Miracle-dz/UniFAR-FTUs huggingface dataset:
Irving Fisher, Simon Newcomb, and their plans to stabilize the dollar

Abstract Irving Fisher dedicated Stabilizing the Dollar (1920) to Simon Newcomb for anticipating him “in proposing plans for stabilizing monetary units. ” The congruence of Newcomb’s and Fisher’s monetary theories and reform proposals was not as straightforward as Fisher’s book dedication suggested. Their plans had different theoretical roots: Fisher’s compensated dollar plan was the outcome of his quantity theory of money, while Newcomb held a classical monetary theory. We compare Newcomb’s and Fisher’s plans to stabilise the dollar and explore the theoretical rationales behind them offering an illustration of how similar proposals can be the result of different theories.
Complete conservative dynamics for inspiralling compact binaries with spins at the fourth post-Newtonian order

In this work we complete the spin-dependent conservative dynamics of inspiralling compact binaries at the fourth post-Newtonian order, and in particular the derivation of the next-to-next-to-leading order spin-squared interaction potential. We derive the physical equations of motion of the position and the spin from a direct variation of the action. Further, we derive the quadratic-in-spin Hamiltonians, as well as their expressions in the center-of-mass frame. We construct the conserved integrals of motion, which form the Poincaré algebra. This construction provided a consistency check for the validity of our result, which is crucial in particular in the current absence of another independent derivation of the next-to-next-to-leading order spin-squared interaction. Finally, we provide here the complete gauge-invariant relations among the binding energy, angular momentum, and orbital frequency of an inspiralling binary with generic compact spinning components to the fourth post-Newtonian order. These high post-Newtonian orders, in particular taking into account the spins of the binary constituents, will enable to gain more accurate information on the constituents from even more sensitive gravitational-wave detections to come.
X-RAY AND RADIO TIMING OF THE PULSAR IN 3C 58

We present timing data spanning 6.4 yr for the young and energetic PSR J0205+6449, in the supernova remnant 3C 58. Data were obtained with the Rossi X-ray Timing Explorer, the Jodrell Bank Observatory, and the Robert C. Byrd Green Bank Telescope. We present phase-coherent timing analyses showing timing noise and two spin-up glitches with fractional frequency increases of ∼3.4 × 10−7 near MJD 52555 and ∼3.8 × 10−6 between MJDs 52777 and 53062. These glitches are unusually large if the pulsar was created in the historical supernova in 1181, as has been suggested. For the X-ray timing, we developed a new unbinned maximum likelihood method for determining pulse arrival times, which performs significantly better than the traditional binned techniques. In addition, we present an X-ray pulse profile analysis of four years of RXTE data showing that the pulsar is detected up to ∼40 keV. We also present the first measurement of the phase offset between the radio and X-ray pulse for this source, showing that the radio pulse leads the X-ray pulse by ϕ = 0.10 ± 0.01 in phase. We compile all known measurements of the phase offsets between radio and X-ray and radio and γ-ray pulses for X-ray and γ-ray pulsars. We show that there is no relationship between pulse period and phase offset, supported by our measurement of the phase offset for PSR J0205+6449.
CHEMICAL SIGNATURE INDICATING A LACK OF MASSIVE STARS IN DWARF GALAXIES

Growing evidence supports an unusual elemental feature appearing in nearby dwarf galaxies, especially dwarf spheroidals (dSphs), indicating a key process of galaxy evolution that is different from that of the Galaxy. In addition to the well-known deficiency of α-elements in dSphs, recent observations have clearly shown that s-process elements (Ba) are significantly enhanced relative to Fe, α-, and r-process elements. This enhancement occurs in some dSphs as well as in the Large Magellanic Cloud, but is unseen in the Galaxy. Here we report that this feature is evidence of the lack of very massive stars (≳25 M☉) as predicted in the low star formation rate environment. We conclude that the unique elemental feature of dwarf galaxies including a low α/Fe ratio in some low-metallicity stars is, at least in some part, characterized by a different form of the initial mass function. We present a detailed model for the Fornax dSph galaxy and discuss its complex chemical enrichment history together with the nucleosynthesis site of the light s-process element Y.
Chemical ordering in Pd81Ge19 metallic glass studied by reverse Monte-Carlo modelling of XRD, ND and EXAFS experimental data

