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First blanktone compilation. Ultraviolet part. vfob fuap-Ambuse Hite Algesis-Somnus Ambulo vfobbfuap-comfortbk Any Of My Names – Will Sepia Undress Her DJ Nemora – Fly in the sky Gedanken – attempt is vfo vfobbfuap –Gestild Tony Deus – Childhood naum sinrike – otnosheniya

The Ultraviolet Imaging Telescope (UIT), part of the Astro-1 Spacelab Mission, was used to obtain high-resolution surface brightness distribution data in six ultraviolet wavelength bands for the bright reflection nebula NGC 7023. The corresponding data from the visible leads us to conclude that the scattering in the near and far ultraviolet in this nebula is more strongly forward directed than it is in the visible. The UIT also obtained near-UV and far-UV images of the giant OB association NGC 206 in M32. Photometry was obtained for thirty massive stars. We analyzed UV imagery of two Sb bulges and two E galaxies obtained with UIT. For NGC 1275, the measured UV colors indicate a mass function which extends to eight solar masses but no higher. Other aspects of this investigation are discussed.

Research was conducted at MSFC on the behavior of elastomeric materials after exposure to simulated space environment. Silicone S383 and Viton V747 samples were exposed to thermal vacuum, ultraviolet radiation, and atomic oxygen and then evaluated for changes in material properties. Characterization of the elastomeric materials included weight, hardness, optical inspection under normal and black light, spectrofluorescence, solar absorptance and emittance, Fourier transform infrared spectroscopy, and permeability. These results indicate a degree of sensitivity to exposure and provided some evidence of UV and atomic oxygen synergism.

We describe the design, fabrication, and testing of a monolithic interferometer consisting entirely of optically contacted fused-silica optical elements that are assembled, adjusted, and permanently bonded in place. The interferometer is part of a spatial heterodyne spectrometer SHS SHIMMER Spatial Heterodyne Imager for Mesospheric Radicals that will be used for near-ultraviolet high-spectral resolution limb imaging of OH solar resonance fluorescence from low Earth orbit aboard the satellite STPSat-1 scheduled for launch in 2006. The stability of the monolith coupled with the relaxed tolerances on optical quality and alignment inherent to SHS make this new instrument extremely robust and especially attractive for applications in harsh environments.

We describe the first results from a six-month long reverberation-mapping experiment in the ultraviolet based on 170 observations of the Seyfert 1 galaxy NGC 5548 with the Cosmic Origins Spectrograph on the Hubble Space Telescope. Significant correlated variability is found in the continuum and broad emission lines, with amplitudes ranging from ~30% to a factor of two in the emission lines and a factor of three in the continuum. The variations of all the strong emission lines lag behind those of the continuum, with He II 1640 lagging behind the continuum by ~2.5 days and Lyman alpha 1215, C IV 1550, and Si IV 1400 lagging by ~5-6 days. The relationship between the continuum and emission lines is complex. In particular, during the second half of the campaign, all emission-line lags increased by a factor of 1.3-2 and differences appear in the detailed structure of the continuum and emission-line light curves. Velocity-resolved cross-correlation analysis shows coherent structure in lag versus line-of-sight velocity for the emission lines; the high-velocity wings of C IV respond to continuum variations more rapidly than the line core, probably indicating higher velocity BLR clouds at smaller distances from the central engine. The velocity-dependent response of Lyman alpha, however, is more complex and will require further analysis.

We have obtained a far-ultraviolet spectrum of the X-ray binary Hercules X-1/HZ Herculis using the Hopkins Ultraviolet Telescope aboard the Astro-1 space shuttle mission in 1990 December. This is the first spectrum of Her X-1 that extends down to the Lyman limit at 912 A. We observed emission lines of O VI, N V, and C IV, and the far UV continuum extending to the Lyman limit. We examine the conditions of the emitting gas through line strengths, line ratios, and doublet ratios. The UV flux is lower by about a factor of 2 than expected at the orbital phase of the observation. We model the UV continuum with a simple power-law and with a detailed model of an X-ray-illuminated accretion disk and companion star. The power-law provides a superior fit, as the detailed model predicts too little flux below 1200 A. We note, however, that there are uncertainties in the interstellar reddening, in the background airglow spectrum, and in the long-term phase of the accretion disk. We have searched the data for UV line and continuum pulsations near the neutron star spin period but found none at a detectable level.

We have obtained a far-ultraviolet spectrum of the X-ray binary Hercules X-1/HZ Herculis using the Hopkins Ultraviolet Telescope aboard the Astro-1 space shuttle mission in 1990 December. This is the first spectrum of Her X-1 that extends down to the Lyman limit at 912 A. We observed emission lines of O VI, N V, and C IV, and the far UV continuum extending to the Lyman limit. We examine the conditions of the emitting gas through line strengths, line ratios, and doublet ratios. The UV flux is lower by about a factor of 2 than expected at the orbital phase of the observation. We model the UV continuum with a simple power-law and with a detailed model of an X-ray-illuminated accretion disk and companion star. The power-law provides a superior fit, as the detailed model predicts too little flux below 1200 A. We note, however, that there are uncertainties in the interstellar reddening, in the background airglow spectrum, and in the long-term phase of the accretion disk. We have searched the data for UV line and continuum pulsations near the neutron star spin period but found none at a detectable level.

