Miracle-dz/UniFAR-FTUs huggingface dataset:
Compression Studies of Single-Crystal SnO2 and PbO2 in a Diamond Cell

Compression behaviors of two single-crystal rutile-structure dioxides, SnO2 (cassiterite) and PbO2 (plattnerite), were studied in a Merrill-Bassett type diamond cell at room temperature. The samples were compressed in a mixture of 4:1 methanolethenol solution with pressure measurements by the ruby scale. A four-circle diffractometer was used to obtain the diffraction patterns of these crystals at high pressures. Compression results on Sn02 did not show significant lattice distortion, with a slight increase in c/a up to 35 kbar. The compression data are in excellent agreement with Hazen and Finger (1981) and in reasonable agreement with Ming and Manghnani (1982). Fitting these data to the Birch-Murnaghan equation gives a bulk modulus (K。 ) of 2.24±0.08 Mbar with K。 ' =6.3. On the other hand, the rutile-type PbO2 was found to transform from a tetragonal to an orthorhombic phase above 5 kbar. The cell parameters a, b and c of this phase have different linear compressibility. This phase is different from the reported orthorhombic phases of lead dioxides (α-PbO2). It could represent an intermediate distorted phase which occurs during the transformation from the β-PbO2 to the α-PbO2 phase. The bulk modulus of Pb02 was determined to be 1.34±0.06 Mbar by fitting the data to the Birch-Murnaghan equation. A linear relationship was found to exist between the bulk sound velocity and mean atomic weight of the rutile-type dioxides.
Evidence for very large-scale coherent orientations of quasar polarization vectors

On the basis of a new sample of quasar optical po- larization measurements, we have found that, in a region of the sky, the quasar polarization vectors are not randomly oriented as naturally expected, but appear concentrated around one pref- erential direction. In order to verify this surprising although preliminary re- sult, we have compiled a large sample of quasar polarization measurements from the literature. With quite severe criteria to eliminate at best the contamination by our Galaxy, a sample of 170 quasars with good quality polarization measurements has been dened. Maps in redshift slices reveal a few regions where the polarization vectors are apparently aligned. To handle the problemmorequantitatively,non-parametric3Dstatisticaltests were designed, as well as a method for visualizing spatially the results. The signicance is evaluated through Monte-Carlo sim- ulations. Applied to our sample of 170 polarized quasars, two differ- ent statistical tests provide evidence, with signicance levels of 0.005 and 0.015 respectively, that the optical polarization vec- tors of quasars are not randomly distributed over the sky but are coherentlyorientedonverylargespatialscales.Thisorientation effectappearsspatiallydelimitedinthe3DUniverse,mainlyoc- curinginafewgroupsof10-20objects.Thepolarizationvectors of objects located along the same line of sight but at different redshifts do not appear accordingly aligned. Essentially for this reason, instrumental bias and contamination by interstellar po- larization in our Galaxy are unlikely to be responsible for the observed effect. The very large scale at which this local orientation effect is observed indicates the presence of correlations in objects or elds on spatial scales 1000h 1 Mpc at redshifts z ' 1-2,
Ophiolitic rocks of the Indo-Myanmar Ranges, NE India: relicts of an inverted and tectonically imbricated hyper-extended continental margin basin?

