Since its launch in 1999, the Far Ultraviolet Spectroscopic Explorer (FUSE) has made over 4900 observations of some 2500 individual targets. The data are reduced by the principal investigator team at the Johns Hopkins University and archived at the Multimission Archive at STScI (MAST). The data reduction software package, called CalFUSE, has evolved considerably over the lifetime of the mission. The entire FUSE data set has recently been reprocessed with CalFUSE version 3.2, the latest version of this software. This paper describes CalFUSE version 3.2, the instrument calibrations on which it is based, and the format of the resulting calibrated data files.

The latest version (3.0) of the calibration pipeline for the Far Ultraviolet Spectroscopic Explorer (FUSE) is considerably faster, easier to maintain and more flexible for the end users than the older versions. It represents a major design change. Data are stored as a photon events (time of arrival, location, pulse height...) list throughout the pipeline. This allows time dependent corrections for such effects as spacecraft jitter and mirror or grating motions. Moreover users can now select and extract subsets of the data without rerunning the pipeline.

A method for determining the geometric distortion of the FUSE detectors using data from the in-orbit stimulation lamp exposures is presented. We use a wavelet approach to smooth the images, while enhancing the shape of the shadows cast by the plasma and QE grids. By tracing the horizontal and vertical shadows, a two dimensional map of the geometric distortion can be created by assuming the wires are straight and evenly spaced.

Long neglected by educators, aged readers now have gained recognition. Most of what is known about the reading performance of elderly readers emanates from library surveys which describe the interests and habits of adults. Unfortunately, these studies provide conflicting data and interpretation. Other library studies are confined to institutionalized elderly, which preclude generalization to other aged populations. Recent studies performed by psychologists and educators provide insight into the learning performance of the elderly. This paper discusses the latest research findings and includes some teaching strategies that are successful with aged readers.

We have obtained a Hubble Space Telescope STIS ultraviolet high-dispersion echelle-mode spectrum of the binary companion of the double-mode classical Cepheid Y Car. The velocity measured for the hot companion from this spectrum is very different from reasonable predictions for binary motion, implying that the companion is itself a short-period binary. The measured velocity changed by 7 km s-1 during the 4 days between two segments of the observation, confirming this interpretation. We summarize "binary" Cepheids that are in fact members of a triple system and find that at least 44% are triples. The summary of information on Cepheids with orbits makes it likely that the fraction is underestimated.

We have obtained FUSE observations of the zeta Aur systems HR 6902 and 22 Vul near and at primary eclipse. These systems axe comprised of a G-type luminous primary star and a late B-type main sequence companion, which can be used as a probe of the outer atmosphere of the G star during partial eclipse phases. They axe objects of interest since the G stars are on different sides of the dividing line in the HR diagram between coronal and non-coronal stars. The spectra of these stars are quite different in the FUSE wavelength region. Outside of eclipse, with the secondary at a height of 2.5 R-G*, 22 Vul already shows numerous absorption features from the G star wind superimposed on the B star spectrum. Surprisingly, O VI emission is seen above the local photospheric level with a pronounced self-reversal, which does not change between the pre-eclipse and totality spectra. During primary eclipse, the spectrum of 22 Vul is dominated by emission lines such as Fe II and Fe III arising from the ground state, caused by resonance scattering of the B star photons in the cool star wind. In contrast, HR 6902 shows very little O VI emission and the wind-scattered lines at totality axe weak. However, interstellar reddening and strong H-2 absorption mask some of the diagnostic lines.

592 Background: The objective of this study is to evaluate the effectiveness of combined modality treatment of lymphedema using the Reid Sleeve and the BioCompression/Optiflow System. Methods: 35 patients (16 upper extremity/19 lower extremity) with refractory lymphedema were enrolled on a study using the Reid Sleeve in combination with the BioCompression/Optiflow system. The patients wore the Reid Sleeve at night. During the daytime, the patients used the BioCompression pump with the Reid Sleeve Optiflow insert for 2 sessions of 60 minutes. Results: Among patients with upper extremity edema, the reduction in lymphedema increased steadily during treatment and was 24.7, 53.8 and 80.2% at 4, 12 and 28 weeks. The volume reduction at these times was 2310, 2753 and 4047 cubic centimeters. Linear regression analysis demonstrates a highly significant (p<0.001) reduction in arm edema during the course of treatment. A plateau phase occurred between weeks 4 and 8. For the patients with leg edema, the average reduction at 4 weeks was 9143 cubic centimeters followed by a period of relatively stable lymphedema until week 12 with an average decrease in lymphedema of 1486 cubic centimeters between weeks 12 and 16. Linear regression analysis demonstrates a significant (p<0.02) decrease in leg edema. The plateau phase may represent a tissue repair phase that occurs with effective resolution of residual lymphedema. Subsequent reductions in lymphedema can occur following tissue healing. The plateau phase appears to be more protracted among patients with more serious lymphedema such as patients with leg edema. Conclusions: The Reid Sleeve used in combination with the BioCopression/Optiflow system provides effective management for lymphedema Author Disclosure Employment or Leadership Consultant or Advisory Role Stock Ownership Honoraria Research Funding Expert Testimony Other Remuneration Peninsula Medical Peninsula Medical

A traffic-related exposure study was conducted among 58 workers (drivers, vendors, traffic police, and gas station attendants) and 10 office workers as controls in Trujillo, Peru, in July 2002. PM2.5 was collected, carbon monoxide (CO) was measured, volatile organic compounds (VOCs) were sampled and analyzed. Newspaper vendors had the highest full-shift CO exposures (mean +/- SD: 11.4 +/- 8.9 ppm), while office workers had the lowest (2.0 +/- 1.7 ppm). Bus drivers had the highest full-shift PM2.5 exposures (161 +/- 8.9 microg/m3), while gas station attendants (64 +/- 26.5 microg/m3) and office workers (65 +/- 8.5 microg/m3) were the lowest. Full-shift benzene/toluene/ethylbenzene/xylene exposures (BTEX) among gas station attendants (111/254/43/214 microg/m3) were much higher than those among van and taxi drivers. Several of the traffic-related occupational exposures studied were elevated and are of occupational health concern.