Pd81Ge19 metallic glass was investigated by neutron diffraction, x-ray diffraction and extended x-ray absorption fine structure spectroscopy at the Ge K-edge. Large scale structural models were obtained by fitting the three measurements simultaneously in the framework of the reverse Monte Carlo simulation technique. It was found that the experimental data sets can be adequately fitted without Ge–Ge nearest neighbours. Mean Pd–Pd and Pd–Ge distances are 2.80 ± 0.02 Å and 2.50 ± 0.02 Å, respectively. The total average coordination number of Pd is 12.1 ± 0.5 while Ge is surrounded by 10.6 ± 1.1 Pd atoms. The coordination numbers calculated from partial pair correlation functions were compared to those obtained by Voronoi tessellation method. It was found that the latter technique overestimates the number of nearest neighbours by about 20% due to the significant contribution of distant pairs.
The H i Chronicles of LITTLE THINGS BCDs. III. Gas Clouds in and around Mrk 178, VII Zw 403, and NGC 3738

In most blue compact dwarf (BCD) galaxies, it remains unclear what triggers their bursts of star formation. We study the H i of three relatively isolated BCDs, Mrk 178, VII Zw 403, and NGC 3738, in detail to look for signatures of star formation triggers, such as gas cloud consumption, dwarf–dwarf mergers, and interactions with companions. High angular and velocity resolution atomic hydrogen (H i) data from the Very Large Array (VLA) dwarf galaxy H i survey, Local Irregulars That Trace Luminosity Extremes, The H i Nearby Galaxy Survey (LITTLE THINGS), allow us to study the detailed kinematics and morphologies of the BCDs in H i. We also present high-sensitivity H i maps from the NRAO Green Bank Telescope (GBT) of each BCD to search their surrounding regions for extended tenuous emission or companions. The GBT data do not show any distinct galaxies obviously interacting with the BCDs. The VLA data indicate several possible star formation triggers in these BCDs. Mrk 178 likely has a gas cloud impacting the southeast end of its disk or it is experiencing ram pressure stripping. VII Zw 403 has a large gas cloud in its foreground or background that shows evidence of accreting onto the disk. NGC 3738 has several possible explanations for its stellar morphology and H i morphology and kinematics: an advanced merger, strong stellar feedback, or ram pressure stripping. Although apparently isolated, the H i data of all three BCDs indicate that they may be interacting with their environments, which could be triggering their bursts of star formation.
Characterization of BV functions on open domains: the Gaussian case and the general case

We provide three different characterizations of the space $BV(O,\gamma)$ of the functions of bounded variation with respect to a centred non-degenerate Gaussian measure $ \gamma$ on open domains $O$ in Wiener spaces. Throughout these different characterizations we deduce a sufficient condition for belonging to $BV(O,\gamma)$ by means of the Ornstein-Uhlenbeck semigroup and we provide an explicit formula for one-dimensional sections of functions of bounded variation. Finally, we apply our technique to Fomin differentiable probability measures $\nu$ on a Hilbert space $X$, inferring a characterization of the space $BV(O,\nu)$ of the functions of bounded variation with respect to $\nu$ on open domains $O\subseteq X$.
Predicting cervical cancer biopsy results using demographic and epidemiological parameters: a custom stacked ensemble machine learning approach

Abstract The human papillomavirus (HPV) is responsible for most cervical cancer cases worldwide. This gynecological carcinoma causes many deaths, even though it can be treated by removing malignant tissues at a preliminary stage. In many developing countries, patients do not undertake medical examinations due to the lack of awareness, hospital resources and high testing costs. Hence, it is vital to design a computer aided diagnostic method which can screen cervical cancer patients. In this research, we predict the probability risk of contracting this deadly disease using a custom stacked ensemble machine learning approach. The technique combines the results of several machine learning algorithms on multiple levels to produce reliable predictions. In the beginning, a deep exploratory analysis is conducted using univariate and multivariate statistics. Later, the one-way ANOVA, mutual information and Pearson’s correlation techniques are utilized for feature selection. Since the data was imbalanced, the Borderline-SMOTE technique was used to balance the data. The final stacked machine learning model obtained an accuracy, precision, recall, F1-score, area under curve (AUC) and average precision of 98%, 97%, 99%, 98%, 100% and 100%, respectively. To make the model explainable and interpretable to clinicians, explainable artificial intelligence algorithms such as Shapley additive values (SHAP), local interpretable model agnostic explanation (LIME), random forest and ELI5 have been effectively utilized. The optimistic results indicate the potential of automated frameworks to assist doctors and medical professionals in diagnosing and screening potential cervical cancer patients.
Half-metallic ferromagnetism in the RbSe and CsTe compounds with CsCl structure: A first-principles study

