Miracle-dz/UniFAR-FTUs huggingface dataset:
Low-energy antiferromagnetic spin fluctuations limit the coherent superconducting gap in cuprates

Motivated by recent attention to a potential antiferromagnetic quantum critical point at $x_c\sim 0.19$, we have used inelastic neutron scattering to investigate the low-energy spin excitations in crystals of La$_{2-x}$Sr$_x$CuO$_4$ bracketing $x_c$. We observe a peak in the normal-state spin-fluctuation weight at $\sim20$~meV for both $x=0.21$ and 0.17, inconsistent with quantum critical behavior. The presence of the peak raises the question of whether low-energy spin fluctuations limit the onset of superconducting order. Empirically evaluating the spin gap $\Delta_{\rm spin}$ in the superconducting state, we find that $\Delta_{\rm spin}$ is equal to the coherent superconducting gap $\Delta_c$ determined by electronic spectroscopies. To test whether this is a general result for other cuprate families, we have checked through the literature and find that $\Delta_c\le\Delta_{\rm spin}$ for cuprates with uniform $d$-wave superconductivity. We discuss the implications of this result.
Cubic Thue inequalities with positive discriminant

We will give an explicit upper bound for the number of solutions to cubic inequality |F(x, y)| \leq h, where F(x, y) is a cubic binary form with integer coefficients and positive discriminant D. Our upper bound is independent of h, provided that h is smaller than D^{1/4}.
Aquatic Exercise on Brain Activity in Type 2 Diabetic: Randomized Clinical Trial

Background: A water-based physical exercise program is extremely important for the rehabilitation of type 2 diabetes. Little is known about its action on cerebral electrical activity. Objective: To evaluate the effect of a water-based physical exercise protocol on electroencephalographic activity, blood glucose levels, and functional capacity, as well as their correlation, in type 2 diabetics. Methods: Study design: Randomized Clinical Trial. Forty volunteers were randomized into two groups: control (n = 20) and study (n = 20). A water-based physical exercise program comprising 50 min sessions was conducted three times a week for five weeks. Assessments were performed at the pre- and post-intervention and follow-up phases. The qualitative data were compared using the Mann–Whitney test and Chi-Square. Quantitative data were compared using the Kruskal–Wallis, Independent t, and ANOVA mixed tests. The Spearman correlation coefficient was used to correlate the data. Results: The data were similar when comparing the groups. Six-minute walk test data increased in the comparison between times (p = 0.01—PrexPos). EEG data decreased in comparison between times (prexfollow-up—p < 0.05), except AF3. EEG data decreased in the timexgroup comparison (prexfollow-up and postxfollow-up—p < 0.05). Conclusions: The water-based exercise protocol maintained electroencephalographic activity, glucose levels, and functional capacity in people with type 2 diabetes, and there was no relationship between brain electrical activity and capillary blood glucose.
How Do the Young Perceive Urban Parks? A Study on Young Adults’ Landscape Preferences and Health Benefits in Urban Parks Based on the Landscape Perception Model

(1) Background: Youth’s physical and mental health is of increasing concern today. However, gaining a more comprehensive knowledge of young people’s landscape preferences for urban parks is challenging. Additionally, young adults’ voices (aged from 20 to 24) are often neglected. (2) Methods: This study collected 349 interview questionnaires from 2014 to 2020 and recorded them into Nvivo10. Firstly, the study did a thematic analysis using the preliminary coding framework based on the landscape perception model to code the interview data and statistics on the frequencies of each theme and code. Then, we used diffractive analysis to interpret original materials to comprehend the underlying significance. (3) Results: Our research showed that young adults’ landscape perceptions are richer in diversity and express more subjective feelings. Their landscape preferences are also related to behavioral activities in addition to environmental features, which have some differences from teenagers. (4) Conclusions: It is helpful to attract more young adults by creating sound and smell landscapes, accommodating more dynamic sports and recreation facilities, and controlling unhygienic and noise problems, which can offer better design, planning, and management for creating inclusive urban parks. The landscape perception model developed in this paper can also provide a reference for related studies in the future.
IS THE GALACTIC BULGE DEVOID OF PLANETS?

