Ultraviolet Spectral Properties Research Articles

Effects of Inhabiting and Life Patterns on the UV Spectral Properties of Small Mammalian Herbivores’ Urine

It is well known that avian predators can use prey excretions such as urine and feces to track their prey, and the urine and feces of small mammalian herbivores can reflect ultraviolet (UV) light and emit fluorescent light. There are still some debates as to whether UV visibility of small mammalian herbivores’ urine is used as a hunting cue by avian raptors. Some studies in Europe have demonstrated that diurnal raptors are capable of utilizing these cues to target key prey species. However, researchers in Australia have argued that raptors do not use the UV visibility of urine while hunting. To our knowledge, there are no reports from Asia concerning the ultraviolet spectral characteristics of small mammal herbivores’ urine. This study examined the UV spectral properties of urine from 6 small mammal herbivores species by comparing the UV reflectance and fluorescence spectra of urine from small mammalian herbivores living in plateau meadows, plateau shrubs, open marshland, farmland, and semi-desert grassland in China. In addition, we compared the UV spectral properties of urine from ground-dwelling species of rodents and subterranean species to determine whether ultraviolet visibility of small mammal herbivores’ urine could be used as a visual signal by Asian vole-eating raptors. The results showed that: 1) the SC370 values of urine from four small mammal herbivores species were ordered as plateau pika (plateau meadow) > root voles (plateau bush) > reed voles (swampland) > Brandt’s vole (desert grassland); and 2) UV fluorescence peak intensity and the wavelengths of urine from ground-dwelling species (such as the root vole, plateau pika, or Brandt’s vole) were significantly higher than those of subterranean-dwelling species (mandarin vole and plateau zokor). These results indicate that UV visibility of small mammal herbivores’ urine may act as a visual cue for raptors.

Study on the Synthesis and Properties of Primary Procyanidins Metal Compounds

Synthetic procyanidins-metallic compounds study the infrared spectral properties and ultraviolet spectral properties of mates, to study the free radical scavenging ability of procyanidins and the antioxidant ability of procyanidins complexes under different pH buffer solutions, provide a certain theoretical basis for future research and application of procyanidins. In addition to antibacterial, anti-radiation, anti-allergy and other functions, proanthocyanidins can also inhibit tumor. However, few people have studied the coordination reaction of procyanidins with Bovine serum albumin and metal ions, so it has great research value. In this paper, the optical activity of the complex will be preliminarily studied, which will lay a theoretical foundation for the development of drug fluorescence probe in the future.

Probing Early Supermassive Black Hole Growth and Quasar Evolution with Near-infrared Spectroscopy of 37 Reionization-era Quasars at 6.3 < z ≤ 7.64

Abstract We report the results of near-infrared spectroscopic observations of 37 quasars in the redshift range 6.3 < z ≤ 7.64, including 32 quasars at z > 6.5, forming the largest quasar near-infrared spectral sample at this redshift. The spectra, taken with Keck, Gemini, VLT, and Magellan, allow investigations of central black hole mass and quasar rest-frame ultraviolet spectral properties. The black hole masses derived from the Mg ii emission lines are in the range (0.3–3.6) × 109 M ⊙, which requires massive seed black holes with masses ≳103–104 M ⊙, assuming Eddington accretion since z = 30. The Eddington ratio distribution peaks at λ Edd ∼ 0.8 and has a mean of 1.08, suggesting high accretion rates for these quasars. The C iv–Mg ii emission-line velocity differences in our sample show an increase of C iv blueshift toward higher redshift, but the evolutionary trend observed from this sample is weaker than the previous results from smaller samples at similar redshift. The Fe ii/Mg ii flux ratios derived for these quasars up to z = 7.6, compared with previous measurements at different redshifts, do not show any evidence of strong redshift evolution, suggesting metal-enriched environments in these quasars. Using this quasar sample, we create a quasar composite spectrum for z > 6.5 quasars and find no significant redshift evolution of quasar broad emission lines and continuum slope, except for a blueshift of the C iv line. Our sample yields a strong broad absorption line quasar fraction of ∼24%, higher than the fractions in lower-redshift quasar samples, although this could be affected by small sample statistics and selection effects.

The MUSE Hubble Ultra Deep Field Survey

We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z > 2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope.

