Miracle-dz/UniFAR-FTUs huggingface dataset:
Testing ΛCDM cosmology at turnaround: where to look for violations of the bound?

In ΛCDM cosmology, structure formation is halted shortly after dark energy dominates the mass/energy budget of the Universe. A manifestation of this effect is that in such a cosmology the turnaround radius—the non-expanding mass shell furthest away from the center of a structure— has an upper bound. Recently, a new, local, test for the existence of dark energy in the form of a cosmological constant was proposed based on this turnaround bound. Before designing an experiment that, through high-precision determination of masses and —independently— turnaround radii, will challenge ΛCDM cosmology, we have to answer two important questions: first, when turnaround-scale structures are predicted to be close enough to their maximum size, so that a possible violation of the bound may be observable. Second, which is the best mass scale to target for possible violations of the bound. These are the questions we address in the present work. Using the Press-Schechter formalism, we find that turnaround structures have in practice already stopped forming, and consequently, the turnaround radius of structures must be very close to the maximum value today. We also find that the mass scale of ∼ 1013 M⊙ characterizes the turnaround structures that start to form in a statistically important number density today —and even at an infinite time in the future, since structure formation has almost stopped. This mass scale also separates turnaround structures with qualitatively different cosmological evolution: smaller structures are no longer readjusting their mass distribution inside the turnaround scale, they asymptotically approach their ultimate abundance from higher values, and they are common enough to have, at some epoch, experienced major mergers with structures of comparable mass; larger structures exhibit the opposite behavior. We call this mass scale the transitional mass scale and we argue that it is the optimal for the purpose outlined above. As a corollary, we explain the different accretion behavior of small and larger structures observed in already conducted numerical simulations.
Circumstellar Disks at White Dwarfs: Observations

The current picture painted by the observations of circumstellar dust at white dwarfs, and the consequent atmospheric pollution, is of a surviving planetary system. This chapter recounts in detail both the discovery and empirical characterization of dust disks at single white dwarfs, including all observational data available up to early 2011. Observations of the disks themselves and the accreted heavy elements within the stellar photospheres are consistent with tidally disrupted asteroid analogs. The observed chemistry supports objects that condensed within the inner regions of main-sequence stars and thus far appear similar in constitution to the terrestrial planets and their building blocks.
SURFACE BRIGHTNESS PROFILES OF DWARF GALAXIES. II. COLOR TRENDS AND MASS PROFILES

In this second paper of a series, we explore the B − V, U − B, and FUV−NUV radial color trends from a multi-wavelength sample of 141 dwarf disk galaxies. Like spirals, dwarf galaxies have three types of radial surface brightness profiles: (I) single exponential throughout the observed extent (the minority), (II) down-bending (the majority), and (III) up-bending. We find that the colors of (1) Type I dwarfs generally become redder with increasing radius, unlike spirals which have a blueing trend that flattens beyond ∼1.5 disk scale lengths, (2) Type II dwarfs come in six different “flavors,” one of which mimics the “U” shape of spirals, and (3) Type III dwarfs have a stretched “S” shape where the central colors are flattish, become steeply redder toward the surface brightness break, then remain roughly constant beyond, which is similar to spiral Type III color profiles, but without the central outward bluing. Faint (−9 > MB > −14) Type II dwarfs tend to have continuously red or “U” shaped colors and steeper color slopes than bright (−14 > MB > −19) Type II dwarfs, which additionally have colors that become bluer or remain constant with increasing radius. Sm dwarfs and BCDs tend to have at least some blue and red radial color trend, respectively. Additionally, we determine stellar surface mass density (Σ) profiles and use them to show that the break in Σ generally remains in Type II dwarfs (unlike Type II spirals) but generally disappears in Type III dwarfs (unlike Type III spirals). Moreover, the break in Σ is strong, intermediate, and weak in faint dwarfs, bright dwarfs, and spirals, respectively, indicating that Σ may straighten with increasing galaxy mass. Finally, the average stellar surface mass density at the surface brightness break is roughly 1−2 M⊙ pc−2 for Type II dwarfs but higher at 5.9 M⊙ pc−2 or 27 M⊙ pc−2 for Type III BCDs and dIms, respectively.
“Legibility” a product of obligatory processes in parametric architectural design: A study of implications of associative modeling on design thinking in a parametric architectural design studio

