Miracle-dz/UniFAR-FTUs huggingface dataset:
ORBITAL SOLUTIONS FOR TWO YOUNG, LOW-MASS SPECTROSCOPIC BINARIES IN OPHIUCHUS

We report the orbital parameters for ROXR1 14 and RX J1622.7−2325Nw, two young, low-mass, and double-lined spectroscopic binaries recently discovered in the Ophiuchus star-forming region. Accurate orbital solutions were determined from over a dozen high-resolution spectra taken with the Keck II and Gemini South telescopes. These objects are T Tauri stars with mass ratios close to unity and periods of ∼5 and ∼3 days, respectively. In particular, RX J1622.7−2325Nw shows a non-circularized orbit with an eccentricity of 0.30, higher than any other short-period pre-main-sequence (PMS) spectroscopic binary known to date. We speculate that the orbit of RX J1622.7−2325Nw has not yet circularized because of the perturbing action of a ∼1″ companion, itself a close visual pair. A comparison of known young spectroscopic binaries (SBs) and main-sequence (MS) SBs in the eccentricity–period plane shows an indistinguishable distribution of the two populations, implying that orbital circularization occurs in the first 1 Myr of a star's lifetime. With the results presented in this paper we increase by ∼4% the small sample of PMS spectroscopic binary stars with known orbital elements.
Helicity and α-effect by current-driven instabilities of helical magnetic fields

Helical magnetic background fields with an adjustable pitch angle are imposed on a conducting fluid in a differentially rotating cylindrical container. The small-scale kinetic and current helicities are calculated for various field geometries, and shown to have the opposite sign to the helicity of the large-scale field. These helicities and also the corresponding α-effect scale with the current helicity of the background field. The α-tensor is highly anisotropic as the components αϕϕ and αzz have opposite signs. The amplitudes of the azimuthal α-effect computed with the cylindrical 3D magnetohydrodynamics code are so small that the operation of an αΩ-dynamo on the basis of the current-driven, kink-type instabilities of toroidal fields is highly questionable. In any case, the low value of the α-effect would lead to very long growth times of a dynamo in the radiation zone of the Sun and early-type stars of the order of megayears.
Nonmetallic Low-Temperature Normal State of K 0.7 Fe 1.46 Se 1.85 Te 0.15

The normal-state in-plane resistivity below the zero-field superconducting transition temperature $T_c$ and the upper critical field Hc2 were measured by suppressing superconductivity in pulsed magnetic fields for K0.70Fe1. 46Se1.85Te0. 15. The normal-state resistivity $\rho_{ab}$ is found to increase logarithmically with decrasing temperature as $\frac{T}{T_c}\rightarrow 0$. Similar to granular metals, our results suggest that a superconductor - insulator transition below zero-field T$_{c}$ may be induced in high magnetic fields. This is related to the intrinsic real-space phase-separated states common to all inhomogeneous superconductors.
Electric field-induced colossal electroresistance and its relaxation in multiferroic La2NiMnO6

In this work, we report direct as well as pulsed electric field-induced resistivity switching and its relaxation in a multiferroic insulator La2NiMnO6. At a fixed base temperature (Tb), the dc resistivity switches abruptly from a high to a low value, which is manifested as an upward jump in the dc current density (J) when the electric field (E) exceeds a threshold value Eth. The fractional change in the resistance is as much as 70 % at room temperature for Eth = 95 V/cm. The Eth increases with lowering Tb and follows the relation Eth(Tb) = Eth(0)exp[-Tb/T0], as similar to the behavior found in charge density wave systems. It is shown that the abrupt jump in J vanishes under pulsed electric fields if the period between pulses is long enough. Surprisingly, a step-like increase in J also occurs at a fixed dc electric field (Ec) and T = Tb, above a threshold waiting time (tth). The tth decreases with increasing Ec and Tb. Simultaneous measurement of surface temperature during the J-E sweep and temporal studies suggest that conductive channels are created in an insulating matrix due to the local self heating, and the coalescence of these channels above a threshold E- field or time causes the observed anomalies in J. However, the dissipated Joule power (P = Ith2R) at the transition from high to low resistive state in the sample decreases with lowering temperature, which suggests that the Joule heating is the consequence of transition from the high to low resistance state rather than itself a driving force of the non linear electrical transport. In addition, non linear J-E characteristics is also found even with a pulsed voltage sweep, which suggests that intrinsic mechanisms other than self heating is still active in this material.
Non-communicable disease policy implementation in Libya: A mixed methods assessment