Preparation and In Vivo Antinociceptive Behavior of Four New 2‐Amino‐6‐trifuromethoxybenzothiazole Carboxylic Acid Derivatives

AbstractFour novel N‐substituted riluzole derivatives (4 a‐4 d) have been prepared and characterized. Their antinociceptive activities have been carefully investigated by hot‐plate test and writhing test. Our results indicated that at dose of 18 mg kg−1, 2‐(N‐propionic acid)‐6‐trifluoromethoxy‐benzothiazole (4 a), 2‐(N‐butanoic acid)‐6‐trifluoromethoxy‐benzothiazole (4 b) and 2‐(N‐n‐caproic acid)‐6‐trifluoromethoxy‐benzothiazole (4 c) significantly increased the nociceptive response latency under hot plate test while chemical nociception induced by intraperitoneal acetic acid was significantly inhibited by 4 a and 2‐(N‐proline)‐6‐trifluoromethoxy‐benzothiazole (4 d) at same dosage. Our research clearly indicates that N‐substituted Riluzole derivatives could be new alternative candidates as potential antinociceptive medicines.

Solvatochromism and quantum mechanical investigation of disazo pyridone dye

Disazo pyridone dye, 4‐methyl‐2,6‐dioxo‐5‐(2‐(4‐(phenyldiazenyl)phenyl)hydrazono)‐1,2,5,6‐tetrahydropyridine‐3‐carbonitrile, is synthesised and thoroughly characterised by a combination of experimental and computational approaches. Fourier Transform‐infrared and nuclear magnetic resonance (NMR) spectra prove the existence of the hydrazone form in the solid state and in dimethyl sulphoxide, which is also supported by vibrational and NMR theoretical studies. Ultraviolet (UV) spectral properties, as well as solvatochromism in 19 solvents of different polarity, are investigated. In most of the solvents, the dye is solely present in the hydrazone form, whereas in certain solvents, an acid–base equilibrium exists. Excellent agreement between computational and experimental UV–visible data was established. Frontier Molecular Orbital analysis was performed and proved the existence of intramolecular charge transfer through the dye molecule. A molecular electrostatic potential surface was plotted over the optimised geometry to lighten the reactivity of the investigated molecule.

Dissolved organic matter characteristics along sabo dammed streams based on ultraviolet visible and fluorescence spectral properties.

Changes in dissolved organic matter (DOM) characteristics were investigated in two mountainous streams with closed-type sabo dams. Surface water was collected from four stations along the two mountainous streams and analyzed using ultraviolet-visible spectrophotometry and excitation-emission fluorescence matrix (EEM) methods. Optical properties of DOM indicated an increase in molecular weight and aromaticity at stations near the sabo dams. Average spectral ratio values were low before and after the dam (i.e., < 0.72) compared to other sections of the stream. Specific ultraviolet absorbance (SUVA254) increased in the vicinities of the dams. While chromophoric DOM characteristics from two sites were influenced by the dam, fluorescence components, however, did not show notable changes around dams. Instead, the three chromophoric components distinguished by EEM-parallel factor analysis, that is, humic-like (C1 and C2) and protein-like (C3) increase along the stream. Fulvic-like component (C1) had a high fluorescence intensity at all stations; all the three components were more abundant in the downstream section. Chromophoric DOM properties varied along the stream based on alterations in molecular size and aromaticity. Using multivariate analysis, the studied sites were grouped into three clusters related to sabo dams and other activities. We conclude that sabo dams modify DOM characteristics which influence the behavior of DOM transported along the stream.

Ultraviolet spectra of extreme nearby star-forming regions – approaching a local reference sample for JWST

