Miracle-dz/UniFAR-FTUs huggingface dataset:
Grid of theoretical NLTE equivalent widths of four Ba II lines and barium abundance in cool stars

We present a grid of computed non-local thermodynamic equilibrium (NLTE) equivalent widths (EW) and NLTE abundance corrections for four Ba II lines: 4554, 5853, 6141, and 6496 A. The grid can be useful in deriving the NLTE barium abundance in stars having parameters in the following ranges: effective temperature from 4000 K to 6500 K, surface gravity log g from 0 to 5, microturbulent velocity 0 km s^-1 to 3 km s^-1, metallicity [Fe/H] from -2 to +0.5, and [Ba/Fe] from -0.4 to +0.6. The NLTE abundance can be either derived by EW interpolation (using the observed Ba II line EW) or by using the NLTE correction applied to a previously determined LTE abundance. Ba II line equivalent widths and the NLTE corrections were calculated using the updated MULTI code and the Ba II atomic model that was previously applied to determine the NLTE barium abundance in different types of stars. The grid is available on-line through the web, and we find that the grid Ba NLTE corrections are almost as accurate as direct NLTE profile fitting (to within 0.05-0.08 dex). For the weakest Ba II line (5853 A) the LTE abundances almost agree with the NLTE abundances, whereas the other three Ba II lines, 4554, 6141, and 6496 A, need NLTE corrections even at the highest metallicities tested here. The 4554 A line is extremely strong and should not be used for abundance analysis above [Fe/H]= -1. Furthermore, we tested the impact of different model atmospheres and spectrum synthesis codes and found average differences of 0.06 dex and 0.09 dex, respectively, for all four lines. At these metallicities we find an average Delta NLTE of +/-0.1 dex for the three useful Ba lines for subsolar cool dwarfs.
Augmenting a COVID-19 Research Knowledge Graph with Influential Papers Prediction

We applied machine learning to predict which of COVID-19-related papers will be highly cited, yielding an extension for the Covid-on-the-Web knowledge graph. Symbolic and deep-learning (BERT) ML performed comparably. LIME-based explanation is also included as part of the produced graph. © 2022 Copyright for this paper by its authors. Use permitted under Creative Commons License Attribution 4.0 International (CC BY 4.0)
Comment on 'To Criticize the Critics,' by Peter C. B. Phillips

In his paper "To Criticize the Critics" (1991), Peter Phillips discusses Bayesian methodology for time series models. The main point that Uhlig and I set out to make, however, was that careful consideration of the implications of the likelihood principle suggests that much of the recent work under the "unit root" label in the econometrics literature is being incorrectly interpreted in practice. We pointed out that time series models with possible unit roots are one of the few domains within which the implications of a likelihood principle approach to inference are difference, even in the large samples, from those of a classical hypothesis testing approach. Phillips addresses this part of our paper only indirectly.
IS THERE A MAXIMUM STAR FORMATION RATE IN HIGH-REDSHIFT GALAXIES?,,,

We use the James Clerk Maxwell Telescope's SCUBA-2 camera to image a 400 arcmin2 area surrounding the GOODS-N field. The 850 μm rms noise ranges from a value of 0.49 mJy in the central region to 3.5 mJy at the outside edge. From these data, we construct an 850 μm source catalog to 2 mJy containing 49 sources detected above the 4σ level. We use an ultradeep (11.5 μJy at 5σ) 1.4 GHz image obtained with the Karl G. Jansky Very Large Array together with observations made with the Submillimeter Array to identify counterparts to the submillimeter galaxies. For most cases of multiple radio counterparts, we can identify the correct counterpart from new and existing Submillimeter Array data. We have spectroscopic redshifts for 62% of the radio sources in the 9′ radius highest sensitivity region (556/894) and 67% of the radio sources in the GOODS-N region (367/543). We supplement these with a modest number of additional photometric redshifts in the GOODS-N region (30). We measure millimetric redshifts from the radio to submillimeter flux ratios for the unidentified submillimeter sample, assuming an Arp 220 spectral energy distribution. We find a radio-flux-dependent K − z relation for the radio sources, which we use to estimate redshifts for the remaining radio sources. We determine the star formation rates (SFRs) of the submillimeter sources based on their radio powers and their submillimeter fluxes and find that they agree well. The radio data are deep enough to detect star-forming galaxies with SFRs >2000 M☉ yr−1 to z ∼ 6. We find galaxies with SFRs up to ∼6000 M☉ yr−1 over the redshift range z = 1.5–6, but we see evidence for a turn-down in the SFR distribution function above 2000 M☉ yr−1.
The thick disk rotation-metallicity correlation as a fossil of an “inverse chemical gradient” in the early Galaxy

