Miracle-dz/UniFAR-FTUs huggingface dataset:
Uric acid effects on glutathione metabolism estimated by induction of glutamate-cysteine ligase, glutathione reductase and glutathione synthetase in mouse J744A.1 macrophage cell line.

INTRODUCTION Elevated plasma levels of uric acid (UA) are considered an independent risk factor for hypertension, diabetes, cardiovascular disease, endothelial and vascular damage, obesity, and metabolic syndrome. Even physiological concentrations of soluble UA have been proved to induce gene expression of macrophage-secreted inflammatory cytokines and stimulate production of reactive oxygen species in mature adipocytes. UA is also described as a powerful endogenous plasma antioxidant, which reveals a paradox of duality for this parameter.
THE MAGELLAN/IMACS CATALOG OF OPTICAL SUPERNOVA REMNANT CANDIDATES IN M83

We present a new optical imaging survey of supernova remnants (SNRs) in M83, using data obtained with the Magellan I 6.5 m telescope and IMACS instrument under conditions of excellent seeing. Using the criterion of strong [S ii] emission relative to Hα, we confirm all but three of the 71 SNR candidates listed in our previous survey, and expand the SNR candidate list to 225 objects, more than tripling the earlier sample. Comparing the optical survey with a new deep X-ray survey of M83 with Chandra, we find that 61 of these SNR candidates have X-ray counterparts. We also identify an additional list of 46 [O iii]-selected nebulae for follow-up as potential ejecta-dominated remnants, seven of which have associated X-ray emission that makes them strong candidates. Some of the other [O iii]-bright objects could also be normal interstellar medium (ISM) dominated SNRs with shocks fast enough to doubly ionize oxygen, but with Hα and [S ii] emission faint enough to have been missed. A few of these objects may also be H ii regions with abnormally high [O iii] emission compared with the majority of M83 H ii regions, compact nebulae excited by young Wolf–Rayet stars, or even background active galactic nuclei. The SNR Hα luminosity function in M83 is shifted by a factor of ∼4.5 times higher than for M33 SNRs, indicative of a higher mean ISM density in M83. We describe the search technique used to identify the SNR candidates and provide basic information and finder charts for the objects.
On a novel approach using massive clusters at high redshifts as cosmological probe

In this work we propose a novel method for testing the validity of the fiducial Λ cold dark matter (ΛCDM) cosmology by measuring the cumulative distribution function of the most massive haloes in a sample of subvolumes of identical size tiled on the sky at a fixed redshift. The fact that the most massive clusters probe the high-mass tail of the mass function, where the difference between ΛCDM and alternative cosmological models is strongest, makes our method particularly interesting as a cosmological probe. We utilize general extreme value (GEV) statistics to obtain a cumulative distribution function of the most massive objects in a given volume. We sample this distribution function according to the number of patches covered by the survey area for a range of different ‘test cosmologies’ and for differently accurate mass estimations of the haloes. By fitting this sample with the GEV distribution function, we can study which parameters are the most sensitive with respect to the test cosmologies. We find that the peak of the probability distribution function of the most massive halo is well suited to test the validity of the fiducial ΛCDM model, once we are able to establish a sufficiently complete large-area survey with Mlim≃ 1014.5 M⊙ h−1 (Mlim≃ 1014 M⊙ h−1) at redshifts above z= 1 (z= 1.5). Being of cumulative nature the proposed measure is robust and an accuracy of 20–30 per cent in the cluster masses would be sufficient to test for alternative models. Since one only needs the most massive system in each angular patch, this method would be ideally suited as a first fast consistency check before going into a more complex statistical analysis of the observed halo sample.
DISCOVERY OF A HIGHLY UNEQUAL-MASS BINARY T DWARF WITH KECK LASER GUIDE STAR ADAPTIVE OPTICS: A COEVALITY TEST OF SUBSTELLAR THEORETICAL MODELS AND EFFECTIVE TEMPERATURES

