Miracle-dz/UniFAR-FTUs huggingface dataset:
The VIMOS Public Extragalactic Redshift Survey (VIPERS) A precise measurement of the galaxy stellar mass function and the abundance of massive galaxies at redshifts 0.5

We measure the evolution of the galaxy stellar mass function from z = 1.3 to z = 0.5 using the first 53 608 redshifts of the ongoing VIMOS Public Extragalactic Survey (VIPERS). Thanks to its large volume and depth, VIPERS provides a detailed picture of the galaxy distribution at z ≃ 0.8, when the Universe was ≃7 Gyr old. We carefully estimate the uncertainties and systematic effects associated with the SED fitting procedure used to derive galaxy stellar masses. We estimate the galaxy stellar mass function at several epochs between z = 0.5 and 1.3, discussing the amount of cosmic variance affecting our estimate in detail. We find that Poisson noise and cosmic variance of the galaxy mass function in the VIPERS survey are comparable to the statistical uncertainties of large surveys in the local universe. VIPERS data allow us to determine with unprecedented accuracy the high-mass tail of the galaxy stellar mass function, which includes a significant number of galaxies that are too rare to detect with any of the past spectroscopic surveys. At the epochs sampled by VIPERS, massive galaxies had already assembled most of their stellar mass. We compare our results with both previous observations and theoretical models. We apply a photometric classification in the (U − V) rest-frame colour to compute the mass function of blue and red galaxies, finding evidence for the evolution of their contribution to the total number density budget: the transition mass above which red galaxies dominate is found to be about 1010.4 ℳ⊙ at z ≃ 0.55, and it evolves proportionally to (1 + z)3. We are able to separately trace the evolution of the number density of blue and red galaxies with masses above 1011.4 ℳ⊙, in a mass range barely studied in previous work. We find that for such high masses, red galaxies show a milder evolution with redshift, when compared to objects at lower masses. At the same time, we detect a population of similarly massive blue galaxies, which are no longer detectable below z = 0.7. These results show the improved statistical power of VIPERS data, and give initial promising indications of mass-dependent quenching of galaxies at z ≃ 1.
IMAGING AND SPECTROSCOPIC OBSERVATIONS OF A TRANSIENT CORONAL LOOP: EVIDENCE FOR THE NON-MAXWELLIAN κ-DISTRIBUTIONS

We report on the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) and Hinode/EUV Imaging Spectrograph (EIS) observations of a transient coronal loop. The loop brightens up in the same location after the disappearance of an arcade formed during a B8.9-class microflare 3 hr earlier. EIS captures this loop during its brightening phase, as observed in most of the AIA filters. We use the AIA data to study the evolution of the loop, as well as to perform the differential emission measure (DEM) diagnostics as a function of κ. The Fe xi–Fe xiii lines observed by EIS are used to perform the diagnostics of electron density and subsequently the diagnostics of κ. Using ratios involving the Fe xi 257.772 Å self-blend, we diagnose κ ≲ 2, i.e., an extremely non-Maxwellian distribution. Using the predicted Fe line intensities derived from the DEMs as a function of κ, we show that, with decreasing κ, all combinations of ratios of line intensities converge to the observed values, confirming the diagnosed κ ≲ 2. These results represent the first positive diagnostics of κ-distributions in the solar corona despite the limitations imposed by calibration uncertainties.
Power Equipment Fault Diagnosis Method Based on Energy Spectrogram and Deep Learning

