Probability,Random Processes,and Statistical Analysis,by H. Kobayashi,B.L. Mark and W. Turin

This article describes the scientific objectives, the scientific and operational plans and the observational programme of the international Atlantic Tropical Experiment in which some 70 countries pclrticipated during Jun-September 1974. The main aim waa to make, for the first time, an intensive study of the structure, evolution and transport properties of tropical weather systems and their role in the global circulation of the atmosphere as a whole. Some preliminary results are described but it will be two or three years before the vast mass of data is fully processed and analysed and made available in the form of validated data sets for detailed researoh studies and for input to numerical models. However, there is already good reason to believe that the major scientific objectives of the experiment will be achieved and that the knowledge gained will lead to improved weather forecasting both in the tropics, and in middle latitudes where accurate predictions for more than about three days ahead may not be possible without taking into account the import of heat and moiature from the tropical oceans through the large convective clouds of the tropical atmosphere.     

Recent developments in millimeter and submillimeter waves

Millimeter and submillimeter-wave observations provide important information for the studies of atmospheric chemistry and astrochemistry (molecular clouds, stars formation, galactic study, comets and cosmology). But, these observations depend strongly on instrumentation techniques and on the site quality. New techniques or higher detector performances result in unprecedented observations and, sometimes, the observational needs drive developments of new detector technologies, for example, superconducting junctions (SIS mixers) because of their high sensitivity in heterodyne detection in the millimeter and submillimeter wave range (100–700 GHz), HEB (Hot Electron Bolometer) mixers which are being developed by several groups for application in THz observations. For the sub-millimetre wavelengths heterodyne receivers, the local oscillator (LO) is still a critical element. So far, solid state fundamental sources are often not powerful enough for most of the applications at millimetre or submillimetre wavelengths: large efforts using new planar components (HBV) and integrated circuits, or new technics (laser mixing) are now in progress, in a few groups.The new large projects as SOFIA, FIRST, ALMA, … for astronomy; SMILES, EOS-MLS, … for aeronomy and other projects for the planetary science (ROSETTA, Mars Explorer, …), will benefit of the new developments.     

Cross sections of excited-state absorption at 800 nm in erbium-doped ZBLAN fiber

4 I_13/2 and ⁴I_11/2 of erbium is measured in a fluorozirconate fiber in the wavelength range 780–840 nm. Using a pump- and probe-beam technique and choosing the pump wavelength such that the perturbation by pump ESA is minimized in the measurement, it is possible to determine the effective ESA cross sections, despite the fact that the excitation is distributed among two metastable levels. The derived ESA cross sections at 793 nm of 1.4×10^-21 cm² from the ⁴I_13/2 level and less than 0.1×10^-21 cm² from the ⁴I_11/2 level are in reasonable agreement with former results obtained from a rate-equation simulation of the erbium 3-μm laser. The corresponding ESA spectrum under 3-μm lasing conditions is derived. At the strongest ground-state absorption around 799 nm, decreasing ESA from the ⁴I_13/2 level is compensated by increasing ESA from the ⁴I_11/2 level, i.e., ESA losses cannot be avoided when pumping around 800 nm. This result is of relevance for possible high-power diode pumping of an erbium 3-μm double-clad fiber laser. Received: 20 January 1998     

First Spectra from a New, Wide Band, Hybrid Digital Correlator Spectrometer for the First-HIFI Instrument

We have designed and built a new, wide band, modulable resolution spectrometer, in view of full astronomical qualifying tests, and to prepare future models for the FIRST satellite's heterodyne instrument. Our spectrometer, a hybrid digital Autocorrelator, offers flexibility in terms of bandwidth (from 170MHz to 680MHz) and resolution (from 700kHz to 3MHz). This spectrometer required the development of a dedicated analog filter bank, homemade samplers, and the design of full custom GaAs integrated circuits.Laboratory tests have shown excellent agreement with expected performances and observations performed with the IRAM 30-m radiotelescope have qualified its capabilities. Despite the relatively limited number of channels of our current prototype compared to others spectrometers, the main advantages are its stability (inherent to digital technique), and its spectral versatility.Recent microelectronics advances and rad-tolerance of our spectrometer components are used to prepare a new, compact, and low power consumption autocorrelator in view of a flight model for HIFI, the heterodyne instrument on the ESA cornerstone mission FIRST.     