Highly unequal-mass ratio binaries are rare among field brown dwarfs, with the mass ratio distribution of the known census described by q(4.9±0.7). However, such systems enable a unique test of the joint accuracy of evolutionary and atmospheric models, under the constraint of coevality for the individual components (the “isochrone test”). We carry out this test using two of the most extreme field substellar binaries currently known, the T1 + T6 ϵ Ind Bab binary and a newly discovered 0. ″14 T2.0 + T7.5 binary, 2MASS J12095613−1004008AB, identified with Keck laser guide star adaptive optics. The latter is the most extreme tight binary resolved to date (q ≈ 0.5). Based on the locations of the binary components on the Hertzsprung–Russell (H-R) diagram, current models successfully indicate that these two systems are coeval, with internal age differences of log(age) = −0.8 ± 1.3(−1.0+1.2−1.3) dex and 0.5+0.4−0.3(0.3+0.3−0.4) dex for 2MASS J1209−1004AB and ϵ Ind Bab, respectively, as inferred from the Lyon (Tucson) models. However, the total mass of ϵ Ind Bab derived from the H-R diagram (≈ 80 MJup using the Lyon models) is strongly discrepant with the reported dynamical mass. This problem, which is independent of the assumed age of the ϵ Ind Bab system, can be explained by a ≈ 50–100 K systematic error in the model atmosphere fitting, indicating slightly warmer temperatures for both components; bringing the mass determinations from the H-R diagram and the visual orbit into consistency leads to an inferred age of ≈ 6 Gyr for ϵ Ind Bab, older than previously assumed. Overall, the two T dwarf binaries studied here, along with recent results from T dwarfs in age and mass benchmark systems, yield evidence for small (≈100 K) errors in the evolutionary models and/or model atmospheres, but not significantly larger. Future parallax, resolved spectroscopy, and dynamical mass measurements for 2MASS J1209−1004AB will enable a more stringent application of the isochrone test. Finally, the binary nature of this object reduces its utility as the primary T3 near-IR spectral typing standard; we suggest SDSS J1206+2813 as a replacement.
Robustness Analysis of the Regional and Interregional Components of the Weighted World Air Transportation Network

The robustness of a system indicates its ability to withstand disturbances while maintaining its properties, performance, and efficiency. There are plenty of studies on the robustness of air transport networks in the literature. However, few works consider its mesoscopic organization. Building on the recently introduced component structure, we explore the impact of targeted attacks on the weighted world air transportation network on its components. Indeed, it contains five local components covering different regions (North America-Caribbean, Europe-Russia, East and Southeast Asia-Oceania, Africa-Middle East-Southern Asia, and South America) and one global component linking these regions. We investigate targeted attacks based on influential weighted centrality measures (strength, betweenness, and PageRank). Results show that the local components gradually separate from the world air transportation network as the fraction of removed airports grows. The weighted betweenness attack removes fewer top airports to isolate the regions compared to its alternatives. Furthermore, it is still convenient to travel locally in the separate areas. In contrast, strength and PageRank attacks need to target more airports to split the network. However, they are more disruptive. Indeed, the size of the isolated local components reduces drastically, so it becomes more challenging to travel locally. Looking at the world air transportation network through its component structure reveals a new viewpoint on its resilence. It opens new perspectives to design more efficient attacks.
Orthogonal bipolar spherical harmonics measures: Scrutinizing sources of isotropy violation

The two-point correlation function of the cosmic microwave background temperature anisotropies is generally assumed to be statistically isotropic (SI). Deviations from this assumption could be traced to physical or observational artifacts and systematic effects. Measurement of nonvanishing power in the bipolar spherical harmonic spectra is a standard statistical technique to search for isotropy violations. Although this is a neat tool allowing a blind search for SI violations in the cosmic microwave background sky, it is not easy to discern the cause of isotropy violation by using this measure. In this article, we propose a novel technique of constructing orthogonal bipolar spherical harmonic estimators, which can be used to discern between models of isotropy violation.
Galactic star formation enhanced and quenched by ram pressure in groups and clusters

