| Item | Title | Total requests | Download | View-only | %Dnld |
|---|---|---|---|---|---|
| 0479k8m1 | Observations of the dynamic turbulence above La Palma using Stereo-SCIDAR | 66 | 47 | 19 | 71.2% |
| 5n84b2z0 | Multi-conjugate Adaptive Optics at Big Bear Solar Observatory | 61 | 13 | 48 | 21.3% |
| 4gr3p2pf | Adaptive Optics Program at TMT | 58 | 27 | 31 | 46.6% |
| 8nb0n5jf | Progress report on the ESO 4LGSF | 54 | 32 | 22 | 59.3% |
| 1qh5b3v0 | Commissioning ShARCS: the Shane Adaptive optics infraRed Camera-Spectrograph for the Lick Observatory 3-m telescope | 51 | 17 | 34 | 33.3% |
| 3wq362xn | Adaptive Optics Point Spread Function Reconstruction at W. M. Keck Observatory in Laser & Natural Guide Star Modes : Final Developments | 49 | 16 | 33 | 32.7% |
| 56v9924z | Experimental implementation of a Pyramid WFS: Towards the | 47 | 13 | 34 | 27.7% |
| 2cr972kt | Aligning the LINC-NIRVANA Natural Guide Stars MCAO system | 46 | 18 | 28 | 39.1% |
| 20x7p7qb | Recent Improvements to the Keck II Laser Guide Star Facility | 43 | 17 | 26 | 39.5% |
| 015808kc | Measuring Segment Piston with a Dispersed Fringe Sensor on the Giant Magellan Telescope | 42 | 23 | 19 | 54.8% |
| 758421jz | Laser Pointing Camera: a valuable tool for the LGS-AO operations | 42 | 22 | 20 | 52.4% |
| 910646qf | Low Wind Effect, the main limitation of the SPHERE instrument | 41 | 5 | 36 | 12.2% |
| 2mn1w74z | Point spread function determination for Keck adaptive optics: overview | 40 | 11 | 29 | 27.5% |
| 2mq7f7k6 | OCAM2S: an integral shutter ultrafast and low noise wavefront sensor camera for laser guide stars adaptive optics systems | 40 | 23 | 17 | 57.5% |
| 5cf394wh | Adaptive Optics for Extremely Large Telescopes 4 - Program Booklet | 40 | 24 | 16 | 60.0% |
| 7019b6vc | AO for MOSAIC, the E-ELT Multiple Object Spectrograph | 40 | 24 | 16 | 60.0% |
| 80j280rv | Filtering the interaction matrix in an adaptive optics system | 40 | 10 | 30 | 25.0% |
| 23w5v4vv | New Cophasing and AO strategies for an extremely large telescope dedicated to extremely high contrast: The Colossus Project | 39 | 12 | 27 | 30.8% |
| 4jh5c19s | Laboratory tests on HeNOS, the MCAO test bench for NFIRAOS | 39 | 14 | 25 | 35.9% |
| 2mq8n4d4 | First Results of the Ground Layer Adaptive Optics System ARGOS | 38 | 18 | 20 | 47.4% |
| 51x9d368 | Calibrating the Non-Common Path Aberrations on the MOAO system RAVEN and | 38 | 23 | 15 | 60.5% |
| 5q66922d | E-ELT M4 Unit updated design and prototype results | 37 | 19 | 18 | 51.4% |
| 93x3m220 | Non common path aberration correction with non linear WFSs | 37 | 11 | 26 | 29.7% |
| 0gt3876k | SPHERE extreme AO system On-sky operation, final performance and future improvements | 36 | 13 | 23 | 36.1% |
| 1367c5xw | Anti-aliasing wave-front reconstruction with Shack-Hartmann sensors | 35 | 8 | 27 | 22.9% |
| 217686nz | Design and Development Status of MKID Integral Field Spectrographs for High Contrast Imaging | 35 | 7 | 28 | 20.0% |
| 2vj6w3gm | The use of CPU, GPU and FPGA in real-time control of adaptive optics systems | 35 | 7 | 28 | 20.0% |
| 7t52h1r1 | Miniaturized Shack-Hartmann Wavefront-Sensors for ELTs | 35 | 11 | 24 | 31.4% |
| 2zm625jk | Selex infrared sensors for astronomy – present and future | 34 | 1 | 33 | 2.9% |
| 7kh262xf | Simulations of AO for the E-ELT and its instruments | 33 | 15 | 18 | 45.5% |
| 8w80k9sp | An Integrated MASS/DIMM Monitor Based on a Low-Noise CCD Detector | 33 | 12 | 21 | 36.4% |
| 3gp3k4kg | Retrieving tip-tilt information from Tomographic Laser Guide Star Adaptive Optics Systems | 32 | 6 | 26 | 18.8% |
| 4h03k92b | Analysis of GeMS tip-tilt on-sky data: LQG implementation for vibration rejections | 32 | 12 | 20 | 37.5% |
| 6809n74d | Durham AO Real-time Controller (DARC) running on Graphics Processing Units (GPUs) | 31 | 4 | 27 | 12.9% |
| 2dm1m7jq | MCAO numerical simulations for EST: analysis and parameter optimization | 30 | 11 | 19 | 36.7% |
| 4p4339x0 | State of the art IR cameras for wavefront sensing using e-APD MCT arrays | 30 | 10 | 20 | 33.3% |
| 4s5364qp | A Fresnel propagation analysis for SPEED (Segmented Pupil Experiment for Exoplanet Detection) | 30 | 10 | 20 | 33.3% |
| 6h92z4q4 | Development of an ELT XAO testbed using a self referenced Mach-Zehnder wavefront sensor | 30 | 14 | 16 | 46.7% |
| 8x09340m | Dissecting Star-forming regions with the GeMS MCAO instrument: lessons learned for optimal post-processing of WFAO data | 30 | 10 | 20 | 33.3% |
| 0bz8t4mv | Commissioning of ARGOS at LBT: adaptive optics procedures | 29 | 13 | 16 | 44.8% |
| 1h5301vq | Coupling of WFS with a segmented DM “Test of different concepts: SH, Pyramid, Zernike phase sensor” | 29 | 12 | 17 | 41.4% |
| 87f6s2zv | The GMT Dynamic Optical Simulation | 29 | 4 | 25 | 13.8% |
| 8ft440wn | Optimizing LGS WFS Pixel Processing in the Context of Evolving Turbulence and Sodium Profile | 29 | 10 | 19 | 34.5% |
| 9q7259nn | Non Boltzmann Modeling of Sodium Guidestar Returns and Implications for Guidestar Linewidth | 29 | 13 | 16 | 44.8% |
| 1x2266wp | Optical design of the Post Focal Relay of MAORY | 28 | 11 | 17 | 39.3% |
| 3416j3cb | Effects of reconstruction layer profiles on atmospheric tomography in E-ELT AO systems | 28 | 10 | 18 | 35.7% |
| 6js4k5m5 | Commissioning of ARGOS at LBT: adaptive optics procedures | 28 | 11 | 17 | 39.3% |
| 8cg2r2p8 | PSF reconstruction for AO photometry and astrometry | 28 | 5 | 23 | 17.9% |
| 16b4h26g | Use of Laser Guide Star with Pyramid Wavefront Sensor | 27 | 1 | 26 | 3.7% |
| 42h0n70s | Implementation of SLODAR atmospheric turbulence profiling to the ARGOS system | 27 | 6 | 21 | 22.2% |
Note: Due to the evolving nature of web traffic, the data presented here should be considered approximate and subject to revision. Learn more.