Abstract The Indo-Myanmar Ranges (IMR) of NE India are host to various ophiolitic rocks, including metamorphosed Alpine-type harzburgite and lherzolite. Compared to abyssal peridotites of normal oceanic lithosphere, these ultramafic rocks are enriched in trace and rare earth elements. Spilitic pillow lavas along with mafic dykes and sills locally intruded into the serpentinized ultramafic rocks and associated pelagic sediments exhibit alkaline compositional affinities. Ophiolite formation and emplacement were by a process analogous to that described for mantle exhumation in hyper-extended continental margin settings and ophiolites in parts of the European Alps, involving very slow passive continental margin rifting accompanied by slow upwelling or extensional unroofing of the subcontinental upper mantle up to the seafloor. Preliminary palaeomagnetic measurements conducted on ultramafic rocks within the IMR ophiolite belt give a virtual geomagnetic pole (VGP) at 47° N, 045° E for thermal demagnetization (TDM) measurements and 33° N, 013° E for the alternating field demagnetization (AfD) measurements, requiring an anticlockwise rotation of the ultramafic bodies by 14° during the subduction process. The original trend of the spreading axis of the ophiolites was probably NE–SW, with spreading directed NW–SE. Computation of palaeolatitude of the ultramafic rocks gives an average value of 24.67°. Comparison between the palaeolatitude and the present latitude of the sample sites provides a mere latitudinal shift of less than 1°. Field studies, combined with an analysis of structural and tectonic features in the IMR, suggest a generalized WNW–ESE (east–west) compression and NNE–SSW (north–south) extension contradictory to the NNE–SSW contraction indicated by seismic data. Area balancing techniques employed along sections orientated perpendicular to regional tectonic strike in the IMR reveal systematic variations in the amount of crustal shortening, with a maximum of approximately 60% recorded in the Nagaland–Manipur segment along 25.644° N, 93.826° E–25.076° N, 95.897° E. The amount of shortening gradually decreases away from the axis of maximum shortening and on both sides. Calculations of relative plate motion based on rotation vectors given by different workers for various plate pairs represented in the region reveal that the interaction between the Indian and Myanmar plates can ideally produce the structural and tectonic features of this range. Dextral shear coupled to oblique subduction of the Indian Plate below the Myanmar Plate can best explain all of the structural and tectonic features present in the IMR.
Mercury bioaccumulation in remote subalpine lakes : assessing the influence of invasive trout on salamanders

approved: ______________________________________________________ Collin A. Eagles-Smith Mercury (Hg) contamination is a global conservation threat to freshwater ecosystems, detected in even the protected lakes of Olympic National Park (Washington, USA). Although considered some of the most remote and pristine US ecosystems, these lakes are currently subject to multiple environmental stressors, including climate change and fish introductions; adding contaminants, such as Hg, could exacerbate the effects of these stressors on native species. Amphibians are undergoing large worldwide declines, which include declines in protected areas, such as our National Parks. Our goal is to better understand the effect of historically stocked fish in Olympic National Park on native amphibian Hg bioaccumulation. To minimize the need for lethal sampling of this already threatened group, we first examine how Hg concentrations in non-lethally sampled amphibian tissues correlated with whole-body Hg concentrations, depending on species and the different type of non-lethal tissue sample used. Second, we aimed to understand how a food web altered by fish impacted Hg bioaccumulation in native species. We measured Hg and stable isotopes of carbon and nitrogen in organisms across trophic levels from 18 subalpine lakes. We detected small shifts in salamander food web indices and minor changes to salamander Hg concentration associated with the presence of fish. Importantly, we found increased mercury trophic magnification slopes in lakes with fish compared to fishless lakes. This research provides evidence that historic fish introductions can elevate mercury exposure in pristine ecosystems compared to natural fishless lakes. ©Copyright by Adam Pfleeger February 23, 2015 All Rights Reserved Mercury Bioaccumulation in Remote Subalpine Lakes: Assessing the Influence of Invasive Trout on Salamanders
Bacterial population in intensive tilapia (Oreochromis niloticus) culture pond sediment in Hai Duong province, Vietnam

Three intensive tilapia ponds were studied to determine the bacterial population during the culture period in Hai Duong province, Vietnam. Bacteria were identified to genus or species level. Total bacteria count in sediment ranged from 6.49 × 105 to 1.29 × 106 cfu g-1. In total, 11 bacterial genera and 13 species were identified from pond sediments, in which both gram-negative and gram-positive rod-shaped bacteria dominated the population accounting for 52 and 48%, respectively. Both beneficial and harmful bacteria were found in sediments, in which the harmful bacterial species dominated (62.5%) and appeared more at the beginning of culture. The harmful bacteria were Pseudomonas fluorescens, Pseudomonas sp. , Vibrio pectenicida, Enterococcus, sp.HD31, Enterococcus sp.HD1, Vibrio damsella, Aeromonas sp.HD5, Vibrio sp. HD7, Vibrio sp.HD331, Aeromonas sp.HD361, Enterococcus sp.HD371, Vibrio sp.V31, Aeromonas hydrophyla and Pseudomonas putida. In contrast, beneficial bacteria accounted for 20.8% only of total isolates. The beneficial bacteria were Carnobacterium inhibens, Lactobacillus plantarum, Bacillus cereus, Lactobacillus delbrueckii and Bacillus pumilus; they appeared more in the later stage of culture period. Key words: Bacteria, Oreochromis niloticus, intensive culture pond, sediment, beneficial bacteria, harmful bacteria.
Evolution of the longitudinal and azimuthal structure of the near-side jet peak in Pb-Pb collisions at root s(NN)=2.76 TeV