In a problem-based, digital-intensive learning environment, the increased proliferation of computational tools used for architectural design has led to a fundamental transformation in architectural studios. Many studies have shown that this has significantly led to the change in cognition of design environments in academia. Design decisions are made through a recursive process that is cyclically refined by allowing constant feedback and testing. This paper represents an observational study with an aim to understand the impact of digital mediums on design processes and design outcomes focusing on associative modeling using VPL. It contextualizes the difference, the associative modeling system as a parametric subset brings to design thinking when used as a medium to explore architectural design. It analyzes specific attributes of associative modeling, otherwise native to computational thinking, that contribute to the legibility of the design process. The paper demonstrates how associative modeling allows the design process to be examined and edited at any stage during and even after algorithmic development, bringing in flexibility. It is argued that digital design tool affordances enable students to develop multilayered and more structured design logic that augments cognition bringing more legibility to the design thinking process.
CORONAL THICK TARGET HARD X-RAY EMISSIONS AND RADIO EMISSIONS

A distinctive class of hard X-ray (HXR) sources located in the corona was recently found, which implies that the collisionally thick target model (CTTM) applies even to the corona. We investigated whether this idea can be independently verified by microwave radiations which have been known as the best companion to HXRs. This study is conducted on the GOES M2.3 class flare which occurred on 2002 September 9 and was observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager and the Owens Valley Solar Array. Interpreting the observed energy-dependent variation of HXR source size under the CTTM, the coronal density should be as high as 5 × 1011 cm−3 over a distance of up to 12″. To explain the cutoff feature of the microwave spectrum at 3 GHz, however, we require a density no higher than 1 × 1011 cm−3. Additional constraints must be placed on the temperature and magnetic field of the coronal source in order to reproduce the microwave spectrum as a whole. First, a spectral feature called the Razin suppression requires a magnetic field in a range of 250–350 G along with high viewing angles around 75°. Second, to avoid excess fluxes at high frequencies due to the free–free emission that was not observed, we need a high temperature ⩾2 × 107 K. These two microwave spectral features, Razin suppression and free–free emissions, become more significant at regions of high thermal plasma density and are essential for validating and determining additional parameters of the coronal HXR sources.
SUZAKU OBSERVATION OF THE FERMI CYGNUS COCOON: THE SEARCH FOR A SIGNATURE OF YOUNG COSMIC-RAY ELECTRONS

The origin of Galactic cosmic rays remains unconfirmed, but promising candidates for their sources are found in star-forming regions. We report a series of X-ray observations, with Suzaku, toward the nearby star-forming region of Cygnus X. They aim at comparing diffuse X-ray emissions on and off the γ-ray cocoon of hard cosmic rays revealed by the Fermi Large Area Telescope. After excluding point sources and small-scale structures and subtracting the non-X-ray and cosmic X-ray backgrounds, the 2–10 keV X-ray intensity distribution is found to monotonically decrease with increasing Galactic latitude. This indicates that most of the extended emission detected by Suzaku originates from the Galactic ridge. In two observations, we derive upper limits of 3.4 × 10 − 8 ? > and 1.3 × 10 − 8 erg s − 1 cm − 2 sr − 1 ? > to X-ray emission in the 2–10 keV range from the γ-ray cocoon. These limits exclude the presence of cosmic-ray electrons with energies above about 50 TeV at a flux level capable of explaining the γ-ray spectrum. They are consistent with the emission cut-off observed near a TeV in γ-rays. The properties of the Galactic-ridge and local diffuse X-rays are also discussed.
Performance of LAD-LASSO and WLAD-LASSO on High Dimensional Regression in Handling Data Containing Outliers