The Libyan Ministry of Health is keen to understand how it can introduce policies to protect its population from non-communicable diseases (NCDs). We aimed to perform an implementation research assessment of the current situation, including challenges and opportunities. We used an explanatory sequential mixed methods design. We started with a quantitative assessment of NCD policy performance based on review of the WHO NCD Progress Monitor Reports. Once we had identified Libya’s NCD policy gaps we performed a systematic review to identify international lessons around barriers and successful strategies for the policies Libya has not yet implemented. Finally, we performed a series of key stakeholder interviews with senior policymakers to explore their perspectives around promising policy actions. We used a realist paradigm, methods triangulation, and a joint display to synthesise the interpretation of our findings and develop recommendations. Libya has not fully implemented any of the recommended policies for diet, physical activity, primary care guidelines & therapeutics, or data collection, targets & surveillance. It does not have robust tobacco policies in place. Evidence from the international literature and policymaker interviews emphasised the centrality of according strong political leadership, governance structures, multisectoral engagement, and adequate financing to policy development activities. Libya’s complex political and security situation are major barriers for policy implementation. Whilst some policies will be very challenging to develop and deploy, there are a number of simple policy actions that could be implemented with minimum effort; from inviting WHO to conduct a second STEPS survey, to signing the international code on breast-milk substitutes. Like many other fragile and conflict-affected states, Libya has not accorded NCDs the policy attention they demand. Whilst strong high-level leadership is the ultimate key to providing adequate protections, there are a range of simple measures that can be implemented with relative ease.
Diabetes Melitus tipe 2 sebagai faktor risiko penyakit jantung koroner (PJK) di RSUD Raden Mattaher Jambi tahun 2019

Penyakit Jantung Koroner (PJK) masih menjadi salah satu penyebab kematian terbanyak di Indonesia. Diabetes Mellitus tipe 2 (DM tipe 2) merupakan salah satu faktor risiko PJK. Di provinsi Jambi pada tahun 2015 diperkirakan jumlah pasien PJK sebanyak ±2000 pasien. Salah satu upaya untuk menurunkan jumlah kasus PJK adalah dengan mengetahui faktor-faktor risiko yang menyebabkan terjadinya PJK. Studi ini bertujuan untuk memberikan gambaran mengenai DM tipe 2 sebagai faktor risiko PJK di Rumah Sakit rujukan terbesar di Jambi, yaitu RSUD Raden Mattaher Jambi pada tahun 2019. Metode studi ini adalah analitik observasional dengan desain case control. Sampel studi terdiri dari 145 pasien PJK (kelompok kasus) dan 145 pasien tanpa PJK (kelompok kontrol). Penggumpulan data dilakukan dengan mengobservasi data sekunder yang didapatkan dari rekam medis pasien. Dilakukan uji korelasi antara DM tipe 2 dan PJK. Hasil tersebut menunjukkan bahwa pasien DM tipe 2 berisiko 2 kali lebih tinggi untuk menderita PJK dibandingkan dengan pasien tanpa DM tipe 2 (OR=2,07). Hasil analisis multivariat menunjukkan bahwa pada Dislipidemia merupakan faktor risiko yang berpengaruh paling signifikan dalam menyebabkan PJK di RSUD Raden Mattaher Jambi pada tahun 2019 dibandingkan faktor risiko lain. Kesimpulan dari penelitian ini adalah DM tipe 2 (p=0.006) memang merupakan faktor risiko PJK di RSUD Raden Mattaher Jambi pada tahun 2019 tetapi, Dislipidemia (p< 0,0001) memiliki pengaruh yang paling signifikan kemudian diikuti oleh Hipertensi (p= 0,004). Penyakit Sistemik (p=0,025) dan riwayat merokok (p= 0,005) juga merupakan faktor risiko yang menyebabkan PJK di RSUD Raden Mattaher Jambi pada tahun 2019.
Spatial scalar correlator in strongly coupled hot N=4 Yang-Mills theory

We use anti-de Sitter/CFT duality to compute in N=4 Yang-Mills theory the finite temperature spatial correlator G(r) of the scalar operator F{sup 2}, integrated over imaginary time. The computation is carried out both at zero frequency and integrating the spectral function over frequencies. The result is compared with a perturbative computation in finite T SU(N{sub c}) Yang-Mills theory.
Magnetic Imprisonment of Dusty Pinballs by a Supernova Remnant