We estimate the UV continuum slope, beta, for 923 galaxies in the range 1 < z < 8 in the Hubble Ultradeep Field (HUDF). These data include 460 galaxies at 1 < z < 2 down to an absolute magnitude M_{UV} = -14 (~0.006 L*_{z=1}; 0.02 L*_{z=0}), comparable to dwarf galaxies in the local universe. We combine deep HST/UVIS photometry in F225W, F275W, F336W wavebands (UVUDF) with recent data from HST/WFC3/IR (HUDF12). Galaxies in the range 1 < z < 2 are significantly bluer than local dwarf galaxies. We find their mean (median) values = -1.382 (-1.830) +/- 0.002 (random) +/- 0.1 (systematic). We find comparable scatter in beta (standard deviation = 0.43) to local dwarf galaxies and 30% larger scatter than z > 2 galaxies. We study the trends of beta with redshift and absolute magnitude for binned sub-samples and find a modest color-magnitude relation, dbeta/dM = -0.11 +/- 0.01 and no evolution in dbeta/dM with redshift. A modest increase in dust reddening with redshift and luminosity, Delta E(B-V) ~ 0.1, and a comparable increase in the dispersion of dust reddening at z < 2, appears likely to explain the observed trends. At z > 2, we find trends that are consistent with previous works; combining our data with the literature in the range 1 < z < 8, we find a color evolution with redshift, dbeta/dz = -0.09 +/-0.01 for low luminosity (0.05 L*_{z=3}), and dbeta/dz = -0.06 +/-0.01 for medium luminosity (0.25 L*_{z=3}) galaxies.

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

A scientific investigation of heating and mass transport in the solar corona that is currently planned for a future Shuttle/Spacelab flight is outlined. The instrument to be used is a near-normal incidence grating spectrograph fed by a grazing incidence Wolter Type 2 telescope. A toroidal grating design provides stigmatic images of the corona up to 8 arc min in extent over the spectral region from 225 A to 370 A. Spatial resolution of at least 2 arc sec and spectral resolution of 0.050 A is achievable throughout the central 4 arc min field or view. Primary scientific data are recorded on Schumann-type film. An H-alpha slit jaw monitor and zero order extreme ultraviolet monitor are also planned to support instrument operation.

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

The design of a suitable coalignment system (CAS) for the Solar Extreme Ultraviolet Telescope and Spectrometer (SEUTS) is presented. The CAS provides offset adjustment capabilities to SEUTS which will be mounted on a single large pointing system with other devices. The suitability of existing designs is determined and modifications are suggested.

The results of a simulation study to predict the IUE imaging chain performance are presented, including simulation photographs and transparencies of ultraviolet echelle spectra. Errors in wavelength determination and radiometric measurements due to system degradation are indicated to be minor. Some order overlap is predicted at the bottom of the echelle format.

Optical constants of metals in far ultraviolet and relation to energy band structure

This article is from Interdisciplinary Toxicology , volume 6 . Abstract Skin exposure to ultraviolet (UV) light evokes a complex stress response in keratinocytes. Keratin filament organization provides structural stability and mechanical integrity of keratinocytes. Involucrin is a transglutaminase substrate protein contributing to the formation of insoluble cornified envelopes. However, a more complex role for keratins and involucrin has been proposed, including the regulation of cell stress response. The aim was to evaluate modulations of keratin 1, 10 and involucrin expression in HaCaT in the light of the complex response of these cells to UV-B radiation, including effects on c-Jun and matrix metalloproteinase 1 (MMP-1) gene expression and production of interleukin (IL) 6 and 8. A UV-B (300±5 nm) dose of 10 mJ/cm2 was selected since this dose resulted in a partial decrease in cell viability in contrast to higher UV-B doses, which induced complete cell death 48 h after treatment. The UV-B radiation induced significant expression of keratin 1 and 10 and decreased expression of involucrin. This was accompanied by increased expression of c-Jun and MMP-1 and IL-6 and IL-8 production. The data suggest that the expression of keratin 1, 10 and involucrin is modulated in HaCaT keratinocytes as a part of the complex stress response to UV radiation.

This image shows a part of the Cygnus loop supernova remnant, taken by the Ultraviolet Imaging Telescope (UIT) on the Astro Observatory during the Astro-1 mission (STS-35) on December 5, 1990. Pictured is a portion of the huge Cygnus loop, an array of interstellar gas clouds that have been blasted by a 900,000 mile per hour shock wave from a prehistoric stellar explosion, which occurred about 20,000 years ago, known as supernova. With ultraviolet and x-rays, astronomers can see emissions from extremely hot gases, intense magnetic fields, and other high-energy phenomena that more faintly appear in visible and infrared light or in radio waves that are crucial to deepening the understanding of the universe. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Three instruments make up the Astro Observatory: The Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE). The Marshall Space Flight Center had managment responsibilities for the Astro-1 mission. The Astro-1 Observatory was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

Onboard the Space Shuttle Orbiter Columbia (STS-35), the various components of the Astro-1 payload are seen backdropped against a blue and white Earth. Parts of the Hopkins Ultraviolet Telescope (HUT), the Ultraviolet Imaging Telescope (UIT), and the Wisconsin Ultraviolet Photo-Polarimetry Experiment (WUPPE) are visible on the Spacelab pallet. The Broad-Band X-Ray Telescope (BBXRT) is behind the pallet and is not visible in this scene. The smaller cylinder in the foreground is the igloo. The igloo was a pressurized container housing the Command Data Management System, that interfaced with the in-cabin controllers to control the Instrument Pointing System (IPS) and the telescopes. The Astro Observatory was designed to explore the universe by observing and measuring the ultraviolet radiation from celestial objects. Astronomical targets of observation selected for Astro missions included planets, stars, star clusters, galaxies, clusters of galaxies, quasars, remnants of exploded stars (supernovae), clouds of gas and dust (nebulae), and the interstellar medium. Managed by the Marshall Space Flight Center, the Astro-1 was launched aboard the Space Shuttle Orbiter Columbia (STS-35) on December 2, 1990.