In two-particle angular correlation measurements, jets give rise to a near-side peak, formed by particles associated to a higher- p T trigger particle. Measurements of these correlations as a function of pseudorapidity ( (cid:2)η ) and azimuthal ( (cid:2)ϕ ) differences are used to extract the centrality and p T dependence of the shape of the near-side peak in the p T range 1 < p T < 8 GeV /c in Pb-Pb and pp collisions at √ s NN = 2.76 TeV. A combined ﬁt of the near-side peak and long-range correlations is applied to the data and the peak shape is quantiﬁed by the variance of the distributions. While the width of the peak in the (cid:2)ϕ direction is almost independent of centrality, a signiﬁcant broadening in the (cid:2)η direction is found from peripheral to central collisions. This feature is prominent for the low- p T region and vanishes above 4 GeV /c . The widths measured in peripheral collisions are equal to those in pp collisions in the (cid:2)ϕ direction and above 3 GeV /c in the (cid:2)η direction. Furthermore, for the 10% most central collisions and 1 < p T , assoc < 2 GeV /c , 1 < p T , trig < 3 GeV /c , a departure from a Gaussian shape is found: a depletion develops around the center of the peak. The results are compared to A Multi-Phase Transport (AMPT) model simulation as well as other theoretical calculations indicating that the broadening and the development of the depletion are connected to the strength of radial and longitudinal ﬂow.
Residence, Resorption and Recycling of Zircons in Devils Kitchen Rhyolite, Coso Volcanic Field, California

Zircons from the Devils Kitchen rhyolite in the Pleistocene Coso Volcanic field, California have been analyzed by in situ Pb/U ion microprobe (SHRIMP-RG) and by detailed cathodoluminescence imaging. The zircons yield common-Pb-corrected and disequilibrium-corrected Pb/U ages that predate a previously reported K–Ar sanidine age by up to 200 kyr, and the range of ages exhibited by the zircons is also approximately 200 kyr. Cathodoluminescence imaging indicates that zircons formed in contrasting environments. Most zircons are euhedral, and a majority of the zircons are weakly zoned, but many also have anhedral, embayed cores, with euhedral overgrowths and multiple internal surfaces that are truncated by later crystal zones. Concentrations of U and Th vary by two orders of magnitude within the zircon population, and by 10–20 times between zones within some zircon crystals, indicating that zircons were transferred between contrasting chemical environments. A zircon saturation temperature of 750 C overlaps within error a previously reported phenocryst equilibration temperature of 740 25 C. Textures in zircons indicative of repeated dissolution and subsequent regrowth are probably caused by punctuated heating by mafic magma input into rhyolite. The overall span of ages and large variation in U and Th concentrations, combined with calculated zircon saturation temperatures and resorption times, are most compatible with crystallization in magma bodies that were emplaced piecemeal in the crust at Coso over 200 kyr prior to eruption, and that were periodically rejuvenated or melted by subsequent basaltic injections.
HUBBL E SPACE T EL ESCOPE IMAGING OF THE CFRS AND LDSS REDSHIFT SURVEYS.