Nearby dwarf galaxies provide a unique laboratory in which to test stellar population models below Z⊙/2. Such tests are particularly important for interpreting the surprising high-ionization ultraviolet (UV) line emission detected at z > 6 in recent years. We present HST/COS UV spectra of 10 nearby metal-poor star-forming galaxies selected to show He ii emission in SDSS optical spectra. The targets span nearly a dex in gas-phase oxygen abundance (7.8 < 12 + log O/H < 8.5) and present uniformly large specific star formation rates (sSFR ∼102 Gyr−1). The UV spectra confirm that metal-poor stellar populations can power extreme nebular emission in high-ionization UV lines, reaching C iii] equivalent widths comparable to those seen in systems at z ∼ 6–7. Our data reveal a marked transition in UV spectral properties with decreasing metallicity, with systems below 12 + log O/H ≲ 8.0 (Z/Z⊙ ≲ 1/5) presenting minimal stellar wind features and prominent nebular emission in He ii and C iv. This is consistent with nearly an order of magnitude increase in ionizing photon production beyond the He+-ionizing edge relative to H-ionizing flux as metallicity decreases below a fifth solar, well in excess of standard stellar population synthesis predictions. Our results suggest that often-neglected sources of energetic radiation such as stripped binary products and very massive O-stars produce a sharper change in the ionizing spectrum with decreasing metallicity than expected. Consequently, nebular emission in C iv and He ii powered by these stars may provide useful metallicity constraints in the reionization era.

Vacuum ultraviolet spectral emission properties of Ga, In and Sn droplet-based laser produced plasmas

The Emission Spectra of gallium, indium and tin droplet-based laser produced plasmas are presented in the Vacuum Ultraviolet (VUV) emission range from 30nm to 160nm. The Ga ion transitions are investigated in detail as a function of background pressure level and laser irradiance. Different wavelength emission regions were detected according to the level of background gas. At short wavelengths (i.e. 30–50nm) the line emission from the higher charge states is reduced with increasing pressure, while at longer wavelengths (i.e. 100–160nm) the trend is inverted, as the plasma emission intensity of the lower charge states increases with higher background gas pressure level. The emitted lines are fitted with Voigt profiles to determine the electron density. The electron temperature is obtained from a fit based on the Planck distribution. These estimations are then used to identify the relevant processes that lead to the different charge state emissions as a function of background gas. Langmuir Probe measurements are also reported for evaluating the ion kinetic energy as a function of background gas. The gallium spectra are calibrated in units of spectral radiance, together with spectra from indium and tin. This calibration allows absolute power estimations from the light source in the VUV region. The presented experimental results are relevant as fundamental plasma emission spectroscopic measurements in an almost unexplored wavelength region as well as for applications such as Extreme Ultraviolet Lithography to determine the so-called Out-of-Band (OoB) radiation emission and for metrology applications for future inspection tools.

Experimental and Density Functional Theoretical Studies on the Spectra of &lt;i&gt;N&lt;/i&gt;, &lt;i&gt;N'&lt;/i&gt;-di[3-hydroxy-4-(2-benzothiazole)phenyl]urea

The experimental infrared (IR), nuclear magnetic resonance (NMR), and ultraviolet (UV) spectra, and density functional theory (DFT) calculations of the novel compoundN,N′-di[3-hydroxy-4-(2-benzothiazole) phenyl]urea (4-DHBTU) are presented. Compared with the UV spectra of the 2-(4-amino-2-hydroxyphenyl) benzothiazole (4-AHBT) monomer, the experimental spectra of 4-DHBTU, a dimer of 4-AHBT, show dual-wavelength absorption with significantly enhanced absorption intensity and an obvious red shift of the maximum absorption peak. Analysis of the experimental spectra and the DFT calculations shows that the structures ofcis-C11 andtrans-C11 are the two most stable conformers, and that the main reason for the different UV spectral properties of the dimer and monomer is the coexistence ofcis-C11,trans-C11,cis-C22, and trans-C22 in the 4-DHBTU sample. In addition, the DFT calculations indicate that a hydrogen-bonding interaction between 4-DHBTU and the dimethyl sulfoxide (DMSO) solvent leads to a large1H NMR chemical shift for atoms 15H and 16H in 4-DHBTU.