We assume the vanishing of the quadratic divergences in the $SU(2)_L \otimes U(1)$ electroweak theory. Using $\,$ the $\,$ top $\,$ mass $\,$ value reported recently by the CDF Collaboration $m_t = 176 \pm 8 \pm 10 GeV$, we predict the mass of the Higgs boson to be $m_H = 321 \pm 29 GeV$. If we assume the vanishing of both quadratic and logarithmic divergencies of the top self-mass, we predict $m_t = 170.5 \pm 0.3 GeV $ and $m_H = 308.6 \pm 0.7 GeV.$

Nonline of sight voice communication has been accomplished in broad daylight via atmospheric scattering of ultraviolet radiation in the solar blind region of the spectrum. A frequency modulated high repetition rate hydrogenxenon flashlamp is used for the transmitter and a combination of solar blind filters and photomultiplier tube is used for the receiver. An analysis is presented to show the potential for a practical, short range, all weather, secure, jam resistant communications system. An experimental study has been performed to systematically determine the scattering and absorption characteristics of ultraviolet light in the lower atmosphere, in both clear and rainy weather. A simplified atmospheric scattering theory has been developed which shows excellent agreement with the observed data. The theory utilizes the generalized Henyey-Greenstein phase function modified to resemble Deirmenjian's phase functions for polydispersed aerosols.

Ultraviolet video imaging system, spectral distribution of UV stimulated luminescence, and measurement of UV reflectance

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

A catalog of observations (experiments) obtained by the Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission (SMM) from Feb. 1980 to Nov. 1989 is presented. The information for each entry includes the time of each observation, the observed position of the Sun, the spacecraft roll angle, the slit used, and instrument parameters such as raster size, pixel spacing, wavelength, polarimeter usage, gate time, etc. The document is split into three volumes: Volume 1 contains experiments 1-30719 (February 1980-April 1985); Volume 2 contains experiments 30720-63057 (April 1985-February 1988); and Volume 3 contains experiments 63058-99771 (February l988-November 1989).

Studies were conducted to determine the relationships, if any, between ultraviolet light, plant growth, and plant response to di-1-para- menthene (a dimer of beta-pinene), the dimethylamine salt of (2,4- dichlorophenoxy)acetic acid, and the combination of the latter two. Greenhouse- grown bean plants (Phaseolus vulgaris L. cv. Black Valentine) were exposed for various time periods to a mid-ultraviolet light source having a major emission peak at 254 nm. The energy level recorded at plant height was 350 ergs/sq cm/ sec. Plants exposed to this light source for 1 hr had chlorotic, malformed leaves. Plants exposed for longer periods (2 hr) had desiccated, discolored leaves, while plants exposed for 3 hr died. An exposure time of 15 min was used as the maximum safe dose for the subsequent studies in which the plants were exposed to the light source 30 min after application of the herbicide treatments. Irradiation of the plants treated with 2,4-D did not result in a significant reduction in herbicide efficacy. The addition of di-1-p-menthene to the spray solution caused significant increases in the phytotoxicity of the herbicide.

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

The purpose of the grant was to obtain and analyze International Ultraviolet Explorer (IUE) spectra of the spiral galaxy NGC 4395, which contains the nearest and least luminous known Seyfert nucleus. The ultraviolet (UV) spectra was to be used to test the intriguing hypothesis that the 'activity' could be explained by purely stellar phenomena, and to further explore the unprecedented properties of this nucleus. To test the feasibility of the project (the nucleus of NGC 4395 is very faint), one IUE shift was allocated, with the possibility of three additional shifts later on. Ultraviolet observations were attempted with IUE on 4 June 1989. Unfortunately, it was found that the only available guide star could no longer be detected sufficiently well with the FES, whose present sensitivity is lower than it was at the beginning of the IUE mission. Thus, it is no longer possible to observe NGC 4395 with IUE. Given these circumstances, as well as the faintness of the nucleus of NGC 4395, a Cycle 2 HST proposal for observations of this object was submitted.

This report describes airglow and stellar observations made on the TEM-1 rocket flight as a part of the Multispectral Measurements Program (MSMP). The observations were in the 1100 to 3000 A wavelength range from 65 to about 230-km altitude, and they include a number of scans of the viewing direction through the earth's horizon. Night airglow emissions observed include the hydrogen Lyman alpha geocorona and the oxygen Herzberg bands. A number of stars were observed including alpha-Eridanus, which is found to match previous intensity measurements. The instrumentation consists of filter photometers with 10 x 10 element digicon spatial detectors and a spectrometer using a 1 x 36 element digicon for spectral resolution. The report describes the instrumentation, discusses the observations, and compares the results with previous measurements. (Author)

No Abstract Available

(abridged) I present and discuss the results of HST STIS observations of IRAS 13224-3809 and 1H 0707-495, two narrow-line Seyfert 1 (NLS1) galaxies. We discovered that high-ionization UV emission lines are much broader and strongly blueshifted compared with the low-ionization and intermediate-ionization lines, which are relatively narrow and centered at the rest wavelength. We interpret this as evidence that the high-ionization lines come from a wind, while the low-ionization lines are emitted from the accretion disk or low-velocity base of the wind. The optically thick disk blocks our view of the receding wind. We also found that not all NLS1s display strongly blueshifted emission lines, and the degree of asymmetry is inversely correlated with the equivalent width and correlated with the SiIII] to CIII] ratio, a density indicator. It may also be significant that these NLS1s display the extreme in the X-ray properties: they have the strongest X-ray soft-excess components and the highest-amplitude, flaring variability. We postulate that this combination of properties are all related to a high value of L/M_BH, even among NLS1s. The high-ionization and low-ionization lines are nearly completely kinematically separated, a fact that allows us to study the conditions in the disk and wind separately.(...)

