S. Dell’Agnello, A. Boni, C. Cantone, E. Ciocci, M. Martini, G. Patrizi, M. Tibuzzi, G. Delle Monache, R. Vittori, G. Bianco, D. Currie, N. Intaglietta, L. Salvatori, C. Lops, S. Contessa, L. Porcelli, C. Mondaini, P. Tuscano, M. Maiello
The SCF_Lab (Satellite/lunar/gnss laser ranging and altimetry Characterization Facility Laboratory) of INFNLNF is designed to cover virtually LRAs (Laser Retroreflector Arrays) of CCRs (Cube Corner Retroreflectors) for missions in the whole solar system, with a modular organization of its instrumentation, two redundant SCF (SCF_Lab Characterization Facilities), and an evolutionary measurement approach, including customization and potentially upgrade on-demand. See http://www.lnf.infn.it/esperimenti/etrusco/ for a general description.
The ultimate limits on high accuracy laser ranging to satellites from the ground appear to be caused by the effects of the earth’s atmosphere. Other impediments in terms of lasers, timing equipment and calibration seem to be evolving to the point of providing very high accuracy. We shall address the role of the earth’s atmosphere for lunar laser ranging. In the near future, the robotic deployment of next generation lunar laser retroreflectors is planned. With proper robotic deployment, these retroreflectors may support single photo-electron ranging accuracy at the 100 micron level or better. In particular, there are questions of the random and systematic delays and broadening of a very narrow laser pulse. Theoretical and experimental results will be discussed that address estimates of the magnitudes of these effects and the issue of precision vs. accuracy. These effects may be roughly divided into three domains: High frequency effects due to atmospheric turbulence, low frequency effects due to atmospheric “slopes” and atmospheric waves and tides and spectral dispersion of the narrow pulse. In conclusion, the route to better ranging through the earth’s atmosphere appears to be more advance modeling of local meteorological effects, in a program that can be implemented at a reasonable cost.
The deployment of next generation lunar laser retroreflectors is planned in the near future. With proper robotic deployment, these will support single shot single photo-electron ranging accuracy at the 100 micron level or better. There are available technologies for the support at this accuracy by advanced ground stations, however, the major question is the ultimate limit imposed on the ranging accuracy due to the changing timing delays due to turbulence and horizontal gradients in the earth’s atmosphere. In particular, there are questions of the delay and temporal broadening of a very narrow laser pulse. Theoretical and experimental results will be discussed that address estimates of the magnitudes of these effects and the issue of precision vs. accuracy.
Airport traffic delays continue to increase, without any relief in sight. A major contributing factor is the lack of low visibility capability for both aircraft landing and movement about an airport surface. Only 39 runways in the USA can operate under CAT III (700 ft. visibility to land) conditions, and just 19 additional runways are in the planning stage. Each will cost $DLR1 billion and take about ten years to place in operation. Ultraviolet (UV) technology may offer a solution. Runways that would normally decrease their traffic throughput, or close, as visibility degrades, can maintain their visual tempo and safety norms through the application of UV fog penetration techniques. These techniques can be applied on a selective and incremental basis such that some relief can be expected within two years and major decreases in delays can be realized a year thereafter. Three progressive steps are involved.
Eta Carinae is an extremely massive and highly evolved member of the Carinae starburst region. It has undergone numerous eruptions over the past millennium. In 1841, a Giant Eruption ejected several solar masses or more of material. Most of this material is currently in the dusty nebula denoted as the 'Homunculus.' ADONIS observations with the Fabry-Perot Interferometer at the Brackett gamma line around 2.16 microns have allowed probing the interior of the major elements of the Homunculus. These elements were not visible in our WFPC observations at the various visible wavelengths. The preliminary results of the analysis of this data have confirmed of the 'Double-Flask' model of the Homunculus; a model that we proposed based upon the Hubble data and spectroscopic data. This approach can also determine the opacity of the Homunculus walls, as well as the total mass and the grain structure of the dust. In a separate recent analysis, small clumps of material have been discovered that were ejected at velocities almost 1% of the speed of light. These 'Malin Bullets' and the material following the bullets, the 'contrails' called the 'Malin Spikes' have been measured using the STARFINDER program. This analysis has discovered about one hundred additional Malin Bullets. This data, as well as other data taken in direct support of the PAPAO program provide new information on the structure of the Homunculus. Inter-comparison of the WFPC data and the ADONIS data is an integral part of the PAPAO program for the validation diffuse astrometry and deconvolution software. Portions of this data will form the database for general community use for the calibration of different programs.