Radio-loud and radio-quiet BAL quasars: a detailed ultraviolet comparison

Studies of radio-loud (RL) broad absorption line (BAL) quasars indicate that popular orientation-based BAL models fail to account for all observations. Are these results extendable to radio-quiet (RQ) BAL quasars? Comparisons of RL and RQ BAL quasars show that many of their properties are quite similar. Here we extend these analyses to the rest-frame ultraviolet (UV) spectral properties, using a sample of 73 RL and 473 RQ BAL quasars selected from the Sloan Digital Sky Survey (SDSS). Each RQ quasar is individually matched to a RL quasar in both redshift (over the range $1.5 < z < 3.5$) and continuum luminosity. We compare several continuum, emission line, and absorption line properties, as well as physical properties derived from these measurements. Most properties in the samples are statistically identical, though we find slight differences in the velocity structure of the BALs that cause apparent differences in CIV emission line properties. Differences in the velocities may indicate an interaction between the radio jets and the absorbing material. We also find that UV FeII emission is marginally stronger in RL BAL quasars. All of these differences are subtle, so in general we conclude that RL and RQ BAL QSOs are not fundamentally different objects, except in their radio properties. They are therefore likely to be driven by similar physical phenomena, suggesting that results from samples of RL BAL quasars can be extended to their RQ counterparts.

The behaviour of quasar C iv emission-line properties with orientation

With a quasar sample designed for studying orientation effects, we investigate the orientation dependence of characteristics of the C IV 1549 broad emission line in approximately 50 Type 1 quasars with z=0.1-1.4. Orientation is measured for the sample via radio core dominance. In our analysis we include measurements of the continuum luminosity and the optical-to-X-ray spectral slope, spectral properties commonly included in the suite known as "Eigenvector 1", and the full-width at half maximum, full-width at one-quarter-maximum, shape, blueshift, and equivalent width of the C IV broad emission line. We also investigate a new prescription that we recently developed for predicting the velocity line width of the H-beta broad emission line based on the velocity line width of the C IV line and the ratio of continuum subtracted peak fluxes of Si IV + O IV] at 1400 A to C IV. In addition to a correlation analysis of the ultraviolet spectral properties and radio core dominance, we provide composite spectra of edge-on and face-on sources for this sample. In particular, we highlight the orientation dependence of the velocity line width predicted for H-beta. We find that this predicted line width depends on orientation in a manner similar to the true velocity line width of H-beta, where no such dependence is observed for C IV. This is an indication that orientation information concerning the line emitting regions can be extracted from ultraviolet spectra. [abridged]

Use of spectroscopic technique to develop a reagent for Mo(VI) utilizing micellar effects on complex formation

Ultraviolet and visible spectral properties of aqueous solutions of molybdenum(VI) (Mo), gallic acid (GA), Lalanine (Ala), and L-Phenylalanine (Phe), and of their binary and ternary solutions were investigated in the absence and presence of anionic, cationic, and nonionic surfactant micelles. Evaluation of the spectra in a comparative way revealed that both Ala and Phe form ternary complexes with Mo and GA. The formation of a quaternary complex between Mo, GA, Phe, and cetyltrimethylammonium bromide at pH 4.5 provided a reagent system with a strikingly high sensitivity (1.2∙106 l/(mol∙cm)) for use in the spectrophotometric determination of Mo. A mechanism of micellar effects was discussed in terms of the substrate molecular charge and hydrophobicity, and rationalized on the basis of the spectral data obtained above and below the isoelectric pH of the amino acids.

THE FIRST MAXIMUM-LIGHT ULTRAVIOLET THROUGH NEAR-INFRARED SPECTRUM OF A TYPE Ia SUPERNOVA ,

We present the first maximum-light ultraviolet (UV) through near-infrared (NIR) Type Ia supernova (SN Ia) spectrum. This spectrum of SN 2011iv was obtained nearly simultaneously by the Hubble Space Telescope at UV/optical wavelengths and the Magellan Baade telescope at NIR wavelengths. These data provide the opportunity to examine the entire maximum-light SN Ia spectral-energy distribution. Since the UV region of a SN Ia spectrum is extremely sensitive to the composition of the outer layers of the explosion, which are transparent at longer wavelengths, this unprecedented spectrum can provide strong constraints on the composition of the SN ejecta, and similarly the SN explosion and progenitor system. SN 2011iv is spectroscopically normal, but has a relatively fast decline (Delta m_15 (B) = 1.69 +/- 0.05 mag). We compare SN 2011iv to other SNe Ia with UV spectra near maximum light and examine trends between UV spectral properties, light-curve shape, and ejecta velocity. We tentatively find that SNe with similar light-curve shapes but different ejecta velocities have similar UV spectra, while those with similar ejecta velocities but different light-curve shapes have very different UV spectra. Through a comparison with explosion models, we find that both a solar-metallicity W7 and a zero-metallicity delayed-detonation model provide a reasonable fit to the spectrum of SN 2011iv from the UV to the NIR.