We investigate how ram pressure of intragroup and intracluster medium can influence the spatial and temporal variations of star formation (SF) of disk galaxies with halo masses (M_h) ranging from 10^10 M_sun to 10^12 M_sun (i.e., from dwarf irregular to Milky Way-type) in groups and clusters with 10^13 < M_h/M_sun < 10^15 by using numerical simulations with a new model for time-varying ram pressure. The long-term evolution of SF rates and H_alpha morphologies corresponding to the distributions of star-forming regions are particularly investigated for different model parameters. The principal results are as follows. Whether ram pressure can enhance or reduce SF depends on M_h of disk galaxies and inclination angles of gas disks with respect to their orbital directions for a given orbit and a given environment. For example, SF can be moderately enhanced in disk galaxies with M_h=10^12 M_sun at the pericenter passages in a cluster with M_h=10^14 M_sun whereas it can be completely shut down (`quenching') for low-mass disks with M_h=10^10 M_sun. Ram pressure can reduce the H_alpha-to-optical-disk-size ratios of disks and the revel of the reduction depends on M_h and orbits of disk galaxies for a given environment. Disk galaxies under strong ram pressure show characteristic H_alpha morphologies such as ring-like, one-sided, and crescent-like distributions.
THE ORIGIN OF THE VIRGO STELLAR SUBSTRUCTURE

We present three-dimensional space velocities of stars selected to be consistent with membership in the Virgo stellar substructure. Candidates were selected from SA 103, a single 40′ × 40′ field from our proper-motion (PM) survey in Kapteyn's Selected Areas (SAs), based on the PMs, Sloan Digital Sky Survey (SDSS) photometry, and follow-up spectroscopy of 215 stars. The signature of the Virgo substructure is clear in the SDSS color–magnitude diagram (CMD) centered on SA 103, and 16 stars are identified that have high Galactocentric-frame radial velocities (VGSR > 50 km s−1) and lie near the CMD locus of Virgo. The implied distance to the Virgo substructure from the candidates is 14 ± 3 kpc. We derive mean kinematics from these 16 stars, finding a radial velocity VGSR = 153 ± 22 km s−1 and proper motions (μαcos δ, μδ) = (− 5.24, −0.91) ± (0.43, 0.46) mas yr−1. From the mean kinematics of these members, we determine that the Virgo progenitor was on an eccentric (e ∼ 0.8) orbit that recently passed near the Galactic center (pericentric distance Rp ∼ 6 kpc). This destructive orbit is consistent with the idea that the substructure(s) in Virgo originated in the tidal disruption of a Milky Way satellite. N-body simulations suggest that the entire cloud-like Virgo substructure (encompassing the “Virgo Overdensity” and the “Virgo Stellar Stream”) is likely the tidal debris remnant from a recently disrupted massive (∼109 M☉) dwarf galaxy. The model also suggests that some other known stellar overdensities in the Milky Way halo (e.g., the Pisces Overdensity and debris near NGC 2419 and SEGUE 1) are explained by the disruption of the Virgo progenitor.
THE METAL-ENRICHED THERMAL COMPOSITE SUPERNOVA REMNANT KESTEVEN 41 (G337.8–0.1) IN A MOLECULAR ENVIRONMENT

The physical nature of thermal composite supernova remnants (SNRs) remains controversial. We have revisited the archival XMM-Newton and Chandra data of the thermal composite SNR Kesteven 41 (Kes 41 or G337.8−0.1) and performed a millimeter observation toward this source in the 12CO, 13CO, and C18O lines. The X-ray emission, mainly concentrated toward the southwestern part of the SNR, is characterized by distinct S and Ar He-like lines in the spectra. The X-ray spectra can be fitted with an absorbed nonequilibrium ionization collisional plasma model at a temperature of 1.3–2.6 keV and an ionization timescale of 0.1–1.2 × 1012 cm−3 s. The metal species S and Ar are overabundant, with 1.2–2.7 and 1.3–3.8 solar abundances, respectively, which strongly indicate the presence of a substantial ejecta component in the X-ray-emitting plasma of this SNR. Kes 41 is found to be associated with a giant molecular cloud (MC) at a systemic local standard of rest velocity of −50 km s−1 and confined in a cavity delineated by a northern molecular shell, a western concave MC that features a discernible shell, and an H i cloud seen toward the southeast of the SNR. The birth of the SNR in a preexisting molecular cavity implies a mass of ≳ 18 M☉ for the progenitor if it was not in a binary system. Thermal conduction and cloudlet evaporation seem to be feasible mechanisms to interpret the X-ray thermal composite morphology, and the scenario of gas reheating by the shock reflected from the cavity wall is quantitatively consistent with the observations. An updated list of thermal composite SNRs is also presented in this paper.
Resolved maps of stellar mass and SED of galaxies from optical/NIR imaging and SPS models

