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International audience; SPIRE, the Spectral and Photometric Imaging Receiver, is one of three instruments to fly on the European Space Agency's Herschel Space Observatory. It contains a three-band imaging photometer operating at 250, 350 and 500 μm, and an imaging Fourier transform spectrometer covering 194-672 μm. The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4 × 8', observed simultaneously in the three spectral bands. The spectrometer has an approximately circular field of view with a diameter of 2.6' The spectral resolution can be adjusted between 0.04 and 2 cm -1 (resolving power of 20-1000 at 250 μm). SPIRE will be used for many galactic and extragalactic science programmes, a number of which will be implemented as Herschel Key Projects. The SPIRE consortium's Guaranteed Time (GT) programme will devote more than 1000 h to Key Projects covering the high-redshift universe and local galaxies, which will be carried out in coordination with other GT programmes, especially that of the PACS consortium. It is also expected that substantial amounts of Herschel Open Time will be used for further extragalactic investigations. The high-redshift part of the SPIRE GT programme will focus on blank-field surveys with a range of depths and areas optimised to sample the luminosity-redshift plane and characterize the bolometric luminosity density of the universe at high-redshift. Fields will be selected that are well covered by Spitzer, SCUBA-2, PACS-GT and near-IR surveys, to facilitate source identifications and enable detailed studies of the redshifts, spectral energy distributions, and other properties of detected galaxies. The local galaxies programme will include a detailed spectral and photometric study of a sample of well resolved nearby galaxies, a survey of more than 300 local galaxies designed to provide a statistical survey of dust in the nearby universe, and a study of the ISM in low-metallicity environments, bridging the gap between the local universe and primordial galaxies.

Canadian deuterium uranium (CANDU) pressurized heavy-water reactors produce 14C by neutron activation of trace quantities of nitrogen in annular gas and reactor components (14N(n,p)14C), and from 17O in the heavy water moderator by (17O(n,α)14C). The radiocarbon produced in the moderator is removed on ion exchange resins incorporated in the water purification systems; however, a much smaller gaseous portion is vented from reactor stacks at activity levels considerably below 1% of permissible derived emission limits. Early measurements of the carbon speciation indicated that >90% of the 14C emitted was in the form of CO2. We conducted surveys of the atmospheric dispersion of 14CO2 at the Chalk River Laboratories and at the Pickering Nuclear Generating Station. We analyzed air, vegetation, soils and tree rings to add to the historical record of 14C emissions at these sites, and to gain an understanding of the relative importance of the various carbon pools that act as sources/sinks within the total 14C budget. Better model parameters than those currently available for calculating the dose to the critical group can be obtained in this manner. Global dose estimates may require the development of techniques for estimating emissions occurring outside the growing season.

The Herschel SPIRE On-Board Software (OBS) is presented. This real time operational software controls the scientific data transmission and keeps a control layer between the SPIRE Mission Timeline (MTL) and the real instruments status. It embeds a multithreaded engine that interprets control procedures for the detector and mechanism subsystems. An autonomous monitoring agent keeps control of subsystems status, and takes local decisions based on pre-loaded reaction maps. The behaviour of low level system functions is configurable remotely via the reactions maps and control procedures.

SPIRE, the Spectral and Photometric Imaging Receiver, is the Herschel Space Observatory's submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 {\mu}m, and an imaging Fourier transform spectrometer (FTS) covering 194-671 {\mu}m (447-1550 GHz). In this paper we describe the initial approach taken to the absolute calibration of the SPIRE instrument using a combination of the emission from the Herschel telescope itself and the modelled continuum emission from solar system objects and other astronomical targets. We present the photometric, spectroscopic and spatial accuracy that is obtainable in data processed through the "standard" pipelines. The overall photometric accuracy at this stage of the mission is estimated as 15% for the photometer and between 15 and 50% for the spectrometer. However, there remain issues with the photometric accuracy of the spectra of low flux sources in the longest wavelength part of the SPIRE spectrometer band. The spectrometer wavelength accuracy is determined to be better than 1/10th of the line FWHM. The astrometric accuracy in SPIRE maps is found to be 2 arcsec when the latest calibration data are used. The photometric calibration of the SPIRE instrument is currently determined by a combination of uncertainties in the model spectra of the astronomical standards and the data processing methods employed for map and spectrum calibration. Improvements in processing techniques and a better understanding of the instrument performance will lead to the final calibration accuracy of SPIRE being determined only by uncertainties in the models of astronomical standards., Comment: Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue

The Spectral and Photometric Imaging Receiver (SPIRE), is the Herschel Space Observatory`s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 microns, and an imaging Fourier Transform Spectrometer (FTS) which covers simultaneously its whole operating range of 194-671 microns (447-1550 GHz). The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4' x 8', observed simultaneously in the three spectral bands. Its main operating mode is scan-mapping, whereby the field of view is scanned across the sky to achieve full spatial sampling and to cover large areas if desired. The spectrometer has an approximately circular field of view with a diameter of 2.6'. The spectral resolution can be adjusted between 1.2 and 25 GHz by changing the stroke length of the FTS scan mirror. Its main operating mode involves a fixed telescope pointing with multiple scans of the FTS mirror to acquire spectral data. For extended source measurements, multiple position offsets are implemented by means of an internal beam steering mirror to achieve the desired spatial sampling and by rastering of the telescope pointing to map areas larger than the field of view. The SPIRE instrument consists of a cold focal plane unit located inside the Herschel cryostat and warm electronics units, located on the spacecraft Service Module, for instrument control and data handling. Science data are transmitted to Earth with no on-board data compression, and processed by automatic pipelines to produce calibrated science products. The in-flight performance of the instrument matches or exceeds predictions based on pre-launch testing and modelling: the photometer sensitivity is comparable to or slightly better than estimated pre-launch, and the spectrometer sensitivity is also better by a factor of 1.5-2., Comment: Accepted for publication in Astronomy & Astrophyics (Herschel first results special issue)

The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments onboard the European Space Agency's Herschel Space Observatory launched on 14 May 2009. The low to medium resolution spectroscopic capability of SPIRE is provided by an imaging Fourier transform spectrometer of the Mach-Zehnder configuration. Results from the in flight performance verification phase of the SPIRE spectrometer are presented and conformance with the instrument design specifications is reviewed.

We describe the on-board electronics chain and the on-ground data processing pipeline that will operate on data from the Herschel-SPIRE photometer to produce calibrated astronomical products. Data from the three photometer arrays will be conditioned and digitised by on-board electronics and sent to the ground with no further on-board data processing. On the ground, the data pipeline will process the data from point source, jiggle-map, and scan-map observations in a fully automatic manner, producing measured flux densities (for point source observations) or maps. It includes calculation of the bolometer voltages from the raw telemetry, glitch removal, and corrections for various effects including time constants associated with the detectors and electronics, electrical and optical crosstalk, detector temperature drifts, flatfielding, and non-linear response of the bolometers to strong sources. Flux density calibration will be with respect to standard astronomical sources with the planets Uranus and Neptune being adopted as the baseline primary standards. The pipeline will compute estimated values of in-beam flux density for a standard flat νS(ν) source spectrum.

International audience; SPIRE, the Spectral and Photometric Imaging Receiver, is a submillimetre camera and spectrometer for Herschel. It comprises a three-band camera operating at 250, 350 and 500 Â\textmum, and an imaging Fourier Transform Spectrometer covering 194-672 \ensuremathμm. The photometer field of view is 4x8 arcmin., viewed simultaneously in the three bands. The FTS has an approximately circular field of view of 2.6 arcmin. diameter and spectral resolution adjustable between 0.04 and 2 cm^-1 ( \ensuremathλ/▵\ensuremathλ=20-1000 at 250 \ensuremathμm). Following successful testing in a dedicated facility designed to simulate the in-flight operational conditions, SPIRE has been integrated in the Herschel spacecraft and is now undergoing system-level testing prior to launch. The main design features of SPIRE are reviewed, the key results of instrument testing are outlined, and a summary of the predicted in-flight performance is given.

International audience; SPIRE, the Spectral and Photometric Imaging Receiver, is Herschel's submillimetre camera and spectrometer. It comprises a three-band imaging photometer operating at 250, 350 and 500 \ensuremathμm, and an imaging Fourier Transform Spectrometer (FTS) covering 194 672 \ensuremathμm. The design of SPIRE is described, and the expected scientific performance is summarised, based on modelling and flight instrument test results.

The Spectral and Photometric Imaging REceiver (SPIRE) is one of the three scientific instruments to fly on the European Space Agency's Herschel Space Observatory, and contains a three-band imaging submillimetre photometer and an imaging Fourier transform spectrometer. The flight model of the SPIRE cold focal plane unit has been built up in stages with a cold test campaign associated with each stage. The first campaign focusing on the spectrometer took place in early 2005 and the second campaign focusing on the photometer was in Autumn 2005. SPIRE is currently undergoing its third cold test campaign following cryogenic vibration testing. Test results to date show that the instrument is performing very well and in general meets not only its requirements but also most of its performance goals. We present an overview of the instrument tests performed to date, and the preliminary results.

