Polychromatic guide star: feasibility study

International audienceAdaptive optics at astronomical telescopes aims at correcting in real time the phase corrugations of incoming wavefronts caused by the turbulent atmosphere, as early proposed by Babcock. Measuring the phase errors requires a bright source located within the isoplanatic patch of the program source. The probability that such a reference source exists is a function of the wavelength, of the required image quality (Strehl ratio), of the turbulence optical properties, and of the direction of the observation. It turns out that the sky coverage is disastrously low in particular in the visible wavelength range where, unfortunately, the gain in spatial resolution brought by adaptive optics is the largest. Foy and Labeyrie have proposed to overcome this difficulty by creating an artificial point source in the sky in the direction of the observation relying on the backscattered light due to a laser beam. This laser guide star (hereinafter referred to as LGS) can be bright enough to allow us to accurately measure the wavefront phase errors, except for two modes which are the piston (not relevant in this case) and the tilt. Pilkington has emphasized that the round trip time of the laser beam to the mesosphere, where the LGS is most often formed, is significantly shorter than the typical tilt coherence time; then the inverse-return-of-light principle causes deflections of the outgoing and the ingoing beams to cancel. The apparent direction of the LGS is independent of the tilt. Therefore the tilt cannot be measured only from the LGS. Until now, the way to overcome this difficulty has been to use a natural guide star to sense the tilt. Although the tilt is sensed through the entire telescope pupil, one cannot use a faint source because $APEX 90% of the variance of the phase error is in the tilt. Therefore, correcting the tilt requires a higher accuracy of the measurements than for higher orders of the wavefront. Hence current adaptive optics devices coupled with a LGS face low sky coverage. Several methods have been proposed to get a partial sky coverage for the tilt. The only one providing us with a full sky coverage is the polychromatic LGS (hereafter referred to as PLGS). We present here a progress report of the R&D; program Etoile Laser Polychromatique et Optique Adaptative (ELP-OA) carried out in France to develop the PLGS concept. After a short recall of the principles of the PLGS, we will review the goal of ELP-OA and the steps to get over to bring it into play. We finally shortly described the effort in Europe to develop the LGS

Polychromatic guide star: feasibility study

International audienceAdaptive optics at astronomical telescopes aims at correcting in real time the phase corrugations of incoming wavefronts caused by the turbulent atmosphere, as early proposed by Babcock. Measuring the phase errors requires a bright source located within the isoplanatic patch of the program source. The probability that such a reference source exists is a function of the wavelength, of the required image quality (Strehl ratio), of the turbulence optical properties, and of the direction of the observation. It turns out that the sky coverage is disastrously low in particular in the visible wavelength range where, unfortunately, the gain in spatial resolution brought by adaptive optics is the largest. Foy and Labeyrie have proposed to overcome this difficulty by creating an artificial point source in the sky in the direction of the observation relying on the backscattered light due to a laser beam. This laser guide star (hereinafter referred to as LGS) can be bright enough to allow us to accurately measure the wavefront phase errors, except for two modes which are the piston (not relevant in this case) and the tilt. Pilkington has emphasized that the round trip time of the laser beam to the mesosphere, where the LGS is most often formed, is significantly shorter than the typical tilt coherence time; then the inverse-return-of-light principle causes deflections of the outgoing and the ingoing beams to cancel. The apparent direction of the LGS is independent of the tilt. Therefore the tilt cannot be measured only from the LGS. Until now, the way to overcome this difficulty has been to use a natural guide star to sense the tilt. Although the tilt is sensed through the entire telescope pupil, one cannot use a faint source because $APEX 90% of the variance of the phase error is in the tilt. Therefore, correcting the tilt requires a higher accuracy of the measurements than for higher orders of the wavefront. Hence current adaptive optics devices coupled with a LGS face low sky coverage. Several methods have been proposed to get a partial sky coverage for the tilt. The only one providing us with a full sky coverage is the polychromatic LGS (hereafter referred to as PLGS). We present here a progress report of the R&D; program Etoile Laser Polychromatique et Optique Adaptative (ELP-OA) carried out in France to develop the PLGS concept. After a short recall of the principles of the PLGS, we will review the goal of ELP-OA and the steps to get over to bring it into play. We finally shortly described the effort in Europe to develop the LGS

PASS-2: quantitative photometric measurements of the polychromatic laser guide star

International audienceWe present results from measurements of the return flux from a polychromatic sodium laser guide star produced in Pierrelatte, France during the PASS-2 experiment. In the experiment, photometry of light at 330, 569, 589, and 589.6 nm emitted by mesospheric sodium under two-color laser excitation (569 and 589 nm) was performed. The variation of oscillator and laser configurations as well as simultaneous measurements of the atmospheric coherence length and the mesospheric sodium density permit a comparison of the results with atomic physics models. Using the results, we can determine the setup that produces the maximum return flux from the polychromatic laser guide star. The knowledge gained will be used to aid the ELP- OA project, which has as its goal the design, testing, and implementation of an adaptive optics system that uses a polychromatic laser guide star for wave front tilt measurements