In several research areas, it is common to have a dataset with more explanatory variables than the number of observations, called high-dimensional data. This condition can lead to multicollinearity problem. The least absolute shrinkage and selection operator (LASSO) solves the problem by shrinking the estimated coefficient to zero so that it can simultaneously carry on the variable selection and the parameter estimation. But LASSO performs poorly when the data contains some outliers in the response or explanatory variables. Robust methods have addressed this problem based on the least-absolute-deviation approach, such as LAD-LASSO and WLAD-LASSO. This current research aims to evaluate the performance of the LAD-LASSO and WLAD-LASSO methods on high-dimensional and low-dimensional data containing outliers. To evaluate the performance of these methods, the simulation study was conducted. The simulation study used three scenarios (without outliers, outliers on the response variable (5%, 10%, 15%), outliers both on the response and explanatory variables (5%, 10%, 15%)). We also used the Minimum Regularized Covariance Determinant (MRCD) estimator in calculating the weights on the WLAD-LASSO. The best method from this simulation then will be applied to sembung leaf extract data to identify antioxidant marker compounds in sembung leaf extract. The simulation results show that LAD-LASSO tends to be very tight in selecting, while LASSO tends to be too loose. Meanwhile, WLAD-LASSO is in the middle of those two techniques and performs the best in identifying the important variables correctly. Even the existence of weights cause WLAD-LASSO more robust against the presence of outliers in the response and explanatory variables compared to LAD-LASSO. Furthermore, performance of these methods on high-dimensional data decrease compared to low-dimensional data. The performance of these methods also tends to decrease when the rate of outlier increases. The WLAD-LASSO was then implemented in actual data to find the compound of antioxidant markers in the sembung leaf extract. The compounds/formulas obtained are Umbelliferone, 12-Hydroxyjasmonic Acid, C22H14N8O2, and Acetyleugenol (with a prediction error is 0.133050). These compounds/formulas can be developed as natural antioxidants and have the potential to be developed as medicinal ingredients.
COMPLEX DIFFUSE RADIO EMISSION IN THE MERGING PLANCK ESZ CLUSTER A3411

We present Very Large Array (VLA) radio and Chandra X-ray observations of the merging galaxy cluster A3411. For the cluster, we find an overall temperature of 6.4 keV and an X-ray luminosity of 2.8 ± 0.1 × 1044 erg s−1 between 0.5 and 2.0 keV. The Chandra observation reveals the cluster to be undergoing a merger event. The VLA observations show the presence of large-scale diffuse emission in the central region of the cluster, which we classify as a 0.9 Mpc size radio halo. In addition, a complex region of diffuse, polarized emission is found in the southeastern outskirts of the cluster along the projected merger axis of the system. We classify this region of diffuse emission as a radio relic. The total extent of this radio relic is 1.9 Mpc. For the combined emission in the cluster region, we find a radio spectral index of −1.0 ± 0.1 between 74 MHz and 1.4 GHz. The morphology of the radio relic is peculiar, as the relic is broken up into five fragments. This suggests that the shock responsible for the relic has been broken up due to interaction with a large-scale galaxy filament connected to the cluster or other substructures in the intracluster medium. Alternatively, the complex morphology reflects the presence of electrons in fossil radio bubbles that are re-accelerated by a shock.
Real holomorphic curves and invariant global surfaces of section

In this paper, we prove that a dynamically convex starshaped hypersurface in C2 which is invariant under complex conjugation admits a global surface of section which is invariant under conjugation as well. We obtain this invariant global surface by embedding C2 into CP2 and applying a stretching argument to real holomorphic curves in CP2 . The motivation for this result arises from recent progress in applying holomorphic curve techniques to gain a deeper understanding on the dynamics of the restricted three‐body problem.
The past, present and future of educational assessment: A transdisciplinary perspective