The celescope instrumentation and data analysis system is described, the major problems encountered during orbital operation are summerized, and a few major problems that were anticipated but did not materialize are listed.

In the Kennedy Space Center (KSC) Operations and Checkout (O and C) Building high bay, the Hopkins Ultraviolet Telescope (HUT), suspended via an overhead crane, is positioned for installation on the STS-35 Astronomy Laboratory 1 (ASTRO-1) unpressurized spacelab pallet by technicians. ASTRO-1 will be loaded into Columbia's, Orbiter Vehicle (OV) 102's, payload bay (PLB) for the STS-35 mission scheduled in April 1990. View provided by KSC with alternate number KSC-89PC-643.

Research during this period has concluded in (1) the revision of the lattice of the Duke FEL ring to suppress magnetic saturation effects, (2) the installation of the major magnetic components for the ring, and (3) the development of a new concept for the production of coherent 40-50 A light using phase-displacement deceleration.

The need to improve the accuracy of measurement of the absolute solar flux within the wavelength range 120 nm to 400 nm requires an extensive effort in contamination control and in tracking the instruments' stability. The techniques used in the solar ultraviolet irradiance monitor are described. These methods resulted in very high calibration stability as proved by preflight and postflight calibration. In-flight calibrating and the pointing accuracy provided by the shuttle attitude control system are discussed.

No Description

(Shortened) Ultraviolet observations of the black hole X-ray binary Cygnus X-1 were obtained using the STIS on HSTubble. We detect P Cygni line features show strong, broad absorption components when the X-ray source is behind the companion star and noticeably weaker absorption when the X-ray source is between us and the companion star. We fit the P Cygni profiles using the SEI method applied to a spherically symmetric stellar wind subject to X-ray photoionization from the black hole. The Si IV doublet provides the most reliable estimates of the parameters of the wind and X-ray illumination. The velocity $v$ increases with radius $r$ according to $v=v_\infty(1-r_\star/r)^\beta$, with$\beta\approx0.75$ and $v_\infty\approx1420$ km s$^{-1}$.The microturbulent velocity was $\approx160$ km s$^{-1}$. Our fit implies a ratio of X-ray luminosity to wind mass-loss rate of L$_{X,38}/\dot M_{-6} \approx 0.33$, measured at $\dot M_{-6}$ = 4.8. Our models determine parameters that may be used to estimate the accretion rate onto the black hole and independently predict the X-ray luminosity. Our predicted L$_x$ matches that determined by contemporaneous RXTE ASM remarkably well, but is a factor of 3 lower than the rate according to Bondi-Hoyle-Littleton spherical wind accretion. We suggest that some of the energy of accretion may go into powering a jet.

Section 1: The Spectra of Hydrogen, Helium, Lithium, Beryllium, Boron, Carbon, Nitrogen, Oxygen, Fluorine, Neon, Sodium, Magnesium, Aluminum, Silicon, Phosphorous, Sulfur, Chlorine, Argon, Potassium, Calcium, Scandium, Titanium, and Vanadium. Section 2: The Spectra of Chromium, Manganese, Iron, Cobalt, Nickel, Copper, Zinc, Gallium, Germanium, Arsenic, Selenium, Bromine, Krypton, Rubidium, Strontium, Yttrium, and Niobium.

A compilation of spectra from the first 36 elements was prepared from published literature available through October 1977. In most cases, only those lines which were actually observed in emission or absorption are listed. The wavelengths included range from 2000 Angstroms to 3200 Angstroms with some additional lines up to 3500 Angstroms. Only lines of stripped atoms are reported; no molecular bands are included.

As part of an observing program using the International Ultraviolet Explorer (IUE) satellite to investigate the ultraviolet properties of stars found within the cores of galactic globular clusters with blue horizontal branches (HBs), we obtained three spectra of the cluster NGC 1904 (M 79). All three were long integration-time, short-wavelength (SWP) spectra obtained at the so called 'center of light' and all three showed evidence of sources within the IUE large aperture (21.4 in. by 10 in.). In this paper we shall describe the analysis of these spectra and present evidence that the UV sources represent individual hot stars in the post-HB stage of evolution.

As part of an observing program using the International Ultraviolet Explorer (IUE) satellite to investigate the ultraviolet properties of stars found within the cores of galactic globular clusters with blue horizontal branches (HBs), we obtained three spectra of the cluster NGC 1904 (M 79). All three were long integration-time, short-wavelength (SWP) spectra obtained at the so called 'center of light' and all three showed evidence of sources within the IUE large aperture (21.4 in. by 10 in.). In this paper we shall describe the analysis of these spectra and present evidence that the UV sources represent individual hot stars in the post-HB stage of evolution.