Context. The thick disk rotation-metallicity correlation, ∂Vφ/∂[Fe/H] = 40 ÷ 50 km s −1 dex −1 represents an important signature of the formation processes of the galactic disk. Aims. We use nondissipative numerical simulations to follow the evolution of a Milky Way (MW)-like disk to verify if secular dynamical processes can account for this correlation in the old thick disk stellar population. Methods. We followed the evolution of an ancient disk population represented by 10 million particles whose chemical abundances were assigned by assuming a cosmologically plausible radial metallicity gradient with lower metallicity in the inner regions, as expected for the 10-Gyr-old MW. The two cases of a disk with and without a bar were simulated to compare the evolution of their kinematics and radial chemical properties. Results. Migration processes act in both cases and appear to be enhanced in the presence of a central bar. Essentially, inner disk stars move towards the outer regions and populate layers located at higher |z|. In the case of an evolved barred disk, a rotation-metallicity correlation appears, which well resembles the behaviour observed in our Galaxy at a galactocentric distance between 8 kpc and 10 kpc. In particular, we measure a correlation of ∂Vφ/∂ [Fe/H] � 60 km s −1 dex −1 for particles at 1.5 kpc < |z| < 2.0 kpc that persists up to 6G yr. Conclusions. Our pure N-body models can account for the Vφ vs. [Fe/H] correlation observed in the thick disk of our Galaxy, suggesting that processes internal to the disk such as heating and radial migration play a role in the formation of this old stellar component. In this scenario, the positive rotation-metallicity correlation of the old thick disk population would represent the relic signature of an ancient inverse chemical (radial) gradient in the inner Galaxy, which resulted from accretion of primordial gas.
Effectiveness of Opioid Analgesic Medicines Prescribed in or at Discharge From Emergency Departments for Musculoskeletal Pain

BACKGROUND The comparative benefits and harms of opioids for musculoskeletal pain in the emergency department (ED) are uncertain. PURPOSE To evaluate the comparative effectiveness and harms of opioids for musculoskeletal pain in the ED setting. DATA SOURCES Electronic databases and registries from inception to 7 February 2022. STUDY SELECTION Randomized controlled trials of any opioid analgesic compared with placebo or a nonopioid analgesic administered or prescribed to adults in or on discharge from the ED. DATA EXTRACTION Pain and disability were rated on a scale of 0 to 100 and pooled using a random-effects model. Certainty of evidence was assessed using the GRADE (Grading of Recommendations Assessment, Development and Evaluation) framework. DATA SYNTHESIS Forty-two articles were included (n = 6128). In the ED, opioids were statistically but not clinically more effective in reducing pain in the short term (about 2 hours) than placebo and paracetamol (acetaminophen) but were not clinically or statistically more effective than nonsteroidal anti-inflammatory drugs (NSAIDs) or local or systemic anesthetics. Opioids may carry higher risk for harms than placebo, paracetamol, or NSAIDs, although evidence is very uncertain. There was no evidence of difference in harms associated with local or systemic anesthetics. LIMITATIONS Low or very low GRADE ratings for some outcomes, unexplained heterogeneity, and little information on long-term outcomes. CONCLUSION The risk-benefit balance of opioids versus placebo, paracetamol, NSAIDs, and local or systemic anesthetics is uncertain. Opioids may have equivalent pain outcomes compared with NSAIDs, but evidence on comparisons of harms is very uncertain and heterogeneous. Although factors such as route of administration or dosage may explain some heterogeneity, more work is needed to identify which subgroups will have a more favorable benefit-risk balance for one analgesic over another. Longer-term pain management once dose thresholds are reached is also uncertain. PRIMARY FUNDING SOURCE None. (PROSPERO: CRD42021275293).
Enterococcus faecium Clade Competition in the Presence of β-Lactam Antibiotics in a Mouse GI Tract Colonization Model