With the development of industrial manufacturing intelligence, the role of rotating machinery in industrial production and life is more and more important. Aiming at the problems of the complex and changeable working environment of rolling bearings and limited computing ability, fault feature information cannot be effectively extracted, and the current deep learning model is difficult to be compatible with lightweight and high efficiency. Therefore, this paper proposes a fault detection method for power equipment based on an energy spectrum diagram and deep learning. Firstly, a novel two-dimensional time-frequency feature representation method and energy spectrum feature map based on wavelet packet transform is proposed, and an energy spectrum feature map dataset is made for subsequent diagnosis. This method can realize multi-resolution analysis, fully extract the feature information contained in the fault signal, and accelerate the convergence of the subsequent diagnosis model. Secondly, a lightweight residual dense convolutional neural network model (LR-DenseNet) is proposed. This model combines the advantages of residual learning and a dense connection, and can not only extract deep features more easily, but can also effectively use shallow features. Then, based on the lightweight residual dense convolutional neural network model, an LR-DenseSENet model is proposed. By introducing the transfer learning strategy and adding the channel domain, an attention mechanism is added to the channel feature fusion layer, with the accuracy of detection up to 99.4%, and the amount of parameter calculation greatly reduced to one-fifth of that of VGG. Finally, through an experimental analysis, it is verified that the fault detection model designed in this paper based on the combination of an energy spectrum feature map and LR-DenseSENet achieves a satisfactory detection effect.
Preparation and characterization of a spherical Cu/Mn/Ce ternary nanocomposite oxide with high adsorption efficiency of tetracycline

Tetracycline (TC) is a new eco toxic antibiotic, which is easy to cause bacterial drug resistance. Considering this, tetracycline in water needs to be removed. In this paper, a Cu/Mn/Ce oxide composite were prepared by a simple coprecipitation method and used as a new and efficient adsorbent to remove tetracycline from water. The morphology and microstructure of the adsorbent were characterized by scanning electron microscopy, energy-dispersive X-ray spectroscopy, Fourier-transform infrared spectroscopy, X-ray photoelectron spectroscopy, Brunauer–Emmett– Teller, X-ray diffraction and zeta potential. The effects of adsorption isotherm, kinetics, molar ratio, initial concentration and pH value of TC solution were studied. The results show that the adsorption capacity towards TC solution is the highest when the molar ratio of Cu/Mn/Ce is 1:1:3, according to the Langmuir isotherm model. The maximum adsorption capacity is 344.83 mg/g. The maximum removal rate is 99.97% at pH = 7, and the adsorption kinetics conforms to the qua- si-second-order model. The adsorption capacity of Cu/Mn/Ce is basically unchanged after three cycles, and the removal rate is still as high as 91%.
Species Traits and Geomorphic Setting as Drivers of Global Soil Carbon Stocks in Seagrass Meadows

Our knowledge of the factors that can influence the stock of organic carbon (OC) that is stored in the soil of seagrass meadows is evolving, and several causal effects have been used to explain the variation of stocks observed at local to national scales. To gain a global‐scale appreciation of the drivers that cause variation in soil OC stocks, we compiled data on published species‐specific traits and OC stocks from monospecific and mixed meadows at multiple geomorphological settings. Species identity was recognized as an influential driver of soil OC stocks, despite their large intraspecific variation. The most important seagrass species traits associated with OC stocks were the number of leaves per seagrass shoot, belowground biomass, leaf lifespan, aboveground biomass, leaf lignin, leaf breaking force and leaf OC plus the coastal geomorphology of the area, particularly for lagoon environments. A revised estimate of the global average soil OC stock to 20 cm depth of 15.4 Mg C ha−1 is lower than previously reported. The largest stocks were still recorded in Mediterranean seagrass meadows. Our results specifically identify Posidonia oceanica from the Mediterranean and, more generally, large and persistent species as key in providing climate regulation services, and as priority species for conservation for this specific ecosystem service.
Sunrise: INSTRUMENT, MISSION, DATA, AND FIRST RESULTS

The Sunrise balloon-borne solar observatory consists of a 1 m aperture Gregory telescope, a UV filter imager, an imaging vector polarimeter, an image stabilization system, and further infrastructure. The first science flight of Sunrise yielded high-quality data that revealed the structure, dynamics, and evolution of solar convection, oscillations, and magnetic fields at a resolution of around 100 km in the quiet Sun. After a brief description of instruments and data, the first qualitative results are presented. In contrast to earlier observations, we clearly see granulation at 214 nm. Images in Ca ii H display narrow, short-lived dark intergranular lanes between the bright edges of granules. The very small-scale, mixed-polarity internetwork fields are found to be highly dynamic. A significant increase in detectable magnetic flux is found after phase-diversity-related reconstruction of polarization maps, indicating that the polarities are mixed right down to the spatial resolution limit and probably beyond.
Reconstructing Phylogenies Using Branch-Variable Substitution Models and Unaligned Biomolecular Sequences: A Performance Study and New Resampling Method