To see the horizon of educational assessment, a history of how assessment has been used and analysed from the earliest records, through the 20th century, and into contemporary times is deployed. Since paper-and-pencil assessments validity and integrity of candidate achievement has mattered. Assessments have relied on expert judgment. With the massification of education, formal group-administered testing was implemented for qualifications and selection. Statistical methods for scoring tests (classical test theory and item response theory) were developed. With personal computing, tests are delivered on-screen and through the web with adaptive scoring based on student performance. Tests give an ever-increasing verisimilitude of real-world processes, and analysts are creating understanding of the processes test-takers use. Unfortunately testing has neglected the complicating psychological, cultural, and contextual factors related to test-taker psychology. Computer testing neglects school curriculum and classroom contexts, where most education takes place and where insights are needed by both teachers and learners. Unfortunately, the complex and dynamic processes of classrooms are extremely difficult to model mathematically and so remain largely outside the algorithms of psychometrics. This means that technology, data, and psychometrics have become increasingly isolated from curriculum, classrooms, teaching, and the psychology of instruction and learning. While there may be some integration of these disciplines within computer-based testing, this is still a long step from where classroom assessment happens. For a long time, educational, social, and cultural psychology related to learning and instruction have been neglected in testing. We are now on the cusp of significant and substantial development in educational assessment as greater emphasis on the psychology of assessment is brought into the world of testing. Herein lies the future for our field: integration of psychological theory and research with statistics and technology to understand processes that work for learning, identify how well students have learned, and what further teaching and learning is needed. The future requires greater efforts by psychometricians, testers, data analysts, and technologists to develop solutions that work in the pressure of living classrooms and that support valid and reliable assessment.
The chaotic dynamics of large-scale structures in a turbulent wake

The dynamics of a 3D bimodal turbulent wake downstream a square-back Ahmed body are experimentally studied in a wind-tunnel through high-frequency wall pressure probes mapping the rear of the model and a horizontal 2D velocity field. The barycenters of the pressure distribution over the rear part of the model and the intensity recirculation are found highly correlated. Both described the most energetic large-scale structures dynamics, confirming the relation between the large-scale recirculation bubble and its wall pressure foot-print. Focusing on the pressure, its barycenter trajectory has a stochastic behavior but its low frequencies dynamics exhibit the same characteristics as a weak strange chaotic attractor system, with two well defined attractors. The low frequencies dynamics associated to the large-scale structures are then analyzed. The largest Lyapunov exponent is first estimated, leading to a low positive value characteristic of strange attractors and weak chaotic systems. Afterwards, analyzing the autocorrelation function of the time-series, we compute the correlation dimension, larger than two. The signal is finally transformed and analyzed as a telegraph signal showing that its dynamics correspond to a quasi-random telegraph signal. This is the first demonstration that the low frequencies dynamics of a turbulent 3D wake are not a purely stochastic process but rather a weak chaotic process exhibiting strange attractors. From the flow-control point of view, it also opens the path to more simple closed-loop flow control strategies aiming at the stabilization of the wake and the control of the dynamics of the wake barycenter.
Arrival time prediction of transport based on recurrent neural network

In this paper, through in-depth study of highway traffic and non-highway arrival time prediction model and algorithm, it is found that the performance of DA-RNN (recurrent neural network based on two-stage attention) is better than other classical prediction models. We choose to introduce an attention mechanism to adaptively select the most relevant factors from heterogeneous information and establish a prediction network based on da-rnn (recurrent neural network based on two-stage attention). In this paper, the real data of Jinan bus driving is used to carry out experiments, and the bus travel prediction is realized. Under the same data condition, a variety of methods are tested. Through the comparative analysis of experimental results, the method proposed in this paper performs better on the data set provided by Jinan bus company.
Weak lensing reconstruction through cosmic magnification - II. Improved power spectrum determination and map-making