Previously, we showed that Enterococcus faecium clade B strains outcompeted health care-associated clade A1 strains in murine gastrointestinal colonization. Here, parenterally administered piperacillin-tazobactam and ceftriaxone significantly promoted colonization by clade A1 over clade B strains except that ceftriaxone, at the dose used, did not favor the least β-lactam-resistant A1 strain. ABSTRACT Previously, we showed that Enterococcus faecium clade B strains outcompeted health care-associated clade A1 strains in murine gastrointestinal colonization. Here, parenterally administered piperacillin-tazobactam and ceftriaxone significantly promoted colonization by clade A1 over clade B strains except that ceftriaxone, at the dose used, did not favor the least β-lactam-resistant A1 strain. The advantage that β-lactam administration gives to more highly ampicillin-resistant E. faecium over ampicillin-susceptible strains mirrors what occurs in hospitalized patients administered these antibiotics.
Relativistic Quantum Mechanics: With Applications in Condensed Matter and Atomic Physics

Preface 1. The theory of special relativity 2. Aspects of angular momentum 3. Particles of spin zero 4. The Dirac equation 5. Free particles/antiparticles 6. Symmetries and operators 7. Separating particles from antiparticles 8. One electron atoms 9. Potential problems 10. More than one electron 11. Scattering theory 12. Electrons and photons 13. Superconductivity Appendices References Index.
IS THERE A MAXIMUM MASS FOR BLACK HOLES IN GALACTIC NUCLEI?

The largest observed supermassive black holes (SMBHs) have a mass of , nearly independent of redshift, from the local ( ) to the early ( ) universe. We suggest that the growth of SMBHs above a few is prevented by small-scale accretion physics, independent of the properties of their host galaxies or of cosmology. Growing more massive BHs requires a gas supply rate from galactic scales onto a nuclear region as high as . At such a high accretion rate, most of the gas converts to stars at large radii (∼10–100 pc), well before reaching the BH. We adopt a simple model for a star-forming accretion disk and find that the accretion rate in the subparsec nuclear region is reduced to the smaller value of at most a few . This prevents SMBHs from growing above in the age of the universe. Furthermore, once an SMBH reaches a sufficiently high mass, this rate falls below the critical value at which the accretion flow becomes advection dominated. Once this transition occurs, BH feeding can be suppressed by strong outflows and jets from hot gas near the BH. We find that the maximum SMBH mass, given by this transition, is between , depending primarily on the efficiency of angular momentum transfer inside the galactic disk, and not on other properties of the host galaxy.
Modeling X-Ray Loops and EUV “Moss” in an Active Region Core

The soft X-ray intensity of loops in active region cores and the corresponding footpoint, or moss, intensity observed in the EUV remain steady for several hours of observation. The steadiness of the emission has prompted many to suggest that the heating in these loops must also be steady, although no direct comparison between the observed X-ray and EUV intensities and the steady heating solutions of the hydrodynamic equations has yet been made. In this paper we perform these simulations and simultaneously model the X-ray and EUV moss intensities in one active region core with steady uniform heating. To perform this task, we introduce a new technique to constrain the model parameters using the measured EUV footpoint intensity to infer a heating rate. Using an ensemble of loop structures derived from magnetic field extrapolation of photospheric field, we associate each field line with an EUV moss intensity, then determine the steady uniform heating rate on that field line that reproduces the observed EUV intensity within 5% for a specific cross-sectional area, or filling factor. We then calculate the total X-ray filter intensities from all loops in the ensemble and compare this to the observed X-ray intensities. We complete this task iteratively to determine the filling factor that returns the best match to the observed X-ray intensities. We find that a filling factor of 8% and loops that expand with height provides the best agreement with the intensity in two X-ray filters, although the simulated SXT Al12 intensity is 147% the observed intensity and the SXT AlMg intensity is 80% the observed intensity. From this solution we determine the required heating rate scales as B̄0.29L−0.95. Finally, we discuss the future potential of this type of modeling, such as the ability to use density measurements to fully constrain filling factor, and its shortcomings, such as the requirement to use potential field extrapolations to approximate the coronal field.
A single-blind, randomised controlled trial of a physical health nurse intervention to prevent weight gain and metabolic complications in first-episode psychosis: the Physical Health Assistance in Early Psychosis (PHAstER) study