We consider a sample of 31 exoplanetary systems detected by gravitational microlensing and investigate whether or not the estimated distances to these systems conform to the Galactic distribution of planets expected from models. We derive the expected distribution of distances and relative proper motions from a simulated microlensing survey, correcting for the dominant selection effects that affect the sensitivity of planet detection as a function of distance, and compare it to the observed distribution using Anderson–Darling (AD) hypothesis testing. Taking the relative abundance of planets in the bulge to that in the disk, , as a model parameter, we find that our model is consistent with the observed distribution only for (for a p-value threshold of 0.01) implying that the bulge may be devoid of planets relative to the disk. Allowing for a dependence of planet abundance on metallicity and host mass, or an additional dependence of planet sensitivity on event timescale, does not restore consistency for . We examine the distance estimates of some events in detail, and conclude that some parallax-based estimates could be significantly in error. Only by combining the removal of one problematic event from our sample and the inclusion of strong dependences of planet abundance or detection sensitivity on host mass, metallicity, and event timescale are we able to find consistency with the hypothesis that the bulge and disk have equal planet abundance.
Metallicities in long gamma-ray burst host galaxies at z < 0.5 calculated by the detailed modelling of optical and infrared line ratios

We revisited the line spectra emitted from long GRB (LGRB) host galaxies at z<0.5 in order to calculate by the detailed modelling of the line ratios the physical conditions and relative abundances in LGRB hosts in this redshift range. We have found lower metallicities than in LGRB hosts at higher z. New results about metallicities and physical conditions in the different regions throughout the LGRB 980425 host at z=0.0085 are presented. In particular, we have found that the effective starburst temperature in the supernova (SN) region is the highest throughout the host galaxy. The low ionization parameter reveals that the radiation source is far or somehow prevented from reaching the emitting gas in the SN region. The models constrained by a few oxygen, nitrogen and sulphur line ratios to Hb in LGRB 980425 host satisfactorily reproduce the HeII/Hb and [ArIII]/Hb line ratios. The modelling of the observed [SIV]10.51\mu/[SIII]18.71\mum and [NeIII]10.6\mum/[NeII]12.81\mum line ratios from LGRB 031203 host galaxy at z=0.105 shows that the mid-IR lines are emitted from geometrically thin shock dominated filaments which are not reached by the photoionizing flux, while the optical lines are emitted from the radiation dominated outflowing clouds.
Geometry of the quantum set on no-signaling faces

Since Bell's theorem we know that quantum mechanics is incompatible with local hidden variable models, the phenomenon known as quantum nonlocality. However, in spite of steady progress over years, the precise characterization of the set of quantum correlations has remained an elusive quest. There are correlations compatible with the no-signaling principle and still beyond what can be achieved within quantum theory, what has motivated the search for physical principles and computational methods to decide the quantum or post-quantum behavior of correlations. Here we identify a yet new feature of Bell correlations that we call quantum voids: faces of the no-signaling set where all nonlocal correlations are postquantum. Considering the simplest possible Bell scenario we give a full characterization of quantum voids, also understanding its connections to known principles and its potential use as a dimension witness.
A deep Chandra observation of the hot gaseous halo around a rare, extremely massive and relativistic jet launching spiral galaxy

We present a deep Chandra observation of the extremely massive spiral galaxy 2MASX J23453268-0449256, the first X-ray observation of this very rare system which features the largest known relativistic jets from a spiral galaxy. We detect extended X-ray emission from the hot halo surrounding the galaxy, reaching out to 80 kpc in radius. The hot halo is elongated along the plane of the spiral galaxy, and one possibility is that the powerful relativistic jets have disrupted the hot halo gas located perpendicular to the disk. Our calculations indicate that it is energetically feasible that the AGN feedback in this system could have uplifted or completely expelled a significant fraction of the gas in the 20-80 kpc radial range. We also detect extended emission which appears to be associated with the inner and outer southern radio lobes, and is possibly the result of inverse Compton emission. Using the observed X-ray and radio luminosity of the central AGN, the fundamental plane of Gultekin et al. predicts a black hole mass of 5x10^8 M_solar, with a range of 1x10^8 - 3x10^9 M_solar when the scatter in the fundamental plane relation is taken into account. This is consistent with the possibility that an exceptionally massive (>10^9 M_solar) black hole lies at the centre of this galaxy, as suggested by the M_BH-sigma scaling relation, but a tighter constraint cannot be made.
Effects of chemical pressure on the Fermi surface and band dispersion of the electron-doped high- T c superconductors