SPIRE, the Spectral and Photometric Imaging Receiver, is a submillimetre camera and spectrometer for the European Space Agency's Herschel Space Observatory. It comprises a three-band imaging photometer operating at 250, 360 and 520

The corrosion rate of a metal (alloy) can be measured using: (1) Immersion tests or weight loss such as in ASTM G 1 and G 31 or (2) Electrochemical techniques such as in ASTM G 59. In the polarization resistance (PR) or linear polarization method (G 59), the resistance to polarization (Rp) of a metal is measured in the electrolyte of interest in the vicinity of the corrosion potential (E{sub corr}). This polarization resistance can be mathematically converted into corrosion rates (CR). A plot of E vs. I in the vicinity of E{sub corr} is generated by increasing the potential at a fixed rate of 0.1667 mV/s and measuring the output current. The polarization resistance (Rp) is defined as the slope of a potential (E) (Y axis) vs. Current (I) (X axis) plot in the vicinity of the corrosion potential (E{sub corr}). When the potential is ramped and the current is measured, E is the independent variable and I is the dependent variable. In a proper mathematical plot, E should be represented in the X axis and I in the Y axis. However, in the conventions of the corrosion community, E is always plotted in the Y axis and Imore » in the X axis. Therefore, how this plot of Delta E/Delta I is analyzed is a matter of current debate.« less

The Spectral and Photometric Imaging REceiver (SPIRE) is one of the three scientific instruments on the European Space Agency's Herschel mission. At the start of 2004 the Cryogenic Qualification Model (CQM) of SPIRE was tested with the aim of verifying the instrument system design and evaluating key performance parameters. We present a description of the test facility, an overview of the instrument tests carried out on the CQM, and the first results from the analysis of the test data. Instrument optical efficiency and detector noise levels are close to the values expected from unit-level tests, and the SPIRE instrument system works well, with no degradation in performance from stray light, electromagnetic interference or microphonically induced noise. Some anomalies and imperfections in the instrument performance, test set-up, and test procedures have been identified and will be addressed in the next test campaign.

The US Department of Energy is characterizing a potential repository site for nuclear waste in Yucca Mountain (NV). In its current design, the nuclear waste containers consist of a double metallic layer. The external layer would be made of NO6022 or Alloy 22 (Ni-22Cr-13Mo-3W-3Fe). Since over their lifetime, the containers may be exposed to multi-ionic aqueous environments, a potential degradation mode of the outer layer could be environmentally assisted cracking (EAC) or stress corrosion cracking (SCC). In general, Alloy 22 is extremely resistant to SCC, especially in concentrated chloride solutions. Current results obtained through slow strain rate testing (SSRT) shows that Alloy 22 may suffer SCC in simulated concentrated water (SCW) at applied potentials approximately 400 mV more anodic than the corrosion potential (E{sub rr}).

The liability to overwhelming infection of children lacking a spleen either as a result of its congenital absence or because of splenectomy, has been frequently documented. Although there have been numerous studies of the consequences of experimental splenectomy in postnatal animals, this is the first study of the effects of this operation in early fetal life.A technique is described for microsurgical removal of the spleen from fetal lambs approximately one-third of the way through gestation, when the fetus is approximately the size of a mouse. Lambs that had been splenectomized in utero were submitted to haematological examination in postnatal life and were challenged with pneumococcal polysaccharide to test their immunological competence.Lambs in which splenectomy had been performed close to the gestational age of initiation of the splenic contribution to differentiation of immune and haemopoietic systems, exhibited insignificant deviations from normality in postnatal life.Provided the spleen is removed from the fetal lamb sufficiently early in gestation, it is possible for other lymphoid tissues to compensate for most of the deficiencies that would be anticipated in animals lacking a spleen. In this experiment, splenectomy was performed at approximately the developmental stage equivalent to that at which the spontaneous interruption of development that leads to human congenital asplenia occurs. The absence of major postnatal abnormalities observed in these lambs reinforces the significance of the associated abnormalities in the development of the clinical deficits observed in children with spontaneous asplenia.

The Long-Wavelength Spectrometer (LWS) is one of two complementary spectrometers aboard the European Space Agency's Infrared Space Observatory (ISO) (Kessler et al., 1996AA a companion paper (Swinyard et al, 1996) describes its performance and calibration.