Abstract We report on the method developed by Zibetti, Charlot & Rix (2009) to construct resolved stellar mass maps of galaxies from optical and NIR imaging. Accurate pixel-by-pixel colour information (specifically g – i and i – H) is converted into stellar mass-to-light ratios with typical accuracy of 30%, based on median likelihoods derived from a Monte Carlo library of 50,000 stellar population synthesis models that include dust and updated TP-AGB phase prescriptions. Hence, surface mass densities are computed. In a pilot study, we analyze 9 galaxies spanning a broad range of morphologies. Among the main results, we find that: i) galaxies appear much smoother in stellar mass maps than at any optical or NIR wavelength; ii) total stellar mass estimates based on unresolved photometry are biased low with respect to the integral of resolved stellar mass maps, by up to 40%, due to dust obscured regions being under-represented in global colours; iii) within a galaxy, on local scales colours correlate with surface stellar mass density; iv) the slope and tightness of this correlation reflect/depend on the morphology of the galaxy.
Scalar potentials, propagators and global symmetries in AdS/CFT

We study the transition of a scalar field in a fixed AdSd+1 background between an extremum and a minimum of a potential. We first prove that two conditions must be met for the solution to exist. First, the potential involved cannot be generic, i.e. a fine-tuning of their parameters is mandatory. Second, at least in some region its second derivative must have a negative upper limit which depends only on the dimensionality d. We then calculate the boundary propagator for small momenta in two different ways: first in a WKB approximation, and second with the usual matching method, generalizing the known calculation to arbitrary order. Finally, we study a system with spontaneously broken non-Abelian global symmetry, and show in the holographic language why the Goldstone modes appear.
The Fermilab Main Injector: high intensity operation and beam loss control

From 2005 through 2012, the Fermilab Main Injector provided intense beams of 120 GeV protons to produce neutrino beams and antiprotons. Hardware improvements in conjunction with improved diagnostics allowed the system to reach sustained operation at ~400 kW beam power. Transmission was very high except for beam lost at or near the 8 GeV injection energy where 95% beam transmission results in about 1.5 kW of beam loss. By minimizing and localizing loss, residual radiation levels fell while beam power was doubled. Lost beam was directed to either the collimation system or to the beam abort. Critical apertures were increased while improved instrumentation allowed optimal use of available apertures. We will summarize the improvements required to achieve high intensity, the impact of various loss control tools and the status and trends in residual radiation in the Main Injector.
Synthesis of control laws for magnetic levitation systems based on serial invariant manifolds

In this paper, a nonlinear controller is designed for a magnetic levitation system (MLS) based on serial invariant manifolds. Synthesized controller based on method of synergetic control theory (SCT) through invariant manifolds, asymptotically stable. In this method, the control law is synthesized to ensure the motion of the closed-loop control object from an arbitrary initial state into the vicinity of the desired invariant manifold. Thereby, the control system not only ensures the necessary control quality, but also ensures the asymptotic stability of the entire system. The quality and efficiency of the control law is proven through simulation results and comparison with the sliding mode controller (SMC).
Robustness of the Blandford–Znajek mechanism

The Blandford–Znajek (BZ) mechanism has long been regarded as a key ingredient in models attempting to explain powerful jets in AGNs, quasars, blazzars, etc. In such a mechanism, energy is extracted from a rotating black hole and dissipated at a load at far distances. In this work we examine the behavior of the BZ mechanism with respect to different boundary conditions, revealing the robustness of the mechanism upon variation of these conditions. Consequently, this work closes a gap in our understanding of this important scenario.
Learning Deformable Kernels for Image and Video Denoising