A novel reagent for spectroscopic determination of Mo(VI)

AbstractA new reagent for spectrophotometric determination of Mo(VI) was developed utilizing micellar effects. For this purpose, differences in the ultraviolet and visible spectral properties of Mo(VI), gallic acid, L-serine, and their binary and ternary solutions were studied in the presence and absence of cationic, anionic, and non-ionic surface active agents. L-serine was observed to form binary complexes and a ternary complex with Mo(VI) and gallic acid below its isoelectric point. The maximum Mo(VI) sensitivity was exerted by the Mo(VI) + gallic acid + L-serine + hexadecyltrimethylammonium bromide system at pH of 4.5. This system was proposed for use in the spectrophotometric determination of Mo(VI) as a superior alternative to the Mo(VI) + gallic acid + hexadecyltrimethylammonium bromide system and to most of the instrumental analysis methods referred to in the literature. The mechanism of micellar effects was discussed on the basis of the spectral data obtained above and below the isoelectric point of L-serine and explained in terms of the molecular charge of the substrates and the surfactants.

Synthesis, Crystal Structure, and Characterization of a Novel Coordinated Polymer [Cu2I4(Nppch)2

Solution reaction of CuI and KI in DMF/H2O with a solution of Nppch in CH3OH/H2O gave rise to a three-dimensional (3D) supramolecular compound based on a binuclear [Cu2I4(Nppch)2] unit (Nppch = N-(4-pyridyl) pyridinium chloride hydrochloride). The crystal structural analysis indicated that the complex crystallized in a monoclinic space group, P2(1)/n, a = 9.6821(19) Å, b = 11.414(2) Å, c = 12.096(2) Å, β = 103.17(3)°, V = 1301.6(4) Å3, Z = 2. The complex possessed a novel three-dimensional supramolecular framework formed by hydrogen bonds among repeating [Cu2I4(Nppch)2] binuclear units. The compound was further characterized with infrared (IR) spectra, ultraviolet spectral properties, thermal analysis, and fluorescence properties.

Far ultraviolet spectral properties of Saturn’s rings from Cassini UVIS

Spectra taken by the Cassini Ultraviolet Imaging Spectrograph (UVIS) of Saturn’s C ring, B ring, Cassini Division, and A ring have been analyzed in order to characterize ring particle surface properties and water ice abundance in the rings. UVIS spectra sense the outer few microns of the ring particles. Spectra of the normalized reflectance ( I/ F) in all four regions show a characteristic water ice absorption feature near 165 nm. Our analysis shows that the fractional abundance of surface water ice is largest in the outer B ring and decreases by over a factor of 2 across the inner C ring. We calculate the mean path length of UV photons through icy ring particle regolith and the scattering asymmetry parameter using a Hapke reflectance model and a Shkuratov reflectance model to match the location of the water ice absorption edge in the data. Both models give similar retrieved values of the photon mean length, however the retrieved asymmetry ( g) values are different. The photon mean path lengths are nearly uniform across the B and A rings. Shortward of 165 nm the rings exhibit a slope that turns up towards shorter wavelengths, while the UV slope of 180/150 nm (reflectance outside the water absorption ratioed to that inside the absorption band) tracks I/ F with maxima in the outer B ring and in the central A ring. Retrieved values of the scattering asymmetry parameter show the regolith grains to be highly backscattering in the FUV spectral regime.

Synthesis and Vacuum Ultraviolet Spectral Properties of Nano-scaled Phosphors

The nano-scaled red phosphor YBO3: Eu3+, green phosphor ZnSiO4: Mn2+ and blue phosphor BaMgAl10O17: Eu2+ were synthesized by wet-chemical techniques. The morphologies and spectral properties of the three nano-phosphors under 147 nm excituation were investigated. For YBO3: Eu3+, nano-sheets was obtained by solvent-thermal process, which reached 78.8% of the commercial red phosphor on emission intensity and exhibited better color purity than the latter. For ZnSiO4: Mn2+, different morphologies were obtained by hydrothermal method with varying ratio of CTAB to TEOS, among which the nano-spheres presented the strongest emission intensity and reached 86% of that of the commercial green phosphor. For BaMgAl10O17: Eu2+, nano-rods were acquired using sol-gel process, which exhibited 78.15% of the commercial blue phosphor on emission intensity and the low y value of color coordinates, which indicated that the nano-rods were efficient for restricting the deteriorate during application.