We analyze Hubble Space Telescope images of a complete sample of 341 galaxies drawn from the CFRS and LDSS ground-based redshift surveys. In this, the -rst paper in the series, each galaxy has been morphologically classi-ed according to a scheme similar to that developed for the Medium Deep Survey. We discuss the reproducibility of these classi-cations and quantify possible biases that may arise from various redshift-dependent e†ects. We then discuss automated classi-cations of the sample and con- clude, from several tests, that we can expect an apparent migration with redshift to later Hubble types that corresponds to a misclassi-cation in our adopted machine classi-cation system of D24% ^ 11 of the true "" spirals II as "" peculiars II at a redshift z ^ 0.9. After allowing for such biases, the redshift dis- tribution for normal spirals, together with their luminosity function derived as a function of redshift, indicates approximately 1 mag of luminosity evolution in by z ^ 1. The elliptical sample is too small B AB for precise evolutionary constraints. However, we -nd a substantial increase in the proportion of galaxies with irregular morphology at large redshift from 9% ^ 3% for 0.3 " z " 0.5 to 32% ^ 12% for 0.7 " z " 0.9. These galaxies also appear to be the dominant cause of the rapid rise with redshift in the blue luminosity density identi-ed in the redshift surveys. Although galaxies with irregular morphology may well comprise a mixture of di†erent physical systems and might not correspond to present-day irregulars, it is clear that the apparently declining abundance and luminosities of our distant "" irregulars II holds an important key to understanding recent evolution in the star formation history of normal galaxies. Subject headings: galaxies: fundamental parameters E galaxies: structure E surveys
Model Adaptation for Sentence Unit Segmentation from Speech Model Adaptation for Sentence Unit Segmentation from Speech

The sentence segmentation task is a classification task that aims at inserting sentence boundaries in a sequence of words. One of the applications of sentence segmentation is to detect the sentence boundaries in the sequence of words that is output by an automatic speech recognition system (ASR). The purpose of correctly finding the sentence boundaries in ASR transcriptions is to make it possible to use further processing tasks, such as automatic summarization, machine translation, and information extraction. Being a classification task, sentence segmentation requires training data. To reduce the labor-intensive labeling task, available labeled data can be used to train the classifier. The high variability of speech among the various speech styles makes it inefficient to use the classifier from one speech style (designated as out-of-domain) to detect sentence boundaries on another speech style (in-domain) and thus, makes it necessary for one classifier to be adapted before it is used on another speech style. In this work, we first justify the need for adapting data among the broadcast news, conversational telephone and meeting speech styles. We then propose methods to adapt sentence segmentation models trained on conversational telephone speech to meeting conversations style. Our results show that using the model adapted from the telephone conversations, instead of the model trained only on meetings conversation style, significantly improves the performance of the sentence segmentation. Moreover, this improvement holds independently from the amount of in-domain data used. In addition, we also study the differences between speech styles, with statistical measures and by examining the performances of various subsets of features. Focusing on broadcast news and meeting speech style, we show that on the meeting speech style, lexical features are more correlated with the sentence boundaries than the prosodic features, whereas it is the contrary on the broadcast news. Furthermore, we observe that prosodic features are more independent from the speech style than lexical features.
The chemical composition of the Orion star forming region - III. C, N, Ne, Mg, and Fe abundances in B-type stars revisited

Context. Early B-type stars are invaluable indicators of elemental abundances of their birth environments. In contrast to the surrounding neutral interstellar matter (ISM) and H ii regions, their chemical composition is unaffected by depletion onto dust grains and the derivation of different abundances from recombination and collisional lines. In combination with ISM or nebular gas-phase abundances, they facilitate the otherwise inaccessible dust-phase composition to be constrained. Aims. We determine precise abundances of C, N, Mg, Ne, and Fe in early B-type stars in the Orion star-forming region to: a) review previous determinations using a self-consistent quantitative spectral analysis based on modern stellar atmospheres and recently updated model atoms; b) complement our previous results for oxygen and silicon; and c) establish an accurate and reliable set of stellar metal abundances to constrain the dust-phase composition of the Orion H ii region. Methods. A detailed, self-consistent spectroscopic study of a sample of 13 narrow-lined B0 V-B2 V stars in Ori OB1 is performed. High-quality spectra obtained with FIES at the NOT are analysed using both a hybrid non-local thermodynamic equilibrium (nonLTE) method (i.e., classical line-blanketed LTE model atmospheres and non-LTE line formation) and line-profile fitting techniques, validating the approach by comparison with previous results obtained using line-blanketed non-LTE model atmospheres and a curveof-growth analysis. Results. The two independent analysis strategies provide consistent results for basic stellar parameters and the abundances of oxygen and silicon. The extended analysis to C, N, Mg, Ne, and Fe finds a high degree of chemical homogeneity, with the 1σ-scatter typically being 0.03−0.07 dex around the mean for the various elements. The present-day abundances of B-type stars in Ori OB1 are compatible at similar precision with cosmic abundance standard values as recently established from early-type stars in the solar neighbourhood and also with the Sun.
Inventering av marina makroalger i Halland 1997: Lilla Middelgrund