We have performed angle-resolved photoemission spectroscopy measurements and first-principles electronic-structure calculations on the electron-doped high-${T}_{c}$ superconductors (HTSCs) $L{n}_{1.85}{\text{Ce}}_{0.15}{\text{CuO}}_{4}$ ($Ln=\text{Nd}$, Sm, and Eu). The observed Fermi surface and band dispersion show such changes that with decreasing ionic size of $L{n}^{3+}$ (increasing chemical pressure), the curvature of the Fermi surface or $\ensuremath{-}{t}^{\ensuremath{'}}/t$ decreases, where $t$ and ${t}^{\ensuremath{'}}$ are transfer integrals between the nearest-neighbor and next-nearest-neighbor Cu sites, respectively, explaining the apparently inconsistent behavior seen in the hole-doped HTSC ${\text{La}}_{2\ensuremath{-}x}{\text{Sr}}_{x}{\text{CuO}}_{4}$ under epitaxial strain. Around the node, the antiferromagnetic gap is opened with increasing chemical pressure. We propose that the nodal gap opening is possibly due to the decrease in $\ensuremath{-}{t}^{\ensuremath{'}}/t$ through the improved nesting, leading to the decrease in ${T}_{c}$.
LOFAR discovery of an ultra-steep radio halo and giant head–tail radio galaxy in Abell 1132

Low-Frequency Array (LOFAR) observations at 144 MHz have revealed large-scale radio sources in the unrelaxed galaxy cluster Abell 1132. The cluster hosts diffuse radio emission on scales of similar to 650 kpc near the cluster centre and a head-tail (HT) radio galaxy, extending up to 1 Mpc, south of the cluster centre. The central diffuse radio emission is not seen in NRAO VLA FIRST Survey, Westerbork Northern Sky Survey, nor in C & D array VLA observations at 1.4 GHz, but is detected in our follow-up Giant Meterwave Radio Telescope (GMRT) observations at 325 MHz. Using LOFAR and GMRT data, we determine the spectral index of the central diffuse emission to be alpha = -1.75 +/- 0.19 (S alpha nu(alpha) ). We classify this emission as an ultra-steep spectrum radio halo and discuss the possible implications for the physical origin of radio haloes. The HT radio galaxy shows narrow, collimated emission extending up to 1 Mpc and another 300 kpc of more diffuse, disturbed emission, giving a full projected linear size of 1.3 Mpc - classifying it as a giant radio galaxy (GRG) and making it the longest HT found to date. The head of the GRG coincides with an elliptical galaxy (SDSS J105851.01+564308.5) belonging to Abell 1132. In our LOFAR image, there appears to be a connection between the radio halo and the GRG. The turbulence that may have produced the halo may have also affected the tail of the GRG. In turn, the GRG may have provided seed electrons for the radio halo.
Detail Analysis for Energy Transfer and Pigment Assembling in C−Phycocyanin through Time−Resolved Spectroscopy and AlphaFold2

The time-resolved fluorescence spectroscopy of the C−phycocyanin (C−PC) complex from the cyanobacterium Spirulina platensis (S. platensis) hexamer with the sub-picosecond resolution was detected, and the energy transfer pathways and related transfer rates were identified through the multiexponential analysis based on Monte-Carlo method. With the purpose to construct the relationship between the functions and the structure in vivo, the three−dimension (3D) protein structure was predicted via AlphaFold2, and the arrangement of chromophores treated as the energy transfer nodes were obtained. The experiment results have been matched well with the structure prediction. This work suggests a new way to investigate structure prediction in vivo and the corresponding functions.
EXTINCTION AND DISTANCE TO ANOMALOUS X-RAY PULSARS FROM X-RAY SCATTERING HALOS