The Infrared Space Observatory (ISO) has a complement of four focal plane instruments for making a range of astronomical observations at infrared wavelengths. The telescope and instruments are operated at cryogenic temperature. Spectroscopy is shared between two of these instruments, with the Long Wavelength Spectrometer (LWS) providing for spectroscopic observation over the wavelength range 43 micrometers to 198 micrometers at two resolving powers. The flight model of the LWS has been completed, following an extensive program of performance testing and calibration at the Rutherford Appleton Laboratory. For this, a test facility has been developed to provide the necessary operating and environmental conditions, including a very low thermal background. The design and operational details of the test facility are given, followed by examples of the LWS performance values obtained. The data from these measurements will provide the initial calibration of the LWS in-orbit.

La region de formation stellaire dans le nuage sombre ρ Oph a ete cartographiee par un photometre a 3 bandes, IR lointain, embarque par un ballon. Les cartes fournissent de nouveaux details relatifs a la structure spatiale et a la temperature des sources connues et permettent la detection de plusieurs autres sources qui n'avaient pas encore ete observees dans l'IR lointain

The food and feeding habits of black oreo and smooth oreo sampled at depths of 600–1200 m from the south-west Chatham Rise in 1983 are described, with notes on prey of eight other fish species. All these fish species fed benthopelagically. Black oreo preyed on hyperiid amphipods, salps and natant decapod crustaceans; smooth oreo on salps and amphipods. Dietary composition of both species changed with size of fish. Aspects of feeding relationships between the fish species were examined including dietary similarity and prey-size selection. Findings are compared with results of research on other New Zealand deepwater fish species.

On presente des cartes de W51 dans des bandes passantes centrees sur 32 et 76 μm, et de resolution superieure a 2 min. d'arc. On observe des regions HII discretes a des stades d'evolution differents. En particulier, on note une tendance qui relie la dimension croissante des sources et la luminosite totale decroissante a la distance a l'est des sources IR jeunes dans IRS2. Cela suggere qu'un processus sequentiel de formation stellaire a eu lieu dans W 51A et tend a soutenir les idees courantes regardant l'evolution des regions H II

Medium resolution (2 cm−1) spectra of Jupiter at far infrared wavelengths have been taken using a balloon-borne Michelson interferometer. The spectra show rotational bands from the ammonia in the Jovian atmosphere. There is no evidence for “emission” features at the centers of the bands as predicted from some atmospheric profiles inferred from previous observations.

The dentist's role primarily involves awareness of the problem of maltreatment, a method of approach to identify and report suspected cases, the documentation of the injuries or neglect which have been observed, and follow-up of any orofacial injuries. Orofacial trauma is present in up to one half of the reported cases of child abuse and consists of bruises, burns, lacerations, and fractures of teeth and jaws. Further studies in the dental field are needed to delineate the types and incidences of orofacial injuries and their relationship to child abuse. Dentists and all professionals must work together, if adequate services are to be provided to protect children and rehabilitate families.

This paper presents observations of far infrared fine structure emission lines of OIII at 52 and 88 μm, 0I at 63 μm and NIII at 57 μm, obtained using a balloon borne telescope with a Michelson interferometer system. The sources M42 and M17 have been mapped with a beam of 1.6’ FWHM. Physical quantities derived from these measurements are presented and some of the results are discussed.

A protein is a simple, nonbranching chain, where any link in the chain is one of approximately twenty different amino acids. The chemical tools available for the determination of the primary structure of a protein (that is, the types of amino acids that are in the protein and the sequence in which they are linked) are relatively few in number and vary greatly in sophistication.

The status of calibration and performance of the ISO Long-Wavelength Spectrometer eleven months after launch is described. The strategy followed for the calibration observations and first results are summarized. The overall performance of the instrument essentially fulfills the expectations; certain changes in sensitivity of the detectors are reported. Some improvements in the way observations are executed, which resulted from the in-flight experience, are explained.

There are several operations in non-numeric processing which can be classified as file operations. These operations include such things as sorting, searching, and table lookup. They are characterized by their repetitious, homogeneous treatment of fields within records within files. Present computer organizations generally require several instructions imbedded in a loop to process each source-operand pair. This paper outlines a computer organization (called a streaming processor) which operates on long data streams with considerably less instruction processing overhead: fetching and decoding. Thus a greater percentage of the storage bandwidth is used for data and consequently the streaming processor is more efficient for such file operations.