In many clades in the Tree of Life, nucleotide substitution rates and base frequencies are hypothesized to have changed as genome evolution unfolded over time. Rigorous testing of this hypothesis relies on accurate phylogenetic reconstruction under suitable models of biomolecular sequence evolution. By far the most common approach for phylogenetic reconstruction is a "two-phase" analysis, where unaligned biomolecular sequence data are first aligned, and the resulting multiple sequence alignment (MSA) is used as input to downstream phylogenetic reconstruction. For a traditional "homogeneous" substitution model that is fixed across a species phylogeny, it has long been established that accurate phylogenetic inference and learning requires accurate upstream multiple sequence alignments. But the same question has not been carefully studied for "heterogeneous" models of substitution processes that can vary across the branches of a phylogeny. We therefore conducted a comprehensive performance study to quantify the impact of upstream MSA estimation error on downstream phylogenetic inference and learning under branch-variable models of nucleotide substitution. Across model conditions with either 10 or 20 taxa and spanning a range of evolutionary divergence, we find a consistent and significantly positive association between upstream and downstream estimation error. The relationship is robust to the choice of MSA estimation method as well as substitution model mis-specification. We further quantify the relatively large contribution of upstream MSA estimation error to downstream phylogenetic reconstruction quality, compared to other experimental factors. We also conducted an empirical study of flowering monocots. Phylogenetic analyses of orthologous genes in the clade confirm the simulation study findings, and species tree estimation using branch-variable substitution models reveals new insights into sequence evolution heterogeneity. Our findings underscore several key gaps in the state of the art, including the need for MSA-aware phylogenetic inference and learning methods under heterogeneous models of sequence evolution. To this end, we introduce a new computational method, NoHTS ("Non-Homogeneous Tree Support"), to directly assess phylogenetic estimation uncertainty due to MSA estimation error and other factors. The new method uses sequence-aware statistical resampling to place confidence intervals on a phylogeny estimated under a branch-variable substitution model. We demonstrate its superior type I and type II error versus a de facto standard in phylogenetic and phylogenomic studies - the phylogenetic bootstrap method.
Thermo-Optical Control of Raman Solitons in a Functionalized Silica Microsphere

The investigation of optical microcavity solitons is in demand both for applications and basic science. Despite the tremendous progress in the study of microresonator solitons, there is still no complete understanding of all features of their nonlinear dynamics in various regimes. Controlling soliton properties is also of great interest. We proposed and investigated experimentally and theoretically a simple and easily reproducible way to generate Raman solitons with controllable spectral width in an anomalous dispersion region in a functionalized silica microsphere with whispering gallery modes (WGMs) driven in a normal dispersion regime. To functionalize the microsphere, coating (TiO2 + graphite powder) was applied at the pole. The coating is used for effective thermalization of the radiation of an auxiliary laser diode launched through the fiber stem holding the microsphere to control detuning of the pump frequency from exact resonance due to the thermo-optical shift of the WGM frequencies. We demonstrated that the thermo-optical control by changing the power of an auxiliary diode makes it possible to switch on/off the generation of Raman solitons and control their spectral width, as well as to switch Raman generation to multimode or single-mode. We also performed a detailed theoretical analysis based on the Raman-modified Lugiato–Lefever equation and explained peculiarities of intracavity nonlinear dynamics of Raman solitons. All experimental and numerically simulated results are in excellent agreement.
THE PROGENITOR OF THE FUor-TYPE YOUNG ERUPTIVE STAR 2MASS J06593158–0405277