Motivated by recent measurements of deposits of 60Fe on the ocean floor and the lunar surface, we model the transport of dust grains containing 60Fe from a near-Earth (i.e., within 100 pc) supernova (SN). We inject dust grains into the environment of an SN remnant (SNR) and trace their trajectories by applying a 1D hydrodynamic description assuming spherical symmetry to describe the plasma dynamics, and we include a rudimentary, 3D magnetic field description to examine its influence on charged dust grains. We assume the interstellar medium (ISM) magnetic fields are turbulent and are amplified by the SNR shock, while the SN wind and ejecta fields are negligible. We examine the various influences on the dust grains within the SNR to determine when/if the dust decouples from the plasma, how much it is sputtered, and where within the SNR the dust grains are located. We find that Rayleigh–Taylor instabilities are important for dust survival, as they influence the location of the SN’s reverse shock. We find that the presence of a magnetic field within the shocked ISM material limits the passage of SN dust grains, with the field either reflecting or trapping the grains within the heart of the SNR. These results have important implications for in situ 60Fe measurements and for dust evolution in SNRs generally.
A NEW RADIO RECOMBINATION LINE MASER OBJECT TOWARD THE MonR2 H ii REGION

We report the detection of a new radio recombination line (RRL) maser object toward the IRS2 source in the MonR2 ultracompact H ii region. The continuum emission at 1.3 mm and 0.85 mm and the H30α and H26α lines were observed with the Submillimeter Array (SMA) at angular resolutions of ∼0. ″5–3″. The SMA observations show that the MonR2-IRS2 source is very compact and remains unresolved at spatial scales ⩽400 AU. Its continuum power spectrum at millimeter wavelengths is almost flat (α = −0.16, with Sν∝να), indicating that this source is dominated by optically thin free–free emission. The H30α and H26α RRL emission is also compact and peaks toward the position of the MonR2-IRS2 source. The measured RRL profiles are double peaked with the H26α line showing a clear asymmetry in its spectrum. Since the derived line-to-continuum flux ratios (∼80 and 180 km s−1 for H30α and H26α, respectively) exceed the LTE predictions, the RRLs toward MonR2-IRS2 are affected by maser amplification. The amplification factors are, however, smaller than those found toward the emission-line star MWC349A, indicating that MonR2-IRS2 is a weakly amplified maser. Radiative transfer modeling of the RRL emission toward this source shows that the RRL masers arise from a dense and collimated jet embedded in a cylindrical ionized wind, oriented nearly along the direction of the line of sight. High-angular resolution observations at submillimeter wavelengths are needed to unveil weakly amplified RRL masers in very young massive stars.
Probing the Hot X-Ray Corona around the Massive Spiral Galaxy, NGC 6753, Using Deep XMM-Newton Observations

X-ray emitting gaseous coronae around massive galaxies are a basic prediction of galaxy formation models. Although the coronae around spiral galaxies offer a fundamental test of these models, observational constraints on their characteristics are still scarce. While the presence of extended hot coronae has been established around a handful of massive spiral galaxies, the short X-ray observations only allowed for measurements of the basic characteristics of the coronae. In this work, we utilize deep XMM-Newton observations of NGC 6753 to explore its extended X-ray corona in unprecedented detail. Specifically, we establish the isotropic morphology of the hot gas, suggesting that it resides in hydrostatic equilibrium. The temperature profile of the gas shows a decrease with an increasing radius: it drops from in the innermost parts to at a 50 kpc radius. The temperature map reveals the complex temperature structure of the gas. We study the metallicity distribution of the gas, which is uniform at Solar. This value is about an order of magnitude lower than that obtained for elliptical galaxies with similar dark matter halo mass, hinting that the hot gas in spiral galaxies predominantly originates from external gas inflows rather than from internal sources. By extrapolating the density profile of the hot gas out to the virial radius, we estimate the total gas mass and derive the total baryon mass of NGC 6753. We conclude that the baryon mass fraction is , implying that about half of the baryons are missing.
Magnetic fields and differential rotation on the pre-main sequence - I. The early-G star HD 141943 - brightness and magnetic topologies