We investigate the electronic structures and magnetic properties of RbSe and CsTe compounds in CsCl, RS and ZB structures by using rst-principles calculation. It is shown that these two compounds exhibit half-metallic ferromagnetism with an integer magnetic moment of 1.00 B per formula in all the three structures. Total energy calculations indicate the CsCl phase is more stable than the other two phases. We investigate these two compounds with CsCl structure in detail. The ferromagnetism results mainly from the spin-polarization of p states of anion Se (Te) for the two compounds. The half-metallicities of RbSe and CsTe compounds can be preserved up to 2.5% and 0.8% compression of lattice constants with respect to their equilibrium lattices, respectively.
Searching for giga-Jansky fast radio bursts from the Milky Way with a global array of low-cost radio receivers

If fast radio bursts (FRBs) originate from galaxies at cosmological distances, then their all-sky rate implies that the Milky Way may host an FRB on average once every 30-1500 years. If FRBs repeat for decades or centuies, a local FRB could be active now. A typical Galactic FRB would produce a millisecond radio pulse with ~1 GHz flux density of ~3E10 Jy, comparable to the radio flux levels and frequencies of cellular communication devices (cell phones, Wi-Fi, GPS). We propose to search for Galactic FRBs using a global array of low-cost radio receivers. One possibility is to use the ~1GHz communication channel in cellular phones through a Citizens-Science downloadable application. Participating phones would continuously listen for and record candidate FRBs and would periodically upload information to a central data processing website, which correlates the incoming data from all participants, to identify the signature of a real, globe-encompassing, FRB from an astronomical distance. Triangulation of the GPS-based pulse arrival times reported from different locations will provide the FRB sky position, potentially to arc-second accuracy. Pulse arrival times from phones operating at diverse frequencies, or from an on-device de-dispersion search, will yield the dispersion measure (DM) which will indicate the FRB source distance within the Galaxy. A variant of this approach would be to use the built-in ~100 MHz FM-radio receivers present in cell phones for an FRB search at lower frequencies. Alternatively, numerous "software-defined radio" (SDR) devices, costing ~$10 US each, could be plugged into USB ports of personal computers around the world (particularly in radio quiet regions) to establish the global network of receivers.
Physico-chemical characterization of detrital sillimanite and garnet: Insights into REE elements, crystal structure and morphology

Abstract The Varkala–Kovalam coastal stretch of Southern Kerala, India, is enriched with economically significant heavy mineral deposits. In the present study, two such minerals like sillimanite, and garnet were recovered from the beach sands and subjected to detailed characterization studies related to their crystal structure, chemical composition, surface chemistry, and surface morphological changes. Advanced characterization studies involve Raman spectroscopy, X-ray photoelectron spectroscopy, ultraviolet–visible–near infrared spectroscopy, energy dispersive X-ray fluorescence, high resolution inductively coupled plasma mass spectrometry, and scanning electron microscopy/energy dispersive X-ray spectroscopy (SEM/EDS). The Raman spectra strictly discriminate sillimanite from other A12SiO5 polymorphs and almandine from other silicate garnets. The average total rare earth elements present in sillimanite is 222 ppm and garnet is 1094 ppm with a maximum for Ce. The surface morphological changes induced by solution activity of chemicals and mechanical impacts during sediment movement and deposition were easily analyzed by SEM images. The study provides a vivid dataset of physico-chemical characteristics of these minerals, which could facilitate determining their grade and industrial applications.
Host condition and pathogen identity influence bacterial infection survival in the common eastern firefly, Photinus pyralis