Makroalgfloran vid Lilla Middelgrund i mellersta Kattegatt har inventerats under sommaren 1997. Omradet bestar av en grundplata belaget i utsjon ca 20 km fran svenska kusten. Genom det relativt sto .
The Luminosity Function of X-Ray-selected Active Galactic Nuclei: Evolution of Supermassive Black Holes at High Redshift

We present a measure of the hard (2-8 keV) X-ray luminosity function (XLF) of AGNs up to z ∼ 5. At high redshifts, the wide area coverage of the Chandra Multiwavength Project is crucial to detect rare and luminous (LX > 1044 ergs s−1) AGNs. The inclusion of samples from deeper published surveys, such as the Chandra Deep Fields, allows us to span the lower LX range of the XLF. Our sample is selected from both the hard (z < 3, f2–8 keV > 6.3 × 10−16 ergs cm −2 s−1) and soft (z > 3, f0.5–2.0 keV > 1.0 × 10−16 ergs cm −2 s−1) energy band detections. Within our optical magnitude limits (r′, i′ < 24), we achieve an adequate level of completeness (>50%) regarding X-ray source identification (i.e., redshift). We find that the luminosity function is similar to that found in previous X-ray surveys up to z ∼ 3 with an evolution dependent on both luminosity and redshift. At z > 3, there is a significant decline in the numbers of AGNs with an evolution rate similar to that found by studies of optically selected QSOs. Based on our XLF, we assess the resolved fraction of the cosmic X-ray background, the cumulative mass density of SMBHs, and the comparison of the mean accretion rate onto SMBHs and the star formation history of galaxies as a function of redshift. A coevolution scenario up to z ∼ 2 is plausible, although at higher redshifts the accretion rate onto SMBHs drops more rapidly. Finally, we highlight the need for better statistics of high-redshift AGNs at z ≳ 3, which is achievable with the upcoming Chandra surveys.
Matrix Model For Polyakov Loops, String Field Theory In The Temporal Gauge, And Winding String Condensation In Anti-de Sitter Space

It has recently been shown that the low energy dynamics of the large $N$ gauge theory on $S^3$ at finite temperature reduces to a one-matrix model, where the matrix is given by the holonomy of the gauge field around the Euclidean time direction compactified on a circle. On the other hand, there is a prescription for constructing a closed string field theory in the temporal gauge from a given one-matrix model via loop equations. I identify the closed string field theory in the temporal gauge constructed from the above matrix model as effective closed string field theory that describes the propagations of closed strings in the radial and Euclidean time directions in the bulk. Then I argue that a coherent state in this string field theory describes winding string condensation, which has been expected to cause the topology change from the thermal AdS geometry to the AdS-Schwarzschild black hole geometry.
Initial fields and instability in the classical model of the heavy-ion collision

Color Glass Condensate (CGC) provides a classical description of dense gluon matter at high energies. Using the McLerran-Venugopalan (MV) model we calculate the initial energy density \epsilon(\tau) in the early stage of the relativistic nucleus-nucleus collision. Our analytical formula reproduces the quantitative results from lattice discretized simulations and leads to an estimate \epsilon(\tau=0.1fm)=40-50GeV/fm^3 in the Au-Au collision at RHIC energy. We then formulate instability with respect to soft fluctuations that violate boost invariance inherent to hard CGC backgrounds. We find unstable modes arising as a result of ensemble average over the initial CGC fields.