We analyze the X-ray scattering halos around three Galactic Anomalous X-ray Pulsars in order to constrain the distance and the optical extinction of each source. We obtain surface brightness distributions from EPIC-pn data obtained with XMM-Newton, compare the profiles of different sources, and fit them with a model based on the standard theory of X-ray scattering by dust grains, both for a uniform distribution of dust along the line of sight, and for dust distributions constrained by previous measurements. Somewhat surprisingly, we find that for all three sources, the uniform distribution reproduces the observed surface brightness as well as or better than the distributions that are informed by previous constraints. Nevertheless, the inferred total dust columns are robust, and serve to confirm that previous measurements based on interstellar edges in high-resolution X-ray spectra and on modeling of broadband X-ray spectra were reliable. Specifically, we find AV ≃ 4, 6, and 8 mag for 4U 0142+61, 1E 1048.1 − 5937, and 1RXS J170849.0 − 400910, respectively. For 1E 1048.1 − 5937, this is well in excess of the extinction expected toward an H i bubble along the line of sight, thus casting further doubt on the suggested association with the source.
THE ORIGIN OF THE HOT GAS IN THE GALACTIC HALO: CONFRONTING MODELS WITH XMM-NEWTON OBSERVATIONS

We compare the predictions of three physical models for the origin of the hot halo gas with the observed halo X-ray emission, derived from 26 high-latitude XMM-Newton observations of the soft X-ray background between l = 120° and l = 240°. These observations were chosen from a much larger set of observations as they are expected to be the least contaminated by solar wind charge exchange emission. We characterize the halo emission in the XMM-Newton band with a single-temperature plasma model. We find that the observed halo temperature is fairly constant across the sky (∼(1.8–2.4) × 106 K), whereas the halo emission measure varies by an order of magnitude (∼0.0005–0.006 cm−6 pc). When we compare our observations with the model predictions, we find that most of the hot gas observed with XMM-Newton does not reside in isolated extraplanar supernova (SN) remnants—this model predicts emission an order of magnitude too faint. A model of an SN-driven interstellar medium, including the flow of hot gas from the disk into the halo in a galactic fountain, gives good agreement with the observed 0.4–2.0 keV surface brightness. This model overpredicts the halo X-ray temperature by a factor of ∼2, but there are a several possible explanations for this discrepancy. We therefore conclude that a major (possibly dominant) contributor to the halo X-ray emission observed with XMM-Newton is a fountain of hot gas driven into the halo by disk SNe. However, we cannot rule out the possibility that the extended hot halo of accreted material predicted by disk galaxy formation models also contributes to the emission.
THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION,

We present the first results from our high-precision infrared (IR) astrometry program at the Canada–France–Hawaii Telescope. We measure parallaxes for 83 ultracool dwarfs (spectral types M6–T9) in 49 systems, with a median uncertainty of 1.1 mas (2.3%) and as good as 0.7 mas (0.8%). We provide the first parallaxes for 48 objects in 29 systems, and for another 27 objects in 17 systems, we significantly improve upon published results, with a median (best) improvement of 1.7 times (5 times). Three systems show astrometric perturbations indicative of orbital motion; two are known binaries (2MASS J0518−2828AB and 2MASS J1404−3159AB) and one is spectrally peculiar (SDSS J0805+4812). In addition, we present here a large set of Keck adaptive optics imaging that more than triples the number of binaries with L6–T5 components that have both multi-band photometry and distances. Our data enable an unprecedented look at the photometric properties of brown dwarfs as they cool through the L/T transition. Going from ≈L8 to ≈T4.5, flux in the Y and J bands increases by ≈0.7 mag and ≈0.5 mag, respectively (the Y- and J-band “bumps”), while flux in the H, K, and L′ bands declines monotonically. This wavelength dependence is consistent with cloud clearing over a narrow range of temperature, since condensate opacity is expected to dominate at 1.0–1.3 μm. Interestingly, despite more than doubling the near-IR census of L/T transition objects, we find a conspicuous paucity of objects on the color–magnitude diagram just blueward of the late-L/early-T sequence. This “L/T gap” occurs at (J − H)MKO = 0.1–0.3 mag, (J − K)MKO = 0.0–0.4 mag, and implies that the last phases of cloud evolution occur rapidly. Finally, we provide a comprehensive update to the absolute magnitudes of ultracool dwarfs as a function of spectral type using a combined sample of 314 objects.
THE HUNT FOR EXOMOONS WITH KEPLER (HEK). III. THE FIRST SEARCH FOR AN EXOMOON AROUND A HABITABLE-ZONE PLANET