The degree to which host, pathogen, and environmental characteristics determine fitness outcomes in response to infection across the tree of life is a key question in ecoimmunology. Because infection experiments require large sample sizes and careful controls, studies have generally been limited to lab‐adapted organisms. Photinus pyralis is a charismatic firefly that is abundant during its annual summer emergence in the Eastern United States. Here, we assess the importance of host condition, pathogen identity and dose, and pre‐infection environment on survival outcomes in response to bacterial infection in wild‐caught adult male P. pyralis. Although survival after sterile saline injection was not statistically different from survival of uninjected controls, survival kinetics support sterile saline injection as the most appropriate control. Serratia marcescens and Providencia rettgeri infections increased mortality, especially at high doses. In contrast to fruit fly studies, Providencia sneebia, Pseudomonas aeruginosa, and Enterococcus faecalis infections did not. Infection with higher doses of P. rettgeri had an increased risk of death for fireflies caught later in the season than those captured earlier, but seasonality did not significantly interact with dose to impact mortality with any of the other bacterial species. These results highlight the importance of considering host, pathogen, and environmental factors when investigating infection outcomes in wild‐caught, non‐model systems. The differences in survival between fireflies and fruit flies emphasise that further studies in a broad array of organisms are needed to explore the diversity of infection responses across the tree of life.
GALAXY GROUPS: A 2MASS CATALOG

A galaxy group catalog is built from the sample of the 2MASS Redshift Survey almost complete to Ks = 11.75 over 91% of the sky. Constraints in the construction of the groups were provided by scaling relations determined by close examination of well defined groups with masses between 1011 and 10 15 M ⊙ ? > . Group masses inferred from Ks luminosities are statistically in agreement with masses calculated from application of the virial theorem. While groups have been identified over the full redshift range of the sample, the properties of the nearest and farthest groups are uncertain and subsequent analysis has only considered groups with velocities between 3000 and 10,000 km s−1. The 24,044 galaxies in this range are identified with 13,607 entities, 3461 of them with two or more members. A group mass function is constructed. The Sheth–Tormen formalism provides a good fit to the shape of the mass function for group masses above 6 h − 1 × 10 12 M ⊙ ? > but the count normalization is poor. Summing all the mass associated with the galaxy groups between 3000 and 10,000 km s−1 gives a density of collapsed matter as a fraction of the critical density of &OHgr; collapsed = 0.16 ? > .
Lagrangian Volume Deformations around Simulated Galaxies

We present a detailed analysis of the local evolution of 206 Lagrangian Volumes (LVs) selected at high redshift around galaxy seeds, identified in a large-volume cold dark matter ( CDM) hydrodynamical simulation. The LVs have a mass range of 1 1500 10 10 M . We follow the dynamical evolution of the density field inside these initially spherical LVs from z = 10 up to zlow = 0:05, witnessing highly non-linear, anisotropic mass rearrangements within them, leading to the emergence of the local cosmic web (CW). These mass arrangements have been analysed in terms of the reduced inertia tensor I r ij , focusing on the evolution of the principal axes of inertia and their corresponding eigendirections, and paying particular attention to the times when the evolution of these two structural elements declines. In addition, mass and component effects along this process have also been investigated. We have found that deformations are led by dark matter dynamics and they transform most of the initially spherical LVs into prolate shapes, i.e. filamentary structures. An analysis of the individual freezing-out time distributions for shapes and eigendirections shows that first most of the LVs fix their three axes of symmetry (like a skeleton) early on, while accretion flows towards them still continue. Very remarkably, we have found that more massive LVs fix their skeleton earlier on than less massive ones. We briefly discuss the astrophysical implications our findings could have, including the galaxy mass-morphology relation and the effects on the galaxy-galaxy merger parameter space, among others.
Significantly high polarization degree of the very low-albedo asteroid (152679) 1998 KU2