Extended wavelength InGaAs infrared (1.0–2.4 μm) detector arrays on SCIAMACHY for space-based spectrometry of the Earth atmosphere

Space qualified InGaAs solid-state array detectors, covering the near-infrared 1–2.4 μm wavelength range, have been developed for application in space-based spectroscopy of the Earth atmosphere. The SCIAMACHY atmospheric chemistry instrument on the ESA ENVISAT satellite (2002–2005) will be equipped with a series of these novel detectors. Detectors are arranged in linear arrays of 1024 pixels of 25×500 μm² dimension and meet requirements on modestly low operating temperature (150 K) and low levels of dark current and noise. In this paper the underlying physics of dark current and noise of the detector system is studied on the basis of a theoretical model in combination with measurements. At 2.4 μm wavelength the dark-current performance achieved is 20–100 fA at an operating temperature of 150 K and a bias voltage of −2 mV. This corresponds to a figure of merit for detector resistance R₀ times detector pixel area A of R₀A=2.5–12.5 MΩ cm². This result has required the development of a customised multiplexer for parallel detector read-out at near-zero bias voltage. Further reduction of the operating temperature will not result in lowering the dark current and noise of the InGaAs detectors which are shown to be limited by tunnelling current. A route to future improvement is discussed.     

Laser mode behavior of the Cassini CIRS Fourier transform spectrometer at Saturn

The CIRS Fourier transform spectrometer aboard the NASA/ESA/ASI Cassini orbiter has been acquiring spectra of the Saturnian system since 2004. The CIRS reference interferometer employs a laser diode to trigger the interferogram sampling. Although the control of laser diode drive current and operating temperature are stringent enough to restrict laser wavelength variation to a small fraction of CIRS finest resolution element, the CIRS instrument does need to be restarted every year or two, at which time it may start in a new laser mode. By monitoring the Mylar absorption features in un-calibrated spectra due to the beam splitter Mylar substrate, it can be shown that these jumps are to adjacent modes and that most of the 8-year operation so far is restricted to three adjacent modes. For a given mode, the wavelength stability appears consistent with the stability of the laser diode drive current and operating temperature.     

Short-pulse, high-peak-power Q-switched Tm–silica fibre laser at 1.9 m

High-performance Tm–silica fibre lasers operating at 1.9 μm when pumped at 1319 or 1064 nm have been Q-switched using a rotating mirror mounted at an asymmetric angle. Pumping by 1319 nm gives better performance compared with 1064 nm pumping due to greater excited state absorption (ESA) at 1064 nm. A short Q-switched pulse duration of 25 ns and a peak pulse power of about 2.7 kW has been obtained from a 1.8 m fibre for 3.5 W launched pump power at 1.3 μm. The Q-switch performance has been studied for variation of fibre length and shown that the optimum length under these pumping conditions is around 2 m.     

MITO: a procedure for CBA measurements and a search for cosmic strings

Summary MITO (Millimetric and Infrared Testa Grigia Observatory) is a 3 m telescope dedicated to the study of Cosmic Background Anisotropies. It is located at 3500 m above sea-level at Plateau Rosa, Cervinia. We describe the Observatory and discuss two on-going research programs: a clearning procedure in order to remove galactic dust signals from cosmological data and a search for cosmic strings toward double-lensed quasars. Both the programs will be carried out by means of a He-3 photometer operating at the frequencies of 5, 10, 12, 30 cm⁻¹.     

A forward scatter CW meteor radar experiment between Bologna and Sheffield

Summary A research programme describing the feasibility of a forward scatter CW meteor radar link over a long baseline has been recently developed. The main scientific objectives with a hint to the proposed system are here summarized.     