Kepler-22b is the first transiting planet to have been detected in the habitable zone of its host star. At 2.4 R⊕, Kepler-22b is too large to be considered an Earth analog, but should the planet host a moon large enough to maintain an atmosphere, then the Kepler-22 system may yet possess a telluric world. Aside from being within the habitable zone, the target is attractive due to the availability of previously measured precise radial velocities and low intrinsic photometric noise, which has also enabled asteroseismology studies of the star. For these reasons, Kepler-22b was selected as a target-of-opportunity by the “Hunt for Exomoons with Kepler” (HEK) project. In this work, we conduct a photodynamical search for an exomoon around Kepler-22b leveraging the transits, radial velocities, and asteroseismology plus several new tools developed by the HEK project to improve exomoon searches. We find no evidence for an exomoon around the planet and exclude moons of mass MS > 0.5 M⊕ to 95% confidence. By signal injection and blind retrieval, we demonstrate that an Earth-like moon is easily detected for this planet even when the time-correlated noise of the data set is taken into account. We provide updated parameters for the planet Kepler-22b, including a revised mass of MP < 53 M⊕ to 95% confidence and an eccentricity of by exploiting Single-body Asterodensity Profiling. Finally, we show that Kepler-22b has a >95% probability of being within the empirical habitable zone but a <5% probability of being within the conservative habitable zone.
Is the proposed SI revision, according to the October 2018 BIPM documents, scientifically and formally satisfactory?

The use of the fundamental constants for the definition of the most important measurement units of the International System, was considered a good solution to found it on more solid bases. From further analysis, this solution was found implying a number of consequences underevaluated by the BIPM until the proposal presented for discussion in November 2018 to the CGPM, or at least never clearly explained to the signatories Countries of the Metre Treaty. This lack of clarity will affect the implementations of the revised System in the future. Following previous illustrations, this v.5 of the paper is focusing on some issues of direct impact on the correctness of the new definition and on its implementation: how many digits, supported by the latest experimental values, can be stipulated for the numerical values of the constants; why the present experimental uncertainties do not support the pretended precision of the constants; how inconsistencies affect some constant final database; why the CODATA LSA analysis alone is insufficient to support the stipulated precision of the constants; how the need should be explained of keeping the former base units, in order to preserve their present magnitudes; which is the true base-units/constants relationship; how the now-installed hierarchy between the constants and the base units makes changes in the future metrological pyramid; how to still use the present top national standards in future.
Gravity vs. Quantum theory: Is electron really pointlike?

The observable gravitational and electromagnetic parameters of an electron: mass m, spin J = ℏ/2, charge e and magnetic moment ea = eℏ/(2m) indicate unambiguously that the electron should had the Kerr-Newman background geometry – exact solution of the Einstein-Maxwell gravity for a charged and rotating black hole. Contrary to the widespread opinion that gravity plays essential role only on the Planck scales, the Kerr-Newman gravity displays a new dimensional parameter a = ℏ/(2m), which for parameters of an electron corresponds to the Compton wavelength and turns out to be very far from the Planck scale. Extremely large spin of the electron with respect to its mass produces the Kerr geometry without horizon, which displays very essential topological changes at the Compton distance resulting in a two-fold structure of the electron background. The corresponding gravitational and electromagnetic fields of the electron are concentrated near the Kerr ring, forming a sort of a closed string, structure of which is close to the described by Sen heterotic string. The indicated by Gravity stringlike structure of the electron contradicts to the statements of Quantum theory that electron is pointlike and structureless. However, it confirms the peculiar role of the Compton zone of the "dressed" electron and matches with the known limit of the localization of the Dirac electron. We discuss the relation of the Kerr string with the low energy string theory and with the Dirac theory of electron and suggest that the predicted by the Kerr-Newman gravity closed string in the core of the electron, should be experimentally observable by the novel regime of the high energy scattering - the Deeply Virtual (or "nonforward") Compton Scattering".