Background Factors that contribute to the early mortality observed in psychotic disorders, specifically obesity, smoking and sedentary behaviour, occur early in the disorder. Aims We aimed to determine whether the integration of a physical health nurse in the care of young people with first-episode psychosis could prevent clinically significant weight gain (≥7% body weight). Secondary outcomes included rates of smoking, metabolic syndrome and sedentary behaviour. Method In this single-blind, randomised controlled trial, participants who had received under 4 weeks of antipsychotic medication were randomly allocated to either the intervention (addition of a physical health nurse to their care) or treatment as usual (TAU) for 12 weeks. Results Of the 77 participants, there were follow-up data for 86.8% (n = 33) of the intervention group and 82.1% (n = 32) of the TAU group. After 12 weeks, 27.3% of the intervention group experienced clinically significant weight gain compared with 34.4% of the TAU group (odds ratio 0.72, 95% CI 0.25–2.06, P = 0.54). After 6 months, 40.7% of the intervention group gained clinically significant weight compared with 44.1% of the TAU group (P = 0.79). There was no difference in mean change in weight between groups after 12 weeks (2.6 kg v. 2.9 kg, P = 0.87) or 6 months (3.6 kg v. 4.3 kg, P = 0.64). There were no differences in the rates of tobacco smoking cessation, prevalence of metabolic syndrome or physical activity levels. Conclusions This intervention failed to prevent the metabolic complications that are highly prevalent in psychotic disorders in the short to medium term, indicating that more intensive interventions are required.
The Proper Motion of SGR A

We have now been measuring the position of Sgr A*, the candidate supermassive black hole at the center of the Galaxy, with the VLBA for about 8 years. Sgr A* appears to move almost entirely along the Galactic Plane at a rate of 6.37±0.02 mas yr. For a distance to the Galactic Center of 8.0±0.5 kpc, this translates to 241 ± 15 km s , consistent with that expected for a stationary object observed from the Sun as it orbits the Galactic Center. The motion of Sgr A* out of the plane of the Galaxy, after removing the 7 km s motion of the Sun in that direction, is less than about 2 km s . Combining stellar orbital information (measured in the infrared) with the upper limit of 2 km s for the intrinsic proper motion of Sgr A* (perpendicular to the Galactic plane), places a lower limit on the mass of Sgr A* of 2 × 10 M⊙. Thus, most of the mass sensed by stellar orbits is tied to the compact radio source Sgr A*, whose size is less than 1 AU, yielding the strongest case ever for a SMBH. This also argues against “exotic” forms of mass, postulated to explain the extreme mass concentration at the Galactic Center.
THE ACCRETION OF DARK MATTER SUBHALOS WITHIN THE COSMIC WEB: PRIMORDIAL ANISOTROPIC DISTRIBUTION AND ITS UNIVERSALITY

The distribution of galaxies displays anisotropy on different scales and it is often referred to as galaxy alignment. To understand the origin of galaxy alignments on small scales, one must investigate how galaxies were accreted in the early universe and quantify their primordial anisotropy at the time of accretion. In this paper we use N-body simulations to investigate the accretion of subhalos, focusing on their alignment with halo shape and the orientation of mass distribution on the large scale, defined using the Hessian matrix of the density field. The large/small (e1/e3) eigenvalues of the Hessian matrix define the fast/slow collapse direction of matter on the large scale. We find that: (1) the halo major axis is well aligned with the e3 (slow collapse) direction, and it is stronger for massive halos; (2) subhalos are predominantly accreted along the major axis of the host halo, and the alignment increases with the host halo mass. Most importantly, this alignment is universal; (3) accretion of subhalos with respect to the e3 direction is not universal. In massive halos, subhalos are accreted along the e3 (even more strongly than the alignment with the halo major axis), but in low-mass halos subhalos are accreted perpendicular to e3. The transitional mass is lower at high redshift. The last result well explains the puzzling correlation (both in recent observations and simulations) that massive galaxies/halos have their spin perpendicular to the filament, and the spin of low-mass galaxies/halos is slightly aligned with the filament, under the assumption that the orbital angular momentum of subhalos is converted to halo spin.
Determinants of Capital Structure of Malaysian SMEs

