By Chris R. Benn, Sebastian Els, Tom Gregory, Ilona Söchting (auth.), Wolfgang Brandner, Markus E. Kasper (eds.)
ISBN-10: 3540250344
ISBN-13: 9783540250340
ISBN-10: 3540316051
ISBN-13: 9783540316053
The box of Adaptive Optics (AO) for astronomy has matured in recent times, and diffraction-limited picture solution within the near-infrared is now in many instances accomplished by means of ground-based eight to 10m category telescopes. This ebook offers the court cases of the ESO Workshop on technological know-how with Adaptive Optics held within the fall of 2003. The ebook offers an summary on AO instrumentation, information acquisition and aid ideas, and covers observations of the sunlight, sunlight process gadgets, circumstellar disks, substellar partners, HII areas, starburst environments, late-type stars, the galactic heart, energetic galaxies, and quasars. The contributions current a brilliant photograph of the multitude of technological know-how themes being addressed via AO in observational astronomy.
Read Online or Download Science with Adaptive Optics: Proceedings of the ESO Workshop Held at Garching, Germany, 16-19 September 2003 PDF
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Extra resources for Science with Adaptive Optics: Proceedings of the ESO Workshop Held at Garching, Germany, 16-19 September 2003
Sample text
A single high order deformable mirror conjugated to the ground is used to correct the ground layer turbulence. The concept is summarized in Fig 1. 2” FWHM) a high order correction is required: the ground layer must be almost fully corrected. This was verified by simulations. We end up with 32×32 sub-apertures on the wavefront sensor, 881 actuators on the deformable mirror. Four sodium laser guide stars are used to provide sufficient flux to the wavefront sensors. Since only one DM is used, the only modes which need to be measured from a single NGS are tip and tilt.
Finally, they are monochromatic, allowing the use of a filter to block their light from entering the spectrograph. This light would otherwise certainly saturate the detector. The estimated performance of the wide field, low resolution mode performance can be seen in Fig. 2. Notice the small amplitude of isoplanatic effect 38 M. Le Louarn et al. Fig. 1. Muse concept showing the location of the laser guide stars, the natural guide star and the science field of view. Fig. 2. Performance in the low resolution mode (shown as encircled energy as a function of distance from PSF center).
3. Strehl loss due to angular anisoplanatism, expressed at H band, as a function of the distance to the guide star. 5)2 ) The results presented above are for guide stars bright enough that the photon noise and the electronic noise on the WFS CCD are negligible. When this is the case, we say that the system works in full correction mode and the performance are pretty much independent of the actual GS brightness. Below a certain brightness however, the WFS noise becomes significant and the performance degrades with decreasing GS brightness, until the GS is too faint to serve as reference.
Science with Adaptive Optics: Proceedings of the ESO Workshop Held at Garching, Germany, 16-19 September 2003 by Chris R. Benn, Sebastian Els, Tom Gregory, Ilona Söchting (auth.), Wolfgang Brandner, Markus E. Kasper (eds.)
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