Initial state-resolved excited state absorption spectroscopy of ZBLAN:Ho<Superscript>3+</Superscript> glass

Phase-sensitive and frequency-resolved detection techniques are used for the initial state-resolved excited state absorption (ESA) measurements in ZBLAN:Ho³⁺ glass. Both experimental techniques were applied simultaneously in a broad spectral range (550–1750 nm) for the first time. Estimated results are compared and discussed in detail. A simple kinetic model, used for qualitative considerations, is presented and successfully compared with the experimental data. The measured spectra will be useful for identifying new up-conversion excitation channels in the considered system, where ESA transitions originating from several excited levels are observed.     

用于1.5μm光波导放大器的高浓度Er3+掺杂玻璃

制备了用于 1.5μm光波导放大器高浓度掺杂 Er3 的氟铝酸盐、氟锆酸盐及磷酸盐玻璃。在 0 .80μm和 0 .98μm连续激光二极管激发下分析比较了这三种玻璃 1.5μm发射的光谱特性、浓度猝灭及其机制。研究表明 :由于在 0 .98μm激发下 ,激发态吸收较 0 .80μm激发下小得多 ,因而其 1.5μm荧光发射量子效率也比 0 .80μm激发下高得多 ;氟铝酸盐玻璃具有最大的荧光强度和最小的浓度猝灭效应 ,是理想的 1.5μm光波导放大器基质玻璃材料     

An inter-comparison of far-infrared line-by-line radiative transfer models

A considerable fraction (>40%) of the outgoing longwave radiation escapes from the Earth's atmosphere-surface system within a region of the spectrum known as the far-infrared (wave-numbers less than 650 cm⁻¹). Dominated by the line and continuum spectral features of the pure rotation band of water vapor, the far-infrared has a strong influence upon the radiative balance of the troposphere, and hence upon the climate of the Earth. Despite the importance of the far-infrared contribution, however, very few spectrally resolved observations have been made of the atmosphere for wave-numbers less than 650 cm⁻¹. The National Aeronautics and Space Administration (NASA), under its Instrument Incubator Program (IIP), is currently developing technology that will enable routine, space-based spectral measurements of the far-infrared. As part of NASA's IIP, the Far-Infrared Spectroscopy of the Troposphere (FIRST) project is developing an instrument that will have the capability of measuring the spectrum over the range from 100 to 1000 cm⁻¹ at a resolution of 0.6 cm⁻¹. To properly analyze the data from the FIRST instrument, accurate radiative transfer models will be required. Unlike the mid-infrared, however, no inter-comparison of codes has been performed for the far-infrared. Thus, in parallel with the development of the FIRST instrument, an investigation has been undertaken to inter-compare radiative transfer models for potential use in the analysis of far-infrared measurements. The initial phase of this investigation has focused upon the inter-comparison of six distinct line-by-line models. The results from this study have demonstrated remarkably good agreement among the models, with differences being of order 0.5%, thereby providing a high measure of confidence in our ability to accurately compute spectral radiances in the far-infrared.     

New short-wavelength laser emissions from partially deuterated methanol isotopes

The partially deuterated isotopes of methanol, CH₂DOH and CHD₂OH, have been reinvestigated as sources of far-infrared (FIR) laser emissions using an optically pumped molecular laser (OPML) system recently designed for wavelengths below 150 μm. With this system, 10 new FIR laser emissions from these isotopes ranging from 32.8 to 174.6 μm have been discovered. This includes the shortest known OPML emission from CHD₂OH, at 32.8 μm. These lines are reported with their operating pressure, polarizations relative to the CO₂ pump laser and wavelengths, measured to ±0.5 μm. In addition, polarizations for three previously observed FIR laser lines from CHD₂OH were measured for the first time. This paper is dedicated to the memory of Dr. K.M. Evenson, a pioneer in the field for his role in the development of optically pumped molecular lasers and their use in laser frequency measurements and the laser magnetic resonance technique. His scientific expertise, guidance, mentoring and friendship will be greatly missed. Received: 27 March 2002 / Published online: 8 May 2002     

Feasibility study for the use of PADC as a radiation detector for living cell cultures

In the framework of an ESA project, a microbiological experiment in space is planned. In this experiment a cell culture will be exposed to cosmic radiation onboard a spacecraft. Because the living cell culture will be directly on a nuclear track detector stack, this detector will be submitted to a different environment than normally used. The temperature will be 37°C and the culture will be in a biological growth medium. Tests have been conducted to assess the possible use of PADC in these conditions. For this, a series of alpha irradiated detectors have been exposed for different periods of time (up to 1 month) to these ‘biological’ conditions. The radiological properties as well as the mechanical properties (swelling…) have been investigated. Results show no influence of the biological environment on the PADC, which makes it useable under these circumstances.     