The European Southern Observatory is currently developing an array of software analysis packages to perform Photometry and Astrometry (P&A) on both stellar and diffuse objects observed with Adaptive Optics (AO) Systems. As they are complete, the component programs of ESO-PAPAO will be made available to AO observers using ADONIS on the 3.6 meter telescope at La Silla and, later, those using the various AO systems being developed for the 8.2 meter VLT telescopes at Paranal, such as NAOS- CONICA and MACAO-SINFONI. The performances of the ESO-PAPAO package are being extensively quantified; both to support their use in astrophysical analysis and as a guide for the definition of AO observing programs. The algorithms are being developed in IDL. A user interface allows immediate access to the ESO-PAPAO by observers not familiar with IDL. We will describe the objectives of the ESO-PAPAO; the calibrated ADONIS data sets that have been collected for distribution to contributors to the ESO-PAPAO program, and the methods and results of numerical tests of photometric precision in comparisons of the various different analysis packages. In particular, the STARFINDER program, developed at the University of Bologna in a collaborative effort with ESO, has been applied to data from ADONIS at La Silla, UHAO at Mauna Kea, and HST. Results from the analysis of this astronomical AO data will be presented -- photometric precision of 0.02 to 0.05 magnitudes, and astrometric precision of approximately 0.1 pixel in crowded fields with strong isoplanatic effects.
KEYWORDS: Point spread functions, Stars, Adaptive optics, Deconvolution, Statistical analysis, Photometry, Superposition, Convolution, Human-machine interfaces, Signal to noise ratio
StarFinder is a new code for the deep analysis of stellar fields, designed for well-sampled images with high and low Strehl ratio. It is organized in the form of a self-contained IDL widget-based application, with a 'user-friendly' graphic interface. We give here a general description of the code along with some applications to real data with space-invariant Point Spread Function (PSF). We present also some methods to handle anisoplanatic effects in wide-field Adaptive Optics (AO) observations.
The aviation industry has long sought a means of conducting all weather operations. Presently, airport lighting systems provide the only means for aiding the pilot's transition from instrument to visual acquisition of the runway environment prior to landing the aircraft. The ability for a pilot to see through fog (cloud ceiling and visibility) define the limitations for conducting operations in instrument meteorological conditions. CAT I approaches are authorized down to a runway visual range (RVR) of 2,400 feet, while CAT IIIa approaches are authorized to an RVR of 700 ft. Enhanced vision technologies are being investigated to improve the ability of the pilot to acquire the visual cues (predominantly airport lighting systems) to the runway environment. If enhanced vision enabled the pilot to see 3.5 times farther than the unaided eye, CAT I operations could be conducted under CAT IIIa conditions. This paper examines the relative theoretical and experimental performance of several enhanced vision technologies. This performance analysis compares the runway light detection capability of various infrared sensors with the eye during the dynamics of an aircraft approach and landing. This analysis further compares the IR performance with FogEye, a UV sensor, and a Laser Visual Approach system. The analysis indicates that although the 1.5 micron and 3 to 5 micron IR sensors are capable of improving on the unaided eye, especially in haze and low density fog conditions, only the UV sensor, coupled with relatively minor changes to airport light lenses (to not attenuate UV light), provides the potential to aid the pilot in seeing airport lighting 3.5 times farther than the unaided eye. An 8 to 11 micron IR sensor can support enhanced vision of the actual airport surface. These electro optical capabilities are further compared with the capabilities of Millimeter Wave (MMW) systems. Additional collateral features that would aid in more orderly and safer landing operations are also described.
KEYWORDS: Actuators, Point spread functions, Systems modeling, Adaptive optics, Stars, Wavefronts, Data modeling, Diffraction, Telescopes, Imaging systems
While still in their infancy, adaptive optics systems give rich promise of providing to ground-based and space-based observers the capability to obtain near-diffraction limited images through the earth's atmosphere or though new lower- cost space optical systems. Close study of the images now being obtained with AO systems on ground-based systems, aiming toward the serious photometric use of the current systems, shows that serious image artifacts exist. These affect both the study of morphology and the photometric accuracy. This paper explores the source of these artifacts by analytic modeling of the AO systems, and compares the result of the modeling with data obtained on the telescopes.
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