Narrow Line Seyfert 1 (NLS1) galaxies are remarkable for their extreme continuum and emission line properties which are not well understood. New results bearing on the spectroscopic characteristics of these objects are presented here, with the aim of establishing their typical ultraviolet and optical spectral behavior. We employ HST observations of 22 NLS1s, which represent a substantial improvement over previous work in terms of data quality and sample size. High signal-to-noise NLS1 composite spectra are constructed, allowing accurate measurements of the continuum shape and the strengths, ratios, and widths for lines, including weak features which are barely identifiable in other Active Galactic Nuclei (AGN) composites. We find that the NLS1 sources have redder UV-blue continua than those typically measured in other quasars and Seyferts. Objects with UV line absorption show redder spectra, suggesting that dust is important in modifying the continuum shapes. The data also permit a detailed investigation of the previously proposed link between NLS1s and z >~ 4 quasars. Direct comparison of their composite spectra, as well as a Principal Component Analysis, suggest that high-z QSOs do not show a strong preference toward NLS1 behavior.

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

We present the first direct measurement of a neutral, intact ion pair photoionization efficiency (PIE) curve for a vaporized ionic liquid, 1-butyl-3- methylimidazolium tricyanomethanide, using tunable vacuum ultraviolet (VUV) photoionization time-of-flight mass spectrometry (PI-TOFMS). The ionization potential (IP) for the ion pair is experimentally determined to be 6.6 0.5 eV, which matches reasonably well with the adiabatic IP of 7.3 0.2 eV calculated at the M06/6-31+G(d,p) level of theory. The lifetime to dissociation of the cation radical complex formed upon ionization of the ion pair is highly dependent upon entropic contributions. Thermal gravimetric analyses (TGA) determined the enthalpy of vaporization to be Hvap(298 K) = 143.5 6.2 kJ/mol and that vaporization of BMIM+TCM as ion pairs is the dominant mechanism for mass loss under the experimental conditions for VUV PI-TOFMS (T = 433 K).

The objective of this work was to study the analytical chemistry of B-1 dye in the areas of process control and dye purity. B-1 dye (p-nitrophenylazo, 2-naphthylamine) exhibits a typical electronic transition in the visible portion of the spectrum. The wavelength of this transition is a function of the hydrogen bonding ability of the dye to the solvent and the polarity of the solvent. A second electronic transition for this dye occurs in the near ultraviolet portion of the spectrum and may be ascribed to the p-nitrophenyl chromophore. The ratio of absorbance of these electronic transitions, (the absorbance index) is used as a criterion of dye purity. Deviations from this ratio are shown to be related to impurities or adulterants of the B-1 dye. The newly investigated Spectral Discrimination Technique is described and found to be insensitive to impurities having similar electronic transitions to that of B-1 dye. This technique appears to have little or no value in determining B-1 dye purity.

We present the first intermediate-resolution (lambda / 3000) spectrum of the bright quasi-stellar object 3C273 at wavelengths between 900 and 1200 A. Observations were performed with the Berkeley spectrograph aboard the ORFEUS-SPAS II mission. We detect Lyman beta counterparts to previously-identified intergalactic Lyman-alpha features at cz = 19900, 1600, and 1000 km/s; counterparts to other putative Lyman-alpha clouds along the sight line are below our detection limit. The strengths of the two very low redshift Lyman-beta features, which are believed to arise in Virgo intracluster gas, exceed preflight expectations, suggesting that the previous determination of the cloud parameters may underestimate the true column densities. A curve-of-growth analysis sets a minimum H I column density of 4 E14/cm^2 for the 1600 km/s cloud. We find marginally significant evidence for Galactic H_2 along the sight line, with a total column density of about 1 E15/cm^2. We detect the stronger interstellar O VI doublet member unambiguously; the weaker member is blended with other features. If the Doppler b value for O VI is comparable to that determined for N V then the O VI column density is 7 +/- 2 E14/cm^2, significantly above the only previous estimate. The O VI / N V ratio is about 10, consistent with the low end of the range observed in the disk. Additional interstellar species detected for the first time toward 3C273 (at modest statistical significance) include P II, Fe III, Ar I, and S III.

We calculate the change in the ultraviolet behaviour of the vortex operator due to the presence of dynamical Higgs field in both 2+1 dimensional QED and the 2+1 dimensional Georgi-Glashow model. We find that in the QED case the presence of the Higgs field leads at the one loop level to power like correction to the propagator of the vortex operator. On the other hand, in the Georgi-Glashow model, the adjoint Higgs at one loop has no affect on the vortex propagator. Thus, as long as the mass of the Higgs field is much larger than the gauge coupling constant, the ultraviolet behaviour of the vortex operator in the Georgi-Glashow model is independent of the Higgs mass.