Effects of energy-transfer up-conversion and excited-state absorption in quasi-three-level Nd:GdVO4 lasers

We investigate in detail the effect of energy-transfer up-conversion (ETU) and excited-state absorption (ESA) in diode-end-pumping quasi-three-level Nd:GdVO₄ lasers. The energy levels of Nd:GdVO₄ crystals and the rate equation involving ETU and ESA effects are presented. The results of simulation show that the ETU effect is important in quasi-three-level lasers and can provide heating approximately two times higher than that induced by the ESA. Moreover, the relationship between the incident pump power and the 912 nm output power was simulated taking into account the ESA; a comparison with experimental data is also presented. As a result, we conclude that the ESA plays an important role in the high-power pumping field; the estimated equivalent cross-section σ_ESA = (1.0 ± 0.5) ? 10^?20 cm².     

Excited state absorption measurements and laser potential of Cr4+ doped Ca2GeO4

4+ doped Ca₂GeO₄ in the 450–2000 nm spectral region at room temperature are presented. Weak ESA bands due to the transition are observed between 1200 and 2000 nm and stronger ESA bands due to peak below 1200 nm. The overlap of the ESA band with the emission which extends from 1100 to about 1600 nm will significantly affect the laser performance of Cr⁴⁺ doped Ca₂GeO₄. The effective peak stimulated emission cross section at 1350 nm in E∥b polarization is only about 3×10^-20 cm². However, our results indicate that tunable laser action between 1300 and 1500 nm should, in principle, be possible. Received: 28 October 1996     

Gamma ray astronomy and search for antimatter in the universe

Gamma ray astronomy provides a powerful tool for searching antimatter in the universe; it probably provides the only means to determine, if the universe has baryon symmetry. Presently existing gamma-ray observations can be interpreted without postulating the existence of antimatter. However, the measurements are not precise enough to definitely exclude the possibility of its existence. The search for antimatter belongs to one of the main scientific objectives of the Gamma Ray Observatory GRO of NASA, which will be launched in 1990 by the Space Shuttle.     

Long wavelength strain-engineered InAs multi-layer stacks quantum dots laser diode on GaAs substrate

The growth of GaAs based 1.5 ??m multi-layer stacked InAs quantum dots (QDs) has been investigated by solid-source molecular beam epitaxy (SSMBE), which was very important devices for transmission window. Owing to a strong electronic coupling between the QDs layers and the quantum wells (QWs), and antimony (Sb) introduced by for long-wavelength semiconductor lasers were obtained. The device structure for QDs laser diodes (LDs) with a cavity length of 1000 ??m and stripe width of 100 ??m as well as the device fabrication results will also be presented. The output performance was achieved with continuous wave (CW) operation, the measurement were from 20 to 60°C with a temperature step of 10°C. The threshold current density was 168 A/cm², and the CW operating up to 20 mW at room temperature (RT) was achieved.     

Science with GRASP

Summary The GRASP mission has been studied by ESA as a candidate mission in Gamma-Ray Astronomy with Spectroscopy and Positioning. The key feature of the mission will be a high-resolution, Ge-based spectrometer, allowing for a resolution of the keV order ∼1 MeV, and a CsI imager, permitting source location accuracies approaching the arcminute over a wide field of view. GRASP, although not yet finally selected, has been placed as the first priority in the ESA astronomy ?medium? class missions, and is currently further studied as a candidate for use on a common bus with the ESA cornerstone XMM. To speed up publication, the proofs were not sent to the authors and were supervised by the Scientific Committee.