ELPOA: toward the tilt measurement from a polychromatic laser guide star

International audienceAdaptive optics at astronomical telescopes aims at correcting in real time the phase corrugations of incoming wavefronts caused by the turbulent atmosphere, as early proposed by Babcock. Measuring the phase errors requires a bright source, which is located within the isoplanatic patch of the program source. The probability that such a reference source exists is a function of the wavelength of the observation, of the required image quality (Strehl ratio), of the turbulence optical properties, and of the direction of the observation. Several papers have addressed the problem of the sky coverage as a function of these parameters (see e.g.: Le Louarn et al). It turns out that the sky coverage is disastrously low in particular in the short (visible) wavelength range where, unfortunately, the gain in spatial resolution brought by adaptive optics is the largest. Foy and Labeyrie have proposed to overcome this difficulty by creating an artificial point source in the sky in the direction of the observation relying on the backscattered light due to a laser beam. This laser guide star (hereafter referred to as LGS) can be bright enough to allow us to accurately measure the wavefront phase errors, except for two modes which are the piston (which is not relevant in this case) and the tilt. Pilkington has emphasized that the round trip time of the laser beam to the mesosphere, where the LGS is most often formed, is significantly shorter than the typical tilt coherence time; then the inverse-return- of-light principle causes deflections of the outgoing and the ingoing beams to cancel. The apparent direction of the LGS is independent of the tilt. Therefore the tilt cannot be measured only from the LGS. Until now, the way to overcome this difficulty has been to use a natural guide star to sense the tilt. Although the tilt is sensed through the entire telescope pupil, one cannot use a faint source because approximately equals 90% of the variance of the phase error is in the tilt. Therefore, correcting the tilt requires a higher accuracy of the measurements than for higher orders of the wavefront. Hence current adaptive optics devices coupled with a LGS face low sky coverage. Several methods have been proposed to get a partial or total sky coverage for the tilt, such as the dual adaptive optics concept, the elongation perspective method, or the polychromatic LGS (hereafter referred to as PLGS). We present here a progress report of the R&D; program Etoile Laser Polychromatique et Optique Adaptative (ELP-OA) carried out in France to develop the PLGS concept. After a short recall of the principles of the PLGS, we will review the goal of ELP-OA and the steps to get over to bring it into play

ELP-OA: measuring the wavefront tilt without a natural guide star

International audienceWe describe the current status of the ELP-OA project in which we try to demonstrate in practice that it is possible to measure the tilt of a wave front using only a polychromatic laser guide star and no natural guide star. The first phase of ELP-OA, consisting of feasibility experiments, has recently been completed successfully. This paper provides an overview over the results of this first phase and over the continuation of the ELP-OA project

Influence of Beam Conditions and Energy for SEE Testing

GANIL/Applications industriellesThe effects of heavy-ion test conditions and beam energy on device response are investigated. These effects are illustrated with two types of test vehicles: SRAMs and power MOSFETs. In addition, GEANT4 simulations have also been performed to better understand the results. Testing to high fluence levels is required to detect rare events. This increases the probability of nuclear interactions. This is typically the case for power MOSFETs, which are tested at high fluences for single event burnout or gate rupture detection, and for single-event-upset (SEU) measurement in SRAMs below the direct ionization threshold. Differences between various test conditions (e.g., "in air" or vacuum irradiations, with or without degraders) are also explored. Nuclear interactions with any materials in the beam's path can increase the number of high collected charge events potentially impacting the experimental results. A "species" effect has been observed in the power MOSFET devices examined in this work. When the beam energy increases, the single-event-burnout (SEB) voltage is constant, such that the SEB voltage is determined only by the species of the ion beam. The species effect is shown to be due to high collected charge events induced by nuclear interactions, which can lead to premature SEB. If a device is sensitive to the species effect, the worst-case test conditions will be for the heaviest ion species, which can produce the largest linear-energy-transfer (LET) secondaries. SRAMs can also be sensitive to the species effect below the direct ionization threshold LET. For the devices used in this work, the worst-case energy for SEU characterization is $sim 10'{rm s}~{rm MeV/u}$ where the species dominates the device response. In the 10's MeV/u range the heaviest species result in the largest cross sections. However, at very high energies (100's MeV/u), the species is not the - ominant parameter because of differences in the population of secondaries created by nuclear interactions. At very high energies the SEU cross section below the direct ionization threshold LET decreases by several orders of magnitude compared to 10's MeV/u SEU data. The results of this work emphasize that there is no such thing as an "ideal" test facility. Nevertheless, these results can be used by experimenters to optimize the integrity of their results for given test conditions