NASA's SR-71 streaks into the twilight on a night/science flight from the Dryden Flight Research Center, Edwards, California. Mounted in the nose of the SR-71 was an ultraviolet video camera aimed skyward to capture images of stars, asteroids and comets. The science portion of the flight is a project of the Jet Propulsion Laboratory, Pasadena, California. Two SR-71 aircraft have been used by NASA as test beds for high-speed and high-altitude aeronautical research. One early research project flown on one of Dryden's SR-71s consisted of a proposal for a series of flights using the SR-71 as a science camera platform for the Jet Propulsion Laboratory (JPL) of the California Institute of Technology, which operates under contract to NASA in much the way that NASA centers do. In March 1993, an upward-looking ultraviolet (UV) video camera placed in the SR-71's nosebay studied a variety of celestial objects in the ultraviolet light spectrum. The SR-71 was proposed as a test bed for the experiment because it is capable of flying at altitudes above 80,000 feet for an extended length of time. Observation of ultraviolet radiation is not possible from the Earth's surface because the atmosphere's ozone layer absorbs UV rays. Study of UV radiation is important because it is known to cause skin cancer with prolonged exposure. UV radiation is also valuable to study from an astronomical perspective. Satellite study of ultraviolet radiation is very expensive. As a result, the South West Research Institute (SWRI) in Texas developed the hypothesis of using a high-flying aircraft such as the SR-71 to conduct UV observations. The SR-71 is capable of flying above 90 percent of the Earth's atmosphere. The flight program was also designed to test the stability of the aircraft as a test bed for UV observation. A joint flight program was developed between the JPL and NASA's Ames-Dryden Flight Research Facility (redesignated the Dryden Flight Research Center, Edwards, California, in 1994) in conjunction with SWRI to test the hypothesis. Dryden modified the nosebay of the SR-71, creating an upward-observing window to carry SWRI's ultraviolet CCD camera so it could make observations. According to Dryden's SR-71 Project Manager Dave Lux, a single flight of the aircraft confirmed the aircraft's capability and stability as a test bed for UV observations. SWRI's principle investigator was Dr. Allen Stern.

We report on spectroscopic observations of periodic comet 9P/Tempel 1 by the Alice ultraviolet spectrograph on the Rosetta spacecraft in conjunction with NASA's Deep Impact mission. Our objectives were to measure an increase in atomic and molecular emissions produced by the excavation of volatile sub-surface material. We unambiguously detected atomic oxygen emission from the quiescent coma but no enhancement at the 10% (1-sigma) level following the impact. We derive a quiescent water production rate of 9 x 10^27 molecules per second with an estimated uncertainty of 30%. Our upper limits to the volatiles produced by the impact are consistent with other estimates.

Raw data from the Solar Backscattered Ultrviolet/Total Ozone Mapping Spectrometer (SBUV/TOMS) Nimbus 7 operation are available on computer tape. These data are contained on two separate sets of RUTs (Raw Units Tapes) for SBUV and TOMS, labelled RUT-S and RUT-T respectively. The RUT-S and RUT-T tapes contain uncalibrated radiance and irradiance data, housekeeping data, wavelength and electronic calibration data, instrument field-of-view location and solar ephemeris information. These tapes also contain colocated cloud, terrain pressure and snow/ice thickness data, each derived from an independent source. The "RUT User's Guide" describes the SBUV and TOMS experiments, the instrument calibration and performance, operating schedules, and data coverage, and provides an assessment of RUT-S and -T data quality. It also provides detailed information on the data available on the computer tapes.

Raw data from the Solar Backscattered Ultrviolet/Total Ozone Mapping Spectrometer (SBUV/TOMS) Nimbus 7 operation are available on computer tape. These data are contained on two separate sets of RUTs (Raw Units Tapes) for SBUV and TOMS, labelled RUT-S and RUT-T respectively. The RUT-S and RUT-T tapes contain uncalibrated radiance and irradiance data, housekeeping data, wavelength and electronic calibration data, instrument field-of-view location and solar ephemeris information. These tapes also contain colocated cloud, terrain pressure and snow/ice thickness data, each derived from an independent source. The "RUT User's Guide" describes the SBUV and TOMS experiments, the instrument calibration and performance, operating schedules, and data coverage, and provides an assessment of RUT-S and -T data quality. It also provides detailed information on the data available on the computer tapes.

1Winesburg, Ohio

By Sherwood Anderson

Published in 1919, and listed on the Modern Library roster of the 20th century's 100 greatest novels in English, Winesburg, Ohio presents a series of loosely related character studies of the inhabitants of a fictional Midwestern town that together form a novel of unusual unity and vision. The inarticulate and lonely citizens of Winesburg, each with his or her own secret tale to tell, frequently relate those tales to, or through their interactions with, the character of George Willard, a young Winesburg citizen on the cusp of manhood with dreams of becoming a writer. Thus Winesburg tells the story of the townspeople's loneliness and alienation in parallel with the tale of George's own coming of age. The citizens of Winesburg are described obliquely as "grotesques," but as the introductory chapter makes clear, "The grotesques were not all horrible. Some were amusing, some almost beautiful . . ." (Description by Stewart Wills)

2Seven O'Clock Stories

By Robert Gordon Anderson

"Not once upon a time but just now, in a white house by the side of a road, live three happy children. Their mother and father gave them very odd names, for two old uncles and one aunt, which pleased the old people very much. Their names are all written in the big family Bible,--Jehosophat Green, Marmaduke Green, and Hepzebiah Green." So begins this collection of bedtime stories for children, one each night for twenty days, involving these three happy children and their playmates. (Summary by P. Cunningham)

3Security

By Poul William Anderson

“Security” tells the story of a compartmentalized government physicist ordered by secret police to complete experiments aimed at developing a new weapon. He is brought to a hidden space station and put in charge of the project but there are many questions. In a world of spies watching spies it’s sometimes hard to know what’s patriotic. -- Poul Anderson was a Golden Age Science Fiction and Fantasy author. “Security” first appeared in the magazine “Space Science Fiction” in February of 1953 (Summary by Gregg Margarite)

