Adaptive Optics for Extremely Large Telescopes 4 – Conference Proceedings
Parent: UC Observatories
eScholarship stats: Breakdown by Item for June through September, 2026
| Item | Title | Total requests | Download | View-only | %Dnld |
|---|---|---|---|---|---|
| 5cf394wh | Adaptive Optics for Extremely Large Telescopes 4 - Program Booklet | 325 | 187 | 138 | 57.5% |
| 015808kc | Measuring Segment Piston with a Dispersed Fringe Sensor on the Giant Magellan Telescope | 288 | 42 | 246 | 14.6% |
| 2vj6w3gm | The use of CPU, GPU and FPGA in real-time control of adaptive optics systems | 274 | 35 | 239 | 12.8% |
| 93x3m220 | Non common path aberration correction with non linear WFSs | 241 | 39 | 202 | 16.2% |
| 2mn1w74z | Point spread function determination for Keck adaptive optics: overview | 223 | 34 | 189 | 15.2% |
| 6809n74d | Durham AO Real-time Controller (DARC) running on Graphics Processing Units (GPUs) | 222 | 21 | 201 | 9.5% |
| 1k41x51n | INO Pyramidal Wavefront Sensor Demonstrator: first closed-loop on-sky operation at Mont-Mégantic Telescope | 221 | 35 | 186 | 15.8% |
| 56v9924z | Experimental implementation of a Pyramid WFS: Towards the | 205 | 26 | 179 | 12.7% |
| 910646qf | Low Wind Effect, the main limitation of the SPHERE instrument | 199 | 35 | 164 | 17.6% |
| 9xx3208w | On-sky results of Raven, a MOAO science demonstrator at Subaru Telescope | 190 | 103 | 87 | 54.2% |
| 7t52h1r1 | Miniaturized Shack-Hartmann Wavefront-Sensors for ELTs | 187 | 46 | 141 | 24.6% |
| 217686nz | Design and Development Status of MKID Integral Field Spectrographs for High Contrast Imaging | 186 | 39 | 147 | 21.0% |
| 2zm625jk | Selex infrared sensors for astronomy – present and future | 185 | 31 | 154 | 16.8% |
| 23w5v4vv | New Cophasing and AO strategies for an extremely large telescope dedicated to extremely high contrast: The Colossus Project | 183 | 82 | 101 | 44.8% |
| 81f1f8pt | Prototyping the GMT phasing camera with the Magellan AO system | 182 | 27 | 155 | 14.8% |
| 5n84b2z0 | Multi-conjugate Adaptive Optics at Big Bear Solar Observatory | 175 | 37 | 138 | 21.1% |
| 4gr3p2pf | Adaptive Optics Program at TMT | 168 | 56 | 112 | 33.3% |
| 3cq132qm | Pyramid versus Shack-Hartmann: Trade Study Results for the NFIRAOS NGS WFS | 165 | 49 | 116 | 29.7% |
| 80j280rv | Filtering the interaction matrix in an adaptive optics system | 162 | 38 | 124 | 23.5% |
| 0479k8m1 | Observations of the dynamic turbulence above La Palma using Stereo-SCIDAR | 160 | 38 | 122 | 23.8% |
| 0gt3876k | SPHERE extreme AO system On-sky operation, final performance and future improvements | 157 | 55 | 102 | 35.0% |
| 5vv5p369 | Self-Coherent Camera as a focal plane phasing sensor - Overview and early comparison with the Zernike Phase Contrast Sensor | 157 | 28 | 129 | 17.8% |
| 8x09340m | Dissecting Star-forming regions with the GeMS MCAO instrument: lessons learned for optimal post-processing of WFAO data | 157 | 84 | 73 | 53.5% |
| 20s3w2j6 | Laser guide star adaptive optics at Lick Observatory | 152 | 40 | 112 | 26.3% |
| 2mq8n4d4 | First Results of the Ground Layer Adaptive Optics System ARGOS | 149 | 34 | 115 | 22.8% |
| 4q40v3ft | Wavefront control simulations for the Giant Magellan Telescope: Field-dependent segment piston control | 145 | 49 | 96 | 33.8% |
| 1367c5xw | Anti-aliasing wave-front reconstruction with Shack-Hartmann sensors | 140 | 31 | 109 | 22.1% |
| 4s5364qp | A Fresnel propagation analysis for SPEED (Segmented Pupil Experiment for Exoplanet Detection) | 138 | 28 | 110 | 20.3% |
| 5q66922d | E-ELT M4 Unit updated design and prototype results | 138 | 37 | 101 | 26.8% |
| 87f6s2zv | The GMT Dynamic Optical Simulation | 135 | 20 | 115 | 14.8% |
| 8w80k9sp | An Integrated MASS/DIMM Monitor Based on a Low-Noise CCD Detector | 135 | 21 | 114 | 15.6% |
| 6317r29b | Near-infrared tip-tilt sensing at Keck: System architecture and on-sky performance | 134 | 40 | 94 | 29.9% |
| 7f60s89n | Optimizing use of multiple stars for near-infrared tip-tilt compensation at the W. M. Keck Observatory | 133 | 21 | 112 | 15.8% |
| 20x7p7qb | Recent Improvements to the Keck II Laser Guide Star Facility | 132 | 33 | 99 | 25.0% |
| 8sq053mx | Progress with the 4m high-order AO demonstrator, CHOUGH | 131 | 31 | 100 | 23.7% |
| 8wj5p4cc | Modeling the pyramidal sensor by a ZEMAXTM user defined surface. | 131 | 30 | 101 | 22.9% |
| 42h0n70s | Implementation of SLODAR atmospheric turbulence profiling to the ARGOS system | 130 | 34 | 96 | 26.2% |
| 3gp3k4kg | Retrieving tip-tilt information from Tomographic Laser Guide Star Adaptive Optics Systems | 129 | 22 | 107 | 17.1% |
| 2cr972kt | Aligning the LINC-NIRVANA Natural Guide Stars MCAO system | 126 | 38 | 88 | 30.2% |
| 8xc125wz | The MAORY first-light adaptive optics module for E-ELT | 126 | 27 | 99 | 21.4% |
| 5t0211tn | SCExAO: the first high contrast exoplanet imager on an ELT? | 125 | 32 | 93 | 25.6% |
| 8p13k3zc | Reducing adaptive optics latency using many-core processors | 125 | 34 | 91 | 27.2% |
| 1h5301vq | Coupling of WFS with a segmented DM “Test of different concepts: SH, Pyramid, Zernike phase sensor” | 124 | 28 | 96 | 22.6% |
| 8d79v3t0 | XAO at LBT: current performances in the visible and upcoming upgrade | 123 | 27 | 96 | 22.0% |
| 56p467d6 | Astrometry with MCAO at Gemini and at ELTs | 121 | 28 | 93 | 23.1% |
| 7019b6vc | AO for MOSAIC, the E-ELT Multiple Object Spectrograph | 121 | 22 | 99 | 18.2% |
| 8nb0n5jf | Progress report on the ESO 4LGSF | 121 | 34 | 87 | 28.1% |
| 9q7259nn | Non Boltzmann Modeling of Sodium Guidestar Returns and Implications for Guidestar Linewidth | 121 | 21 | 100 | 17.4% |
| 4jh5c19s | Laboratory tests on HeNOS, the MCAO test bench for NFIRAOS | 120 | 31 | 89 | 25.8% |
| 0bz8t4mv | Commissioning of ARGOS at LBT: adaptive optics procedures | 118 | 30 | 88 | 25.4% |
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