Étonnante physique

International audienceDiscipline multimillénaire, la physique explore l’espace et le temps. De l’immensité des amas de galaxies à l’infinie petitesse des particules élémentaires, des échelles humaines – du mètre au centimètre – jusqu’au nanomonde, de l’extrême brièveté du mouvement de l’électron jusqu’au fond des âges d’où nous parviennent les premières lumières de l’Univers : les domaines couverts par cette discipline n’ont pas fini de nous étonner.Cette science est celle de l’expérimentation méthodique qui met au point des instruments originaux pour observer la matière, inerte ou vivante, en laboratoire ou à distance. Celle qui pose encore de grandes questions fondamentales. Mais aussi celle qui accompagne notre vie quotidienne avec ses développements dans les domaines des matériaux, de la santé, de l’énergie, du climat…Pour montrer toute sa richesse, cet ouvrage réunit 70 contributions de physiciennes et de physiciens récemment récompensés par une médaille du CNRS pour l’originalité et l’importance de leurs travaux. Abondamment illustré, accessible à tout amateur de science, Étonnante Physique lève un voile sur les recherches les plus actuelles

Étonnante physique

International audienceDiscipline multimillénaire, la physique explore l’espace et le temps. De l’immensité des amas de galaxies à l’infinie petitesse des particules élémentaires, des échelles humaines – du mètre au centimètre – jusqu’au nanomonde, de l’extrême brièveté du mouvement de l’électron jusqu’au fond des âges d’où nous parviennent les premières lumières de l’Univers : les domaines couverts par cette discipline n’ont pas fini de nous étonner.Cette science est celle de l’expérimentation méthodique qui met au point des instruments originaux pour observer la matière, inerte ou vivante, en laboratoire ou à distance. Celle qui pose encore de grandes questions fondamentales. Mais aussi celle qui accompagne notre vie quotidienne avec ses développements dans les domaines des matériaux, de la santé, de l’énergie, du climat…Pour montrer toute sa richesse, cet ouvrage réunit 70 contributions de physiciennes et de physiciens récemment récompensés par une médaille du CNRS pour l’originalité et l’importance de leurs travaux. Abondamment illustré, accessible à tout amateur de science, Étonnante Physique lève un voile sur les recherches les plus actuelles

Étonnante physique

International audienceDiscipline multimillénaire, la physique explore l’espace et le temps. De l’immensité des amas de galaxies à l’infinie petitesse des particules élémentaires, des échelles humaines – du mètre au centimètre – jusqu’au nanomonde, de l’extrême brièveté du mouvement de l’électron jusqu’au fond des âges d’où nous parviennent les premières lumières de l’Univers : les domaines couverts par cette discipline n’ont pas fini de nous étonner.Cette science est celle de l’expérimentation méthodique qui met au point des instruments originaux pour observer la matière, inerte ou vivante, en laboratoire ou à distance. Celle qui pose encore de grandes questions fondamentales. Mais aussi celle qui accompagne notre vie quotidienne avec ses développements dans les domaines des matériaux, de la santé, de l’énergie, du climat…Pour montrer toute sa richesse, cet ouvrage réunit 70 contributions de physiciennes et de physiciens récemment récompensés par une médaille du CNRS pour l’originalité et l’importance de leurs travaux. Abondamment illustré, accessible à tout amateur de science, Étonnante Physique lève un voile sur les recherches les plus actuelles

Étonnante physique

International audienceDiscipline multimillénaire, la physique explore l’espace et le temps. De l’immensité des amas de galaxies à l’infinie petitesse des particules élémentaires, des échelles humaines – du mètre au centimètre – jusqu’au nanomonde, de l’extrême brièveté du mouvement de l’électron jusqu’au fond des âges d’où nous parviennent les premières lumières de l’Univers : les domaines couverts par cette discipline n’ont pas fini de nous étonner.Cette science est celle de l’expérimentation méthodique qui met au point des instruments originaux pour observer la matière, inerte ou vivante, en laboratoire ou à distance. Celle qui pose encore de grandes questions fondamentales. Mais aussi celle qui accompagne notre vie quotidienne avec ses développements dans les domaines des matériaux, de la santé, de l’énergie, du climat…Pour montrer toute sa richesse, cet ouvrage réunit 70 contributions de physiciennes et de physiciens récemment récompensés par une médaille du CNRS pour l’originalité et l’importance de leurs travaux. Abondamment illustré, accessible à tout amateur de science, Étonnante Physique lève un voile sur les recherches les plus actuelles