Ultraviolet spectral reflectance properties of common planetary minerals

Ultraviolet spectral reflectance properties (200–400 nm) of a large number of minerals known or presumed to exist on the surfaces of Mars, the Moon, and asteroids, and in many meteorites, were investigated. Ultraviolet reflectance spectra (200–400 nm) of these minerals range from slightly blue-sloped (reflectance decreasing toward longer wavelengths) to strongly red-sloped (reflectance increasing toward longer wavelengths). Most exhibit one or two absorption features that are attributable to FeO charge transfers involving Fe3+ or Fe2+. The UV region is a very sensitive indicator of the presence of even trace amounts (<0.01 wt%) of Fe3+ and Fe2+. The major Fe3+O absorption band occurs at shorter wavelengths (∼210–230 nm), and is more intense than the major Fe2+O absorption band (∼250–270 nm). Ti-bearing minerals, such as ilmenite, rutile and anatase exhibit UV absorption bands attributable to Ti4+O charge transfers. While the positions of metal–O charge transfer bands sometimes differ for different minerals, the variation is often not diagnostic enough to permit unique mineral identification. However, iron oxides and oxyhydroxides can generally be distinguished from Fe-bearing silicates in the 200–400 nm region on the basis of absorption band positions. Within a given mineral group (e.g., low-calcium pyroxene, olivine, plagioclase feldspar), changes in Fe2+ or Fe3+ abundance do not appear to result in a measurable change in absorption band minima positions. Absorption band positions can vary as a function of grain size, however, and this variation is likely due to band saturation effects. The intensity of metal–O charge transfers means that some minerals will exhibit saturated UV absorption bands even for fine-grained (<45 μm) powders. In cases where absorption bands are not saturated (e.g., Fe2+O bands in some plagioclase feldspars and pyroxenes), changes in Fe2+ content do not appear to cause variations in band position. In other minerals (e.g., olivine), changes in band positions are correlated with compositional and/or grain size variations, but this is likely due to increasing band saturation rather than compositional variations. Overall, we find that the UV spectral region is sensitive to different mineral properties than longer wavelength regions, and thus offers the potential to provide complementary capabilities and unique opportunities for planetary remote sensing.

Verifying the Cosmological Utility of Type Ia Supernovae: Implications of a Dispersion in the Ultraviolet Spectra

We analyze the mean rest-frame ultraviolet (UV) spectrum of Type Ia Supernovae (SNe Ia) and its dispersion using high signal-to-noise Keck-I/LRIS-B spectroscopy for a sample of 36 events at intermediate redshift (z=0.5) discovered by the Canada-France-Hawaii Telescope Supernova Legacy Survey (SNLS). We introduce a new method for removing host galaxy contamination in our spectra, exploiting the comprehensive photometric coverage of the SNLS SNe and their host galaxies, thereby providing the first quantitative view of the UV spectral properties of a large sample of distant SNe Ia. Although the mean SN Ia spectrum has not evolved significantly over the past 40% of cosmic history, precise evolutionary constraints are limited by the absence of a comparable sample of high quality local spectra. Within the high-redshift sample, we discover significant UV spectral variations and exclude dust extinction as the primary cause by examining trends with the optical SN color. Although progenitor metallicity may drive some of these trends, the variations we see are much larger than predicted in recent models and do not follow expected patterns. An interesting new result is a variation seen in the wavelength of selected UV features with phase. We also demonstrate systematic differences in the SN Ia spectral features with SN light curve width in both the UV and the optical. We show that these intrinsic variations could represent a statistical limitation in the future use of high-redshift SNe Ia for precision cosmology. We conclude that further detailed studies are needed, both locally and at moderate redshift where the rest-frame UV can be studied precisely, in order that future missions can confidently be planned to fully exploit SNe Ia as cosmological probes [ABRIDGED].