Spectroscopic and spectropolarimetric observations of the pre-main sequence early-G star HD 141943 were obtained at four observing epochs (in 2006, 2007, 2009 and 2010). The observations were undertaken at the 3.9-m Anglo-Australian Telescope using the UCLES echelle spectrograph and the SEMPOL spectropolarimeter visitor instrument. Brightness and surface magnetic field topologies were reconstructed for the star using the technique of least-squares deconvolution to increase the signal-to-noise ratio of the data. The reconstructed brightness maps show that HD 141943 had a weak polar spot and a significant amount of low-latitude features, with little change in the latitude distribution of the spots over the 4 yr of observations. The surface magnetic field was reconstructed at three of the epochs from a high-order (l≤ 30) spherical harmonic expansion of the spectropolarimetric observations. The reconstructed magnetic topologies show that in 2007 and 2010 the surface magnetic field was reasonably balanced between poloidal and toroidal components. However, we find tentative evidence of a change in the poloidal/toroidal ratio in 2009 with the poloidal component becoming more dominant. At all epochs the radial magnetic field is predominantly non-axisymmetric while the azimuthal field is predominantly axisymmetric with a ring of positive azimuthal field around the pole similar to that seen on other active stars.
Synthesis and characterization of a lactose-based biosurfactant by a novel nanodendritic catalyst and evaluating its efficacy as an emulsifier in a food emulsion system

Nonionic lactose fatty acid esters are a class of synthetic biosurfactants with various uses in the food, pharmaceutical, personal care, and cosmetic industries. The objective of this research was the preparation and full characterization of a series of novel metallic encapsulated magnetic core/dendrimer shell composites as catalysts (CoII/MnII G2.0L1/2@SCMBNP) and their use in the chemo- and regioselective synthesis of a biosurfactant for the first time. Surface-active properties (such as contact angle (CA), surface tension (SFT), interfacial tension (IFT), critical micelle concentration (CMC), hydrophilic–lipophilic balance (HLB), foamability (FA) & foam stability (FS), emulsion ability (EmA) & emulsion stability (EmS), surface excess (Γ) and free energy of adsorption (ΔG) were also determined for all synthesized biosurfactants. In comparison to other works, these results suggested that the synthesized lactose fatty acid esters have potential application as synthetic emulsifiers featuring surface properties and are comparable with Ryoto sugar ester L-1695 (sucrose laurate) & Tween-20 (polysorbate 20) as industrial emulsifiers. The optimized conditions for biosurfactant syntheses are 8 days at 2 : 1 molar ratio of lactose sugar to lauric acid at 50 °C. Lactose ester as a biosurfactant exhibited a decrease of SFT & IFT and was able to stabilize a 20% soybean O/W emulsion. Furthermore, high conversion & yield, excellent chemo- and regioselectivity, and high operational stability over 5 runs were achieved for CoII/MnII-G2.0L1/2@SCMBNP, indicating the suitable efficiency of the catalytic process.
Testing the hadro-quarkonium model on the lattice

Recently the LHCb experiment found evidence for the existence of two exotic resonances consisting of $c\bar{c}uud$ quarks. Among the possible interpretations is the hadro-charmonium model, in which charmonium is bound "within" a light hadron. We test this idea on CLS $N_f$=2+1 lattices using the static formulation for the heavy quarks. We find that the static potential is modified by the presence of a hadron such that it becomes more attractive. The effect is of the order of a few MeV.
Photometry and spectroscopy of SN 2015bh in the galaxy NGC 2770

We present medium-resolution spectroscopy and multicolor photometry for the optical transient PSN J09093496+3307204 (SN 2015bh) in the galaxy NGC 2770, which has transferred into the supernova phase. The observations were carried out between February 2015 to May 2016. Both at the phase of the SN impostor (2015a) and at the supernova phase (2015b), besides Balmer emissions, the strong Fe II emissions are seen in the spectrum; so, these spectra resemble those of Williams Fe II type classical novae. The star is located near the edge of a dark nebula and notably absorbed (Av = 1.14 +/-0.15 mag). Taking into account this absorption, we determined maximum absolute magnitudes of Mv = -15.0 +/-0.3 mag at the 2015a phase and of Mv = -18.14 +/-0.30 mag at the 2015b phase. The light curve at the 2015b phase is similar to those of SN IIL. The supernova progenitor is a luminous blue variable (LBV) star with the powerful H{\alpha} emission. We considered several hypotheses of supernovae explosions following optical transients related with LBV. The hypothesis of core collapse of an evolved massive star interrupting the process of its merging with massive companion in a binary system (a failed luminous red nova) was chosen as the preferable one for this event.
Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera

The summit of the Antarctic plateau, Dome A, is proving to be an excellent site for optical, near-infrared, and terahertz astronomical observations. Gattini is a wide-field camera installed on the PLATO instrument module as part of the Chinese-led traverse to Dome A in 2009 January. We present here the measurements of sky brightness with the Gattini ultra-large field of view ( ) in the photometric B-, V-, and R-bands; cloud cover statistics measured during the 2009 winter season; and an estimate of the sky transparency. A cumulative probability distribution indicates that the darkest 10% of the nights at Dome A have sky brightness of SB = 22.98, SV = 21.86, and SR = 21.68 mag arcsec−2. These values were obtained during the year 2009 with minimum aurora, and they are comparable to the faintest sky brightness at Maunakea and the best sites of northern Chile. Since every filter includes strong auroral lines that effectively contaminate the sky brightness measurements, for instruments working around the auroral lines, either with custom filters or with high spectral resolution instruments, these values could be easily obtained on a more routine basis. In addition, we present example light curves for bright targets to emphasize the unprecedented observational window function available from this ground-based site. These light curves will be published in a future paper.
ULTRAFAINT DWARFS—STAR FORMATION AND CHEMICAL EVOLUTION IN THE SMALLEST GALAXIES

In earlier work, we showed that a dark matter halo with a virial mass of 107 M☉ can retain a major part of its baryons in the face of the pre-ionization phase and supernova (SN) explosion from a 25 M☉ star. Here, we expand on the results of that work, investigating the star formation and chemical evolution of the system beyond the first SN. In a galaxy with a mass Mvir = 107 M☉, sufficient gas is retained by the potential for a second period of star formation to occur. The impact of a central explosion is found to be much stronger than that of an off-center explosion both in blowing out the gas and in enriching it, as in the off-center case most of the SN energy and metals escape into the intergalactic medium. We model the star formation and metallicity, given the assumption that stars form for 100, 200, 400, and 600 Myr, and discuss the results in the context of recent observations of very low-mass galaxies. We show that we can account for most features of the observed relationship between [α/Fe] and [Fe/H] in ultra-faint dwarf galaxies with the assumption that the systems formed at a low mass, rather than being remnants of much larger systems.
Numerical solutions of Einstein's equations for cosmological spacetimes with spatial topology S 3 and symmetry group U(1)

We apply a single patch pseudo-spectral scheme based on integer spin-weighted spherical harmonics presented in [1, 2] to Einstein’s equations. The particular hyperbolic reduction of Einstein’s equations which we use is obtained by a covariant version of the generalized harmonic formalism and Geroch’s symmetry reduction. In this paper we focus on spacetimes with a spatial S 3 -topology and symmetry group U(1). We discuss analytical and numerical issues related to our implementation. As a test, we reproduce numerically exact inhomogeneous cosmological solutions of the vacuum Einstein eld equations obtained in [3].
Stellar population gradients in brightest cluster galaxies

Abstract We present the stellar population and velocity dispersion gradients for a sample of 24 brightest cluster galaxies (BCGs) in the nearby Universe for which we have obtained high quality long-slit spectra at the Gemini telescopes. With the aim of studying the possible connection between the formation of the BCGs and their host clusters, we explore the relations between the stellar population gradients and properties of the host clusters, as well as the possible connections between the stellar population gradients and other properties of the galaxies. We find mean stellar population gradients (negative Δ[Z/H]/log r gradient of − 0.285 ± 0.064; small positive Δlog(age)/log r gradient of +0.069 ± 0.049; and null Δ[E/Fe]/log r gradient of -0.008 ± 0.032), that are consistent with those of normal massive elliptical galaxies. However, we find a trend between metallicity gradients and velocity dispersion (with a negative slope of − 1.616 ± 0.539), that is not found for the most massive ellipticals. Furthermore, we find trends between the metallicity gradients and K-band luminosities (with a slope of 0.173 ± 0.081) as well as the distance from the BCG to the X-ray peak of the host cluster (with a slope of − 7.546 ± 2.752). The latter indicates a possible relation between the formation of the cluster and that of the central galaxy.