Most of the classical denoising methods restore clear results by selecting and averaging pixels in the noisy input. Instead of relying on hand-crafted selecting and averaging strategies, we propose to explicitly learn this process with deep neural networks. Specifically, we propose deformable 2D kernels for image denoising where the sampling locations and kernel weights are both learned. The proposed kernel naturally adapts to image structures and could effectively reduce the oversmoothing artifacts. Furthermore, we develop 3D deformable kernels for video denoising to more efficiently sample pixels across the spatial-temporal space. Our method is able to solve the misalignment issues of large motion from dynamic scenes. For better training our video denoising model, we introduce the trilinear sampler and a new regularization term. We demonstrate that the proposed method performs favorably against the state-of-the-art image and video denoising approaches on both synthetic and real-world data.
E-nose: A low-cost fruit ripeness monitoring system

All fruits emit some specific volatile organic compounds (VOCs) during their life cycle. These VOCs have specific characteristics, by using these characteristics fruit ripening stage can be identified without destructing the fruit. In this study, an application-specific electronic nose device was designed for monitoring fruit ripeness.The proposed electronic nose is cost-efficient and does not require any modern or costly laboratory instruments. Metal oxide semiconductor (MOS) sensors were used for designing the proposed electronic nose. These MOS sensors were integrated with a microcontroller board to detect and extract the meaningful features of VOCs, and an artificial neural network (ANN) algorithm was used for pattern recognition. Measurements were done with apples, bananas, oranges, grapes, and pomegranates. The designed electronic nose proved to be reliable in classifying fruit samples into three different fruit ripening stage (unripe, ripe, and over-ripe) with high precision and recall. The proposed electronic nose performed uniformly on all three fruit ripening stages with an average accuracy of ≥ 95%.
The Accuracy of MRI in the Local Staging of Endometrial Cancer: An Experience From a Tertiary Care Oncology Institute in Pakistan

Objective Our objective is to assess the diagnostic accuracy of contrast-enhanced magnetic resonance imaging (MRI) in identifying the depth of myometrial invasion and cervical stromal involvement in endometrial carcinoma (EC) along with nodal status and its correlation with surgical and histopathological (HP) findings. Materials and methods We performed a retrospective study on female patients at Shaukat Khanum Memorial Cancer Hospital and Research Centre, Lahore, Pakistan. Patients with endometrial carcinoma (CA) were searched from the electronic record system, and a total of 188 patients fulfilling the study criteria were selected. All the patients were evaluated using a 1.5T MRI and underwent a hysterectomy. The outcome of preoperative MRI was correlated with histopathology results, keeping pathology as the gold standard. Results A total of 188 patients were included in the study, with a mean age of 56.67 ± 12.47 years. Of the patients, 72 (38.3%) were diagnosed with stage 1a. The second common stage was 1b, seen in 43 (22.9%) patients. It was found that the staging of endometrial CA on MRI and HP were significantly correlated for myometrial invasion (stage 1a and 1b), cervical stromal involvement (stage 2b), serosal and adnexal (stage 3a), vaginal (stage 3b), and nodal (stage 3c) involvement as shown by their p-values of <0.01. However, in cases of parametrial invasion (stage 3b), bladder involvement, and rectal involvement (stage 4), MRI showed decreased sensitivity as shown by their p-values of 0.833, 0.87, and 0.9, respectively. Conclusion Preoperative MRI can predict local disease and low-risk patients accurately, thereby helping in proper surgical planning and avoiding more extensive surgery such as lymphadenectomy in these patients.
Phenomenologically varying Λ and a toy model for the universe

We consider a model of the Universe with variable G and Λ. The subject of interest is a phenomenological model for Λ proposed and considered in this article for the first time (to our knowledge), with the assumption that ghost dark energy exists and interacts with the Universe through Λ. We consider the possibility that there exist unusual connections between different components of the fluids in Universe. We would like to stress that this is simply an assumption and could be very far from reality. This model is interesting phenomenologically and mathematically but we will not discuss physical conditions or possibilities of implementing the modifications. To test our assumption and to observe the behavior of the Universe, we will consider toy models filled by a barotropic fluid and modified Chaplyagin gas. Finally, we will consider interaction between barotropic fluid or Chaplygin gas and ghost dark energy as a separate scenario. The statefinder diagnostic provided stability analysis of the models. All fr.