront Sensingmentioning

confidence: 99%

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Performance and First Science Observations with ARGOS

Rabien¹

2017

Proceedings of the Adaptive Optics for Extremely Large Telescopes 5

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Coming online for scientific operations, the ARGOS facility is boosting the imaging and spectroscopic capabilities at the LBT. With six Rayleigh laser guide stars and the corresponding wavefront sensing, ARGOS corrects the ground layer distortions for both LBT 8.4 m telescopes with its adaptive secondary mirrors. Under most conditions this setup delivers a PSF size reduction by a factor ~2-3. With the two LUCI infrared imaging and MOS spectroscopy instruments receiving the corrected images, observations in the near infrared can be performed at high spatial and spectral resolution. We will briefly discuss the final ARGOS technical setup and the adaptive optics performances. With first scientific observations been conducted, we will show that imaging cases with GLAO are nicely boosting several science programs from cluster CMD, Milky Way embedded star formation and Cepheids, BHs in nearby galaxies to extragalactic deep fields. In the unique combination of ARGOS with the multi-object NIR spectroscopy available in LUCI, first scientific observations have been performed on local and high-z objects. Those high spatial and spectral resolution observations nicely demonstrate the capabilities now at hand with ARGOS at the LBT. Inhere we describe briefly the system and show examples of science observations from nearby clusters to high redshift gravitationally lensed objects.

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Section: Wavefront Sensingmentioning

confidence: 99%

Section: Wavefront Sensingmentioning

confidence: 99%

Performance and First Science Observations with ARGOS

Rabien¹

2017

Proceedings of the Adaptive Optics for Extremely Large Telescopes 5

Self Cite

View full text Add to dashboard Cite

show abstract

“…The optics is adjusted such that the three SH patterns a nicely distributed over the CCD, each sub-aperture owns 8x8 pixels and the split frame transfer does not cross sub-apertures. More information on the wavefront sensor performance is given in [8].…”

Section: Wavefront Sensing and Controlmentioning

confidence: 99%

Status of the ARGOS project

et al. 2014

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ARGOS is the Laser Guide Star and Wavefront sensing facility for the Large Binocular Telescope. With first laser light on sky in 2013, the system is currently undergoing commissioning at the telescope. We present the overall status and design, as well as first results on sky. Aiming for a wide field ground layer correction, ARGOS is designed as a multi-Rayleigh beacon adaptive optics system. A total of six powerful pulsed lasers are creating the laser guide stars in constellations above each of the LBTs primary mirrors. With a range gated detection in the wavefront sensors, and the adaptive correction by the deformable secondary's, we expect ARGOS to enhance the image quality over a large range of seeing conditions. With the two wide field imaging and spectroscopic instruments LUCI1 and LUCI2 as receivers, a wide range of scientific programs will benefit from ARGOS. With an increased resolution, higher encircled energy, both imaging and MOS spectroscopy will be boosted in signal to noise by a large amount. Apart from the wide field correction ARGOS delivers in its ground layer mode, we already foresee the implementation of a hybrid Sodium with Rayleigh beacon combination for a diffraction limited AO performance.

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“…This is a compromise between spot elongation and the number of collected photons, both influencing the accuracy of the wavefront gradient measurements. This system and its performances are described in detail in [4,5].…”

Section: Argos Lgs Wavefront Detectionmentioning

confidence: 99%

“…The Argos WFS detector and the computer have been first successfully integrated to the WFS in Europe in spring 2013 and have undergone system test development in the following year [4,5]. In March 2014, a first (Right) NGS correction using the pyramid WFS on a central star, with the measurements routed to the Argos wavefront computer, and operating the ASM.…”

Section: Argos Wavefront Sensing First Operationmentioning

confidence: 99%

ARGOS wavefront sensing: from detection to correction

Xivry¹,

Bonaglia

Borelli

et al. 2014

SPIE Proceedings

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Argos is the ground-layer adaptive optics system for the Large Binocular Telescope. In order to perform its wide-field correction, Argos uses three laser guide stars which sample the atmospheric turbulence. To perform the correction, Argos has at disposal three different wavefront sensing measurements : its three laser guide stars, a NGS tip-tilt, and a third wavefront sensor. We present the wavefront sensing architecture and its individual components, in particular : the finalized Argos pnCCD camera detecting the 3 laser guide stars at 1kHz, high quantum efficiency and 4e − noise; the Argos tip-tilt sensor based on a quad-cell avalanche photo-diodes; and the Argos wavefront computer. Being in the middle of the commissioning, we present the first wavefront sensing configurations and operations performed at LBT, and discuss further improvements in the measurements of the 3 laser guide star slopes as detected by the pnCCD.

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Pre-shipment test of the ARGOS laser guide star wavefront sensor

Cited by 5 publications

References 4 publications

Performance and First Science Observations with ARGOS

Performance and First Science Observations with ARGOS

Status of the ARGOS project

ARGOS wavefront sensing: from detection to correction

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