This study tries to predict the determinants of Malaysian small and medium-sized enterprises (SMEs) financial structure. The study adds to the literature on SME financial structure by formally testing the impact of the quantity of accounting information on SME financial structure, a variable that has not been explicitly tested in the Malaysian context. Previous studies were also conducted in developed countries. Hence, the results may not be applicable in a developing countries like Malaysia. Using a sample of 100 manufacturing SMEs, their annual reports were analysed for selected variables. Financial structure (i.e. the dependent variable) was measured using the ratio of total liabilities to total assets. The explanatory variables employed were accounting quantity (type of accounting standard), firm size, firm age, asset structure, liquidity and profitability. Consistent with the traditional view that asymmetric or incomplete information restricts access to external funds, the result indicates that the quantity of financial statement information is positively related to SME leverage. Secondly, because the results for the control variables are consistent with prior studies, it can be concluded that the financial behaviour of Malaysian SMEs is comparable to that of SMEs in other developed countries. Specifically, the result shows that leverage is negatively related to firm size, liquidity and profitability. The findings also indicate that the traditional capital structure theories [i.e. Pecking-order theory (POT), trade-off theory and agency theory] are only partially relevant in explaining Malaysian SME capital structures, thus supporting the argument that no single theory gives a general explanation of firms’ financing strategies.
Mid-infrared period-luminosity relations for globular cluster RR Lyrae

The period - metallicity - WISE W1- and W2-band luminosity relations are derived for RR Lyrae stars based on WISE epoch photometry for 360 and 275 stars in 15 and 9 Galactic globular clusters, respectively. Our final relations have the form =γW1 -(2.381±0.097)log PF + (0.096±0.021)[Fe/H] and =γW2 -(2.269±0.127)log PF + (0.108±0.021)[Fe/H], where [Fe/H] values are on the scale of Carretta et al. (2009). We obtained two appreciably discrepant estimates for the zero points γW1 and γW2 of both relations: one based on a statistical-parallax analysis – γW1=-0.829±0.093 and γW2=-0.776±0.093 and another, significantly brighter one, based on HST FGS trigonometric parallaxes – γW1,HST=-1.150±0.077and γW2,HST=1.105±0.077. The period-metallicity-luminosity relations in the two bands yield highly consistent distance moduli for the calibrator clusters and the distance moduli computed using the W1- and W2-band relations with the HST zero points agree well with those computed by Sollima et al. (2006) based on their derived period-metallicity-Kband luminosity relation whose zero point is tied to the HST trigonometric parallax of RR Lyrae itself (�DM0 = 0.04 and 0.06, respectively, with a scatter of only 0.06).
Alignment without Decoupling: the Portal to Light Dark Matter in the MSSM

Author(s): Profumo, Stefano; Stefaniak, Tim | Abstract: We study light, thermal neutralino dark matter in the sub-GeV to 65 GeV mass range in the Minimal Supersymmetric extension of the Standard Model (MSSM). We consider realizations of the limit of alignment without decoupling in the Higgs sector where the heavier CP-even Higgs impersonates the observed Higgs state at 125 GeV, while the lighter CP-even Higgs is the mediator of dark matter annihilation. We single out three distinct and novel possibilities for light dark matter: (i) a neutralino with mass around half the light Higgs mass, in the sub-GeV to 30 GeV mass range; (ii) a neutralino with a mass around half the pseudoscalar Higgs boson mass, in our examples around 60 to 65 GeV; (iii) a very light neutralino with mass around the light Higgs mass, pair-annihilating to Higgs pairs. We discuss the implications of all these possibilities for indirect and direct dark matter detection experiments, and we demonstrate that all scenarios will be tested by next generation direct detection experiments. We also emphasize that the unique Higgs phenomenology of these scenarios warrants a dedicated search program at the LHC.
Über die Berechnung der Fourierkoeffizienten der Funktion j().

entwickelbar, wobei alle Foürierkoeffizienten natürliche Zahlen sind. Die ersten 25 dieser Foürierkoeffizienten wurden von Zuckerman [7] berechnet. Um diese Foürierkoeffizienten auf Kongruenzeigenschaften zu testen, wurden von mir die ersten 6002 dieser Foürierkoeffizienten berechnet. Das starke Anwachsen dieser Foürierkoeffizienten bewirkt, daß diese Tabelle nicht veröffentlicht werden kann. Auswertungen dieser Tabelle können nur wiederum mit Hilfe einer Rechenmaschine vorgenommen werden. Die Funktion j ( r ) erzeugt den Körper aller Modulfunktionen, d. h. jede unter der vollen Modulgruppe invariante, in der oberen Halbebene einschließlich der rationalen Randpunkte meromorphe Funktion ist eine rationale Funktion von j ( r ) . Diese rationale Funktion ist ein Polynom in J(T), falls sie im Inneren der oberen Halbebene holomorph ist. Sei p eine feste Primzahl. Bildet man die folgenden p + l Funktionen