Only a dozen confirmed FU Orionis-type young outbursting stars (FUors) are known today; this explains the interest in the recent FUor eruption of 2MASS J06593158–0405277. Its outburst and expected decline will be subject to numerous studies in the future. Almost equally important for the understanding of the eruption mechanism, however, is the physical characterization of the FUor’s precursor. Here we analyze unpublished archival data and summarize—and partly revise—all relevant photometry from optical to submillimeter wavelengths. Our analysis implies that the FUor is possibly associated with eight T Tauri star candidates and a strong Class 0 source. Adopting a distance of 450 pc for the FUor, we derive a quiescent bolometric luminosity and temperature of L bol ? > = 4.8 L ⊙ ? > and T bol ? > = 1190 K, typical for young Class II sources. The central star has a temperature of T eff ? > = 4000 K, a mass of 0.75 M ⊙ ? > , and an age of about 6 × 105 yr. The SED implies a circumstellar mass of 0.01–0.06 M ⊙ ? > , and the system is surrounded by a faint infrared nebulosity. Our results provide an almost complete picture of a FUor progenitor, supporting the interpretation of future post-outburst studies.
THE IONIZATION STRUCTURE OF SHARPLESS 2-264: MULTIWAVELENGTH OBSERVATIONS OF THE λ Ori H II REGION

We present velocity-resolved maps taken with the Wisconsin H-Alpha Mapper (WHAM) in Hα, [S ii] λ 6716 , and [N ii] λ 6583 around the well-known O8 III star λ Ori A (HD 36861) ( ℓ = 185 ° to 205 ° , b = − 24 ° to − 1 ° ). The integrated intensity ( v LSR = − 80 to +80 km s−1), I H α , within WHAM’s one-degree beams varies from ∼190 R near the center to ∼10 R on the periphery of the nebula where it becomes comparable to foreground and/or background emission in this complex region. Intensity ratios for [N ii]/Hα and [S ii]/Hα average 0.28 and 0.35, respectively. In both ratios, higher values are found preferentially at larger radii from λ Ori, although the behavior of [N ii]/Hα is complicated near the edges of the nebula. The [S ii]/[N ii] intensity ratio ranges from ∼0.5 to ∼1.0, with the value increasing toward larger radii (and lower Hα intensities). Variations of the [S ii]/Hα, [N ii]/Hα, and [S ii]/[N ii] line ratios in this diffuse region show some similar trends to those seen in the warm ionized medium (WIM) but with generally lower metal-line ratios. As with the WIM, the trends are driven by changes in the underlying physical parameters, most notably the ionization states and gas temperature. To investigate which cause might be dominant in this region, we use these extremely high signal-to-noise observations to construct a map of temperature and non-thermal velocity throughout the nebula. Using the line widths of Hα and [S ii], we separate thermal and non-thermal components and find spatial trends of these parameters within the nebula. Ion temperatures range between 4000 and 8000 K throughout the nebula. The non-thermal velocity map reveals a decrease in velocity from about 10 to 5 km s−1 from the center to the edge of the lower half of the H ii region. In addition to using the widths as a measure of temperature, we also use the variation in [N ii]/Hα to estimate electron temperature. The results obtained from this diffuse H ii region around λ Ori can be compared to studies of the WIM to provide important insight into the nature of the diffuse ionized gas throughout the disk and halo of the Galaxy.
A Needs Learning Algorithm Applied to Stable Gait Generation of Quadruped Robot

Based on Maslow’s hierarchy of needs theory, we have proposed a novel machine learning algorithm that combines factors of the environment and its own needs to make decisions for different states of an agent. This means it can be applied to the gait generation of a quadruped robot, which needs to make demand decisions. To evaluate the design, we created an experimental task in order to compare the needs learning algorithm with a reinforcement learning algorithm, which was also derived from psychological motivation theory. It was found that the needs learning algorithm outperformed the reinforcement learning in tasks that involved making decisions between different levels of needs. Finally, we applied the needs learning algorithm to the problem of stable gait generation of quadruped robot, and it had achieved good results in simulation and real robot.
Model and Visualization of Ray Tracing using JavaScript and HTML5 for TIR Measurement System Equipped with Equilateral Right Angle Prism

Trace of ray deviated by a prism, which is common in a TIR (total internal reflection) measurement system, is sometimes difficult to manage, especially if the prism is an equilateral right angle prism (ERAP). The point where the ray is reflected inside the right-angle prism is also changed as the angle of incident ray changed. In an ATR (attenuated total reflectance) measurement system, range of this point determines size of sample. Using JavaScript and HTML5 model and visualization of ray tracing deviated by an ERAP is perform and reported in this work. Some data are obtained from this visualization and an empirical relations between angle of incident ray source \theta_S, angle of ray detector hand \theta_D, and angle of ray detector \theta'_D are presented for radial position of ray source R_S, radial position of ray detector R_D, height of right-angle prism t, and refractive index of the prism n. Keywords: deviation angle, equilateral right angle prism, total internal reflection, JavaScript, HTML5.
Absolute astrometry in the next 50 years