We present a unique and significant polarimetric result regarding the near-Earth asteroid (152679) 1998 KU 2 , which has a very low geometric albedo. From our observations, we find that the linear polarization degrees of 1998 KU 2 are 44.6 ± 0.5% in the R C band and 44.0 ± 0.6% in the V band at a solar phase angle of 81.0°. These values are the highest of any known airless body in the solar system (i.e., high-polarization comets, asteroids, and planetary satellites) at similar phase angles. This polarimetric observation is not only the first for primitive asteroids at large phase angles, but also for low-albedo ( 2 has a highly microporous regolith structure comprising nano-sized carbon grains on the surface.
A New Radio Loudness Diagnostic for Active Galaxies: a Radio-To-Mid-Infrared Parameter

We have studied the relationship between the nuclear (high-resolution) radio emission, at 8.4GHz (3.6cm) and I.4GHz (20cm), the [0 IV) A25.89 f.lm, [NeIll] Al5.56 f.lm and [Nell] Al2.8I f.lm emission lines and the black hole mass accretion rate for a sample of Seyfert galaxies. In order to characterize the radio contribution for the Seyfert nuclei we used the 8.4 GHzJ[O IV] ratio, assuming that [0 IV) scales with the luminosity of the active galactic nuclei (AGN). From this we find that Seyfert 1 s (i.e. Seyfert 1.0s, I.2s and l.5s) and Seyfert 2s (i.e. Seyfert 1.8s, 1.9s and 2.0s) have similar radio contributions, relative to the AGN. On the other hand, sources in which the [Ne u] emission is dominated either by the AGN or star formation have statistically different radio contributions, with star formation dominated sources more 'radio loud', by a factor of "-'2.8 on average, than AGN dominated sources. We show that star formation dominated sources with relatively larger radio contribution have smaller mass accretion rates. Overall, we suggest that 8.4 GHzJ[O IV], or alternatively, 1.4 GHzJ[O IV] ratios, can be used to characterize the radio contribution, relative to the AGN, without the limitation of previous methods that rely on optical observables.
Online Guided ACT Intervention for Enhancing the Psychological Well-being of Female Soccer Players in Pre-season

This study investigated whether an internet-based intervention aimed at enhancing the psychological well-being of female soccer players before the competitive season could be effective approach to meet the needs of the players. Players (n= 43; 17–26 years old)on the four separated teams in Finland’shighest league were assigned to either a guided six-week online Acceptance and Commitment Therapy intervention (ACTi) or to a control condition (CON). A between-groups pre–post (ACTi vs. CON) design was implemented before the competitive season. Players in the ACTi were offered three group sessions, performed internet-based tasks, and were individually supported by a guide. The results demonstrated that the ACTi players maintained their sports-related well-being (between-group, d = 0.72), while the sports-related well-being of the CON players, especially emotional and social well-being, had declined. In addition, ACTi players’perceived stress (d = 0.60) and depression (d = 0.88) declined, while their psychological flexibility in sports (d = 0.41) increased compared to the CON players. These results suggest that before the competitive season, players’ sports-related well-being decreases. The ACT intervention seemed to prevent this decrease and provide players with the skills to cope with emotional and social stressors related to the competitive season.
Evolutionary Design in Biological Quantum Computing

The unique capability of quantum mechanics to evolve alternative possibilities in parallel is appealing and over the years a number of quantum algorithms have been developed offering great computational benefits. Systems coupled to the environment lose quantum coherence quickly and realization of schemes based on unitarity might be impossible. Recent discovery of room temperature quantum coherence in light harvesting complexes opens up new possibilities to borrow concepts from biology to use quantum effects for computational purposes. While it has been conjectured that light harvesting complexes such as the Fenna-Matthews-Olson (FMO) complex in the green sulfur bacteria performs an efficient quantum search similar to the quantum Grover's algorithm the analogy has yet to be established. In this work we show that quantum dissipation plays an essential role in the quantum search performed in the FMO complex and it is fundamentally different from known algorithms. In the FMO complex not just the optimal level of phase breaking is present to avoid both quantum localization and Zeno trapping but it can harness quantum dissipation as well to speed the process even further up. With detailed quantum calculations taking into account both phase breaking and quantum dissipation we show that the design of the FMO complex has been evolutionarily optimized and works faster than pure quantum or classical-stochastic algorithms. Inspired by the findings we introduce a new computational concept based on decoherent quantum evolution. While it is inspired by light harvesting systems, the new computational devices can also be realized on different material basis opening new magnitude scales for miniaturization and speed.