4Chapter Ends

By Poul William Anderson

Far, far in the future the Earth is still spinning around the Sun, on the edge of the galaxy, dozing in obscurity, forgotten by it's trillions of progeny and completely irrelevant. But this doesn't matter to the few millions who still live there in simplicity and quiet happiness. But then interstellar politics dictates that they must all leave Earth because ... well, listen to the story as told by the great Poul Anderson as he explores what the Earth means to humans and to one man in particular. (Summary by Phil Chenevert)

5Spell of the Hawaiian Islands and the Philippines

By Isabel Anderson

Isabel Anderson has written a most interesting travelogue of Hawaii and The Philippines. Actually it is more of a history lesson. Anyone with any interest whatsoever in the South Pacific will find this book very interesting indeed, to note all that has changed since Mrs. Anderson had traveled there. (Summary by William Tomcho)

Eamont was an opium clipper built in Cowes. It was the subject of an 1891 book, A cruise in an opium clipper, by Captain Lindsay Anderson. Eamont was involved in the opening of Japan to foreigners in 1858, serving as a dispatch boat between Nagasaki and Shanghai, and was one of the first vessels to open up a trade with Formosa…. The Eamont was sent on some very dangerous trips. She was one of the first vessels to open up a trade with Formosa, and made the first survey of the port of Taku, which she entered by bumping over the reef in spite of a tremendous surf beating upon it at the time, a most daring performance. And in her efforts to trade with the Formosans she had to withstand the attack of hundreds of armed natives right on top of a typhoon, which she succeeded in riding out on her moorings. But the captain of the Eamont was a famous fighting man, as the Chinese pirates knew to their cost…. The Eamont was also employed in the negotiations for the first commercial treaty with Japan. (See Wikipedia article on Eamont (schooner)) - Summary by Wikipedia and david wales

Anderson served as third officer aboard the Eamont. Eamont was an opium clipper built in Cowes. Eamont was involved in the opening of Japan to foreigners in 1858, serving as a dispatch boat between Nagasaki and Shanghai, and was one of the first vessels to open up a trade with Formosa. The Eamont was employed in the negotiations for the first commercial treaty with Japan. On this occasion she ran into Nagasaki and quietly dropped anchor, in spite of the fact that opposition to the proposed commercial treaty was very strong at the time. On the following morning 150 boat-loads of Japanese attempted to tow her to sea, being evidently ignorant of an anchor's raison d'etre. But though they attempted several similar methods to get rid of her they refrained from any armed attack, and, eventually, her mission was completely successful. This was in 1858, and the Eamont's crew saw many wonderful sights in that tierra incognita. The September Typhoon of 1858 destroyed several well-known opium clippers at Double Island, including the Anonyma, Gazelle, Pantaloon, and Mazeppa. Eamont was anchored off Double Island, with "150 fathoms of chain out and a second anchor backed on it at 60 fathoms." The waves in the anchorage were estimated to be as large as 40 feet, and the Eamont’s crew had to cut away her masts. Eamont was one of only two ships in that anchorage to survive the night, the other being the Hazard. (See Wikipedia article on Eamont (schooner)) (Wikipedia and david wales)

A Voice from Harper's Ferry is the abolitionist testament of Osborne Perry Anderson, the only surviving black participant in the 1859 raid on Harpers Ferry organized by John Brown. The book details the motivations and preparations for the raid, the events that unfolded over several days in October 1859, and Anderson's subsequent escape. It ends with a short selection of poems from various sources honoring Brown and the movement for abolition. (summary by JR Martin)

9Sentiment, Inc.

By Poul William Anderson

The way we feel about another person, or about objects, is often bound up in associations that have no direct connection with the person or object at all. Often, what we call a "change of heart" comes about sheerly from a change in the many associations which make up our present viewpoint. Now, suppose that these associations could be altered artificially, at the option of the person who was in charge of the process.... (from the Blurb)

“The Triumph of the Egg” is a collection of stories and poems by Sherwood Anderson. Abandoning the interconnected quality of his more famous “Winesburg, Ohio,” the author adopts a variety of perspectives and settings while exploring similar themes: personal growth, disillusionment, loneliness, and urban-rural contrast. In the North American Review, critic Lawrence Gilman wrote, “Mr. Anderson has achieved a beauty that irradiates his page.” Though largely overshadowed by that celebrated, earlier book, “The Triumph of the Egg” remains a foundational work for Modernist literature, proven by its winning the first annual Dial Award from the influential journal The Dial.<br /><br /> NOTE TO LISTENERS: The second story in this collection, “I Want to Know Why,” contains language that may be offensive.<br /> (summary by Ben Adams)

11How to Do Chemical Tricks

By A. T. Anderson

While a bit outdated in many of the more complex descriptions of several of the phenomena described, this book is nonetheless still fun and relevant for a person interested in basic chemistry or physics tricks, and the devices built in the book can be easily replicated with more modern materials. The book is split up into many little experiments, tricks, with an explanation on how it works, what's happening, and how to reproduce the effects at home.(summary by Kyle Van DeGlast)

12American Big-Game Hunting

By George S. Anderson, Winthrop Chanler, Oscar F. C. Crocker, Walter Bourchier Devereux, George Bird Grinnell, Arnold Hague, W. D. Pickett, Archibald Rogers, Theodore Roosevelt, Bronson Rumsey, Dean Sage, Roger D. Williams and Owen Wister