We continue our investigations into the mechanisms heating the outer layers of cool dwarf stars. In this study we specifically seek to determine whether in the layers with temperatures around 250,000-300,000 K, in which the O VI lines are emitted, the temperatures are determined by heat conduction from the coronae or by the same processes that heat the lower temperature regions. To study this we discuss here 22 spectra of Hyades F stars taken by the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite to study the O VI lines at 1032 Å and the C III lines at 977 Å and compare them with other lower transition layer lines, observed with HST and IUE, and with existing X-ray data. For our targets with B-V > 0.4, the X-ray fluxes of single F stars increase, on average, slowly with increasing B-V, while the O VI line fluxes show the same steep decrease around B-V = 0.43 as previously found for the lower temperature transition layer lines. For single stars the X-ray fluxes decrease with increasing v sin i, except for the stars with B-V between 0.418 and 0.455, while for the O VI lines, as for the other transition layer lines, fluxes increase with increasing v sin i, if v sin i is larger than 30 km s-1. For smaller v sin i, line fluxes are independent of v sin i. The B-V and v sin i dependences of the O VI line fluxes are then very different from those of the X-ray fluxes. We thus conclude that for electron temperature Te below 300,000 K, the transition layers for Hyades F stars are not mainly heated by heat conduction from their coronae.

γ Cas is the prototypical classical B0.5e star and is now known to be the primary in a wide binary system. It has long been famous for its unique hard X-ray characteristics, among which are variations that correlate with changes in a number of optical light and UV line and continuum properties. These peculiarities have led to a picture in which processes on or near the Be star produce the observed X-ray emission. In this paper we report on a 53 ks Chandra High Energy Transmission Grating Spectrometer observation of this target. An inspection of our spectrum shows that it is quite atypical for a massive star. The emission lines appear weak because of a strong short-wavelength continuum that arises from a hot plasma with kT = 11-12 keV. The spectrum exhibits many lines, the strongest of which are Lyα features of H-like species from Fe through the even-Z intermediate elements (S, Si, Mg, and Ne), down to O and N. Line ratios of the "rif triplet" for a variety of He-like ions and of Fe XVII are consistent with the dominance of collisional atomic processes. However, the presence of Fe and Si fluorescence K features indicates that photoionization also occurs in nearby cold gas. The line profiles indicate a mean velocity at rest with an rms line broadening of 500 km s-1 and little or no asymmetry. An empirical global-fitting analysis of the line and continuum spectrum suggests that there are actually three or four plasma emission components. The first is the dominant hot (12 keV) component, of which some fraction (10%-30%) is heavily absorbed, while the remainder is affected by a much lower column density of only 3 × 1021 cm-2. The hot component has a Fe abundance of only 0.22 ± 0.05 solar. The other two or three major emission components are "warm" and are responsible for most other emission lines. These components are dominated by plasma having temperatures near 0.1, 0.4, and 3 keV. Altogether, the warm components have an emission measure of about 14% of the hot component, a low column density, and a more nearly solar composition. The 100 eV component is consistent with X-ray temperatures associated with a wind in a typical early B star. Nonetheless, its emission measure is a few times higher than would be expected from this explanation. The strength of the fluorescence features and the dual-column absorption model for the hot plasma component suggest the presence near the hot sites of a cold gas structure with a column density of ~1023 cm-2. Because this is also the value determined by Millar and Marlborough for the vertical column of the Be disk of γ Cas, these attributes suggest that the X-ray-emitting sources could be close to the disk and hence to the Be star. Finally, we discuss the probably related issues of the origin of the warm emission components, as well as the puzzling deficient Fe abundance in the hot component. It is possible that the latter anomaly is related to the FIP (abundance fractionation) effect found in certain coronal structures on the Sun and RS CVn stars. This would be yet another indication that the X-rays are produced in the immediate vicinity of the Be star.

We continue our investigations into the mechanisms heating the outer layers of cool dwarf stars. In this study we specifically seek to determine whether in the layers with temperatures around 250,000-300,000 K, in which the O VI lines are emitted, the temperatures are determined by heat conduction from the coronae or by the same processes that heat the lower temperature regions. To study this we discuss here 22 spectra of Hyades F stars taken by the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite to study the O VI lines at 1032 Angstrom and the C III lines at 977 Angstrom and compare them with other lower transition layer lines, observed with HST and IUE, and with existing X-ray data. For our targets with B-V>0.4, the X-ray fluxes of single F stars increase, on average, slowly with increasing B-V, while the O VI line fluxes show the same steep decrease around B-V=0.43 as previously found for the lower temperature transition layer lines. For single stars the X-ray fluxes decrease with increasing v sin i, except for the stars with B-V between 0.418 and 0.455, while for the O VI lines, as for the other transition layer lines, fluxes increase with increasing v sin i, if v sin i is larger than 30 km s(-1). For smaller v sin i, line fluxes are independent of v sin i. The B-V and v sin i dependences of the O VI line fluxes are then very different from those of the X-ray fluxes. We thus conclude that for electron temperature T-e below 300,000 K, the transition layers for Hyades F stars are not mainly heated by heat conduction from their coronae.