The existence of galaxy intrinsic clustering severely hampers the weak lensing reconstruction from cosmic magnification. In Paper I, we proposed a minimal variance estimator to overcome this problem. By utilizing the different dependences of cosmic magnification and galaxy intrinsic clustering on galaxy flux, we demonstrated that the otherwise overwhelming galaxy intrinsic clustering can be significantly suppressed such that lensing maps can be reconstructed with promising accuracy. This procedure relies heavily on the accuracy of determining the galaxy bias from the same data. Paper I adopts an iterative approach, which degrades towards high redshift. The current paper presents an alternative method, improving over Paper I. We prove that the measured galaxy clustering between flux bins allows for simultaneous determination of the lensing power spectrum and the flux dependence of galaxy bias, at this redshift bin. Compared to Paper I, the new approach is not only more straightforward but also more robust. It identifies an ambiguity in determining the galaxy bias and further discovers a mathematically robust way to suppress this ambiguity to negligible level (similar to 0.1 per cent). The accurately determined galaxy bias can then be applied to the minimal variance estimator proposed in Paper I to improve the lensing map-making. The gain at high redshift is significant. These maps can be used to measure other statistics, such as cluster finding and peak statistics. Furthermore, by including galaxy clustering measurement between different redshift bins, we can also determine the lensing cross power spectrum between these bins, up to a small and correctable multiplicative factor (similar to 0.2-1 per cent for different redshift bin couples).
Aroma and terpenoid profile of Chardonnay clone 809: from berry to sparkling wine

Clone selection is a viticultural practice applied to evaluate the behaviour and agronomic and flavour characteristics of a material in a determined environment to obtain wines with different aromatic attributes. The clones of the cultivar Chardonnay comprise aromatic and non-aromatic clones that can provide different sensorial qualities. This work aimed to evaluate the volatile compounds formed in clone 809 (aromatic) to produce a more aromatic sparkling wine in Serra da Mantiqueira (southeast Brazil) and compare it to clone 76 (non-aromatic) from the berry to the wine. The vineyards are in Caldas (Minas Gerais – Brazil) at the Agronomical Research Centre of Minas Gerais (EPAMIG), and the vinification was performed using the Champenoise method (18 months in sur lie). HS-SPME/GC-MS identified free volatile compounds in two consecutive seasons, 2017 and 2018, in grape, musts, base wines and sparkling wines. The number and abundance of monoterpenoid compounds in clone 809 were statistically significant compared to clone 76 for all sample steps. Multivariate and principal component analyses (PCA) made it possible to differentiate the base and sparkling wines by the clones in both vintages for the second component (16.8 %). Furthermore, the sparkling wines of clone 809 were discriminated for the third component (15.1 %) by the monoterpenes: α-terpineol, linalool, ß-myrcene, hotrienol, nerol oxide, and limonene. The data suggest that Chardonnay clone 809 can contribute to obtaining a sparkling wine with an additional floral and sweet character.
Local multifractal analysis in metric spaces

We study the local dimensions and local multifractal properties of measures on doubling metric spaces. Our aim is twofold. On one hand, we show that there are plenty of multifractal type measures in all metric spaces which satisfy only mild regularity conditions. On the other hand, we consider a local spectrum that can be used to gain finer information on the local behaviour of measures than its global counterpart.
Template-Less and Surfactant-Less Synthesis of CeO2 Nanostructures for Catalytic Application in Ipso-hydroxylation of Aryl Boronic Acids and the aza-Michael Reaction

Due to its excellent physicochemical properties, CeO2 has found great importance as an electrochemical and in electronics, photocatalysis, sensing, and heterogeneous catalysis. Herein, we report the surfactant-less and template-less synthesis of CeO2 nanostructures by the hydrothermal method. The synthesized CeO2 nanostructures have been characterized in detail by electron microscopy, spectroscopy, diffractometry, and other analytical methods. The XRD studies revealed the formation of pure crystalline CeO2, possessing a cubic fluorite structure with an average crystallite size of 15.6 to 16.4 nm. Electron microscopy studies reveal the formation of cube-shaped CeO2 nanostructures with sizes below 25 nm. The cube-shaped CeO2 nanostructures exhibited a higher BET surface area compared to their bulk counterparts. The XPS analysis has confirmed the existence of Ce in the mixed oxidation states of +3 and +4, while O is present as O2– in the sample. The as-synthesized CeO2 nanostructures exhibit excellent catalytic activity in both the ipso-hydroxylation of aryl boronic acids and the aza-Michael reaction. The analysis of the used catalyst has confirmed its stability under the reported reaction conditions. The catalysts retain their catalytic activity up to the fifth run in both types of reactions, which is economically beneficial for industrial application.