The first book published by The Boone and Crockett Club founded by Theodore Roosevelt and George Grinnell, who declared in their Editors Note: "Hunting big game in the wilderness is, above all things, a sport for a vigorous and masterful people. The rifle-bearing hunter, whether he goes on foot or on horseback, whether he voyages in a canoe or travels with a dog-sled, must be sound of body and firm of mind, and must possess energy, resolution, manliness, self-reliance, and capacity for hardy self-help. In short, the big-game hunter must possess qualities without which no race can do its life-work well; and these are the very qualities which it is the purpose of this Club, so far as may be, to develop and foster."<br /><br /> A bit outdated as to the equipment they used, this book is nevertheless an intense look at the west in early days, and at the beginnings of the conservationist movement in America. Each chapter focuses on a different animal, from buffalo, mountain goat, elk, pronghorn sheep, grizzlies, etc., indigenous peoples, different areas like the Rockies and Yellowstone, and it still captures the essence of the spirit of the hunt.<br /><br /> The book ends with a list of the club's original 100 members, a veritable Who's Who of Generals, Colonels, Doctors, Senators and Representatives, amongst them that most illustrious Gen'l William T. Sherman. ( ~ Michele Fry, read by LibriVox Volunteers)

13Windy McPherson's Son

By Sherwood Anderson

Windy McPherson's Son is the story of Sam McPherson's rise in the world of business and search for emotional enlightenment in later life. McPherson starts out as an ambitious newsboy in Caxton, Ohio, with drunkard of a father who constantly embarrasses him. Eventually, after his mother's death and an episode with a middle-aged schoolteacher, McPherson leaves Caxton for Chicago. In Chicago, he gets a job as a buyer of farm implements and establishes his reputation in business. While his professional life is blossoming, his personal life suffers. After meeting Sue Rainey, the daughter of his boss Colonel Rainey, they get married and twice fail to have children. Following a business deal that forces his father-in-law out of his own company, McPherson and Sue Rainey separate. One day, once McPherson had become quite wealthy, he gets a telegram saying that Colonel Rainey committed suicide. This causes Sam to realize that he is unhappy with his life. This feeling inspires him to leave Chicago and travel all over becoming involved in various adventures. Finally, McPherson's comes across a promiscuous and alcoholic mother of three children. A deal is made and McPherson gets custody of the children. Showing up with the children at Sue's current place of residence, the five of them become family. ( Wikipedia)

14Inside Earth

By Poul William Anderson

This story takes place in the not so distant future. Earth has been conquered and is a subjugated planet, the much too humanoid new rulers now extract heavy taxes, control industry and reproduction and interfere in every aspect of life. Rumors of their brutality and vicious massacres increase every day. Obviously, they must be thrown out and rebellion seethes among the patriots. But on the other hand, others are not so eager to get rid of the overlords: the terrible nationalistic wars have been stopped, famine is long gone and health care is almost universally available. Still, the elite intellectual portion of the earth's population plot to remove the heavy heel of the oppressors from their necks and let earth be free again. But time and again the attempts for freedom have been crushed the Valgolians mainly because national, ethnic, religious and racial prejudices and hatred among the earthlings keep the conspirators from working together. Obviously, no conqueror wants his subjects to revolt against his rule. Obviously? This one would go to any lengths to start a rebellion!

15Sensitive Man

By Poul William Anderson

Poul Anderson delves into the realm of human potential in this exciting story and asks some penetrating questions for us to think about. What if psychology finally enabled people to even partially control all those automatic reactions of our minds and bodies? What if we were not slaves to anger, fear, emotions, hormones, blood pressure and the thousand other things that our bodies 'take care of' from instant to instant? What if those things could be brought under the control even partially of our reason and minds? In this story one man stood between a power-hungry cabal and their world mastery—but a man of, shall we say, unusual talents.

16Hunting In Many Lands

By Henry T. Allen, George S. Anderson, Daniel Moreau Barringer, Winthrop Chanler, George H. Gould, Madison Grant, William Woodville Rockhill, Theodore Roosevelt, Elliott Bulloch Roosevelt, Alden Sampson, Henry L. Stimson, Charles E. Whitehead, Caspar W. Whitney and Roger D. Williams

The first volume published by the Boone and Crockett Club, entitled "American Big Game Hunting," confined itself to sport on the American continent. This second volume presents a number of interesting sketches written by club members who have hunted big game in other lands. Essays include: Hunting in East Africa, To the Gulf of Cortez, A Canadian Moose Hunt, A Hunting Trip in India, Dog Sledging in the North, Wolf-Hunting in Russia, A Bear-Hunt in the Sierras, The Ascent of Chief Mountain, The Cougar, Big Game of Mongolia and Tibet, Hunting in the Cattle Country, Wolf-Coursing, Game Laws, and Protection of the Yellowstone National Park. - Summary by Michele Fry

Margaret Steele Anderson was born in Louisville, Kentucky in 1867 and was educated in the public school of Louisville, with special courses at Wellesley College. From 1901 Miss Anderson was Literary Editor of the `Evening Post' of Louisville, and was known as one of the most discriminating critics of the South. She published only one volume of verse, "The Flame in the Wind", 1914. (David Lawrence

Frederick Irving Anderson was a New York newspaperman who had a second career writing mystery stories for the "slick" magazines such as the Saturday Evening Post. The Infallible Godahl is a collection of some of his first stories. Godahl is a clever gentleman thief, who might be thought of as an American version of Raffles or Arsene Lupin. - Summary by Winston Tharp

Margaret Steele Anderson's tribute to the men left on board the doomed ship, some of whom followed the "Women and children first" tradition of the sea. - Summary by David Lawrence