With Gaia in orbit since December 2013 it is time to look at the future of fundamental astrometry and a time frame of 50 years is needed in this matter. A space mission with Gaia-like astrometric performance is required, but not necessarily a Gaia-like satellite. It should be studied whether this can be obtained within the budget of a medium-size ESA mission. A dozen science issues for a Gaia successor mission in twenty years, with launch about 2033, are presented and in this context also other possibilities for absolute astrometry with milliarcsecond (mas) or sub-mas accuracies are discussed. The three powerful techniques: VLBI, the MICADO camera on the E-ELT, and the LSST are described and documented by literature references and by an extensive correspondence with leading astronomers who readily responded with all the information I needed. In brief, the two Gaia-like missions would provide an astrometric foundation for all branches of astronomy from the solar system and stellar systems, including exo-planet systems, to compact galaxies, quasars and dark matter (DM) substructures by data which cannot be surpassed in the next 50 years. - In April 2017 ESA selected our proposal Hobbs et al. (2016) for study of a detector with NIR sensitivity for a Gaia successor mission, called GaiaNIR.
Complex Management of Nephrotic Syndrome and Kidney Failure during Pregnancy in a Type 1 Diabetes Patient: A Challenging Case

Pregnancy with chronic kidney disease is challenging, and patients with diabetic nephropathy are at particular risk of a rapid kidney function decline during pregnancy. While indications for the management of pregnant patients with initial diabetic nephropathy are widely available in the literature, data on patients with severe nephrotic syndrome and kidney function impairment are lacking, and the decision on whether and when dialysis should be initiated is not univocal. We report a type 1 diabetes patient who started pregnancy with a severe nephrotic syndrome and shifted from CKD stage 3b to stage 5 during pregnancy. The management was complicated by a fetal heart malformation and by poorly controlled diabetes. The evidence for and against starting dialysis was carefully evaluated, and the choice of strict nephrological and obstetrical monitoring, nutritional management, and diuretic treatment made it possible to avoid dialysis in pregnancy, after ruling out pre-eclampsia. This experience enables examination of some open issues and contributes to the discussion of when to start dialysis in pregnancy.
Nuclear equation of state and finite nucleon volumes

It is shown how the equation of state (EoS) depends on nucleon properties inside nuclear matter (NM). We propose to benefit from the concept of enthalpy in order to include volume corrections to the nucleon rest energy, which are proportional to pressure and absent in a standard relativistic mean field (RMF) with point-like nucleons. As a result, the nucleon mass can decrease inside NM, making the model nonlinear and the EoS softer. The course of the EoS in our RMF model agrees with a semi-empirical estimate and is close to the results obtained from extensive DBHF calculations with a Bonn A potential, which produce an EoS stiff enough to describe neutron star properties (mass–radius constraint), especially the masses of ‘PSR J16142230’ and ‘PSR J0348 + 0432’, known as the most massive () neutron stars. The presented model has proper saturation properties, including a good value of compressibility.
Optomechanical deformation and strain in elastic dielectrics

Light forces induced by scattering and absorption in elastic dielectrics lead to local density modulations and deformations. These perturbations in turn modify light propagation in the medium and generate an intricate nonlinear response. We generalize an analytic approach where light propagation in one-dimensional media of inhomogeneous density is modelled as a result of multiple scattering between polarizable slices. Using the Maxwell stress tensor formalism we compute the local optical forces and iteratively approach self-consistent density distributions where the elastic back-action balances gradient- and scattering forces. For an optically trapped dielectric we derive the nonlinear dependence of trap position, stiffness and total deformation on the object's size and field configuration. Generally trapping is enhanced by deformation, which exhibits a periodic change between stretching and compression. This strongly deviates from qualitative expectations based on the change of photon momentum of light crossing the surface of a dielectric. We conclude that optical forces have to be treated as volumetric forces and that a description using the change of photon momentum at the surface of a medium is inappropriate.